Keyword: astrophysics - astrophysics of galaxies
2022 (3)
A machine learning approach to mapping baryons on to dark matter haloes using the EAGLE and C-EAGLE simulations. Lovell, C. C., Wilkins, S. M., Thomas, P. A., Schaller, M., Baugh, C. M., Fabbian, G., & Bahé, Y. Monthly Notices of the Royal Astronomical Society, 509:5046–5061, February, 2022. ADS Bibcode: 2022MNRAS.509.5046L
![A machine learning approach to mapping baryons on to dark matter haloes using the EAGLE and C-EAGLE simulations [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper doi abstract bibtex 1 download
Paper doi abstract bibtex 1 download High-resolution cosmological hydrodynamic simulations are currently limited to relatively small volumes due to their computational expense. However, much larger volumes are required to probe rare, overdense environments, and measure clustering statistics of the large-scale structure. Typically, zoom simulations of individual regions are used to study rare environments, and semi-analytic models and halo occupation models applied to dark-matter-only (DMO) simulations are used to study the Universe in the large-volume regime. We propose a new approach, using a machine learning framework, to explore the halo-galaxy relationship in the periodic EAGLE simulations, and zoom C-EAGLE simulations of galaxy clusters. We train a tree-based machine learning method to predict the baryonic properties of galaxies based on their host dark matter halo properties. The trained model successfully reproduces a number of key distribution functions for an infinitesimal fraction of the computational cost of a full hydrodynamic simulation. By training on both periodic simulations and zooms of overdense environments, we learn the bias of galaxy evolution in differing environments. This allows us to apply the trained model to a larger DMO volume than would be possible if we only trained on a periodic simulation. We demonstrate this application using the (800 Mpc)3 P-Millennium simulation, and present predictions for key baryonic distribution functions and clustering statistics from the EAGLE model in this large volume.
@article{lovell_machine_2022,
title = {A machine learning approach to mapping baryons on to dark matter haloes using the {EAGLE} and {C}-{EAGLE} simulations},
volume = {509},
issn = {0035-8711},
url = {https://ui.adsabs.harvard.edu/abs/2022MNRAS.509.5046L},
doi = {10.1093/mnras/stab3221},
abstract = {High-resolution cosmological hydrodynamic simulations are currently limited to relatively small volumes due to their computational expense. However, much larger volumes are required to probe rare, overdense environments, and measure clustering statistics of the large-scale structure. Typically, zoom simulations of individual regions are used to study rare environments, and semi-analytic models and halo occupation models applied to dark-matter-only (DMO) simulations are used to study the Universe in the large-volume regime. We propose a new approach, using a machine learning framework, to explore the halo-galaxy relationship in the periodic EAGLE simulations, and zoom C-EAGLE simulations of galaxy clusters. We train a tree-based machine learning method to predict the baryonic properties of galaxies based on their host dark matter halo properties. The trained model successfully reproduces a number of key distribution functions for an infinitesimal fraction of the computational cost of a full hydrodynamic simulation. By training on both periodic simulations and zooms of overdense environments, we learn the bias of galaxy evolution in differing environments. This allows us to apply the trained model to a larger DMO volume than would be possible if we only trained on a periodic simulation. We demonstrate this application using the (800 Mpc)3 P-Millennium simulation, and present predictions for key baryonic distribution functions and clustering statistics from the EAGLE model in this large volume.},
urldate = {2022-01-11},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Lovell, Christopher C. and Wilkins, Stephen M. and Thomas, Peter A. and Schaller, Matthieu and Baugh, Carlton M. and Fabbian, Giulio and Bahé, Yannick},
month = feb,
year = {2022},
note = {ADS Bibcode: 2022MNRAS.509.5046L},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics, galaxies: abundances, galaxies: luminosity function, mass function, software: simulations},
pages = {5046--5061},
}Are the Newly-Discovered \$z {\textbackslash}sim 13\$ Drop-out Sources Starburst Galaxies or Quasars?. Pacucci, F., Dayal, P., Harikane, Y., Inoue, A. K., & Loeb, A. arXiv:2201.00823 [astro-ph], January, 2022. arXiv: 2201.00823
Paper abstract bibtex
Paper abstract bibtex The detection of two \$z {\textbackslash}sim 13\$ galaxy candidates (Harikane et al. 2021b) has opened a new window on galaxy formation at an era only \$330\$ Myr after the Big Bang. Here, we investigate the physical nature of these sources: are we witnessing star forming galaxies or quasars at such early epochs? If powered by star formation, the observed ultraviolet (UV) luminosities and number densities can be jointly explained if: (i) these galaxies are extreme star-formers with star formation rates \$5-25{\textbackslash}times\$ higher than those expected from extrapolations of average lower-redshift relations; (ii) the star formation efficiency increases with halo mass and is countered by increasing dust attenuation from \$z {\textbackslash}sim 10-5\$; (iii) they form stars with an extremely top-heavy initial mass function. The quasar hypothesis is also plausible, with the UV luminosity produced by black holes of \${\textbackslash}sim 10{\textasciicircum}8 {\textbackslash}, {\textbackslash}mathrm\{M_\{{\textbackslash}odot\}\}\$ accreting at or slightly above the Eddington rate (\$f_\{{\textbackslash}rm Edd\}{\textbackslash}sim 1.0\$). This black hole mass at \$z {\textbackslash}sim 13\$ would require challenging, but not implausible, growth parameters, in line with what required for \$z{\textbackslash}sim 7.5\$ quasars detected thus far. If spectroscopically confirmed, these two sources will represent a remarkable laboratory to study the Universe at previously inaccessible redshifts.
@article{pacucci_are_2022,
title = {Are the {Newly}-{Discovered} \$z {\textbackslash}sim 13\$ {Drop}-out {Sources} {Starburst} {Galaxies} or {Quasars}?},
url = {http://arxiv.org/abs/2201.00823},
abstract = {The detection of two \$z {\textbackslash}sim 13\$ galaxy candidates (Harikane et al. 2021b) has opened a new window on galaxy formation at an era only \$330\$ Myr after the Big Bang. Here, we investigate the physical nature of these sources: are we witnessing star forming galaxies or quasars at such early epochs? If powered by star formation, the observed ultraviolet (UV) luminosities and number densities can be jointly explained if: (i) these galaxies are extreme star-formers with star formation rates \$5-25{\textbackslash}times\$ higher than those expected from extrapolations of average lower-redshift relations; (ii) the star formation efficiency increases with halo mass and is countered by increasing dust attenuation from \$z {\textbackslash}sim 10-5\$; (iii) they form stars with an extremely top-heavy initial mass function. The quasar hypothesis is also plausible, with the UV luminosity produced by black holes of \${\textbackslash}sim 10{\textasciicircum}8 {\textbackslash}, {\textbackslash}mathrm\{M\_\{{\textbackslash}odot\}\}\$ accreting at or slightly above the Eddington rate (\$f\_\{{\textbackslash}rm Edd\}{\textbackslash}sim 1.0\$). This black hole mass at \$z {\textbackslash}sim 13\$ would require challenging, but not implausible, growth parameters, in line with what required for \$z{\textbackslash}sim 7.5\$ quasars detected thus far. If spectroscopically confirmed, these two sources will represent a remarkable laboratory to study the Universe at previously inaccessible redshifts.},
urldate = {2022-01-05},
journal = {arXiv:2201.00823 [astro-ph]},
author = {Pacucci, Fabio and Dayal, Pratika and Harikane, Yuichi and Inoue, Akio K. and Loeb, Abraham},
month = jan,
year = {2022},
note = {arXiv: 2201.00823},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena},
}Deep Learning of DESI Mock Spectra to Find Damped Ly\\textbackslashalpha\ Systems. Wang, B., Zou, J., Cai, Z., Prochaska, J. X., Sun, Z., Ding, J., Font-Ribera, A., Gonzalez, A., Herrera-Alcantar, H. K., Irsic, V., Lin, X., Brooks, D., Chabanier, S., de Belsunce, R., Palanque-Delabrouille, N., Tarle, G., & Zhou, Z. arXiv:2201.00827 [astro-ph], January, 2022. arXiv: 2201.00827
Paper abstract bibtex
Paper abstract bibtex We have updated and applied a convolutional neural network (CNN) machine learning model to discover and characterize damped Ly\${\textbackslash}alpha\$ systems (DLAs) based on Dark Energy Spectroscopic Instrument (DESI) mock spectra. We have optimized the training process and constructed a CNN model that yields a DLA classification accuracy above 99\${\textbackslash}%\$ for spectra which have signal-to-noise (S/N) above 5 per pixel. Classification accuracy is the rate of correct classifications. This accuracy remains above 97\${\textbackslash}%\$ for lower signal-to-noise (S/N) \${\textbackslash}approx1\$ spectra. This CNN model provides estimations for redshift and HI column density with standard deviations of 0.002 and 0.17 dex for spectra with S/N above 3 per pixel. Also, this DLA finder is able to identify overlapping DLAs and sub-DLAs. Further, the impact of different DLA catalogs on the measurement of Baryon Acoustic Oscillation (BAO) is investigated. The cosmological fitting parameter result for BAO has less than \$0.61{\textbackslash}%\$ difference compared to analysis of the mock results with perfect knowledge of DLAs. This difference is lower than the statistical error for the first year estimated from the mock spectra: above \$1.7{\textbackslash}%\$. We also compared the performance of CNN and Gaussian Process (GP) model. Our improved CNN model has moderately 14\${\textbackslash}%\$ higher purity and 7\${\textbackslash}%\$ higher completeness than an older version of GP code, for S/N \${\textgreater}\$ 3. Both codes provide good DLA redshift estimates, but the GP produces a better column density estimate by \$24{\textbackslash}%\$ less standard deviation. A credible DLA catalog for DESI main survey can be provided by combining these two algorithms.
@article{wang_deep_2022,
title = {Deep {Learning} of {DESI} {Mock} {Spectra} to {Find} {Damped} {Ly}\{{\textbackslash}alpha\} {Systems}},
url = {http://arxiv.org/abs/2201.00827},
abstract = {We have updated and applied a convolutional neural network (CNN) machine learning model to discover and characterize damped Ly\${\textbackslash}alpha\$ systems (DLAs) based on Dark Energy Spectroscopic Instrument (DESI) mock spectra. We have optimized the training process and constructed a CNN model that yields a DLA classification accuracy above 99\${\textbackslash}\%\$ for spectra which have signal-to-noise (S/N) above 5 per pixel. Classification accuracy is the rate of correct classifications. This accuracy remains above 97\${\textbackslash}\%\$ for lower signal-to-noise (S/N) \${\textbackslash}approx1\$ spectra. This CNN model provides estimations for redshift and HI column density with standard deviations of 0.002 and 0.17 dex for spectra with S/N above 3 per pixel. Also, this DLA finder is able to identify overlapping DLAs and sub-DLAs. Further, the impact of different DLA catalogs on the measurement of Baryon Acoustic Oscillation (BAO) is investigated. The cosmological fitting parameter result for BAO has less than \$0.61{\textbackslash}\%\$ difference compared to analysis of the mock results with perfect knowledge of DLAs. This difference is lower than the statistical error for the first year estimated from the mock spectra: above \$1.7{\textbackslash}\%\$. We also compared the performance of CNN and Gaussian Process (GP) model. Our improved CNN model has moderately 14\${\textbackslash}\%\$ higher purity and 7\${\textbackslash}\%\$ higher completeness than an older version of GP code, for S/N \${\textgreater}\$ 3. Both codes provide good DLA redshift estimates, but the GP produces a better column density estimate by \$24{\textbackslash}\%\$ less standard deviation. A credible DLA catalog for DESI main survey can be provided by combining these two algorithms.},
urldate = {2022-01-05},
journal = {arXiv:2201.00827 [astro-ph]},
author = {Wang, Ben and Zou, Jiaqi and Cai, Zheng and Prochaska, J. Xavier and Sun, Zechang and Ding, Jiani and Font-Ribera, Andreu and Gonzalez, Alma and Herrera-Alcantar, Hiram K. and Irsic, Vid and Lin, Xiaojing and Brooks, David and Chabanier, Solène and de Belsunce, Roger and Palanque-Delabrouille, Nathalie and Tarle, Gregory and Zhou, Zhimin},
month = jan,
year = {2022},
note = {arXiv: 2201.00827},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
}2021 (48)
Massive black hole binary inspiral and spin evolution in a cosmological framework. Sayeb, M., Blecha, L., Kelley, L. Z., Gerosa, D., Kesden, M., & Thomas, J. Monthly Notices of the Royal Astronomical Society, 501(2):2531-2546, February, 2021.
doi bibtex
doi bibtex
@article{2021MNRAS.501.2531S,
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
adsurl = {https://ui.adsabs.harvard.edu/abs/2021MNRAS.501.2531S},
archiveprefix = {arXiv},
author = {{Sayeb}, Mohammad and {Blecha}, Laura and {Kelley}, Luke Zoltan and {Gerosa}, Davide and {Kesden}, Michael and {Thomas}, July},
doi = {10.1093/mnras/staa3826},
eprint = {2006.06647},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {gravitational waves, Astrophysics - Astrophysics of Galaxies, General Relativity and Quantum Cosmology},
month = feb,
number = {2},
pages = {2531-2546},
primaryclass = {astro-ph.GA},
title = {{Massive black hole binary inspiral and spin evolution in a cosmological framework}},
volume = {501},
year = 2021,
bdsk-url-1 = {https://doi.org/10.1093/mnras/staa3826}}Deciphering Star Cluster Evolution by Shape Morphology. Hu, Q., Zhang, Y., Esamdin, A., Liu, J., & Zeng, X. arXiv:2103.02912 [astro-ph], March, 2021. arXiv: 2103.02912
Paper abstract bibtex
Paper abstract bibtex We analyze the morphological evolution of open clusters and provide shape parameters for 265 open clusters. The results show that the overall shape of sample clusters becomes more elliptical as they grow older, while their core remains circular or slightly trend to circularize. There is a negative correlation of the ellipticities with the number of members of the sample clusters. A significant negative correlation between the overall ellipticities and masses is also detected for the sample clusters with log(age/year) ${\}geq$ 8, suggesting that the overall shapes of the clusters are possibly influenced by the number of members and masses, in addition to the external forces and the surrounding environment. For most young sample clusters, the radial stratification degree of the short axis direction is greater than that of the long, implying that the radial stratification degree in the two directions within the young sample cluster may be unevenly affected by an internal evolutionary process. Older sample clusters exhibit lower stratification in the tangential direction, which possibly means those clusters may continue to survive for a long time at a low level of stratification. Our analysis shows that the overall shape of the sample clusters may be more susceptible to the influence of Galactic tides toward the Galactic center than the shear forces embedded in Galactic differential rotation. By analyzing the distribution of the ages and number of members of star clusters, we suggest that NGC 6791 may originate from superclusters.
@article{hu_deciphering_2021,
title = {Deciphering {Star} {Cluster} {Evolution} by {Shape} {Morphology}},
url = {http://arxiv.org/abs/2103.02912},
abstract = {We analyze the morphological evolution of open clusters and provide shape parameters for 265 open clusters. The results show that the overall shape of sample clusters becomes more elliptical as they grow older, while their core remains circular or slightly trend to circularize. There is a negative correlation of the ellipticities with the number of members of the sample clusters. A significant negative correlation between the overall ellipticities and masses is also detected for the sample clusters with log(age/year) \${\textbackslash}geq\$ 8, suggesting that the overall shapes of the clusters are possibly influenced by the number of members and masses, in addition to the external forces and the surrounding environment. For most young sample clusters, the radial stratification degree of the short axis direction is greater than that of the long, implying that the radial stratification degree in the two directions within the young sample cluster may be unevenly affected by an internal evolutionary process. Older sample clusters exhibit lower stratification in the tangential direction, which possibly means those clusters may continue to survive for a long time at a low level of stratification. Our analysis shows that the overall shape of the sample clusters may be more susceptible to the influence of Galactic tides toward the Galactic center than the shear forces embedded in Galactic differential rotation. By analyzing the distribution of the ages and number of members of star clusters, we suggest that NGC 6791 may originate from superclusters.},
urldate = {2021-03-09},
journal = {arXiv:2103.02912 [astro-ph]},
author = {Hu, Qingshun and Zhang, Yu and Esamdin, Ali and Liu, Jinzhong and Zeng, Xiangyun},
month = mar,
year = {2021},
note = {arXiv: 2103.02912},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics},
}The case for thermalization as a contributor to the [C II] deficit. Sutter, J., Dale, D. A., Sandstrom, K., Smith, J., Bolatto, A., Boquien, M., Calzetti, D., Croxall, K. V., De Looze, I., Galametz, M., Groves, B. A., Helou, G., Herrera-Camus, R., Hunt, L. K., Kennicutt, R. C., Pelligrini, E. W., Wilson, C., & Wolfire, M. G. \mnras, 503(1):911-919, May, 2021.
doi bibtex
doi bibtex
@ARTICLE{2021MNRAS.503..911S,
author = {{Sutter}, Jessica and {Dale}, Daniel A. and {Sandstrom}, Karin and {Smith}, J.~D.~T. and {Bolatto}, Alberto and {Boquien}, Mederic and {Calzetti}, Daniela and {Croxall}, Kevin V. and {De Looze}, Ilse and {Galametz}, Maud and {Groves}, Brent A. and {Helou}, George and {Herrera-Camus}, Rodrigo and {Hunt}, Leslie K. and {Kennicutt}, Robert C. and {Pelligrini}, Eric W. and {Wilson}, Christine and {Wolfire}, Mark G.},
title = "{The case for thermalization as a contributor to the [C II] deficit}",
journal = {\mnras},
keywords = {(ISM:) H ii Regions, (ISM:) photodissociation regions, galaxies: ISM, Astrophysics - Astrophysics of Galaxies},
year = 2021,
month = may,
volume = {503},
number = {1},
pages = {911-919},
doi = {10.1093/mnras/stab490},
archivePrefix = {arXiv},
eprint = {2102.08865},
primaryClass = {astro-ph.GA},
adsurl = {https://ui.adsabs.harvard.edu/abs/2021MNRAS.503..911S},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}Hierarchical mergers of stellar-mass black holes and their gravitational-wave signatures. Gerosa, D. & Fishbach, M. Nature Astronomy, 5:749-760, July, 2021.
doi bibtex 1 download
doi bibtex 1 download
@article{2021NatAs...5..749G,
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
adsurl = {https://ui.adsabs.harvard.edu/abs/2021NatAs...5..749G},
archiveprefix = {arXiv},
author = {{Gerosa}, Davide and {Fishbach}, Maya},
doi = {10.1038/s41550-021-01398-w},
eprint = {2105.03439},
journal = {Nature Astronomy},
keywords = {Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics, General Relativity and Quantum Cosmology},
month = jul,
pages = {749-760},
primaryclass = {astro-ph.HE},
title = {{Hierarchical mergers of stellar-mass black holes and their gravitational-wave signatures}},
volume = {5},
year = 2021,
bdsk-url-1 = {https://doi.org/10.1038/s41550-021-01398-w}}The Global Magneto-ionic Medium Survey: A Faraday Depth Survey of the Northern Sky Covering 1280-1750 MHz. Wolleben, M., Landecker, T., Douglas, K., Gray, A., Ordog, A., Dickey, J., Hill, A., Carretti, E., Brown, J., Gaensler, B., Han, J., Haverkorn, M., Kothes, R., Leahy, J., McClure-Griffiths, N., McConnell, D., Reich, W., Taylor, A., Thomson, A., & West, J. \aj, 162(1):35, July, 2021.
doi bibtex
doi bibtex
@ARTICLE{2021AJ....162...35W,
author = {{Wolleben}, M. and {Landecker}, T.~L. and {Douglas}, K.~A. and {Gray}, A.~D. and {Ordog}, A. and {Dickey}, J.~M. and {Hill}, A.~S. and {Carretti}, E. and {Brown}, J.~C. and {Gaensler}, B.~M. and {Han}, J.~L. and {Haverkorn}, M. and {Kothes}, R. and {Leahy}, J.~P. and {McClure-Griffiths}, N. and {McConnell}, D. and {Reich}, W. and {Taylor}, A.~R. and {Thomson}, A.~J.~M. and {West}, J.~L.},
title = "{The Global Magneto-ionic Medium Survey: A Faraday Depth Survey of the Northern Sky Covering 1280-1750 MHz}",
journal = {\aj},
keywords = {Polarimetry, Polarimeters, Spectropolarimetry, Radio telescopes, Calibration, Interstellar magnetic fields, Milky Way magnetic fields, 1278, 1277, 1973, 1360, 2179, 845, 1057, Astrophysics - Astrophysics of Galaxies},
year = 2021,
month = jul,
volume = {162},
number = {1},
eid = {35},
pages = {35},
doi = {10.3847/1538-3881/abf7c1},
archivePrefix = {arXiv},
eprint = {2106.00945},
primaryClass = {astro-ph.GA},
adsurl = {https://ui.adsabs.harvard.edu/abs/2021AJ....162...35W},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}The Global Magneto-Ionic Medium Survey (GMIMS): the brightest polarized region in the southern sky at 75 cm and its implications for Radio Loop II. Thomson, A. J., Landecker, T., McClure-Griffiths, N., Dickey, J. M., Campbell, J., Carretti, E., Clark, S., Federrath, C., Gaensler, B., Han, J., Haverkorn, M., Hill, A. S., Mao, S., Ordog, A., Pratley, L., Reich, W., Van Eck, C. L., West, J., & Wolleben, M. \mnras, 507(3):3495-3518, November, 2021.
doi bibtex
doi bibtex
@ARTICLE{2021MNRAS.507.3495T,
author = {{Thomson}, Alec J.~M. and {Landecker}, T.~L. and {McClure-Griffiths}, N.~M. and {Dickey}, John M. and {Campbell}, J.~L. and {Carretti}, Ettore and {Clark}, S.~E. and {Federrath}, Christoph and {Gaensler}, B.~M. and {Han}, J.~L. and {Haverkorn}, Marijke and {Hill}, Alex S. and {Mao}, S.~A. and {Ordog}, Anna and {Pratley}, Luke and {Reich}, Wolfgang and {Van Eck}, Cameron L. and {West}, J.~L. and {Wolleben}, M.},
title = "{The Global Magneto-Ionic Medium Survey (GMIMS): the brightest polarized region in the southern sky at 75 cm and its implications for Radio Loop II}",
journal = {\mnras},
keywords = {polarization, ISM: bubbles, ISM: magnetic fields, radio continuum: ISM, Astrophysics - Astrophysics of Galaxies},
year = 2021,
month = nov,
volume = {507},
number = {3},
pages = {3495-3518},
doi = {10.1093/mnras/stab1805},
archivePrefix = {arXiv},
eprint = {2106.12595},
primaryClass = {astro-ph.GA},
adsurl = {https://ui.adsabs.harvard.edu/abs/2021MNRAS.507.3495T},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}The SPHERE infrared survey for exoplanets (SHINE). III. The demographics of young giant exoplanets below 300 au with SPHERE. Vigan, A., Fontanive, C., Meyer, M., Biller, B., Bonavita, M., Feldt, M., Desidera, S., Marleau, G. -., Emsenhuber, A., Galicher, R., Rice, K., Forgan, D., Mordasini, C., Gratton, R., Le Coroller, H., Maire, A. -., Cantalloube, F., Chauvin, G., Cheetham, A., Hagelberg, J., Lagrange, A. -., Langlois, M., Bonnefoy, M., Beuzit, J. -., Boccaletti, A., D'Orazi, V., Delorme, P., Dominik, C., Henning, T., Janson, M., Lagadec, E., Lazzoni, C., Ligi, R., Menard, F., Mesa, D., Messina, S., Moutou, C., Müller, A., Perrot, C., Samland, M., Schmid, H., Schmidt, T., Sissa, E., Turatto, M., Udry, S., Zurlo, A., Abe, L., Antichi, J., Asensio-Torres, R., Baruffolo, A., Baudoz, P., Baudrand, J., Bazzon, A., Blanchard, P., Bohn, A., Brown Sevilla, S., Carbillet, M., Carle, M., Cascone, E., Charton, J., Claudi, R., Costille, A., De Caprio, V., Delboulbé, A., Dohlen, K., Engler, N., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Girard, J., Giro, E., Gisler, D., Gluck, L., Gry, C., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Le Mignant, D., Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Möller-Nilsson, O., Mouillet, D., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rickman, E., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Wahhaj, Z., Weber, L., & Wildi, F. åp, 651:A72, July, 2021.
doi bibtex
doi bibtex
@ARTICLE{2021A&A...651A..72V,
author = {{Vigan}, A. and {Fontanive}, C. and {Meyer}, M. and {Biller}, B. and {Bonavita}, M. and {Feldt}, M. and {Desidera}, S. and {Marleau}, G. -D. and {Emsenhuber}, A. and {Galicher}, R. and {Rice}, K. and {Forgan}, D. and {Mordasini}, C. and {Gratton}, R. and {Le Coroller}, H. and {Maire}, A. -L. and {Cantalloube}, F. and {Chauvin}, G. and {Cheetham}, A. and {Hagelberg}, J. and {Lagrange}, A. -M. and {Langlois}, M. and {Bonnefoy}, M. and {Beuzit}, J. -L. and {Boccaletti}, A. and {D'Orazi}, V. and {Delorme}, P. and {Dominik}, C. and {Henning}, Th. and {Janson}, M. and {Lagadec}, E. and {Lazzoni}, C. and {Ligi}, R. and {Menard}, F. and {Mesa}, D. and {Messina}, S. and {Moutou}, C. and {M{\"u}ller}, A. and {Perrot}, C. and {Samland}, M. and {Schmid}, H.~M. and {Schmidt}, T. and {Sissa}, E. and {Turatto}, M. and {Udry}, S. and {Zurlo}, A. and {Abe}, L. and {Antichi}, J. and {Asensio-Torres}, R. and {Baruffolo}, A. and {Baudoz}, P. and {Baudrand}, J. and {Bazzon}, A. and {Blanchard}, P. and {Bohn}, A.~J. and {Brown Sevilla}, S. and {Carbillet}, M. and {Carle}, M. and {Cascone}, E. and {Charton}, J. and {Claudi}, R. and {Costille}, A. and {De Caprio}, V. and {Delboulb{\'e}}, A. and {Dohlen}, K. and {Engler}, N. and {Fantinel}, D. and {Feautrier}, P. and {Fusco}, T. and {Gigan}, P. and {Girard}, J.~H. and {Giro}, E. and {Gisler}, D. and {Gluck}, L. and {Gry}, C. and {Hubin}, N. and {Hugot}, E. and {Jaquet}, M. and {Kasper}, M. and {Le Mignant}, D. and {Llored}, M. and {Madec}, F. and {Magnard}, Y. and {Martinez}, P. and {Maurel}, D. and {M{\"o}ller-Nilsson}, O. and {Mouillet}, D. and {Moulin}, T. and {Orign{\'e}}, A. and {Pavlov}, A. and {Perret}, D. and {Petit}, C. and {Pragt}, J. and {Puget}, P. and {Rabou}, P. and {Ramos}, J. and {Rickman}, E.~L. and {Rigal}, F. and {Rochat}, S. and {Roelfsema}, R. and {Rousset}, G. and {Roux}, A. and {Salasnich}, B. and {Sauvage}, J. -F. and {Sevin}, A. and {Soenke}, C. and {Stadler}, E. and {Suarez}, M. and {Wahhaj}, Z. and {Weber}, L. and {Wildi}, F.},
title = "{The SPHERE infrared survey for exoplanets (SHINE). III. The demographics of young giant exoplanets below 300 au with SPHERE}",
journal = {\aap},
keywords = {techniques: high angular resolution, methods: statistical, infrared: planetary systems, planetary systems, planets and satellites: formation, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics},
year = 2021,
month = jul,
volume = {651},
eid = {A72},
pages = {A72},
doi = {10.1051/0004-6361/202038107},
archivePrefix = {arXiv},
eprint = {2007.06573},
primaryClass = {astro-ph.EP},
adsurl = {https://ui.adsabs.harvard.edu/abs/2021A&A...651A..72V},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}Sengi: A small, fast, interactive viewer for spectral outputs from stellar population synthesis models. Lovell, C. C. Astronomy and Computing, 34:100444, January, 2021.
Paper doi abstract bibtex
Paper doi abstract bibtex We present Sengi, (https://christopherlovell.github.io/sengi), an online tool for viewing the spectral outputs of stellar population synthesis (SPS) codes. Typical SPS codes require significant disk space or computing resources to produce spectra for simple stellar populations with arbitrary parameters. This makes it difficult to present their results in an interactive, web-friendly format. Sengi uses Non-negative Matrix Factorisation (NMF) and bilinear interpolation to estimate output spectra for arbitrary values of stellar age and metallicity. The reduced disk requirements and computational expense allows the result to be served as a client-based Javascript application. In this paper we present the method for generating grids of spectra, fitting those grids with NMF, bilinear interpolation across the fitted coefficients, and finally provide estimates of the prediction and interpolation errors.
@article{lovell_sengi_2021,
title = {Sengi: {A} small, fast, interactive viewer for spectral outputs from stellar population synthesis models},
volume = {34},
issn = {2213-1337},
shorttitle = {Sengi},
url = {http://www.sciencedirect.com/science/article/pii/S2213133720300986},
doi = {10.1016/j.ascom.2020.100444},
abstract = {We present Sengi, (https://christopherlovell.github.io/sengi), an online tool for viewing the spectral outputs of stellar population synthesis (SPS) codes. Typical SPS codes require significant disk space or computing resources to produce spectra for simple stellar populations with arbitrary parameters. This makes it difficult to present their results in an interactive, web-friendly format. Sengi uses Non-negative Matrix Factorisation (NMF) and bilinear interpolation to estimate output spectra for arbitrary values of stellar age and metallicity. The reduced disk requirements and computational expense allows the result to be served as a client-based Javascript application. In this paper we present the method for generating grids of spectra, fitting those grids with NMF, bilinear interpolation across the fitted coefficients, and finally provide estimates of the prediction and interpolation errors.},
language = {en},
urldate = {2021-01-14},
journal = {Astronomy and Computing},
author = {Lovell, C. C.},
month = jan,
year = {2021},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics},
pages = {100444},
}An orientation bias in observations of submillimetre galaxies. Lovell, C. C., Geach, J. E., Davé, R., Narayanan, D., Coppin, K. E. K., Li, Q., Franco, M., & Privon, G. C. arXiv:2106.11588, June, 2021. arXiv: 2106.11588
Paper abstract bibtex
Paper abstract bibtex Recent high-resolution interferometric images of submillimetre galaxies (SMGs) reveal fascinatingly complex morphologies. This raises a number of questions: how does the relative orientation of a galaxy affect its observed submillimetre emission, and does this result in an `orientation bias' in the selection and analysis of such galaxies in flux-limited cosmological surveys? We investigate these questions using the Simba cosmological simulation paired with the dust radiative transfer code Powderday. We select eight simulated SMGs ($S_\{850\}{\}gtrsim2$ mJy) at $z = 2$, and measure the variance of their `observed' emission over 50 random orientations. Each galaxy exhibits significant scatter in its emission close to the peak of the thermal dust emission, with variation in flux density of up to ${\}sim$50 mJy at the peak. This results in an appreciable dispersion in the inferred dust temperatures and infrared luminosities ($16{\textasciicircum}\{{\}mathrm\{th\}\}-84{\textasciicircum}\{{\}mathrm\{th\}\}$ percentile ranges of 5 K and 0.1 dex, respectively) and therefore a fundamental uncertainty in derived parameters such as dust mass and star formation rate (${\}sim$30% for the latter using simple calibrations). Using a Monte Carlo simulation we also assess the impact of orientation on flux-limited surveys, finding a bias in the selection of SMGs towards those with face-on orientations, as well as those at lower redshifts. We predict that the orientation bias will affect flux-limited single-dish surveys, most significantly at THz frequencies, and this bias should be taken into account when placing the results of targeted follow-up studies in a statistical context.
@article{lovell_orientation_2021,
title = {An orientation bias in observations of submillimetre galaxies},
url = {http://arxiv.org/abs/2106.11588},
abstract = {Recent high-resolution interferometric images of submillimetre galaxies (SMGs) reveal fascinatingly complex morphologies. This raises a number of questions: how does the relative orientation of a galaxy affect its observed submillimetre emission, and does this result in an `orientation bias' in the selection and analysis of such galaxies in flux-limited cosmological surveys? We investigate these questions using the Simba cosmological simulation paired with the dust radiative transfer code Powderday. We select eight simulated SMGs (\$S\_\{850\}{\textbackslash}gtrsim2\$ mJy) at \$z = 2\$, and measure the variance of their `observed' emission over 50 random orientations. Each galaxy exhibits significant scatter in its emission close to the peak of the thermal dust emission, with variation in flux density of up to \${\textbackslash}sim\$50 mJy at the peak. This results in an appreciable dispersion in the inferred dust temperatures and infrared luminosities (\$16{\textasciicircum}\{{\textbackslash}mathrm\{th\}\}-84{\textasciicircum}\{{\textbackslash}mathrm\{th\}\}\$ percentile ranges of 5 K and 0.1 dex, respectively) and therefore a fundamental uncertainty in derived parameters such as dust mass and star formation rate (\${\textbackslash}sim\$30\% for the latter using simple calibrations). Using a Monte Carlo simulation we also assess the impact of orientation on flux-limited surveys, finding a bias in the selection of SMGs towards those with face-on orientations, as well as those at lower redshifts. We predict that the orientation bias will affect flux-limited single-dish surveys, most significantly at THz frequencies, and this bias should be taken into account when placing the results of targeted follow-up studies in a statistical context.},
urldate = {2021-09-07},
journal = {arXiv:2106.11588},
author = {Lovell, C. C. and Geach, J. E. and Davé, R. and Narayanan, D. and Coppin, K. E. K. and Li, Q. and Franco, M. and Privon, G. C.},
month = jun,
year = {2021},
note = {arXiv: 2106.11588},
keywords = {Astrophysics - Astrophysics of Galaxies},
}First Light And Reionization Epoch Simulations (FLARES) – II: The photometric properties of high-redshift galaxies. Vijayan, A. P, Lovell, C. C, Wilkins, S. M, Thomas, P. A, Barnes, D. J, Irodotou, D., Kuusisto, J., & Roper, W. J Monthly Notices of the Royal Astronomical Society, 501(3):3289–3308, March, 2021.
Paper doi abstract bibtex
Paper doi abstract bibtex We present the photometric properties of galaxies in the First Light And Reionization Epoch Simulations (FLARES). The simulations trace the evolution of galaxies in a range of overdensities through the epoch of reionization. With a novel weighting scheme, we combine these overdensities, extending significantly the dynamic range of observed composite distribution functions compared to periodic simulation boxes. FLARES predicts a significantly larger number of intrinsically bright galaxies, which can be explained through a simple model linking dust attenuation to the metal content of the interstellar medium, using a line-of-sight extinction model. With this model, we present the photometric properties of the FLARES galaxies for z ∈ [5, 10]. We show that the ultraviolet (UV) luminosity function (LF) matches the observations at all redshifts. The function is fitted by Schechter and double power-law forms, with the latter being favoured at these redshifts by the FLARES composite UV LF. We also present predictions for the UV-continuum slope as well as the attenuation in the UV. The impact of environment on the UV LF is also explored, with the brightest galaxies forming in the densest environments. We then present the line luminosity and equivalent widths of some prominent nebular emission lines arising from the galaxies, finding rough agreement with available observations. We also look at the relative contribution of obscured and unobscured star formation, finding comparable contributions at these redshifts.
@article{vijayan_first_2021,
title = {First {Light} {And} {Reionization} {Epoch} {Simulations} ({FLARES}) -- {II}: {The} photometric properties of high-redshift galaxies},
volume = {501},
issn = {0035-8711},
shorttitle = {First {Light} {And} {Reionization} {Epoch} {Simulations} ({FLARES}) -- {II}},
url = {https://doi.org/10.1093/mnras/staa3715},
doi = {10.1093/mnras/staa3715},
abstract = {We present the photometric properties of galaxies in the First Light And Reionization Epoch Simulations (FLARES). The simulations trace the evolution of galaxies in a range of overdensities through the epoch of reionization. With a novel weighting scheme, we combine these overdensities, extending significantly the dynamic range of observed composite distribution functions compared to periodic simulation boxes. FLARES predicts a significantly larger number of intrinsically bright galaxies, which can be explained through a simple model linking dust attenuation to the metal content of the interstellar medium, using a line-of-sight extinction model. With this model, we present the photometric properties of the FLARES galaxies for z ∈ [5, 10]. We show that the ultraviolet (UV) luminosity function (LF) matches the observations at all redshifts. The function is fitted by Schechter and double power-law forms, with the latter being favoured at these redshifts by the FLARES composite UV LF. We also present predictions for the UV-continuum slope as well as the attenuation in the UV. The impact of environment on the UV LF is also explored, with the brightest galaxies forming in the densest environments. We then present the line luminosity and equivalent widths of some prominent nebular emission lines arising from the galaxies, finding rough agreement with available observations. We also look at the relative contribution of obscured and unobscured star formation, finding comparable contributions at these redshifts.},
number = {3},
urldate = {2022-02-09},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Vijayan, Aswin P and Lovell, Christopher C and Wilkins, Stephen M and Thomas, Peter A and Barnes, David J and Irodotou, Dimitrios and Kuusisto, Jussi and Roper, William J},
month = mar,
year = {2021},
keywords = {Astrophysics - Astrophysics of Galaxies, galaxies: evolution, galaxies: formation, galaxies: general, galaxies: high-redshift, galaxies: photometry},
pages = {3289--3308},
}Cosmic Evolution of the H2 Mass Density and the Epoch of Molecular Gas. Garratt, T. K., Coppin, K. E. K., Geach, J. E., Almaini, O., Hartley, W. G., Maltby, D. T., Simpson, C. J., Wilkinson, A., Conselice, C. J., Franco, M., Ivison, R. J., Koprowski, M. P., Lovell, C. C., Pope, A., Scott, D., & Werf, P. v. d. The Astrophysical Journal, 912(1):62, May, 2021. Publisher: American Astronomical Society
Paper doi abstract bibtex
Paper doi abstract bibtex We present new empirical constraints on the evolution of , the cosmological mass density of molecular hydrogen, back to z ≈ 2.5. We employ a statistical approach measuring the average observed 850 μm flux density of near-infrared selected galaxies as a function of redshift. The redshift range considered corresponds to a span where the 850 μm band probes the Rayleigh–Jeans tail of thermal dust emission in the rest frame, and can therefore be used as an estimate of the mass of the interstellar medium. Our sample comprises of ≈150,000 galaxies in the UK InfraRed Telescope Infrared Deep Sky Survey Ultra-Deep Survey field with near-infrared magnitudes K AB ≤ 25 mag and photometric redshifts with corresponding probability distribution functions derived from deep 12-band photometry. With a sample approximately 2 orders of magnitude larger than in previous works we significantly reduce statistical uncertainties on to z ≈ 2.5. Our measurements are in broad agreement with recent direct estimates from blank field molecular gas surveys, finding that the epoch of molecular gas coincides with the peak epoch of star formation with at z ≈ 2. We demonstrate that can be broadly modeled by inverting the star formation rate (SFR) density with a fixed or weakly evolving star formation efficiency. This “constant efficiency” model shows a similar evolution to our statistically derived , indicating that the dominant factor driving the peak star formation history at z ≈ 2 is a larger supply of molecular gas in galaxies rather than a significant evolution of the SFR efficiency within individual galaxies.
@article{garratt_cosmic_2021,
title = {Cosmic {Evolution} of the {H2} {Mass} {Density} and the {Epoch} of {Molecular} {Gas}},
volume = {912},
issn = {0004-637X},
url = {https://doi.org/10.3847/1538-4357/abec81},
doi = {10.3847/1538-4357/abec81},
abstract = {We present new empirical constraints on the evolution of , the cosmological mass density of molecular hydrogen, back to z ≈ 2.5. We employ a statistical approach measuring the average observed 850 μm flux density of near-infrared selected galaxies as a function of redshift. The redshift range considered corresponds to a span where the 850 μm band probes the Rayleigh–Jeans tail of thermal dust emission in the rest frame, and can therefore be used as an estimate of the mass of the interstellar medium. Our sample comprises of ≈150,000 galaxies in the UK InfraRed Telescope Infrared Deep Sky Survey Ultra-Deep Survey field with near-infrared magnitudes K AB ≤ 25 mag and photometric redshifts with corresponding probability distribution functions derived from deep 12-band photometry. With a sample approximately 2 orders of magnitude larger than in previous works we significantly reduce statistical uncertainties on to z ≈ 2.5. Our measurements are in broad agreement with recent direct estimates from blank field molecular gas surveys, finding that the epoch of molecular gas coincides with the peak epoch of star formation with at z ≈ 2. We demonstrate that can be broadly modeled by inverting the star formation rate (SFR) density with a fixed or weakly evolving star formation efficiency. This “constant efficiency” model shows a similar evolution to our statistically derived , indicating that the dominant factor driving the peak star formation history at z ≈ 2 is a larger supply of molecular gas in galaxies rather than a significant evolution of the SFR efficiency within individual galaxies.},
language = {en},
number = {1},
urldate = {2022-01-11},
journal = {The Astrophysical Journal},
author = {Garratt, T. K. and Coppin, K. E. K. and Geach, J. E. and Almaini, O. and Hartley, W. G. and Maltby, D. T. and Simpson, C. J. and Wilkinson, A. and Conselice, C. J. and Franco, M. and Ivison, R. J. and Koprowski, M. P. and Lovell, C. C. and Pope, A. and Scott, D. and Werf, P. van der},
month = may,
year = {2021},
note = {Publisher: American Astronomical Society},
keywords = {Astrophysics - Astrophysics of Galaxies},
pages = {62},
}The emergence of passive galaxies in the early Universe. Santini, P., Castellano, M., Merlin, E., Fontana, A., Fortuni, F., Kodra, D., Magnelli, B., Menci, N., Calabrò, A., Lovell, C. C., Pentericci, L., Testa, V., & Wilkins, S. M. Astronomy and Astrophysics, 652:A30, August, 2021.
Paper doi abstract bibtex 2 downloads
Paper doi abstract bibtex 2 downloads The emergence of passive galaxies in the early Universe results from the delicate interplay among the different physical processes responsible for their rapid assembly and the abrupt shut-down of their star formation activity. Investigating the individual properties and demographics of early passive galaxies improves our understanding of these mechanisms. In this work we present a follow-up analysis of the z > 3 passive galaxy candidates selected by Merlin et al. (2019, MNRAS, 490, 3309) in the CANDELS fields. We begin by first confirming the accuracy of their passive classification by exploiting their sub-millimetre emission to demonstrate the lack of ongoing star formation. Using archival ALMA observations we are able to confirm at least 61% of the observed candidates as passive. While the remainder lack sufficiently deep data for confirmation, we are able to validate the entire sample in a statistical sense. We then estimate the stellar mass function (SMF) of all 101 passive candidates in three redshift bins from z = 5 to z = 3. We adopt a stepwise approach that has the advantage of taking into account photometric errors, mass and selection completeness issues, as well as the Eddington bias, without any a posteriori correction. We observe a pronounced evolution in the SMF around z ∼ 4, indicating that we are witnessing the emergence of the passive population at this epoch. Massive (M > 10\textlessSUP\textgreater11\textless/SUP\textgreater M\textlessSUB\textgreater⊙\textless/SUB\textgreater) passive galaxies, only accounting for a small (< 10%) fraction of galaxies at z > 4, become dominant at later epochs. Thanks to a combination of photometric quality, sample selection, and methodology, we overall find a higher density of passive galaxies than in previous works. The comparison with theoretical predictions, despite a qualitative agreement (at least for some of the models considered), denotes a still incomplete understanding of the physical processes responsible for the formation of these galaxies. Finally, we extrapolate our results to predict the number of early passive galaxies expected in surveys carried out with future facilities.
@article{santini_emergence_2021,
title = {The emergence of passive galaxies in the early {Universe}},
volume = {652},
issn = {0004-6361},
url = {https://ui.adsabs.harvard.edu/abs/2021A&A...652A..30S/abstract},
doi = {10.1051/0004-6361/202039738},
abstract = {The emergence of passive galaxies in the early Universe results from the delicate interplay among the different physical processes responsible for their rapid assembly and the abrupt shut-down of their star formation activity. Investigating the individual properties and demographics of early passive galaxies improves our understanding of these mechanisms. In this work we present a follow-up analysis of the z \> 3 passive galaxy candidates selected by Merlin et al. (2019, MNRAS, 490, 3309) in the CANDELS fields. We begin by first confirming the accuracy of their passive classification by exploiting their sub-millimetre emission to demonstrate the lack of ongoing star formation. Using archival ALMA observations we are able to confirm at least 61\% of the observed candidates as passive. While the remainder lack sufficiently deep data for confirmation, we are able to validate the entire sample in a statistical sense. We then estimate the stellar mass function (SMF) of all 101 passive candidates in three redshift bins from z = 5 to z = 3. We adopt a stepwise approach that has the advantage of taking into account photometric errors, mass and selection completeness issues, as well as the Eddington bias, without any a posteriori correction. We observe a pronounced evolution in the SMF around z ∼ 4, indicating that we are witnessing the emergence of the passive population at this epoch. Massive (M \> 10{\textless}SUP{\textgreater}11{\textless}/SUP{\textgreater} M{\textless}SUB{\textgreater}⊙{\textless}/SUB{\textgreater}) passive galaxies, only accounting for a small (\< 10\%) fraction of galaxies at z \> 4, become dominant at later epochs. Thanks to a combination of photometric quality, sample selection, and methodology, we overall find a higher density of passive galaxies than in previous works. The comparison with theoretical predictions, despite a qualitative agreement (at least for some of the models considered), denotes a still incomplete understanding of the physical processes responsible for the formation of these galaxies. Finally, we extrapolate our results to predict the number of early passive galaxies expected in surveys carried out with future facilities.},
language = {en},
urldate = {2021-09-07},
journal = {Astronomy and Astrophysics},
author = {Santini, P. and Castellano, M. and Merlin, E. and Fontana, A. and Fortuni, F. and Kodra, D. and Magnelli, B. and Menci, N. and Calabrò, A. and Lovell, C. C. and Pentericci, L. and Testa, V. and Wilkins, S. M.},
month = aug,
year = {2021},
keywords = {Astrophysics - Astrophysics of Galaxies},
pages = {A30},
}Reproducing submillimetre galaxy number counts with cosmological hydrodynamic simulations. Lovell, C. C., Geach, J. E., Davé, R., Narayanan, D., & Li, Q. Monthly Notices of the Royal Astronomical Society, 502:772–793, March, 2021.
Paper doi abstract bibtex 2 downloads
Paper doi abstract bibtex 2 downloads Matching the number counts of high-z submillimetre-selected galaxies (SMGs) has been a long-standing problem for galaxy formation models. In this paper, we use 3D dust radiative transfer to model the submm emission from galaxies in the SIMBA cosmological hydrodynamic simulations, and compare predictions to the latest single-dish observational constraints on the abundance of 850 μm-selected sources. We find good agreement with the shape of the integrated 850 μm luminosity function, and the normalization is within 0.25 dex at \textgreater3 mJy, unprecedented for a fully cosmological hydrodynamic simulation, along with good agreement in the redshift distribution of bright SMGs. The agreement is driven primarily by SIMBA's good match to infrared measures of the star formation rate (SFR) function between z = 2 and 4 at high SFRs. Also important is the self-consistent on-the-fly dust model in SIMBA, which predicts, on average, higher dust masses (by up to a factor of 2.5) compared to using a fixed dust-to-metals ratio of 0.3. We construct a light-cone to investigate the effect of far-field blending, and find that 52 per cent of sources are blends of multiple components, which makes a small contribution to the normalization of the bright end of the number counts. We provide new fits to the 850 μm luminosity as a function of SFR and dust mass. Our results demonstrate that solutions to the discrepancy between submm counts in simulations and observations, such as a top-heavy initial mass function, are unnecessary, and that submillimetre-bright phases are a natural consequence of massive galaxy evolution.
@article{lovell_reproducing_2021,
title = {Reproducing submillimetre galaxy number counts with cosmological hydrodynamic simulations},
volume = {502},
issn = {0035-8711},
url = {http://adsabs.harvard.edu/abs/2021MNRAS.502..772L},
doi = {10.1093/mnras/staa4043},
abstract = {Matching the number counts of high-z submillimetre-selected galaxies
(SMGs) has been a long-standing problem for galaxy formation models. In
this paper, we use 3D dust radiative transfer to model the submm
emission from galaxies in the SIMBA cosmological hydrodynamic
simulations, and compare predictions to the latest single-dish
observational constraints on the abundance of 850 μm-selected
sources. We find good agreement with the shape of the integrated 850
μm luminosity function, and the normalization is within 0.25 dex at
{\textgreater}3 mJy, unprecedented for a fully cosmological hydrodynamic
simulation, along with good agreement in the redshift distribution of
bright SMGs. The agreement is driven primarily by SIMBA's good match to
infrared measures of the star formation rate (SFR) function between z =
2 and 4 at high SFRs. Also important is the self-consistent on-the-fly
dust model in SIMBA, which predicts, on average, higher dust masses (by
up to a factor of 2.5) compared to using a fixed dust-to-metals ratio of
0.3. We construct a light-cone to investigate the effect of far-field
blending, and find that 52 per cent of sources are blends of multiple
components, which makes a small contribution to the normalization of the
bright end of the number counts. We provide new fits to the 850 μm
luminosity as a function of SFR and dust mass. Our results demonstrate
that solutions to the discrepancy between submm counts in simulations
and observations, such as a top-heavy initial mass function, are
unnecessary, and that submillimetre-bright phases are a natural
consequence of massive galaxy evolution.},
urldate = {2021-03-19},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Lovell, Christopher C. and Geach, James E. and Davé, Romeel and Narayanan, Desika and Li, Qi},
month = mar,
year = {2021},
keywords = {Astrophysics - Astrophysics of Galaxies, galaxies: abundances, galaxies: active, galaxies: evolution, galaxies: formation, galaxies: high-redshift},
pages = {772--793},
}powderday: Dust Radiative Transfer for Galaxy Simulations. Narayanan, D., Turk, M. J., Robitaille, T., Kelly, A. J., McClellan, B. C., Sharma, R. S., Garg, P., Abruzzo, M., Choi, E., Conroy, C., Johnson, B. D., Kimock, B., Li, Q., Lovell, C. C., Lower, S., Privon, G. C., Roberts, J., Sethuram, S., Snyder, G. F., Thompson, R., & Wise, J. H. The Astrophysical Journal Supplement Series, 252(1):12, January, 2021. Publisher: American Astronomical Society
Paper doi abstract bibtex
Paper doi abstract bibtex We present powderday (available at https://github.com/dnarayanan/powderday), a flexible, fast, open-source dust radiative transfer package designed to interface with both idealized and cosmological galaxy formation simulations. powderday builds on fsps stellar population synthesis models, and hyperion dust radiative transfer, and employs yt to interface between different software packages. We include our stellar population synthesis modeling on the fly, allowing significant flexibility in the assumed stellar physics and nebular line emission. The dust content follows either simple observationally motivated prescriptions (i.e., constant dust-to-metals ratios, or dust-to-gas ratios that vary with metallicity), direct modeling from galaxy formation simulations that include dust physics, as well as a novel approach that includes the dust content via learning-based algorithms from the simba cosmological galaxy formation simulation. Active galactic nuclei (AGNs) can additionally be included via a range of prescriptions. The output of these models are broadband (912 Å–1 mm) spectral energy distributions (SEDs), as well as filter-convolved monochromatic images. powderday is designed to eliminate last-mile efforts by researchers that employ different hydrodynamic galaxy formation models and seamlessly interfaces with gizmo, arepo, gasoline, changa, and enzo. We demonstrate the capabilities of the code via three applications: a model for the star formation rate–infrared luminosity relation in galaxies (including the impact of AGNs), the impact of circumstellar dust around AGB stars on the mid-infrared emission from galaxy SEDs, and the impact of galaxy inclination angle on dust attenuation laws.
@article{narayanan_powderday_2021,
title = {powderday: {Dust} {Radiative} {Transfer} for {Galaxy} {Simulations}},
volume = {252},
issn = {0067-0049},
shorttitle = {powderday},
url = {https://doi.org/10.3847/1538-4365/abc487},
doi = {10.3847/1538-4365/abc487},
abstract = {We present powderday (available at https://github.com/dnarayanan/powderday), a flexible, fast, open-source dust radiative transfer package designed to interface with both idealized and cosmological galaxy formation simulations. powderday builds on fsps stellar population synthesis models, and hyperion dust radiative transfer, and employs yt to interface between different software packages. We include our stellar population synthesis modeling on the fly, allowing significant flexibility in the assumed stellar physics and nebular line emission. The dust content follows either simple observationally motivated prescriptions (i.e., constant dust-to-metals ratios, or dust-to-gas ratios that vary with metallicity), direct modeling from galaxy formation simulations that include dust physics, as well as a novel approach that includes the dust content via learning-based algorithms from the simba cosmological galaxy formation simulation. Active galactic nuclei (AGNs) can additionally be included via a range of prescriptions. The output of these models are broadband (912 Å–1 mm) spectral energy distributions (SEDs), as well as filter-convolved monochromatic images. powderday is designed to eliminate last-mile efforts by researchers that employ different hydrodynamic galaxy formation models and seamlessly interfaces with gizmo, arepo, gasoline, changa, and enzo. We demonstrate the capabilities of the code via three applications: a model for the star formation rate–infrared luminosity relation in galaxies (including the impact of AGNs), the impact of circumstellar dust around AGB stars on the mid-infrared emission from galaxy SEDs, and the impact of galaxy inclination angle on dust attenuation laws.},
language = {en},
number = {1},
urldate = {2021-01-20},
journal = {The Astrophysical Journal Supplement Series},
author = {Narayanan, Desika and Turk, Matthew J. and Robitaille, Thomas and Kelly, Ashley J. and McClellan, B. Connor and Sharma, Ray S. and Garg, Prerak and Abruzzo, Matthew and Choi, Ena and Conroy, Charlie and Johnson, Benjamin D. and Kimock, Benjamin and Li, Qi and Lovell, Christopher C. and Lower, Sidney and Privon, George C. and Roberts, Jonathan and Sethuram, Snigdaa and Snyder, Gregory F. and Thompson, Robert and Wise, John H.},
month = jan,
year = {2021},
note = {Publisher: American Astronomical Society},
keywords = {Astrophysics - Astrophysics of Galaxies},
pages = {12},
}First Light And Reionization Epoch Simulations (FLARES) - I. Environmental dependence of high-redshift galaxy evolution. Lovell, C. C., Vijayan, A. P., Thomas, P. A., Wilkins, S. M., Barnes, D. J., Irodotou, D., & Roper, W. Monthly Notices of the Royal Astronomical Society, 500:2127–2145, January, 2021.
Paper doi abstract bibtex
Paper doi abstract bibtex We introduce the First Light And Reionisation Epoch Simulations (FLARES), a suite of zoom simulations using the EAGLE model. We resimulate a range of overdensities during the Epoch of Reionization (EoR) in order to build composite distribution functions, as well as explore the environmental dependence of galaxy formation and evolution during this critical period of galaxy assembly. The regions are selected from a large $(3.2 {\}, {\}mathrm\{cGpc\}){\textasciicircum}\{3\}$ parent volume, based on their overdensity within a sphere of radius 14 h-1 cMpc. We then resimulate with full hydrodynamics, and employ a novel weighting scheme that allows the construction of composite distribution functions that are representative of the full parent volume. This significantly extends the dynamic range compared to smaller volume periodic simulations. We present an analysis of the galaxy stellar mass function (GSMF), the star formation rate distribution function (SFRF), and the star-forming sequence (SFS) predicted by FLARES, and compare to a number of observational and model constraints. We also analyse the environmental dependence over an unprecedented range of overdensity. Both the GSMF and the SFRF exhibit a clear double-Schechter form, up to the highest redshifts (z = 10). We also find no environmental dependence of the SFS normalization. The increased dynamic range probed by FLARES will allow us to make predictions for a number of large area surveys that will probe the EoR in coming years, carried out on new observatories such as Roman and Euclid.
@article{lovell_first_2021,
title = {First {Light} {And} {Reionization} {Epoch} {Simulations} ({FLARES}) - {I}. {Environmental} dependence of high-redshift galaxy evolution},
volume = {500},
issn = {0035-8711},
url = {http://adsabs.harvard.edu/abs/2021MNRAS.500.2127L},
doi = {10.1093/mnras/staa3360},
abstract = {We introduce the First Light And Reionisation Epoch Simulations
(FLARES), a suite of zoom simulations using the EAGLE model. We
resimulate a range of overdensities during the Epoch of Reionization
(EoR) in order to build composite distribution functions, as well as
explore the environmental dependence of galaxy formation and evolution
during this critical period of galaxy assembly. The regions are selected
from a large \$(3.2 {\textbackslash}, {\textbackslash}mathrm\{cGpc\}){\textasciicircum}\{3\}\$ parent volume, based on
their overdensity within a sphere of radius 14 h-1 cMpc. We
then resimulate with full hydrodynamics, and employ a novel weighting
scheme that allows the construction of composite distribution functions
that are representative of the full parent volume. This significantly
extends the dynamic range compared to smaller volume periodic
simulations. We present an analysis of the galaxy stellar mass function
(GSMF), the star formation rate distribution function (SFRF), and the
star-forming sequence (SFS) predicted by FLARES, and compare to a number
of observational and model constraints. We also analyse the
environmental dependence over an unprecedented range of overdensity.
Both the GSMF and the SFRF exhibit a clear double-Schechter form, up to
the highest redshifts (z = 10). We also find no environmental dependence
of the SFS normalization. The increased dynamic range probed by FLARES
will allow us to make predictions for a number of large area surveys
that will probe the EoR in coming years, carried out on new
observatories such as Roman and Euclid.},
urldate = {2021-01-14},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Lovell, Christopher C. and Vijayan, Aswin P. and Thomas, Peter A. and Wilkins, Stephen M. and Barnes, David J. and Irodotou, Dimitrios and Roper, Will},
month = jan,
year = {2021},
keywords = {Astrophysics - Astrophysics of Galaxies, galaxies: abundances, galaxies: evolution, galaxies: high-redshift},
pages = {2127--2145},
}A Search for Massive Galaxy Population in a Protocluster of LAEs at \$z = 2.39\$ near the Radio Galaxy 53W002. Yonekura, N., Kajisawa, M., Hamaguchi, E., Mawatari, K., & Yamada, T. Technical Report September, 2021. Publication Title: arXiv e-prints ADS Bibcode: 2021arXiv210902019Y Type: article
Paper abstract bibtex
Paper abstract bibtex We searched massive galaxy population in the known large-scale high-density structure of Lyman\${\textasciitilde}{\textbackslash}alpha\$ emitters (LAEs) at \$z=2.39\$ near the radio galaxy 53W002 by using \$B,{\textasciitilde}V,{\textasciitilde}i{\textasciicircum}{\textbackslash}prime,{\textasciitilde}J,{\textasciitilde}H,\$ and \${\textasciitilde}K_s\$-bands imaging data taken with Suprime-Cam and MOIRCS on the Subaru telescope. We selected 62 protocluster member candidates by their \$JHK_s\$-band colors and photometric redshift analysis (\$JHK_s\$-selected galaxies) in our survey field of \$70.2{\textasciitilde}\{{\textbackslash}rm\{arcmin\}\}{\textasciicircum}\{2\}\$, and compared their physical properties estimated from the SED fitting with a comparison sample in the COSMOS field. We found significant number density excesses for the \$JHK_s\$-selected galaxies in the 53W002 field at \$K_s{\textless}22.25,{\textasciitilde}J-K_s{\textgreater}2,\$ or \$V-K_s{\textgreater}4\$. In particular the number density of the \$JHK_s\$-selected galaxies with \$K_s{\textless}22.25\$ and \$J-K_s{\textgreater}2\$ in the 53W002 field is eight times higher than the comparison sample. Most of those with \$K_s{\textless}22.25\$ and \$J-K_s{\textgreater}2\$ are massive galaxies with \$M_s{\textgreater}10{\textasciicircum}\{11\}{\textasciitilde}M_{\textbackslash}odot\$, and their sSFRs of \$10{\textasciicircum}\{-11\}\$–\$10{\textasciicircum}\{-10\}{\textasciitilde}{\textbackslash}rm\{yr{\textasciicircum}\{-1\}\}\$ suggest that the star formation has not yet stopped completely. We also found a density excess of quiescent galaxies with \$M_s=5{\textbackslash}times10{\textasciicircum}\{10\}\$–\$10{\textasciicircum}\{11\}{\textasciitilde}M_{\textbackslash}odot\$ and \$\{{\textbackslash}rm\{sSFR\}\}{\textless}10{\textasciicircum}\{-11\}{\textasciitilde}{\textbackslash}rm\{yr{\textasciicircum}\{-1\}\}\$ as well as that of low-mass galaxies with \$M_s=10{\textasciicircum}\{9.75\}\$–\$10{\textasciicircum}\{10\}{\textasciitilde}M_{\textbackslash}odot\$ and various sSFRs. The massive galaxies with \$M_s{\textgreater}10{\textasciicircum}\{11\}{\textasciitilde}M_{\textbackslash}odot\$ are not located at the density peaks of LAEs, but they show a wide distribution along the similar direction with the structure of LAEs over \${\textbackslash}sim15\$–\$20\$ comoving Mpc. On the other hand, the quiescent galaxies with \$\{{\textbackslash}rm\{sSFR\}\}{\textless}10{\textasciicircum}\{-11\}{\textasciitilde}{\textbackslash}rm\{yr{\textasciicircum}\{-1\}\}\$ clearly avoid the structure of LAEs. Our results suggest that massive galaxies also exist in this protocluster discovered by the moderate overdensity of LAEs and their star formation activity depends on location in the protocluster.
@techreport{yonekura_search_2021,
title = {A {Search} for {Massive} {Galaxy} {Population} in a {Protocluster} of {LAEs} at \$z = 2.39\$ near the {Radio} {Galaxy} {53W002}},
url = {https://ui.adsabs.harvard.edu/abs/2021arXiv210902019Y},
abstract = {We searched massive galaxy population in the known large-scale high-density structure of Lyman\${\textasciitilde}{\textbackslash}alpha\$ emitters (LAEs) at \$z=2.39\$ near the radio galaxy 53W002 by using \$B,{\textasciitilde}V,{\textasciitilde}i{\textasciicircum}{\textbackslash}prime,{\textasciitilde}J,{\textasciitilde}H,\$ and \${\textasciitilde}K\_s\$-bands imaging data taken with Suprime-Cam and MOIRCS on the Subaru telescope. We selected 62 protocluster member candidates by their \$JHK\_s\$-band colors and photometric redshift analysis (\$JHK\_s\$-selected galaxies) in our survey field of \$70.2{\textasciitilde}\{{\textbackslash}rm\{arcmin\}\}{\textasciicircum}\{2\}\$, and compared their physical properties estimated from the SED fitting with a comparison sample in the COSMOS field. We found significant number density excesses for the \$JHK\_s\$-selected galaxies in the 53W002 field at \$K\_s{\textless}22.25,{\textasciitilde}J-K\_s{\textgreater}2,\$ or \$V-K\_s{\textgreater}4\$. In particular the number density of the \$JHK\_s\$-selected galaxies with \$K\_s{\textless}22.25\$ and \$J-K\_s{\textgreater}2\$ in the 53W002 field is eight times higher than the comparison sample. Most of those with \$K\_s{\textless}22.25\$ and \$J-K\_s{\textgreater}2\$ are massive galaxies with \$M\_s{\textgreater}10{\textasciicircum}\{11\}{\textasciitilde}M\_{\textbackslash}odot\$, and their sSFRs of \$10{\textasciicircum}\{-11\}\$--\$10{\textasciicircum}\{-10\}{\textasciitilde}{\textbackslash}rm\{yr{\textasciicircum}\{-1\}\}\$ suggest that the star formation has not yet stopped completely. We also found a density excess of quiescent galaxies with \$M\_s=5{\textbackslash}times10{\textasciicircum}\{10\}\$--\$10{\textasciicircum}\{11\}{\textasciitilde}M\_{\textbackslash}odot\$ and \$\{{\textbackslash}rm\{sSFR\}\}{\textless}10{\textasciicircum}\{-11\}{\textasciitilde}{\textbackslash}rm\{yr{\textasciicircum}\{-1\}\}\$ as well as that of low-mass galaxies with \$M\_s=10{\textasciicircum}\{9.75\}\$--\$10{\textasciicircum}\{10\}{\textasciitilde}M\_{\textbackslash}odot\$ and various sSFRs. The massive galaxies with \$M\_s{\textgreater}10{\textasciicircum}\{11\}{\textasciitilde}M\_{\textbackslash}odot\$ are not located at the density peaks of LAEs, but they show a wide distribution along the similar direction with the structure of LAEs over \${\textbackslash}sim15\$--\$20\$ comoving Mpc. On the other hand, the quiescent galaxies with \$\{{\textbackslash}rm\{sSFR\}\}{\textless}10{\textasciicircum}\{-11\}{\textasciitilde}{\textbackslash}rm\{yr{\textasciicircum}\{-1\}\}\$ clearly avoid the structure of LAEs. Our results suggest that massive galaxies also exist in this protocluster discovered by the moderate overdensity of LAEs and their star formation activity depends on location in the protocluster.},
urldate = {2022-01-05},
author = {Yonekura, Naoki and Kajisawa, Masaru and Hamaguchi, Erika and Mawatari, Ken and Yamada, Toru},
month = sep,
year = {2021},
note = {Publication Title: arXiv e-prints
ADS Bibcode: 2021arXiv210902019Y
Type: article},
keywords = {Astrophysics - Astrophysics of Galaxies},
}Starduster: A multi-wavelength SED model based on radiative transfer simulations and deep learning. Qiu, Y. & Kang, X. Technical Report December, 2021. Publication Title: arXiv e-prints ADS Bibcode: 2021arXiv211214434Q Type: article
Paper abstract bibtex
Paper abstract bibtex We present Starduster, a supervised deep learning model that predicts the multi-wavelength SED from galaxy geometry parameters and star formation history by emulating dust radiative transfer simulations. The model is comprised of three specifically designed neural networks, which take into account the features of dust attenuation and emission. We utilise the Skirt radiative transfer simulation to produce data for the training data of neural networks. Each neural network can be trained using \${\textbackslash}sim 4000 - 5000\$ samples. Compared with the direct results of the Skirt simulation, our deep learning model produces \$0.1 - 0.2\$ mag errors in FUV to FIR wavelengths. At some bands, the uncertainty is only \$0.01\$ mag. As an application, we fit our model to the observed SEDs of IC4225 and NGC5166. Our model can reproduce the observations, and successfully predicts that both IC4225 and NGC5166 are edge-on galaxies. However, the predicted geometry parameters are different from image-fitting studies. Our analysis implies that the inconsistency is mainly due to the degeneracy in the star formation history of the stellar disk and bulge. In addition, we find that the predicted fluxes at \$20 {\textbackslash}, {\textbackslash}rm {\textbackslash}mu m - 80 {\textbackslash}, {\textbackslash}rm {\textbackslash}mu m\$ by our SED model are correlated with bulge radius. Our SED code is public available and can be applied to both SED-fitting and SED-modelling of galaxies from semi-analytic models.
@techreport{qiu_starduster_2021,
title = {Starduster: {A} multi-wavelength {SED} model based on radiative transfer simulations and deep learning},
shorttitle = {Starduster},
url = {https://ui.adsabs.harvard.edu/abs/2021arXiv211214434Q},
abstract = {We present Starduster, a supervised deep learning model that predicts the multi-wavelength SED from galaxy geometry parameters and star formation history by emulating dust radiative transfer simulations. The model is comprised of three specifically designed neural networks, which take into account the features of dust attenuation and emission. We utilise the Skirt radiative transfer simulation to produce data for the training data of neural networks. Each neural network can be trained using \${\textbackslash}sim 4000 - 5000\$ samples. Compared with the direct results of the Skirt simulation, our deep learning model produces \$0.1 - 0.2\$ mag errors in FUV to FIR wavelengths. At some bands, the uncertainty is only \$0.01\$ mag. As an application, we fit our model to the observed SEDs of IC4225 and NGC5166. Our model can reproduce the observations, and successfully predicts that both IC4225 and NGC5166 are edge-on galaxies. However, the predicted geometry parameters are different from image-fitting studies. Our analysis implies that the inconsistency is mainly due to the degeneracy in the star formation history of the stellar disk and bulge. In addition, we find that the predicted fluxes at \$20 {\textbackslash}, {\textbackslash}rm {\textbackslash}mu m - 80 {\textbackslash}, {\textbackslash}rm {\textbackslash}mu m\$ by our SED model are correlated with bulge radius. Our SED code is public available and can be applied to both SED-fitting and SED-modelling of galaxies from semi-analytic models.},
urldate = {2022-01-05},
author = {Qiu, Yisheng and Kang, Xi},
month = dec,
year = {2021},
note = {Publication Title: arXiv e-prints
ADS Bibcode: 2021arXiv211214434Q
Type: article},
keywords = {Astrophysics - Astrophysics of Galaxies},
}Exploring the High-Redshift Universe with ALMA. Hatziminaoglou, E., Popping, G., & Zwaan, M. arXiv:2112.07452 [astro-ph], December, 2021. arXiv: 2112.07452
Paper abstract bibtex
Paper abstract bibtex The properties of the interstellar medium (ISM) of the highest-redshift galaxies and quasars provide important indications of the complex interplay between the accretion of baryons onto galaxies, the physics that drives the build-up of stars out of this gas, the subsequent chemical evolution and feedback processes and the reionisation of the Universe. The Atacama Large Millimeter/submillimeter Array (ALMA) continues to play a pivotal role in the characterisation of the ISM of high-redshift galaxies. Observations of the dust continuum emission, atomic fine-structure and molecular lines arising from high-redshift galaxies are now carried out routinely, providing ever more constraints on the theoretical models of galaxy formation and evolution in the early Universe. The European Astronomical Society's EAS 2021 symposium dedicated to the exploration of the high-redshift Universe with ALMA provided a forum for the observational and theoretical high-redshift ALMA communities to exchange their views and recent results in this rapidly evolving field. The article summarises the exciting results that were presented at the meeting.
@article{hatziminaoglou_exploring_2021,
title = {Exploring the {High}-{Redshift} {Universe} with {ALMA}},
url = {http://arxiv.org/abs/2112.07452},
abstract = {The properties of the interstellar medium (ISM) of the highest-redshift galaxies and quasars provide important indications of the complex interplay between the accretion of baryons onto galaxies, the physics that drives the build-up of stars out of this gas, the subsequent chemical evolution and feedback processes and the reionisation of the Universe. The Atacama Large Millimeter/submillimeter Array (ALMA) continues to play a pivotal role in the characterisation of the ISM of high-redshift galaxies. Observations of the dust continuum emission, atomic fine-structure and molecular lines arising from high-redshift galaxies are now carried out routinely, providing ever more constraints on the theoretical models of galaxy formation and evolution in the early Universe. The European Astronomical Society's EAS 2021 symposium dedicated to the exploration of the high-redshift Universe with ALMA provided a forum for the observational and theoretical high-redshift ALMA communities to exchange their views and recent results in this rapidly evolving field. The article summarises the exciting results that were presented at the meeting.},
urldate = {2022-01-03},
journal = {arXiv:2112.07452 [astro-ph]},
author = {Hatziminaoglou, Evanthia and Popping, Gergö and Zwaan, Martin},
month = dec,
year = {2021},
note = {arXiv: 2112.07452},
keywords = {Astrophysics - Astrophysics of Galaxies},
}Strong Ly\${\textbackslash}alpha\$ Emission in an Overdense Region at \$z=6.8\$: A Very Large (\${R}{\textbackslash}sim3\$ physical Mpc) Ionized Bubble in COSMOS?. Endsley, R. & Stark, D. P. arXiv:2112.14779 [astro-ph], December, 2021. arXiv: 2112.14779
Paper abstract bibtex
Paper abstract bibtex Our understanding of reionization has advanced considerably over the past decade, with several results now demonstrating that the IGM transitioned from substantially neutral at \$z=7\$ to largely reionized at \$z=6\$. However, little remains known about the sizes of ionized bubbles at \$z{\textbackslash}gtrsim7\$ as well as the galaxy overdensities which drive their growth. Fortunately, rest-UV spectroscopic observations offer a pathway towards characterizing these ionized bubbles thanks to the resonant nature of Lyman-alpha photons. In a previous work, we presented Ly\${\textbackslash}alpha\$ detections from three closely-separated Lyman-break galaxies at \$z{\textbackslash}simeq6.8\$, suggesting the presence of a large (\$R{\textgreater}1\$ physical Mpc) ionized bubble in the 1.5 deg\${\textasciicircum}2\$ COSMOS field. Here, we present new deep Ly\${\textbackslash}alpha\$ spectra of ten UV-bright (\${\textbackslash}mathrm\{M\}_\{{\textbackslash}mathrm\{UV\}\}{\textasciicircum}\{\} {\textbackslash}leq -20.4\$) \$z{\textbackslash}simeq6.6-6.9\$ galaxies in the surrounding area, enabling us to better characterize this potential ionized bubble. We confidently detect (S/N\${\textgreater}\$7) Ly\${\textbackslash}alpha\$ emission at \$z=6.701-6.882\$ in nine of ten observed galaxies, revealing that the large-scale volume spanned by these sources (characteristic radius \$R = 3.2\$ physical Mpc) traces a strong galaxy overdensity (\$N/{\textbackslash}langle N{\textbackslash}rangle {\textbackslash}gtrsim 3\$). Our data additionally confirm that the Ly\${\textbackslash}alpha\$ emission of UV-bright galaxies in this volume is significantly enhanced, with 40% (4/10) showing strong Ly\${\textbackslash}alpha\$ emission (equivalent width\${\textgreater}\$25 \${\textbackslash}mathrm\{{\textbackslash}mathring\{A\}\}\$) compared to the 8\$-\$9% found on average at \$z{\textbackslash}sim7\$. The median Ly\${\textbackslash}alpha\$ equivalent width of our observed galaxies is also \${\textbackslash}approx\$2\${\textbackslash}times\$ that typical at \$z{\textbackslash}sim7\$, consistent with expectations if a very large (\$R{\textbackslash}sim3\$ physical Mpc) ionized bubble is allowing the Ly\${\textbackslash}alpha\$ photons to cosmologically redshift far into the damping wing before encountering HI.
@article{endsley_strong_2021,
title = {Strong {Ly}\${\textbackslash}alpha\$ {Emission} in an {Overdense} {Region} at \$z=6.8\$: {A} {Very} {Large} (\${R}{\textbackslash}sim3\$ physical {Mpc}) {Ionized} {Bubble} in {COSMOS}?},
shorttitle = {Strong {Ly}\${\textbackslash}alpha\$ {Emission} in an {Overdense} {Region} at \$z=6.8\$},
url = {http://arxiv.org/abs/2112.14779},
abstract = {Our understanding of reionization has advanced considerably over the past decade, with several results now demonstrating that the IGM transitioned from substantially neutral at \$z=7\$ to largely reionized at \$z=6\$. However, little remains known about the sizes of ionized bubbles at \$z{\textbackslash}gtrsim7\$ as well as the galaxy overdensities which drive their growth. Fortunately, rest-UV spectroscopic observations offer a pathway towards characterizing these ionized bubbles thanks to the resonant nature of Lyman-alpha photons. In a previous work, we presented Ly\${\textbackslash}alpha\$ detections from three closely-separated Lyman-break galaxies at \$z{\textbackslash}simeq6.8\$, suggesting the presence of a large (\$R{\textgreater}1\$ physical Mpc) ionized bubble in the 1.5 deg\${\textasciicircum}2\$ COSMOS field. Here, we present new deep Ly\${\textbackslash}alpha\$ spectra of ten UV-bright (\${\textbackslash}mathrm\{M\}\_\{{\textbackslash}mathrm\{UV\}\}{\textasciicircum}\{\} {\textbackslash}leq -20.4\$) \$z{\textbackslash}simeq6.6-6.9\$ galaxies in the surrounding area, enabling us to better characterize this potential ionized bubble. We confidently detect (S/N\${\textgreater}\$7) Ly\${\textbackslash}alpha\$ emission at \$z=6.701-6.882\$ in nine of ten observed galaxies, revealing that the large-scale volume spanned by these sources (characteristic radius \$R = 3.2\$ physical Mpc) traces a strong galaxy overdensity (\$N/{\textbackslash}langle N{\textbackslash}rangle {\textbackslash}gtrsim 3\$). Our data additionally confirm that the Ly\${\textbackslash}alpha\$ emission of UV-bright galaxies in this volume is significantly enhanced, with 40\% (4/10) showing strong Ly\${\textbackslash}alpha\$ emission (equivalent width\${\textgreater}\$25 \${\textbackslash}mathrm\{{\textbackslash}mathring\{A\}\}\$) compared to the 8\$-\$9\% found on average at \$z{\textbackslash}sim7\$. The median Ly\${\textbackslash}alpha\$ equivalent width of our observed galaxies is also \${\textbackslash}approx\$2\${\textbackslash}times\$ that typical at \$z{\textbackslash}sim7\$, consistent with expectations if a very large (\$R{\textbackslash}sim3\$ physical Mpc) ionized bubble is allowing the Ly\${\textbackslash}alpha\$ photons to cosmologically redshift far into the damping wing before encountering HI.},
urldate = {2022-01-05},
journal = {arXiv:2112.14779 [astro-ph]},
author = {Endsley, Ryan and Stark, Daniel P.},
month = dec,
year = {2021},
note = {arXiv: 2112.14779},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
}The evolution of barred galaxies in the EAGLE simulations. Cavanagh, M. K., Bekki, K., Groves, B. A., & Pfeffer, J. arXiv:2112.12935 [astro-ph], December, 2021. arXiv: 2112.12935
Paper abstract bibtex
Paper abstract bibtex We study the morphologies of 3,964 galaxies and their progenitors with \$M_{\textbackslash}star {\textgreater} 10{\textasciicircum}\{10\} M_{\textbackslash}odot\$ in the reference EAGLE hydrodynamical simulation from redshifts \$z=1\$ to \$z=0\$, concentrating on the redshift evolution of the bar fraction. We apply two convolutional neural networks (CNNs) to classify 35,082 synthetic g-band images across 10 snapshots in redshift. We identify galaxies as either barred or unbarred, while also classifying each sample into one of four morphological types: elliptical (E), lenticular (S0), spiral (Sp), and irregular/miscellaneous (IrrM). We find that the bar fraction is roughly constant between \$z = 0.0\$ to \$z = 0.5\$ (32% to 33%), before exhibiting a general decline to 26% out to \$z = 1\$. The bar fraction is highest in spiral galaxies, from 49% at \$z = 0\$ to 39% at \$z = 1\$. The bar fraction in S0s is lower, ranging from 22% to 18%, with similar values for the miscellaneous category. Under 5% of ellipticals were classified as barred. We find that the bar fraction is highest in low mass galaxies (\$M_{\textbackslash}star {\textbackslash}leq 10{\textasciicircum}\{10.5\} M_{\textbackslash}odot\$). Through tracking the evolution of galaxies across each snapshot, we find that some barred galaxies undergo episodes of bar creation, destruction and regeneration, with a mean bar lifetime of 2.24 Gyr. We further find that incidences of bar destruction are more commonly linked to major merging, while minor merging and accretion is linked to both bar creation and destruction.
@article{cavanagh_evolution_2021,
title = {The evolution of barred galaxies in the {EAGLE} simulations},
url = {http://arxiv.org/abs/2112.12935},
abstract = {We study the morphologies of 3,964 galaxies and their progenitors with \$M\_{\textbackslash}star {\textgreater} 10{\textasciicircum}\{10\} M\_{\textbackslash}odot\$ in the reference EAGLE hydrodynamical simulation from redshifts \$z=1\$ to \$z=0\$, concentrating on the redshift evolution of the bar fraction. We apply two convolutional neural networks (CNNs) to classify 35,082 synthetic g-band images across 10 snapshots in redshift. We identify galaxies as either barred or unbarred, while also classifying each sample into one of four morphological types: elliptical (E), lenticular (S0), spiral (Sp), and irregular/miscellaneous (IrrM). We find that the bar fraction is roughly constant between \$z = 0.0\$ to \$z = 0.5\$ (32\% to 33\%), before exhibiting a general decline to 26\% out to \$z = 1\$. The bar fraction is highest in spiral galaxies, from 49\% at \$z = 0\$ to 39\% at \$z = 1\$. The bar fraction in S0s is lower, ranging from 22\% to 18\%, with similar values for the miscellaneous category. Under 5\% of ellipticals were classified as barred. We find that the bar fraction is highest in low mass galaxies (\$M\_{\textbackslash}star {\textbackslash}leq 10{\textasciicircum}\{10.5\} M\_{\textbackslash}odot\$). Through tracking the evolution of galaxies across each snapshot, we find that some barred galaxies undergo episodes of bar creation, destruction and regeneration, with a mean bar lifetime of 2.24 Gyr. We further find that incidences of bar destruction are more commonly linked to major merging, while minor merging and accretion is linked to both bar creation and destruction.},
urldate = {2022-01-05},
journal = {arXiv:2112.12935 [astro-ph]},
author = {Cavanagh, Mitchell K. and Bekki, Kenji and Groves, Brent A. and Pfeffer, Joel},
month = dec,
year = {2021},
note = {arXiv: 2112.12935},
keywords = {Astrophysics - Astrophysics of Galaxies},
}DeepAdversaries: Examining the Robustness of Deep Learning Models for Galaxy Morphology Classification. Ćiprijanović, A., Kafkes, D., Snyder, G., Sánchez, F. J., Perdue, G. N., Pedro, K., Nord, B., Madireddy, S., & Wild, S. M. arXiv:2112.14299 [astro-ph], December, 2021. arXiv: 2112.14299
Paper abstract bibtex
Paper abstract bibtex Data processing and analysis pipelines in cosmological survey experiments introduce data perturbations that can significantly degrade the performance of deep learning-based models. Given the increased adoption of supervised deep learning methods for processing and analysis of cosmological survey data, the assessment of data perturbation effects and the development of methods that increase model robustness are increasingly important. In the context of morphological classification of galaxies, we study the effects of perturbations in imaging data. In particular, we examine the consequences of using neural networks when training on baseline data and testing on perturbed data. We consider perturbations associated with two primary sources: 1) increased observational noise as represented by higher levels of Poisson noise and 2) data processing noise incurred by steps such as image compression or telescope errors as represented by one-pixel adversarial attacks. We also test the efficacy of domain adaptation techniques in mitigating the perturbation-driven errors. We use classification accuracy, latent space visualizations, and latent space distance to assess model robustness. Without domain adaptation, we find that processing pixel-level errors easily flip the classification into an incorrect class and that higher observational noise makes the model trained on low-noise data unable to classify galaxy morphologies. On the other hand, we show that training with domain adaptation improves model robustness and mitigates the effects of these perturbations, improving the classification accuracy by 23% on data with higher observational noise. Domain adaptation also increases by a factor of \textasciitilde2.3 the latent space distance between the baseline and the incorrectly classified one-pixel perturbed image, making the model more robust to inadvertent perturbations.
@article{ciprijanovic_deepadversaries_2021,
title = {{DeepAdversaries}: {Examining} the {Robustness} of {Deep} {Learning} {Models} for {Galaxy} {Morphology} {Classification}},
shorttitle = {{DeepAdversaries}},
url = {http://arxiv.org/abs/2112.14299},
abstract = {Data processing and analysis pipelines in cosmological survey experiments introduce data perturbations that can significantly degrade the performance of deep learning-based models. Given the increased adoption of supervised deep learning methods for processing and analysis of cosmological survey data, the assessment of data perturbation effects and the development of methods that increase model robustness are increasingly important. In the context of morphological classification of galaxies, we study the effects of perturbations in imaging data. In particular, we examine the consequences of using neural networks when training on baseline data and testing on perturbed data. We consider perturbations associated with two primary sources: 1) increased observational noise as represented by higher levels of Poisson noise and 2) data processing noise incurred by steps such as image compression or telescope errors as represented by one-pixel adversarial attacks. We also test the efficacy of domain adaptation techniques in mitigating the perturbation-driven errors. We use classification accuracy, latent space visualizations, and latent space distance to assess model robustness. Without domain adaptation, we find that processing pixel-level errors easily flip the classification into an incorrect class and that higher observational noise makes the model trained on low-noise data unable to classify galaxy morphologies. On the other hand, we show that training with domain adaptation improves model robustness and mitigates the effects of these perturbations, improving the classification accuracy by 23\% on data with higher observational noise. Domain adaptation also increases by a factor of {\textasciitilde}2.3 the latent space distance between the baseline and the incorrectly classified one-pixel perturbed image, making the model more robust to inadvertent perturbations.},
urldate = {2022-01-05},
journal = {arXiv:2112.14299 [astro-ph]},
author = {Ćiprijanović, Aleksandra and Kafkes, Diana and Snyder, Gregory and Sánchez, F. Javier and Perdue, Gabriel Nathan and Pedro, Kevin and Nord, Brian and Madireddy, Sandeep and Wild, Stefan M.},
month = dec,
year = {2021},
note = {arXiv: 2112.14299},
keywords = {Astrophysics - Astrophysics of Galaxies, Computer Science - Artificial Intelligence, Computer Science - Computer Vision and Pattern Recognition, Computer Science - Machine Learning},
}Unsupervised Domain Adaptation for Constraining Star Formation Histories. Gilda, S., de Mathelin, A., Bellstedt, S., & Richard, G. arXiv:2112.14072 [astro-ph], December, 2021. arXiv: 2112.14072
Paper abstract bibtex
Paper abstract bibtex The prevalent paradigm of machine learning today is to use past observations to predict future ones. What if, however, we are interested in knowing the past given the present? This situation is indeed one that astronomers must contend with often. To understand the formation of our universe, we must derive the time evolution of the visible mass content of galaxies. However, to observe a complete star life, one would need to wait for one billion years! To overcome this difficulty, astrophysicists leverage supercomputers and evolve simulated models of galaxies till the current age of the universe, thus establishing a mapping between observed radiation and star formation histories (SFHs). Such ground-truth SFHs are lacking for actual galaxy observations, where they are usually inferred – with often poor confidence – from spectral energy distributions (SEDs) using Bayesian fitting methods. In this investigation, we discuss the ability of unsupervised domain adaptation to derive accurate SFHs for galaxies with simulated data as a necessary first step in developing a technique that can ultimately be applied to observational data.
@article{gilda_unsupervised_2021,
title = {Unsupervised {Domain} {Adaptation} for {Constraining} {Star} {Formation} {Histories}},
url = {http://arxiv.org/abs/2112.14072},
abstract = {The prevalent paradigm of machine learning today is to use past observations to predict future ones. What if, however, we are interested in knowing the past given the present? This situation is indeed one that astronomers must contend with often. To understand the formation of our universe, we must derive the time evolution of the visible mass content of galaxies. However, to observe a complete star life, one would need to wait for one billion years! To overcome this difficulty, astrophysicists leverage supercomputers and evolve simulated models of galaxies till the current age of the universe, thus establishing a mapping between observed radiation and star formation histories (SFHs). Such ground-truth SFHs are lacking for actual galaxy observations, where they are usually inferred -- with often poor confidence -- from spectral energy distributions (SEDs) using Bayesian fitting methods. In this investigation, we discuss the ability of unsupervised domain adaptation to derive accurate SFHs for galaxies with simulated data as a necessary first step in developing a technique that can ultimately be applied to observational data.},
urldate = {2022-01-03},
journal = {arXiv:2112.14072 [astro-ph]},
author = {Gilda, Sankalp and de Mathelin, Antoine and Bellstedt, Sabine and Richard, Guillaume},
month = dec,
year = {2021},
note = {arXiv: 2112.14072},
keywords = {Astrophysics - Astrophysics of Galaxies, Computer Science - Artificial Intelligence},
}Galaxy evolution through infrared and submillimeter spectroscopy: Measuring star formation and black hole accretion with JWST and ALMA. Mordini, S., Spinoglio, L., & Fernández-Ontiveros, J. A. arXiv:2112.11969 [astro-ph], December, 2021. arXiv: 2112.11969
Paper abstract bibtex
Paper abstract bibtex Rest-frame mid- to far-infrared spectroscopy is a powerful tool to study how galaxies formed and evolved, because a major part of their evolution occurs in heavily dust enshrouded environments, especially at the so-called Cosmic Noon. Using the calibrations of IR lines we predict the expected fluxes of lines and features, with the aim to measure the star formation rate and the Black Hole Accretion rate in intermediate to high redshift galaxies. The launch of the James Webb Space Telescope will allow us a deep investigation of both the SF and the BHA obscured processes as a function of cosmic time. We assess the spectral lines and features that can be detected by JWST-MIRI in galaxies and Active Galactic Nuclei up to redshift z= 3. We confirm the fine-structure lines of [MgIV]4.49um and [ArVI]4.53um as good BHA rate tracers for the 1\textlessz\textless3 range, and we propose the [NeVI]7.65um line as the best tracer for redshifts of z\textless1.5. We suggest the use of the [ArII]6.98um and [ArIII]8.99um lines to measure the SF rate, for z\textless3 and z\textless2. At higher redshifts, the PAH features at 6.2um and 7.7um can be observed at z\textless3 and z\textless2.7 respectively. Rest-frame far-IR spectroscopy is currently being collected in high redshift galaxies (z\textgreater3) with the Atacama Large Millimeter Array. We confirm that the [CII]158um line is a good tracer of the SF rate and can in most cases (0.9\textlessz\textless2 and 3\textlessz\textless9) be observed, and we propose the use of the combination of [OIII]88um and [OI]145um lines as an alternative SF rate tracer, that can be detected above z\textgreater3. We conclude, however, that the current and foreseen facilities will not be able to cover properly the peak of the obscured SF and BHA activities at the Cosmic Noon of galaxy evolution and a new IR space telescope, actively cooled to obtain very good sensitivities, covering the full IR spectral range from about 10um to 300um, will be needed.
@article{mordini_galaxy_2021,
title = {Galaxy evolution through infrared and submillimeter spectroscopy: {Measuring} star formation and black hole accretion with {JWST} and {ALMA}},
shorttitle = {Galaxy evolution through infrared and submillimeter spectroscopy},
url = {http://arxiv.org/abs/2112.11969},
abstract = {Rest-frame mid- to far-infrared spectroscopy is a powerful tool to study how galaxies formed and evolved, because a major part of their evolution occurs in heavily dust enshrouded environments, especially at the so-called Cosmic Noon. Using the calibrations of IR lines we predict the expected fluxes of lines and features, with the aim to measure the star formation rate and the Black Hole Accretion rate in intermediate to high redshift galaxies. The launch of the James Webb Space Telescope will allow us a deep investigation of both the SF and the BHA obscured processes as a function of cosmic time. We assess the spectral lines and features that can be detected by JWST-MIRI in galaxies and Active Galactic Nuclei up to redshift z= 3. We confirm the fine-structure lines of [MgIV]4.49um and [ArVI]4.53um as good BHA rate tracers for the 1{\textless}z{\textless}3 range, and we propose the [NeVI]7.65um line as the best tracer for redshifts of z{\textless}1.5. We suggest the use of the [ArII]6.98um and [ArIII]8.99um lines to measure the SF rate, for z{\textless}3 and z{\textless}2. At higher redshifts, the PAH features at 6.2um and 7.7um can be observed at z{\textless}3 and z{\textless}2.7 respectively. Rest-frame far-IR spectroscopy is currently being collected in high redshift galaxies (z{\textgreater}3) with the Atacama Large Millimeter Array. We confirm that the [CII]158um line is a good tracer of the SF rate and can in most cases (0.9{\textless}z{\textless}2 and 3{\textless}z{\textless}9) be observed, and we propose the use of the combination of [OIII]88um and [OI]145um lines as an alternative SF rate tracer, that can be detected above z{\textgreater}3. We conclude, however, that the current and foreseen facilities will not be able to cover properly the peak of the obscured SF and BHA activities at the Cosmic Noon of galaxy evolution and a new IR space telescope, actively cooled to obtain very good sensitivities, covering the full IR spectral range from about 10um to 300um, will be needed.},
urldate = {2022-01-05},
journal = {arXiv:2112.11969 [astro-ph]},
author = {Mordini, Sabrina and Spinoglio, Luigi and Fernández-Ontiveros, Juan Antonio},
month = dec,
year = {2021},
note = {arXiv: 2112.11969},
keywords = {Astrophysics - Astrophysics of Galaxies},
}A census of optically dark massive galaxies in the early Universe from magnification by lensing galaxy clusters. Shu, X., Yang, L., Liu, D., Wang, W., Wang, T., Han, Y., Huang, X., Lim, C., Chang, Y., Zheng, W., Zheng, X., Wang, J., & Kong, X. arXiv:2112.03709 [astro-ph], December, 2021. arXiv: 2112.03709
Paper abstract bibtex
Paper abstract bibtex We present ALMA 870um and JCMT SCUBA2 850um dust continuum observations of a sample of optically dark and strongly lensed galaxies in the cluster fields. The ALMA and SCUBA2 observations reach a median rms of about 0.11 mJy and 0.44 mJy, respectively, with the latter close to the confusion limit of the data at 850um. This represents one of the most sensitive searches for dust emission in optically dark galaxies. We detect the dust emission in 12 out of 15 galaxies at \textgreater3.8 sigma, corresponding to a detection rate of 80 per cent. Thanks to the gravitational lensing, our observations reach a deeper limiting flux than previous surveys in blank fields by a factor of 3. We estimate delensed infrared luminosities in the range log(LIR)=11.5-12.7 Lsun, which correspond to dust-obscured star formation rates (SFRs) of 30 to 520 Msun per year. Stellar population fits to the optical-to-NIR photometric data yield a median redshift z=4.26 and de-lensed stellar mass log(Mstar)=10.78 Msun. They contribute a lensing-corrected star-formation rate density at least an order of magnitude higher than that of equivalently massive UV-selected galaxies at z\textgreater3. The results suggest that there is a missing population of massive star-forming galaxies in the early Universe, which may dominate the SFR density at the massive end. Five optically dark galaxies are located within r\textless50 arcsec in one cluster field, representing a potential overdensity structure that has a physical origin at a confidence level \textgreater99.974% from Poisson statistics. Follow-up spectroscopic observations with ALMA and JWST are crucial to confirm whether it is associated with a protocluster at similar redshifts.
@article{shu_census_2021,
title = {A census of optically dark massive galaxies in the early {Universe} from magnification by lensing galaxy clusters},
url = {http://arxiv.org/abs/2112.03709},
abstract = {We present ALMA 870um and JCMT SCUBA2 850um dust continuum observations of a sample of optically dark and strongly lensed galaxies in the cluster fields. The ALMA and SCUBA2 observations reach a median rms of about 0.11 mJy and 0.44 mJy, respectively, with the latter close to the confusion limit of the data at 850um. This represents one of the most sensitive searches for dust emission in optically dark galaxies. We detect the dust emission in 12 out of 15 galaxies at {\textgreater}3.8 sigma, corresponding to a detection rate of 80 per cent. Thanks to the gravitational lensing, our observations reach a deeper limiting flux than previous surveys in blank fields by a factor of 3. We estimate delensed infrared luminosities in the range log(LIR)=11.5-12.7 Lsun, which correspond to dust-obscured star formation rates (SFRs) of 30 to 520 Msun per year. Stellar population fits to the optical-to-NIR photometric data yield a median redshift z=4.26 and de-lensed stellar mass log(Mstar)=10.78 Msun. They contribute a lensing-corrected star-formation rate density at least an order of magnitude higher than that of equivalently massive UV-selected galaxies at z{\textgreater}3. The results suggest that there is a missing population of massive star-forming galaxies in the early Universe, which may dominate the SFR density at the massive end. Five optically dark galaxies are located within r{\textless}50 arcsec in one cluster field, representing a potential overdensity structure that has a physical origin at a confidence level {\textgreater}99.974\% from Poisson statistics. Follow-up spectroscopic observations with ALMA and JWST are crucial to confirm whether it is associated with a protocluster at similar redshifts.},
urldate = {2021-12-20},
journal = {arXiv:2112.03709 [astro-ph]},
author = {Shu, Xinwen and Yang, Lei and Liu, Daizhong and Wang, Wei-Hao and Wang, Tao and Han, Yunkun and Huang, Xingxing and Lim, Chen-Fatt and Chang, Yu-Yen and Zheng, Wei and Zheng, Xianzhong and Wang, Junxian and Kong, Xu},
month = dec,
year = {2021},
note = {arXiv: 2112.03709},
keywords = {Astrophysics - Astrophysics of Galaxies},
}Deep Extragalactic VIsible Legacy Survey (DEVILS): Evolution of the \${\textbackslash}sigma_\{{\textbackslash}mathrm\{{SFR}\}\}\$-M\$_\{{\textbackslash}star\}\$ relation and implications for self-regulated star formation. Davies, L. J. M., Thorne, J. E., Bellstedt, S., Bravo, M., Robotham, A. S. G., Driver, S. P., Cook, R. H. W., Cortese, L., D'Silva, J., Grootes, M. W., Holwerda, B. W., Hopkins, A. M., Jarvis, M. J., Lidman, C., Phillipps, S., & Siudek, M. Monthly Notices of the Royal Astronomical Society, 509(3):4392–4410, December, 2021. arXiv: 2112.06279
Paper doi abstract bibtex
Paper doi abstract bibtex We present the evolution of the star-formation dispersion - stellar mass relation (\${\textbackslash}sigma_\{SFR\}\$-M\$_\{{\textbackslash}star\}\$) in the DEVILS D10 region using new measurements derived using the ProSpect spectral energy distribution fitting code. We find that \${\textbackslash}sigma_\{SFR\}\$-M\$_\{{\textbackslash}star\}\$ shows the characteristic 'U-shape' at intermediate stellar masses from 0.1\textlessz\textless0.7 for a number of metrics, including using the deconvolved intrinsic dispersion. A physical interpretation of this relation is the combination of stochastic star-formation and stellar feedback causing large scatter at low stellar masses and AGN feedback causing asymmetric scatter at high stellar masses. As such, the shape of this distribution and its evolution encodes detailed information about the astrophysical processes affecting star-formation, feedback and the lifecycle of galaxies. We find that the stellar mass that the minimum \$\{{\textbackslash}sigma\}_\{SFR\}\$ occurs evolves linearly with redshift, moving to higher stellar masses with increasing lookback time and traces the turnover in the star-forming sequence. This minimum \$\{{\textbackslash}sigma\}_\{SFR\}\$ point is also found to occur at a fixed specific star-formation rate (sSFR) at all epochs (sSFR\textasciitilde10\${\textasciicircum}\{-9.6\}\$yr\${\textasciicircum}\{-1\}\$). The physical interpretation of this is that there exists a maximum sSFR at which galaxies can internally self-regulate on the tight sequence of star-formation. At higher sSFRs, stochastic stellar processes begin to cause galaxies to be pushed both above and below the star-forming sequence leading to increased SFR dispersion. As the Universe evolves, a higher fraction of galaxies will drop below this sSFR threshold, causing the dispersion of the low-stellar mass end of the star-forming sequence to decrease with time.
@article{davies_deep_2021,
title = {Deep {Extragalactic} {VIsible} {Legacy} {Survey} ({DEVILS}): {Evolution} of the \${\textbackslash}sigma\_\{{\textbackslash}mathrm\{{SFR}\}\}\$-{M}\$\_\{{\textbackslash}star\}\$ relation and implications for self-regulated star formation},
volume = {509},
issn = {0035-8711, 1365-2966},
shorttitle = {Deep {Extragalactic} {VIsible} {Legacy} {Survey} ({DEVILS})},
url = {http://arxiv.org/abs/2112.06279},
doi = {10.1093/mnras/stab3145},
abstract = {We present the evolution of the star-formation dispersion - stellar mass relation (\${\textbackslash}sigma\_\{SFR\}\$-M\$\_\{{\textbackslash}star\}\$) in the DEVILS D10 region using new measurements derived using the ProSpect spectral energy distribution fitting code. We find that \${\textbackslash}sigma\_\{SFR\}\$-M\$\_\{{\textbackslash}star\}\$ shows the characteristic 'U-shape' at intermediate stellar masses from 0.1{\textless}z{\textless}0.7 for a number of metrics, including using the deconvolved intrinsic dispersion. A physical interpretation of this relation is the combination of stochastic star-formation and stellar feedback causing large scatter at low stellar masses and AGN feedback causing asymmetric scatter at high stellar masses. As such, the shape of this distribution and its evolution encodes detailed information about the astrophysical processes affecting star-formation, feedback and the lifecycle of galaxies. We find that the stellar mass that the minimum \$\{{\textbackslash}sigma\}\_\{SFR\}\$ occurs evolves linearly with redshift, moving to higher stellar masses with increasing lookback time and traces the turnover in the star-forming sequence. This minimum \$\{{\textbackslash}sigma\}\_\{SFR\}\$ point is also found to occur at a fixed specific star-formation rate (sSFR) at all epochs (sSFR{\textasciitilde}10\${\textasciicircum}\{-9.6\}\$yr\${\textasciicircum}\{-1\}\$). The physical interpretation of this is that there exists a maximum sSFR at which galaxies can internally self-regulate on the tight sequence of star-formation. At higher sSFRs, stochastic stellar processes begin to cause galaxies to be pushed both above and below the star-forming sequence leading to increased SFR dispersion. As the Universe evolves, a higher fraction of galaxies will drop below this sSFR threshold, causing the dispersion of the low-stellar mass end of the star-forming sequence to decrease with time.},
number = {3},
urldate = {2021-12-20},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Davies, L. J. M. and Thorne, J. E. and Bellstedt, S. and Bravo, M. and Robotham, A. S. G. and Driver, S. P. and Cook, R. H. W. and Cortese, L. and D'Silva, J. and Grootes, M. W. and Holwerda, B. W. and Hopkins, A. M. and Jarvis, M. J. and Lidman, C. and Phillipps, S. and Siudek, M.},
month = dec,
year = {2021},
note = {arXiv: 2112.06279},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
pages = {4392--4410},
}A High-Resolution Investigation of the Multi-Phase ISM in a Galaxy during the First Two Billion Years. Dye, S., Eales, S. A., Gomez, H. L., Jones, G. C., Smith, M. W. L., Borsato, E., Moss, A., Dunne, L., Maresca, J., Amvrosiadis, A., Negrello, M., Marchetti, L., Corsini, E. M., Ivison, R. J., Bendo, G. J., Bakx, T., Cooray, A., Cox, P., Dannerbauer, H., Serjeant, S., Riechers, D., Temi, P., & Vlahakis, C. Monthly Notices of the Royal Astronomical Society, December, 2021. arXiv: 2112.03936
Paper doi abstract bibtex
Paper doi abstract bibtex We have carried out the first spatially-resolved investigation of the multi-phase interstellar medium (ISM) at high redshift, using the z=4.24 strongly-lensed sub-millimetre galaxy H-ATLASJ142413.9+022303 (ID141). We present high-resolution (down to \textasciitilde350 pc) ALMA observations in dust continuum emission and in the CO(7-6), H_2O (2_\1,1\ - 2_\0,2\), CI(1-0) and CI(2-1) lines, the latter two allowing us to spatially resolve the cool phase of the ISM for the first time. Our modelling of the kinematics reveals that the system appears to be dominated by a rotationally-supported gas disk with evidence of a nearby perturber. We find that the CI(1-0) line has a very different distribution to the other lines, showing the existence of a reservoir of cool gas that might have been missed in studies of other galaxies. We have estimated the mass of the ISM using four different tracers, always obtaining an estimate in the range (3.2-3.8) x 10\textasciicircum\11\ M_sol, significantly higher than our dynamical mass estimate of (0.8-1.3) x 10\textasciicircum\11\ M_sol. We suggest that this conflict and other similar conflicts reported in the literature is because the gas-to-tracer ratios are \textasciitilde4 times lower than the Galactic values used to calibrate the ISM in high-redshift galaxies. We demonstrate that this could result from a top-heavy initial mass function and strong chemical evolution. Using a variety of quantitative indicators, we show that, extreme though it is at z=4.24, ID141 will likely join the population of quiescent galaxies that appears in the Universe at z\textasciitilde3.
@article{dye_high-resolution_2021,
title = {A {High}-{Resolution} {Investigation} of the {Multi}-{Phase} {ISM} in a {Galaxy} during the {First} {Two} {Billion} {Years}},
issn = {0035-8711, 1365-2966},
url = {http://arxiv.org/abs/2112.03936},
doi = {10.1093/mnras/stab3569},
abstract = {We have carried out the first spatially-resolved investigation of the multi-phase interstellar medium (ISM) at high redshift, using the z=4.24 strongly-lensed sub-millimetre galaxy H-ATLASJ142413.9+022303 (ID141). We present high-resolution (down to {\textasciitilde}350 pc) ALMA observations in dust continuum emission and in the CO(7-6), H\_2O (2\_\{1,1\} - 2\_\{0,2\}), CI(1-0) and CI(2-1) lines, the latter two allowing us to spatially resolve the cool phase of the ISM for the first time. Our modelling of the kinematics reveals that the system appears to be dominated by a rotationally-supported gas disk with evidence of a nearby perturber. We find that the CI(1-0) line has a very different distribution to the other lines, showing the existence of a reservoir of cool gas that might have been missed in studies of other galaxies. We have estimated the mass of the ISM using four different tracers, always obtaining an estimate in the range (3.2-3.8) x 10{\textasciicircum}\{11\} M\_sol, significantly higher than our dynamical mass estimate of (0.8-1.3) x 10{\textasciicircum}\{11\} M\_sol. We suggest that this conflict and other similar conflicts reported in the literature is because the gas-to-tracer ratios are {\textasciitilde}4 times lower than the Galactic values used to calibrate the ISM in high-redshift galaxies. We demonstrate that this could result from a top-heavy initial mass function and strong chemical evolution. Using a variety of quantitative indicators, we show that, extreme though it is at z=4.24, ID141 will likely join the population of quiescent galaxies that appears in the Universe at z{\textasciitilde}3.},
urldate = {2021-12-20},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Dye, S. and Eales, S. A. and Gomez, H. L. and Jones, G. C. and Smith, M. W. L. and Borsato, E. and Moss, A. and Dunne, L. and Maresca, J. and Amvrosiadis, A. and Negrello, M. and Marchetti, L. and Corsini, E. M. and Ivison, R. J. and Bendo, G. J. and Bakx, T. and Cooray, A. and Cox, P. and Dannerbauer, H. and Serjeant, S. and Riechers, D. and Temi, P. and Vlahakis, C.},
month = dec,
year = {2021},
note = {arXiv: 2112.03936},
keywords = {Astrophysics - Astrophysics of Galaxies},
pages = {stab3569},
}A Search for H-Dropout Lyman Break Galaxies at z\textasciitilde13. Harikane, Y., Inoue, A. K., Mawatari, K., Hashimoto, T., Yamanaka, S., Fudamoto, Y., Matsuo, H., Tamura, Y., Dayal, P., Yung, L. Y. A., Hutter, A., Pacucci, F., & Sugahara, Y. arXiv:2112.09141 [astro-ph], December, 2021. arXiv: 2112.09141
Paper abstract bibtex
Paper abstract bibtex We present two bright galaxy candidates at z\textasciitilde13 identified in our H-dropout Lyman break selection with 2.3 deg\textasciicircum2 near-infrared deep imaging data. These galaxy candidates, selected after careful screening of foreground interlopers, have spectral energy distributions showing a sharp discontinuity around 1.7 um, a flat continuum at 2-5 um, and non-detections at \textless1.2 um in the available photometric datasets, all of which are consistent with a z\textasciitilde13 galaxy. An ALMA program targeting one of the candidates shows a tentative 4sigma [OIII]88um line at z=13.27, in agreement with its photometric redshift estimate. The number density of the z\textasciitilde13 candidates is comparable to that of bright z\textasciitilde10 galaxies, and is consistent with a recently proposed double power-law luminosity function rather than the Schechter function, indicating little evolution in the abundance of bright galaxies from z\textasciitilde4 to 13. Comparisons with theoretical models show that the models cannot reproduce the bright end of rest-frame ultraviolet luminosity functions at z\textasciitilde10-13. Combined with recent studies reporting similarly bright galaxies at z\textasciitilde9-11 and mature stellar populations at z\textasciitilde6-9, our results indicate the existence of a number of star-forming galaxies at z\textgreater10, which will be detected with upcoming space missions such as James Webb Space Telescope, Nancy Grace Roman Space Telescope, and GREX-PLUS.
@article{harikane_search_2021,
title = {A {Search} for {H}-{Dropout} {Lyman} {Break} {Galaxies} at z{\textasciitilde}13},
url = {http://arxiv.org/abs/2112.09141},
abstract = {We present two bright galaxy candidates at z{\textasciitilde}13 identified in our H-dropout Lyman break selection with 2.3 deg{\textasciicircum}2 near-infrared deep imaging data. These galaxy candidates, selected after careful screening of foreground interlopers, have spectral energy distributions showing a sharp discontinuity around 1.7 um, a flat continuum at 2-5 um, and non-detections at {\textless}1.2 um in the available photometric datasets, all of which are consistent with a z{\textasciitilde}13 galaxy. An ALMA program targeting one of the candidates shows a tentative 4sigma [OIII]88um line at z=13.27, in agreement with its photometric redshift estimate. The number density of the z{\textasciitilde}13 candidates is comparable to that of bright z{\textasciitilde}10 galaxies, and is consistent with a recently proposed double power-law luminosity function rather than the Schechter function, indicating little evolution in the abundance of bright galaxies from z{\textasciitilde}4 to 13. Comparisons with theoretical models show that the models cannot reproduce the bright end of rest-frame ultraviolet luminosity functions at z{\textasciitilde}10-13. Combined with recent studies reporting similarly bright galaxies at z{\textasciitilde}9-11 and mature stellar populations at z{\textasciitilde}6-9, our results indicate the existence of a number of star-forming galaxies at z{\textgreater}10, which will be detected with upcoming space missions such as James Webb Space Telescope, Nancy Grace Roman Space Telescope, and GREX-PLUS.},
urldate = {2022-01-03},
journal = {arXiv:2112.09141 [astro-ph]},
author = {Harikane, Yuichi and Inoue, Akio K. and Mawatari, Ken and Hashimoto, Takuya and Yamanaka, Satoshi and Fudamoto, Yoshinobu and Matsuo, Hiroshi and Tamura, Yoichi and Dayal, Pratika and Yung, L. Y. Aaron and Hutter, Anne and Pacucci, Fabio and Sugahara, Yuma},
month = dec,
year = {2021},
note = {arXiv: 2112.09141},
keywords = {Astrophysics - Astrophysics of Galaxies},
}The initial mass function of stars and the star-formation rates of galaxies. Kroupa, P. & Jerabkova, T. arXiv:2112.10788 [astro-ph], May, 2021. arXiv: 2112.10788
Paper doi abstract bibtex
Paper doi abstract bibtex The measured star-formation rates (SFRs) of galaxies comprise an important constraint on galaxy evolution and also on their cosmological boundary conditions. Any available tracer of the SFR depends on the shape of the mass-distribution of formed stars, i.e. on the stellar initial mass function (IMF). The luminous massive stars dominate the observed photon flux while the dim low-mass stars dominate the mass in the freshly formed population. Errors in the number ratio of the massive to low-mass stars lead to errors in SFR measurements and thus to errors concerning the gas-accretion-rates and the gas-consumption time-scales of galaxies. The stellar IMF has traditionally been interpreted to be a scale-invariant probability density distribution function (PDF), but it may instead be an optimal distribution function. In the PDF interpretation, the stellar IMF observed on the stales of individual star clusters is equal to the galaxy-wide IMF (gwIMF) which, by implication, would be invariant. In this Chapter we discuss the fundamental properties of the IMF and of the gwIMF, the nature of both and their systematic variability as indicated by measurements and theoretical expectations, and we discuss the implications for the SFRs of galaxies and their main sequence. The importance of the putative most-massive-star-mass vs stellar-mass-of-the-hosting-embedded-cluster (mmax-Mecl) relation and its possible establishment during the proto-stellar formation phase, is emphasised.
@article{kroupa_initial_2021,
title = {The initial mass function of stars and the star-formation rates of galaxies},
url = {http://arxiv.org/abs/2112.10788},
doi = {10.1017/9781316875445},
abstract = {The measured star-formation rates (SFRs) of galaxies comprise an important constraint on galaxy evolution and also on their cosmological boundary conditions. Any available tracer of the SFR depends on the shape of the mass-distribution of formed stars, i.e. on the stellar initial mass function (IMF). The luminous massive stars dominate the observed photon flux while the dim low-mass stars dominate the mass in the freshly formed population. Errors in the number ratio of the massive to low-mass stars lead to errors in SFR measurements and thus to errors concerning the gas-accretion-rates and the gas-consumption time-scales of galaxies. The stellar IMF has traditionally been interpreted to be a scale-invariant probability density distribution function (PDF), but it may instead be an optimal distribution function. In the PDF interpretation, the stellar IMF observed on the stales of individual star clusters is equal to the galaxy-wide IMF (gwIMF) which, by implication, would be invariant. In this Chapter we discuss the fundamental properties of the IMF and of the gwIMF, the nature of both and their systematic variability as indicated by measurements and theoretical expectations, and we discuss the implications for the SFRs of galaxies and their main sequence. The importance of the putative most-massive-star-mass vs stellar-mass-of-the-hosting-embedded-cluster (mmax-Mecl) relation and its possible establishment during the proto-stellar formation phase, is emphasised.},
urldate = {2022-01-03},
journal = {arXiv:2112.10788 [astro-ph]},
author = {Kroupa, Pavel and Jerabkova, Tereza},
month = may,
year = {2021},
note = {arXiv: 2112.10788},
keywords = {Astrophysics - Astrophysics of Galaxies},
}Empirical relations defining the growth of supermassive black holes: Implications for the origins of black hole seeds. Aggarwal, Y. arXiv:2112.06338 [astro-ph], December, 2021. arXiv: 2112.06338
Paper abstract bibtex
Paper abstract bibtex We compiled available mass and redshift z data for supermassive black holes (SMBHs) at z \textgreater7.5, ranging in mass over 2 orders of magnitude and in age by nearly 300 million years. The data reveal that a large subset covering the entire age spectrum has markedly similar masses. The most likely implication is that SMBHs within the subset had seeds with similar masses and formed essentially concurrently. Based on this inference, the data of the subset are used derive quantitative empirical relations that provide insights into the origins of black hole seeds and constraints for models of seed formation. The relationships are tested and applied to thousands of SMBHs at nearly all redshifts. The results show that the masses of SMBHs \textgreater a million solar masses are accounted for with seeds formed at or near z=30 and ranging from Sun's mass to about 50-thousand solar masses. Apparently, the seeds grew at an exponentially increasing accretion rate that reached a maximum near z=7 and decreased thereafter. From z=30 to 15, the average accretion rate either exceeded the Eddington limit by a factor of 2 or less, or the radiative efficiency was less than its canonical value of 0.1 and increased thereafter. About half of the growth apparently occurs from z=30 to 3.5 at an average rate of about 614 solar masses per million years per unit solar seed mass, and the rest in the succeeding 12-billion years. The maximum mass that a black hole can accrete is about 2.35-million times the seed mass, and the largest observable black hole should not exceed about 100-billion solar masses. The seed of Sagittarius A* is inferred to have had a mass a few times Sun's mass and may have stopped accreting recently having achieved its maximum growth potential.
@article{aggarwal_empirical_2021,
title = {Empirical relations defining the growth of supermassive black holes: {Implications} for the origins of black hole seeds},
shorttitle = {Empirical relations defining the growth of supermassive black holes},
url = {http://arxiv.org/abs/2112.06338},
abstract = {We compiled available mass and redshift z data for supermassive black holes (SMBHs) at z {\textgreater}7.5, ranging in mass over 2 orders of magnitude and in age by nearly 300 million years. The data reveal that a large subset covering the entire age spectrum has markedly similar masses. The most likely implication is that SMBHs within the subset had seeds with similar masses and formed essentially concurrently. Based on this inference, the data of the subset are used derive quantitative empirical relations that provide insights into the origins of black hole seeds and constraints for models of seed formation. The relationships are tested and applied to thousands of SMBHs at nearly all redshifts. The results show that the masses of SMBHs {\textgreater} a million solar masses are accounted for with seeds formed at or near z=30 and ranging from Sun's mass to about 50-thousand solar masses. Apparently, the seeds grew at an exponentially increasing accretion rate that reached a maximum near z=7 and decreased thereafter. From z=30 to 15, the average accretion rate either exceeded the Eddington limit by a factor of 2 or less, or the radiative efficiency was less than its canonical value of 0.1 and increased thereafter. About half of the growth apparently occurs from z=30 to 3.5 at an average rate of about 614 solar masses per million years per unit solar seed mass, and the rest in the succeeding 12-billion years. The maximum mass that a black hole can accrete is about 2.35-million times the seed mass, and the largest observable black hole should not exceed about 100-billion solar masses. The seed of Sagittarius A* is inferred to have had a mass a few times Sun's mass and may have stopped accreting recently having achieved its maximum growth potential.},
urldate = {2021-12-20},
journal = {arXiv:2112.06338 [astro-ph]},
author = {Aggarwal, Yash},
month = dec,
year = {2021},
note = {arXiv: 2112.06338},
keywords = {Astrophysics - Astrophysics of Galaxies},
}The cosmic environment overtakes the local density in shaping galaxy star formation. Ren, J., Pan, Z., Zheng, X., Qin, J., Shi, D., Gonzalez, V., Bian, F., Huang, J., Fang, M., Liu, W., Wen, R., Zhang, Y., Qiao, M., & Liu, S. arXiv:2112.06466 [astro-ph], December, 2021. arXiv: 2112.06466
Paper abstract bibtex
Paper abstract bibtex The gas supply from the cosmic web is the key to sustain star formation in galaxies. It remains to be explored how the cosmic large-scale structure (LSS) effects on galaxy evolution at given local environments. We examine galaxy specific star formation rate as a function of local density in a LSS at \$z=0.735\$ in the Extended Chandra Deep Field South. The LSS is mapped by 732 galaxies with \$R{\textless}24\$\textbackslash,mag and redshift at \$0.72{\textbackslash}le z {\textbackslash}le 0.75\$ collected from the literature and our spectroscopic observations with Magellan/IMACS, consisting of five galaxy clusters/groups and surrounding filaments over an area of \$23.9 {\textbackslash}times22.7\$\textbackslash,co-moving\textbackslash,Mpc\${\textasciicircum}2\$. The spread of spectroscopic redshifts corresponds a velocity dispersion of 494\textbackslash,km\textbackslash,s\${\textasciicircum}\{-1\}\$, indicating the LSS likely to be a thin sheet with a galaxy density \${\textbackslash}gtrsim 3.9\$ times that of the general field. These clusters/groups in this LSS mostly exhibit elongated morphologies and multiple components connected with surrounding filaments. Strikingly, we find that star-forming galaxies in the LSS keep star formation at the same level as field, and show no dependence on local density but stellar mass. Meanwhile, an increasing fraction of quiescent galaxies is detected at increasing local density in both the LSS and the field, consistent with the expectation that galaxy mass and local dense environment hold the key to quench star formation. Combined together, we conclude that the cosmic environment of the LSS overtakes the local environment in remaining galaxy star formation to the level of the field.
@article{ren_cosmic_2021,
title = {The cosmic environment overtakes the local density in shaping galaxy star formation},
url = {http://arxiv.org/abs/2112.06466},
abstract = {The gas supply from the cosmic web is the key to sustain star formation in galaxies. It remains to be explored how the cosmic large-scale structure (LSS) effects on galaxy evolution at given local environments. We examine galaxy specific star formation rate as a function of local density in a LSS at \$z=0.735\$ in the Extended Chandra Deep Field South. The LSS is mapped by 732 galaxies with \$R{\textless}24\${\textbackslash},mag and redshift at \$0.72{\textbackslash}le z {\textbackslash}le 0.75\$ collected from the literature and our spectroscopic observations with Magellan/IMACS, consisting of five galaxy clusters/groups and surrounding filaments over an area of \$23.9 {\textbackslash}times22.7\${\textbackslash},co-moving{\textbackslash},Mpc\${\textasciicircum}2\$. The spread of spectroscopic redshifts corresponds a velocity dispersion of 494{\textbackslash},km{\textbackslash},s\${\textasciicircum}\{-1\}\$, indicating the LSS likely to be a thin sheet with a galaxy density \${\textbackslash}gtrsim 3.9\$ times that of the general field. These clusters/groups in this LSS mostly exhibit elongated morphologies and multiple components connected with surrounding filaments. Strikingly, we find that star-forming galaxies in the LSS keep star formation at the same level as field, and show no dependence on local density but stellar mass. Meanwhile, an increasing fraction of quiescent galaxies is detected at increasing local density in both the LSS and the field, consistent with the expectation that galaxy mass and local dense environment hold the key to quench star formation. Combined together, we conclude that the cosmic environment of the LSS overtakes the local environment in remaining galaxy star formation to the level of the field.},
urldate = {2021-12-20},
journal = {arXiv:2112.06466 [astro-ph]},
author = {Ren, Jian and Pan, Zhizheng and Zheng, XianZhong and Qin, Jianbo and Shi, DongDong and Gonzalez, Valentino and Bian, Fuyan and Huang, Jia-Sheng and Fang, Min and Liu, Wenhao and Wen, Run and Zhang, Yuheng and Qiao, Man and Liu, Shuang},
month = dec,
year = {2021},
note = {arXiv: 2112.06466},
keywords = {Astrophysics - Astrophysics of Galaxies},
}Deep Extragalactic VIsible Legacy Survey (DEVILS): Identification of AGN through SED Fitting and the Evolution of the Bolometric AGN Luminosity Function. Thorne, J. E., Robotham, A. S. G., Davies, L. J. M., Bellstedt, S., Brown, M. J. I., Croom, S. M., Delvecchio, I., Groves, B., Jarvis, M. J., Shabala, S. S., Seymour, N., Whittam, I. H., Bravo, M., Cook, R. H. W., Driver, S. P., Holwerda, B., Phillipps, S., & Siudek, M. arXiv:2112.06366 [astro-ph], December, 2021. arXiv: 2112.06366
Paper abstract bibtex
Paper abstract bibtex Active galactic nuclei (AGN) are typically identified through radio, mid-infrared, or X-ray emission or through the presence of broad and/or narrow emission lines. AGN can also leave an imprint on a galaxy's spectral energy distribution (SED) through the re-processing of photons by the dusty torus. Using the SED fitting code ProSpect with an incorporated AGN component, we fit the far ultraviolet to far-infrared SEDs of \${\textbackslash}sim\$494,00 galaxies in the D10-COSMOS field and \${\textbackslash}sim\$230,000 galaxies from the GAMA survey. By combining an AGN component with a flexible star formation and metallicity implementation, we obtain estimates for the AGN luminosities, stellar masses, star formation histories, and metallicity histories for each of our galaxies. We find that ProSpect can identify AGN components in 91 per cent of galaxies pre-selected as containing AGN through narrow-emission line ratios and the presence of broad lines. Our ProSpect-derived AGN luminosities show close agreement with luminosities derived for X-ray selected AGN using both the X-ray flux and previous SED fitting results. We show that incorporating the flexibility of an AGN component when fitting the SEDs of galaxies with no AGN has no significant impact on the derived galaxy properties. However, in order to obtain accurate estimates of the stellar properties of AGN host galaxies, it is crucial to include an AGN component in the SED fitting process. We use our derived AGN luminosities to map the evolution of the AGN luminosity function for \$0{\textless}z{\textless}2\$ and find good agreement with previous measurements and predictions from theoretical models.
@article{thorne_deep_2021,
title = {Deep {Extragalactic} {VIsible} {Legacy} {Survey} ({DEVILS}): {Identification} of {AGN} through {SED} {Fitting} and the {Evolution} of the {Bolometric} {AGN} {Luminosity} {Function}},
shorttitle = {Deep {Extragalactic} {VIsible} {Legacy} {Survey} ({DEVILS})},
url = {http://arxiv.org/abs/2112.06366},
abstract = {Active galactic nuclei (AGN) are typically identified through radio, mid-infrared, or X-ray emission or through the presence of broad and/or narrow emission lines. AGN can also leave an imprint on a galaxy's spectral energy distribution (SED) through the re-processing of photons by the dusty torus. Using the SED fitting code ProSpect with an incorporated AGN component, we fit the far ultraviolet to far-infrared SEDs of \${\textbackslash}sim\$494,00 galaxies in the D10-COSMOS field and \${\textbackslash}sim\$230,000 galaxies from the GAMA survey. By combining an AGN component with a flexible star formation and metallicity implementation, we obtain estimates for the AGN luminosities, stellar masses, star formation histories, and metallicity histories for each of our galaxies. We find that ProSpect can identify AGN components in 91 per cent of galaxies pre-selected as containing AGN through narrow-emission line ratios and the presence of broad lines. Our ProSpect-derived AGN luminosities show close agreement with luminosities derived for X-ray selected AGN using both the X-ray flux and previous SED fitting results. We show that incorporating the flexibility of an AGN component when fitting the SEDs of galaxies with no AGN has no significant impact on the derived galaxy properties. However, in order to obtain accurate estimates of the stellar properties of AGN host galaxies, it is crucial to include an AGN component in the SED fitting process. We use our derived AGN luminosities to map the evolution of the AGN luminosity function for \$0{\textless}z{\textless}2\$ and find good agreement with previous measurements and predictions from theoretical models.},
urldate = {2021-12-20},
journal = {arXiv:2112.06366 [astro-ph]},
author = {Thorne, Jessica E. and Robotham, Aaron S. G. and Davies, Luke J. M. and Bellstedt, Sabine and Brown, Michael J. I. and Croom, Scott M. and Delvecchio, Ivan and Groves, Brent and Jarvis, Matt J. and Shabala, Stanislav S. and Seymour, Nick and Whittam, Imogen H. and Bravo, Matias and Cook, Robin H. W. and Driver, Simon P. and Holwerda, Benne and Phillipps, Steven and Siudek, Malgorzata},
month = dec,
year = {2021},
note = {arXiv: 2112.06366},
keywords = {Astrophysics - Astrophysics of Galaxies},
}Sizes of Lensed Lower-luminosity z=4-8 Galaxies from the Hubble Frontier Field Program. Bouwens, R. J., Illingworth, G. D., van Dokkum, P. G., Oesch, P. A., Stefanon, M., & Ribeiro, B. arXiv:2112.02948 [astro-ph], December, 2021. arXiv: 2112.02948
Paper abstract bibtex
Paper abstract bibtex We constrain the rest-UV size-luminosity relation for star-forming galaxies at z\textasciitilde4 and z\textasciitilde6, 7, and 8 identified behind clusters from the Hubble Frontier Fields (HFF) program. The size-luminosity relation is key to deriving accurate luminosity functions (LF) for faint galaxies. Making use of the latest lensing models and full data set for these clusters, lensing-corrected sizes and luminosities are derived for 68 z\textasciitilde4, 184 z\textasciitilde6, 93 z\textasciitilde7, and 53 z\textasciitilde8 galaxies. We show that size measurements can be reliably measured up to linear magnifications of 30x, where the lensing models are well calibrated. The sizes we measure span a \textgreater1-dex range, from \textless50 pc to \textgreater\textasciitilde500 pc. Uncertainties are based on both the formal fit errors and systematic differences between the public lensing models. These uncertainties range from \textasciitilde20 pc for the smallest sources to 50 pc for the largest. Using a forward-modeling procedure to model the impact of incompleteness and magnification uncertainties, we characterize the size-luminosity relation at both z\textasciitilde4 and z\textasciitilde6-8. We find that the source sizes of star-forming galaxies at z\textasciitilde4 and z\textasciitilde6-8 scale with luminosity L as L\textasciicircum\0.54\textbackslashpm0.08\ and L\textasciicircum\0.40+/-0.04\, respectively, such that lower luminosity (\textgreater\textasciitilde-18 mag) galaxies are smaller than expected from extrapolating the size-luminosity relation at high luminosities (\textless\textasciitilde-18 mag). The new evidence for a steeper size-luminosity relation (3 sigma) adds to earlier evidence for small sizes based on the prevalence of highly magnified galaxies in high shear regions, theoretical arguments against upturns in the LFs, and other independent determinations of the size-luminosity relation from the HFF clusters.
@article{bouwens_sizes_2021,
title = {Sizes of {Lensed} {Lower}-luminosity z=4-8 {Galaxies} from the {Hubble} {Frontier} {Field} {Program}},
url = {http://arxiv.org/abs/2112.02948},
abstract = {We constrain the rest-UV size-luminosity relation for star-forming galaxies at z{\textasciitilde}4 and z{\textasciitilde}6, 7, and 8 identified behind clusters from the Hubble Frontier Fields (HFF) program. The size-luminosity relation is key to deriving accurate luminosity functions (LF) for faint galaxies. Making use of the latest lensing models and full data set for these clusters, lensing-corrected sizes and luminosities are derived for 68 z{\textasciitilde}4, 184 z{\textasciitilde}6, 93 z{\textasciitilde}7, and 53 z{\textasciitilde}8 galaxies. We show that size measurements can be reliably measured up to linear magnifications of 30x, where the lensing models are well calibrated. The sizes we measure span a {\textgreater}1-dex range, from {\textless}50 pc to {\textgreater}{\textasciitilde}500 pc. Uncertainties are based on both the formal fit errors and systematic differences between the public lensing models. These uncertainties range from {\textasciitilde}20 pc for the smallest sources to 50 pc for the largest. Using a forward-modeling procedure to model the impact of incompleteness and magnification uncertainties, we characterize the size-luminosity relation at both z{\textasciitilde}4 and z{\textasciitilde}6-8. We find that the source sizes of star-forming galaxies at z{\textasciitilde}4 and z{\textasciitilde}6-8 scale with luminosity L as L{\textasciicircum}\{0.54{\textbackslash}pm0.08\} and L{\textasciicircum}\{0.40+/-0.04\}, respectively, such that lower luminosity ({\textgreater}{\textasciitilde}-18 mag) galaxies are smaller than expected from extrapolating the size-luminosity relation at high luminosities ({\textless}{\textasciitilde}-18 mag). The new evidence for a steeper size-luminosity relation (3 sigma) adds to earlier evidence for small sizes based on the prevalence of highly magnified galaxies in high shear regions, theoretical arguments against upturns in the LFs, and other independent determinations of the size-luminosity relation from the HFF clusters.},
urldate = {2021-12-20},
journal = {arXiv:2112.02948 [astro-ph]},
author = {Bouwens, R. J. and Illingworth, G. D. and van Dokkum, P. G. and Oesch, P. A. and Stefanon, M. and Ribeiro, B.},
month = dec,
year = {2021},
note = {arXiv: 2112.02948},
keywords = {Astrophysics - Astrophysics of Galaxies},
}The relationship between fine galaxy stellar morphology and star formation activity in cosmological simulations: a deep learning view. Zanisi, L., Huertas-Company, M., Lanusse, F., Bottrell, C., Pillepich, A., Nelson, D., Rodriguez-Gomez, V., Shankar, F., Hernquist, L., Dekel, A., Margalef-Bentabol, B., Vogelsberger, M., & Primack, J. Monthly Notices of the Royal Astronomical Society, 501(3):4359–4382, January, 2021. arXiv: 2007.00039 version: 2
Paper doi abstract bibtex
Paper doi abstract bibtex Hydrodynamical simulations of galaxy formation and evolution attempt to fully model the physics that shapes galaxies. The agreement between the morphology of simulated and real galaxies, and the way the morphological types are distributed across galaxy scaling relations are important probes of our knowledge of galaxy formation physics. Here we propose an unsupervised deep learning approach to perform a stringent test of the fine morphological structure of galaxies coming from the Illustris and IllustrisTNG (TNG100 and TNG50) simulations against observations from a subsample of the Sloan Digital Sky Survey. Our framework is based on PixelCNN, an autoregressive model for image generation with an explicit likelihood. We adopt a strategy that combines the output of two PixelCNN networks in a metric that isolates the fine morphological details of galaxies from the sky background. We are able to \textbackslashemph\quantitatively\ identify the improvements of IllustrisTNG, particularly in the high-resolution TNG50 run, over the original Illustris. However, we find that the fine details of galaxy structure are still different between observed and simulated galaxies. This difference is driven by small, more spheroidal, and quenched galaxies which are globally less accurate regardless of resolution and which have experienced little improvement between the three simulations explored. We speculate that this disagreement, that is less severe for quenched disky galaxies, may stem from a still too coarse numerical resolution, which struggles to properly capture the inner, dense regions of quenched spheroidal galaxies.
@article{zanisi_relationship_2021,
title = {The relationship between fine galaxy stellar morphology and star formation activity in cosmological simulations: a deep learning view},
volume = {501},
issn = {0035-8711, 1365-2966},
shorttitle = {The relationship between fine galaxy stellar morphology and star formation activity in cosmological simulations},
url = {http://arxiv.org/abs/2007.00039},
doi = {10.1093/mnras/staa3864},
abstract = {Hydrodynamical simulations of galaxy formation and evolution attempt to fully model the physics that shapes galaxies. The agreement between the morphology of simulated and real galaxies, and the way the morphological types are distributed across galaxy scaling relations are important probes of our knowledge of galaxy formation physics. Here we propose an unsupervised deep learning approach to perform a stringent test of the fine morphological structure of galaxies coming from the Illustris and IllustrisTNG (TNG100 and TNG50) simulations against observations from a subsample of the Sloan Digital Sky Survey. Our framework is based on PixelCNN, an autoregressive model for image generation with an explicit likelihood. We adopt a strategy that combines the output of two PixelCNN networks in a metric that isolates the fine morphological details of galaxies from the sky background. We are able to {\textbackslash}emph\{quantitatively\} identify the improvements of IllustrisTNG, particularly in the high-resolution TNG50 run, over the original Illustris. However, we find that the fine details of galaxy structure are still different between observed and simulated galaxies. This difference is driven by small, more spheroidal, and quenched galaxies which are globally less accurate regardless of resolution and which have experienced little improvement between the three simulations explored. We speculate that this disagreement, that is less severe for quenched disky galaxies, may stem from a still too coarse numerical resolution, which struggles to properly capture the inner, dense regions of quenched spheroidal galaxies.},
number = {3},
urldate = {2021-12-20},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Zanisi, Lorenzo and Huertas-Company, Marc and Lanusse, Francois and Bottrell, Connor and Pillepich, Annalisa and Nelson, Dylan and Rodriguez-Gomez, Vicente and Shankar, Francesco and Hernquist, Lars and Dekel, Avishai and Margalef-Bentabol, Berta and Vogelsberger, Mark and Primack, Joel},
month = jan,
year = {2021},
note = {arXiv: 2007.00039
version: 2},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics},
pages = {4359--4382},
}Predicting the water content of interstellar objects from galactic star formation histories. Lintott, C., Bannister, M. T., & Mackereth, J. T. arXiv:2112.05773 [astro-ph], December, 2021. arXiv: 2112.05773
Paper abstract bibtex
Paper abstract bibtex Planetesimals inevitably bear the signatures of their natal environment, preserving in their composition a record of the metallicity of their system's original gas and dust, albeit one altered by the formation process. When planetesimals are dispersed from their system of origin, this record is carried with them. As each star is likely to contribute at least \$10{\textasciicircum}\{12\}\$ interstellar objects, the Galaxy's drifting population of interstellar objects (ISOs) provides an overview of the properties of its stellar population through time. Using the EAGLE cosmological simulation and models of protoplanetary formation, our modelling predicts an ISO population with a bimodal distribution in their water mass fraction. Objects formed in low-metallicity, typically older, systems have a higher water fraction than their counterparts formed in high-metallicity protoplanetary disks, and these water-rich objects comprise the majority of the population. Both detected ISOs seem to belong to the lower water fraction population; these results suggest they come from recently formed systems. We show that the population of ISOs in galaxies with different star formation histories will have different proportions of objects with high and low water fractions. This work suggests that it is possible that the upcoming Vera C. Rubin Observatory Legacy Survey of Space and Time will detect a large enough population of ISOs to place useful constraints on models of protoplanetary disks, as well as galactic structure and evolution.
@article{lintott_predicting_2021,
title = {Predicting the water content of interstellar objects from galactic star formation histories},
url = {http://arxiv.org/abs/2112.05773},
abstract = {Planetesimals inevitably bear the signatures of their natal environment, preserving in their composition a record of the metallicity of their system's original gas and dust, albeit one altered by the formation process. When planetesimals are dispersed from their system of origin, this record is carried with them. As each star is likely to contribute at least \$10{\textasciicircum}\{12\}\$ interstellar objects, the Galaxy's drifting population of interstellar objects (ISOs) provides an overview of the properties of its stellar population through time. Using the EAGLE cosmological simulation and models of protoplanetary formation, our modelling predicts an ISO population with a bimodal distribution in their water mass fraction. Objects formed in low-metallicity, typically older, systems have a higher water fraction than their counterparts formed in high-metallicity protoplanetary disks, and these water-rich objects comprise the majority of the population. Both detected ISOs seem to belong to the lower water fraction population; these results suggest they come from recently formed systems. We show that the population of ISOs in galaxies with different star formation histories will have different proportions of objects with high and low water fractions. This work suggests that it is possible that the upcoming Vera C. Rubin Observatory Legacy Survey of Space and Time will detect a large enough population of ISOs to place useful constraints on models of protoplanetary disks, as well as galactic structure and evolution.},
urldate = {2021-12-17},
journal = {arXiv:2112.05773 [astro-ph]},
author = {Lintott, Chris and Bannister, Michele T. and Mackereth, J. Ted},
month = dec,
year = {2021},
note = {arXiv: 2112.05773},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Earth and Planetary Astrophysics},
}Massive Star-Forming Galaxies Have Converted Most of Their Halo Gas into Stars. Zhang, Z., Wang, H., Luo, W., Zhang, J., Mo, H. J., Jing, Y., Yang, X., & Li, H. arXiv:2112.04777 [astro-ph], December, 2021. arXiv: 2112.04777
Paper abstract bibtex
Paper abstract bibtex In the local Universe, the efficiency for converting baryonic gas into stars is very low. In dark matter halos where galaxies form and evolve, the average efficiency varies with galaxy stellar mass and has a maximum of about twenty percent for Milky-Way-like galaxies. The low efficiency at higher mass is believed to be produced by some quenching processes, such as the feedback from active galactic nuclei. We perform an analysis of weak lensing and satellite kinematics for SDSS central galaxies. Our results reveal that the efficiency is much higher, more than sixty percent, for a large population of massive star-forming galaxies around \$10{\textasciicircum}\{11\}{\textbackslash} {\textbackslash}rm M_{\textbackslash}odot\$. This suggests that these galaxies acquired most of the gas in their halos and converted it into stars without being affected significantly by quenching processes. This population of galaxies is not reproduced in current galaxy formation models, indicating that our understanding of galaxy formation is incomplete. The implications of our results on circumgalactic media, star formation quenching and disc galaxy rotation curves are discussed. We also examine systematic uncertainties in halo-mass and stellar-mass measurements that might influence our results.
@article{zhang_massive_2021,
title = {Massive {Star}-{Forming} {Galaxies} {Have} {Converted} {Most} of {Their} {Halo} {Gas} into {Stars}},
url = {http://arxiv.org/abs/2112.04777},
abstract = {In the local Universe, the efficiency for converting baryonic gas into stars is very low. In dark matter halos where galaxies form and evolve, the average efficiency varies with galaxy stellar mass and has a maximum of about twenty percent for Milky-Way-like galaxies. The low efficiency at higher mass is believed to be produced by some quenching processes, such as the feedback from active galactic nuclei. We perform an analysis of weak lensing and satellite kinematics for SDSS central galaxies. Our results reveal that the efficiency is much higher, more than sixty percent, for a large population of massive star-forming galaxies around \$10{\textasciicircum}\{11\}{\textbackslash} {\textbackslash}rm M\_{\textbackslash}odot\$. This suggests that these galaxies acquired most of the gas in their halos and converted it into stars without being affected significantly by quenching processes. This population of galaxies is not reproduced in current galaxy formation models, indicating that our understanding of galaxy formation is incomplete. The implications of our results on circumgalactic media, star formation quenching and disc galaxy rotation curves are discussed. We also examine systematic uncertainties in halo-mass and stellar-mass measurements that might influence our results.},
urldate = {2021-12-20},
journal = {arXiv:2112.04777 [astro-ph]},
author = {Zhang, Ziwen and Wang, Huiyuan and Luo, Wentao and Zhang, Jun and Mo, H. J. and Jing, YiPeng and Yang, Xiaohu and Li, Hao},
month = dec,
year = {2021},
note = {arXiv: 2112.04777},
keywords = {Astrophysics - Astrophysics of Galaxies},
}The galaxy starburst/main-sequence bimodality over five decades in stellar mass at z \textasciitilde 3-6.5. Rinaldi, P., Caputi, K. I., van Mierlo, S., Ashby, M. L. N., Caminha, G. B., & Iani, E. arXiv:2112.03935 [astro-ph], December, 2021. arXiv: 2112.03935
Paper abstract bibtex
Paper abstract bibtex We study the relation between stellar mass (M*) and star formation rate (SFR) for star-forming galaxies over approximately five decades in stellar mass (5.5 \textless\textasciitilde log10(M*/Msun) \textless\textasciitilde 10.5) at z \textasciitilde 3-6.5. This unprecedented coverage has been possible thanks to the joint analysis of blank non-lensed fields (COSMOS/SMUVS) and cluster lensing fields (Hubble Frontier Fields) which allow us to reach very low stellar masses. Previous works have revealed the existence of a clear bimodality in the SFR-M* plane with a star-formation Main Sequence and a starburst cloud at z \textasciitilde 4-5. Here we show that this bimodality extends to all star-forming galaxies and is valid in the whole redshift range z \textasciitilde 3-6.5. We find that starbursts constitute at least 20% of all star-forming galaxies with M* \textgreater\textasciitilde 10\textasciicircum9 Msun at these redshifts and reach a peak of 40% at z=4-5. More importantly, 60% to 90% of the total SFR budget at these redshifts is contained in starburst galaxies, indicating that the starburst mode of star-formation is dominant at high redshifts. Almost all the low stellar-mass starbursts with log10(M*/Msun) \textless\textasciitilde 8.5 have ages comparable to the typical timescales of a starburst event, suggesting that these galaxies are being caught in the process of formation. Interestingly, galaxy formation models fail to predict the starburst/main-sequence bimodality and starbursts overall, suggesting that the starburst phenomenon may be driven by physical processes occurring at smaller scales than those probed by these models.
@article{rinaldi_galaxy_2021,
title = {The galaxy starburst/main-sequence bimodality over five decades in stellar mass at z {\textasciitilde} 3-6.5},
url = {http://arxiv.org/abs/2112.03935},
abstract = {We study the relation between stellar mass (M*) and star formation rate (SFR) for star-forming galaxies over approximately five decades in stellar mass (5.5 {\textless}{\textasciitilde} log10(M*/Msun) {\textless}{\textasciitilde} 10.5) at z {\textasciitilde} 3-6.5. This unprecedented coverage has been possible thanks to the joint analysis of blank non-lensed fields (COSMOS/SMUVS) and cluster lensing fields (Hubble Frontier Fields) which allow us to reach very low stellar masses. Previous works have revealed the existence of a clear bimodality in the SFR-M* plane with a star-formation Main Sequence and a starburst cloud at z {\textasciitilde} 4-5. Here we show that this bimodality extends to all star-forming galaxies and is valid in the whole redshift range z {\textasciitilde} 3-6.5. We find that starbursts constitute at least 20\% of all star-forming galaxies with M* {\textgreater}{\textasciitilde} 10{\textasciicircum}9 Msun at these redshifts and reach a peak of 40\% at z=4-5. More importantly, 60\% to 90\% of the total SFR budget at these redshifts is contained in starburst galaxies, indicating that the starburst mode of star-formation is dominant at high redshifts. Almost all the low stellar-mass starbursts with log10(M*/Msun) {\textless}{\textasciitilde} 8.5 have ages comparable to the typical timescales of a starburst event, suggesting that these galaxies are being caught in the process of formation. Interestingly, galaxy formation models fail to predict the starburst/main-sequence bimodality and starbursts overall, suggesting that the starburst phenomenon may be driven by physical processes occurring at smaller scales than those probed by these models.},
urldate = {2021-12-17},
journal = {arXiv:2112.03935 [astro-ph]},
author = {Rinaldi, Pierluigi and Caputi, Karina I. and van Mierlo, Sophie and Ashby, Matthew L. N. and Caminha, Gabriel B. and Iani, Edoardo},
month = dec,
year = {2021},
note = {arXiv: 2112.03935},
keywords = {Astrophysics - Astrophysics of Galaxies},
}The evolution of the oxygen abundance gradients in star-forming galaxies in the EAGLE simulations. Tissera, P. B., Rosas-Guevara, Y., Sillero, E., Pedrosa, S. E., Theuns, T., & Bignone, L. arXiv:2112.06553 [astro-ph], December, 2021. arXiv: 2112.06553
Paper abstract bibtex
Paper abstract bibtex We analyse the evolution of the oxygen abundance gradient of star-forming galaxies with stellar mass Mstar \textgreater 10\textasciicircum9 Mo in the EAGK simulation over the redshift range z=[0, 2.5]. We find that the median metallicity gradient of the simulated galaxies is close to zero at all z, whereas the scatter around the median increases with z. The metallicity gradients of individual galaxies can evolve from strong to weak and vice-versa, since mostly low-metallicity gas accretes onto the galaxy, resulting in enhanced star formation and ejection of metal enriched gas by energy feedback. Such episodes of enhanced accretion, mainly dominated by major mergers, are more common at higher z, and hence contribute to increasing the diversity of gradients. For galaxies with negative metallicity gradients, we find a redshift evolution of \textasciitilde -0.03 dex/kpc/\textbackslashdelta z\$. A positive mass dependence is found at z{\textless} 0.5, which becomes slightly stronger for higher redshifts and, mainly, for Mstar {\textless} 10{\textasciicircum}9.5 Mo. Only galaxies with negative metallicity gradients define a correlation with galaxy size, consistent with an inside-out formation scenario. Our findings suggest that major mergers and/or significant gas accretion can drive strong negative or positive metallicity gradients. The first ones are preferentially associated with disc-dominated galaxies, and the second ones with dispersion-dominated systems. The comparison with forthcoming observations at high redshift will allow a better understanding of the potential role of metallicity gradients as a chemical probe of galaxy formation.
@article{tissera_evolution_2021,
title = {The evolution of the oxygen abundance gradients in star-forming galaxies in the {EAGLE} simulations},
url = {http://arxiv.org/abs/2112.06553},
abstract = {We analyse the evolution of the oxygen abundance gradient of star-forming galaxies with stellar mass Mstar {\textgreater} 10{\textasciicircum}9 Mo in the EAGK simulation over the redshift range z=[0, 2.5]. We find that the median metallicity gradient of the simulated galaxies is close to zero at all z, whereas the scatter around the median increases with z. The metallicity gradients of individual galaxies can evolve from strong to weak and vice-versa, since mostly low-metallicity gas accretes onto the galaxy, resulting in enhanced star formation and ejection of metal enriched gas by energy feedback. Such episodes of enhanced accretion, mainly dominated by major mergers, are more common at higher z, and hence contribute to increasing the diversity of gradients. For galaxies with negative metallicity gradients, we find a redshift evolution of {\textasciitilde} -0.03 dex/kpc/{\textbackslash}delta z\$. A positive mass dependence is found at z{\textless} 0.5, which becomes slightly stronger for higher redshifts and, mainly, for Mstar {\textless} 10{\textasciicircum}9.5 Mo. Only galaxies with negative metallicity gradients define a correlation with galaxy size, consistent with an inside-out formation scenario. Our findings suggest that major mergers and/or significant gas accretion can drive strong negative or positive metallicity gradients. The first ones are preferentially associated with disc-dominated galaxies, and the second ones with dispersion-dominated systems. The comparison with forthcoming observations at high redshift will allow a better understanding of the potential role of metallicity gradients as a chemical probe of galaxy formation.},
urldate = {2021-12-17},
journal = {arXiv:2112.06553 [astro-ph]},
author = {Tissera, Patricia B. and Rosas-Guevara, Yetli and Sillero, Emanuel and Pedrosa, Susana E. and Theuns, Tom and Bignone, Lucas},
month = dec,
year = {2021},
note = {arXiv: 2112.06553},
keywords = {Astrophysics - Astrophysics of Galaxies},
}Modelling high-resolution ALMA observations of strongly lensed dustystar forming galaxies detected by Herschel. Maresca, J., Dye, S., Amvrosiadis, A., Bendo, G., Cooray, A., De Zotti, G., Dunne, L., Eales, S., Furlanetto, C., González-Nuevo, J., Greener, M., Ivison, R., Lapi, A., Negrello, M., Riechers, D., Serjeant, S., Tergolina, M., & Wardlow, J. arXiv:2111.09680 [astro-ph], November, 2021. arXiv: 2111.09680
Paper abstract bibtex
Paper abstract bibtex We present modelling of \textasciitilde0.1arcsec resolution Atacama Large Millimetre/sub-millimeter Array imaging of seven strong gravitationally lensed galaxies detected by the Herschel Space Observatory. Four of these systems are galaxy-galaxy scale strong lenses, with the remaining three being group-scale lenses. Through careful modelling of visibilities, we infer the mass profiles of the lensing galaxies and by determining the magnification factors, we investigate the intrinsic properties and morphologies of the lensed sub-millimetre sources. We find that these sub-millimetre sources all have ratios of star formation rate to dust mass that is consistent with or in excess of the mean ratio for high-redshift sub-millimetre galaxies and low redshift ultra-luminous infrared galaxies. The contribution to the infrared luminosity from possible AGN is not quantified and so could be biasing our star formation rates to higher values. The majority of our lens models have mass density slopes close to isothermal, but some systems show significant differences.
@article{maresca_modelling_2021,
title = {Modelling high-resolution {ALMA} observations of strongly lensed dustystar forming galaxies detected by {Herschel}},
url = {http://arxiv.org/abs/2111.09680},
abstract = {We present modelling of {\textasciitilde}0.1arcsec resolution Atacama Large Millimetre/sub-millimeter Array imaging of seven strong gravitationally lensed galaxies detected by the Herschel Space Observatory. Four of these systems are galaxy-galaxy scale strong lenses, with the remaining three being group-scale lenses. Through careful modelling of visibilities, we infer the mass profiles of the lensing galaxies and by determining the magnification factors, we investigate the intrinsic properties and morphologies of the lensed sub-millimetre sources. We find that these sub-millimetre sources all have ratios of star formation rate to dust mass that is consistent with or in excess of the mean ratio for high-redshift sub-millimetre galaxies and low redshift ultra-luminous infrared galaxies. The contribution to the infrared luminosity from possible AGN is not quantified and so could be biasing our star formation rates to higher values. The majority of our lens models have mass density slopes close to isothermal, but some systems show significant differences.},
urldate = {2021-12-20},
journal = {arXiv:2111.09680 [astro-ph]},
author = {Maresca, Jacob and Dye, Simon and Amvrosiadis, Aristeidis and Bendo, George and Cooray, Asantha and De Zotti, Gianfranco and Dunne, Loretta and Eales, Stephen and Furlanetto, Cristina and González-Nuevo, Joaquin and Greener, Michael and Ivison, Robert and Lapi, Andrea and Negrello, Mattia and Riechers, Dominik and Serjeant, Stephen and Tergolina, Mônica and Wardlow, Julie},
month = nov,
year = {2021},
note = {arXiv: 2111.09680},
keywords = {Astrophysics - Astrophysics of Galaxies},
}DSPS: Differentiable Stellar Population Synthesis. Hearin, A. P., Chaves-Montero, J., Alarcon, A., Becker, M. R., & Benson, A. arXiv:2112.06830 [astro-ph], December, 2021. arXiv: 2112.06830
Paper abstract bibtex
Paper abstract bibtex Models of stellar population synthesis (SPS) are the fundamental tool that relates the physical properties of a galaxy to its spectral energy distribution (SED). In this paper, we present DSPS: a python package for stellar population synthesis. All of the functionality in DSPS is implemented natively in the JAX library for automatic differentiation, and so our predictions for galaxy photometry are fully differentiable, and directly inherit the performance benefits of JAX, including portability onto GPUs. DSPS also implements several novel features, such as i) a flexible empirical model for stellar metallicity that incorporates correlations with stellar age, and ii) support for the diffstar model that provides a physically-motivated connection between the star formation history of a galaxy (SFH) and the mass assembly of its underlying dark matter halo. We detail a set of theoretical techniques for using autodiff to calculate gradients of predictions for galaxy SEDs with respect to SPS parameters that control a range of physical effects, including SFH, stellar metallicity, nebular emission, and dust attenuation. When forward modeling the colors of a synthetic galaxy population, we find that DSPS can provide a factor of 20 speedup over standard SPS codes on a CPU, and a factor of over 1000 on a modern GPU. When coupled with gradient-based techniques for optimization and inference, DSPS makes it practical to conduct expansive likelihood analyses of simulation-based models of the galaxy–halo connection that fully forward model galaxy spectra and photometry.
@article{hearin_dsps_2021,
title = {{DSPS}: {Differentiable} {Stellar} {Population} {Synthesis}},
shorttitle = {{DSPS}},
url = {http://arxiv.org/abs/2112.06830},
abstract = {Models of stellar population synthesis (SPS) are the fundamental tool that relates the physical properties of a galaxy to its spectral energy distribution (SED). In this paper, we present DSPS: a python package for stellar population synthesis. All of the functionality in DSPS is implemented natively in the JAX library for automatic differentiation, and so our predictions for galaxy photometry are fully differentiable, and directly inherit the performance benefits of JAX, including portability onto GPUs. DSPS also implements several novel features, such as i) a flexible empirical model for stellar metallicity that incorporates correlations with stellar age, and ii) support for the diffstar model that provides a physically-motivated connection between the star formation history of a galaxy (SFH) and the mass assembly of its underlying dark matter halo. We detail a set of theoretical techniques for using autodiff to calculate gradients of predictions for galaxy SEDs with respect to SPS parameters that control a range of physical effects, including SFH, stellar metallicity, nebular emission, and dust attenuation. When forward modeling the colors of a synthetic galaxy population, we find that DSPS can provide a factor of 20 speedup over standard SPS codes on a CPU, and a factor of over 1000 on a modern GPU. When coupled with gradient-based techniques for optimization and inference, DSPS makes it practical to conduct expansive likelihood analyses of simulation-based models of the galaxy--halo connection that fully forward model galaxy spectra and photometry.},
urldate = {2021-12-17},
journal = {arXiv:2112.06830 [astro-ph]},
author = {Hearin, Andrew P. and Chaves-Montero, Jonás and Alarcon, Alex and Becker, Matthew R. and Benson, Andrew},
month = dec,
year = {2021},
note = {arXiv: 2112.06830},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
}Evolution of dust grain size distribution and grain porosity in galaxies. Hirashita, H. & Il'in, V. B. Monthly Notices of the Royal Astronomical Society, 509(4):5771–5789, December, 2021. arXiv: 2111.12868
Paper doi abstract bibtex
Paper doi abstract bibtex The radiative properties of interstellar dust are affected not only by the grain size distribution but also by the grain porosity. We develop a model for the evolution of size-dependent grain porosity and grain size distribution over the entire history of galaxy evolution. We include stellar dust production, supernova dust destruction, shattering, coagulation, and accretion. Coagulation is \assumed to be\ the source of grain porosity. We use a one-zone model with a constant dense gas fraction (\${\textbackslash}eta_{\textbackslash}mathrm\{dense\}\$), which regulates the balance between shattering and coagulation. We find that porosity develops after small grains are sufficiently created by the interplay between shattering and accretion (at age \$t{\textbackslash}sim 1\$ Gyr for star formation time-scale \${\textbackslash}tau_{\textbackslash}mathrm\{SF\}=5\$ Gyr) and are coagulated. The filling factor drops down to 0.3 at grain radii \${\textbackslash}sim 0.03{\textasciitilde}{\textbackslash}mu\$m for \${\textbackslash}eta_{\textbackslash}mathrm\{dense\}=0.5\$. The grains are more porous for smaller \${\textbackslash}eta_{\textbackslash}mathrm\{dense\}\$ because small grains, from which porous coagulated grains form, are more abundant. We also calculate the extinction curves based on the above results. The porosity steepens the extinction curve significantly for silicate, but not much for amorphous carbon. The porosity also increases the collisional cross-sections and produces slightly more large grains through the enhanced coagulation; however, the extinction curve does not necessarily become flatter because of the steepening effect by porosity. We also discuss the implication of our results for the Milky Way extinction curve.
@article{hirashita_evolution_2021,
title = {Evolution of dust grain size distribution and grain porosity in galaxies},
volume = {509},
issn = {0035-8711, 1365-2966},
url = {http://arxiv.org/abs/2111.12868},
doi = {10.1093/mnras/stab3455},
abstract = {The radiative properties of interstellar dust are affected not only by the grain size distribution but also by the grain porosity. We develop a model for the evolution of size-dependent grain porosity and grain size distribution over the entire history of galaxy evolution. We include stellar dust production, supernova dust destruction, shattering, coagulation, and accretion. Coagulation is \{assumed to be\} the source of grain porosity. We use a one-zone model with a constant dense gas fraction (\${\textbackslash}eta\_{\textbackslash}mathrm\{dense\}\$), which regulates the balance between shattering and coagulation. We find that porosity develops after small grains are sufficiently created by the interplay between shattering and accretion (at age \$t{\textbackslash}sim 1\$ Gyr for star formation time-scale \${\textbackslash}tau\_{\textbackslash}mathrm\{SF\}=5\$ Gyr) and are coagulated. The filling factor drops down to 0.3 at grain radii \${\textbackslash}sim 0.03{\textasciitilde}{\textbackslash}mu\$m for \${\textbackslash}eta\_{\textbackslash}mathrm\{dense\}=0.5\$. The grains are more porous for smaller \${\textbackslash}eta\_{\textbackslash}mathrm\{dense\}\$ because small grains, from which porous coagulated grains form, are more abundant. We also calculate the extinction curves based on the above results. The porosity steepens the extinction curve significantly for silicate, but not much for amorphous carbon. The porosity also increases the collisional cross-sections and produces slightly more large grains through the enhanced coagulation; however, the extinction curve does not necessarily become flatter because of the steepening effect by porosity. We also discuss the implication of our results for the Milky Way extinction curve.},
number = {4},
urldate = {2021-12-17},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Hirashita, Hiroyuki and Il'in, Vladimir B.},
month = dec,
year = {2021},
note = {arXiv: 2111.12868},
keywords = {Astrophysics - Astrophysics of Galaxies},
pages = {5771--5789},
}Large-scale dark matter simulations. Angulo, R. E. & Hahn, O. arXiv:2112.05165 [astro-ph], December, 2021. arXiv: 2112.05165
Paper abstract bibtex
Paper abstract bibtex We review the field of collisionless numerical simulations for the large-scale structure of the Universe. We start by providing the main set of equations solved by these simulations and their connection with General Relativity. We then recap the relevant numerical approaches: discretization of the phase-space distribution (focusing on N-body but including alternatives, e.g., Lagrangian submanifold and Schr\textbackslash"odinger-Poisson) and the respective techniques for their time evolution and force calculation (Direct summation, mesh techniques, and hierarchical tree methods). We pay attention to the creation of initial conditions and the connection with Lagrangian Perturbation Theory. We then discuss the possible alternatives in terms of the micro-physical properties of dark matter (e.g., neutralinos, warm dark matter, QCD axions, Bose-Einstein condensates, and primordial black holes), and extensions to account for multiple fluids (baryons and neutrinos), primordial non-Gaussianity and modified gravity. We continue by discussing challenges involved in achieving highly accurate predictions. A key aspect of cosmological simulations is the connection to cosmological observables, we discuss various techniques in this regard: structure finding, galaxy formation and baryonic modelling, the creation of emulators and light-cones, and the role of machine learning. We finalise with a recount of state-of-the-art large-scale simulations and conclude with an outlook for the next decade.
@article{angulo_large-scale_2021,
title = {Large-scale dark matter simulations},
url = {http://arxiv.org/abs/2112.05165},
abstract = {We review the field of collisionless numerical simulations for the large-scale structure of the Universe. We start by providing the main set of equations solved by these simulations and their connection with General Relativity. We then recap the relevant numerical approaches: discretization of the phase-space distribution (focusing on N-body but including alternatives, e.g., Lagrangian submanifold and Schr{\textbackslash}"odinger-Poisson) and the respective techniques for their time evolution and force calculation (Direct summation, mesh techniques, and hierarchical tree methods). We pay attention to the creation of initial conditions and the connection with Lagrangian Perturbation Theory. We then discuss the possible alternatives in terms of the micro-physical properties of dark matter (e.g., neutralinos, warm dark matter, QCD axions, Bose-Einstein condensates, and primordial black holes), and extensions to account for multiple fluids (baryons and neutrinos), primordial non-Gaussianity and modified gravity. We continue by discussing challenges involved in achieving highly accurate predictions. A key aspect of cosmological simulations is the connection to cosmological observables, we discuss various techniques in this regard: structure finding, galaxy formation and baryonic modelling, the creation of emulators and light-cones, and the role of machine learning. We finalise with a recount of state-of-the-art large-scale simulations and conclude with an outlook for the next decade.},
urldate = {2021-12-17},
journal = {arXiv:2112.05165 [astro-ph]},
author = {Angulo, Raul E. and Hahn, Oliver},
month = dec,
year = {2021},
note = {arXiv: 2112.05165},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
}Characterizing protoclusters and protogroups at \${\textbackslash}mathrm\{z {\textbackslash}sim 2.5\}\$ using Lyman-\${\textbackslash}alpha\$ Tomography. Qezlou, M., Newman, A. B., Rudie, G. C., & Bird, S. arXiv:2112.03930 [astro-ph], December, 2021. arXiv: 2112.03930
Paper abstract bibtex
Paper abstract bibtex Ly-\${\textbackslash}alpha\$ tomography surveys have begun to produce three-dimensional (3D) maps of the intergalactic medium (IGM) opacity at \$z {\textbackslash}sim 2.5\$ with Mpc resolution. These surveys provide an exciting new way to discover and characterize high-redshift overdensities, including the progenitors of today's massive groups and clusters of galaxies, known as protogroups and protoclusters. We use the IllustrisTNG-\$300\$ hydrodynamical simulation to build mock maps that realistically mimic those observed in the Ly-\${\textbackslash}alpha\$ Tomographic IMACS Survey (LATIS). We introduce a novel method for delineating the boundaries of structures detected in 3D Ly-\${\textbackslash}alpha\$ flux maps by applying the watershed algorithm. We provide estimators for the dark matter masses of these structures (at \$z{\textbackslash}sim2.5\$), their descendant halo masses at \$z=0\$, and the corresponding uncertainties. We also investigate the completeness of this method for the detection of protogroups and protoclusters. Compared to earlier work, we apply and characterize our method over a wider mass range that extends to massive protogroups. We also assess the widely used fluctuating Gunn-Peterson approximation (FGPA) applied to dark-matter-only simulations; we conclude while it is adequate for estimating the Ly-\${\textbackslash}alpha\$ absorption signal from moderate-to-massive protoclusters (\${\textbackslash}gtrsim 10{\textasciicircum}\{14.2\} {\textbackslash} h{\textasciicircum}\{-1\} M_\{{\textbackslash}odot\}\$), it artificially merges a minority of lower-mass structures with more massive neighbors. Our methods will be applied to current and future Ly-\${\textbackslash}alpha\$ tomography surveys to create catalogs of overdensities and study environment-dependent galaxy evolution in the Cosmic Noon era.
@article{qezlou_characterizing_2021,
title = {Characterizing protoclusters and protogroups at \${\textbackslash}mathrm\{z {\textbackslash}sim 2.5\}\$ using {Lyman}-\${\textbackslash}alpha\$ {Tomography}},
url = {http://arxiv.org/abs/2112.03930},
abstract = {Ly-\${\textbackslash}alpha\$ tomography surveys have begun to produce three-dimensional (3D) maps of the intergalactic medium (IGM) opacity at \$z {\textbackslash}sim 2.5\$ with Mpc resolution. These surveys provide an exciting new way to discover and characterize high-redshift overdensities, including the progenitors of today's massive groups and clusters of galaxies, known as protogroups and protoclusters. We use the IllustrisTNG-\$300\$ hydrodynamical simulation to build mock maps that realistically mimic those observed in the Ly-\${\textbackslash}alpha\$ Tomographic IMACS Survey (LATIS). We introduce a novel method for delineating the boundaries of structures detected in 3D Ly-\${\textbackslash}alpha\$ flux maps by applying the watershed algorithm. We provide estimators for the dark matter masses of these structures (at \$z{\textbackslash}sim2.5\$), their descendant halo masses at \$z=0\$, and the corresponding uncertainties. We also investigate the completeness of this method for the detection of protogroups and protoclusters. Compared to earlier work, we apply and characterize our method over a wider mass range that extends to massive protogroups. We also assess the widely used fluctuating Gunn-Peterson approximation (FGPA) applied to dark-matter-only simulations; we conclude while it is adequate for estimating the Ly-\${\textbackslash}alpha\$ absorption signal from moderate-to-massive protoclusters (\${\textbackslash}gtrsim 10{\textasciicircum}\{14.2\} {\textbackslash} h{\textasciicircum}\{-1\} M\_\{{\textbackslash}odot\}\$), it artificially merges a minority of lower-mass structures with more massive neighbors. Our methods will be applied to current and future Ly-\${\textbackslash}alpha\$ tomography surveys to create catalogs of overdensities and study environment-dependent galaxy evolution in the Cosmic Noon era.},
urldate = {2021-12-17},
journal = {arXiv:2112.03930 [astro-ph]},
author = {Qezlou, Mahdi and Newman, Andrew B. and Rudie, Gwen C. and Bird, Simeon},
month = dec,
year = {2021},
note = {arXiv: 2112.03930},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
}Construct the emission line galaxy-host halo connection through auto and cross correlations. Gao, H., Jing, Y. P., Zheng, Y., & Xu, K. Technical Report November, 2021. Publication Title: arXiv e-prints ADS Bibcode: 2021arXiv211111657G Type: article
Paper abstract bibtex
Paper abstract bibtex We investigate the [O\textbackslash,II] emission line galaxy (ELG)-host halo connection via auto and cross correlations, and propose a concise and effective method to populate ELGs in dark matter halos without assuming a parameterized halo occupation distribution (HOD) model. Using the observational data from VIMOS Public Extragalactic Redshift Survey (VIPERS), we measure the auto and cross correlation functions between ELGs selected by [O\textbackslash,II] luminosity and normal galaxies selected by stellar mass. Combining the stellar-halo mass relation (SHMR) derived for the normal galaxies and the fraction of ELGs observed in the normal galaxy population, we demonstrate that we can establish an accurate ELG-halo connection. With the ELG-halo connection, we can accurately reproduce the auto and cross correlation functions of ELGs and normal galaxies both in real-space and in redshift-space, once the satellite fraction is properly reduced. Our method provides a novel strategy to generate ELG mock catalogs for ongoing and upcoming galaxy redshift surveys. We also provide a simple description for the HOD of ELGs.
@techreport{gao_construct_2021,
title = {Construct the emission line galaxy-host halo connection through auto and cross correlations},
url = {https://ui.adsabs.harvard.edu/abs/2021arXiv211111657G},
abstract = {We investigate the [O{\textbackslash},II] emission line galaxy (ELG)-host halo connection via auto and cross correlations, and propose a concise and effective method to populate ELGs in dark matter halos without assuming a parameterized halo occupation distribution (HOD) model. Using the observational data from VIMOS Public Extragalactic Redshift Survey (VIPERS), we measure the auto and cross correlation functions between ELGs selected by [O{\textbackslash},II] luminosity and normal galaxies selected by stellar mass. Combining the stellar-halo mass relation (SHMR) derived for the normal galaxies and the fraction of ELGs observed in the normal galaxy population, we demonstrate that we can establish an accurate ELG-halo connection. With the ELG-halo connection, we can accurately reproduce the auto and cross correlation functions of ELGs and normal galaxies both in real-space and in redshift-space, once the satellite fraction is properly reduced. Our method provides a novel strategy to generate ELG mock catalogs for ongoing and upcoming galaxy redshift surveys. We also provide a simple description for the HOD of ELGs.},
urldate = {2021-12-17},
author = {Gao, Hongyu and Jing, Y. P. and Zheng, Yun and Xu, Kun},
month = nov,
year = {2021},
note = {Publication Title: arXiv e-prints
ADS Bibcode: 2021arXiv211111657G
Type: article},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
}Geoastronomy: Rocky planets as the Lavosier-Lomonosov Bridge from the non-living to the living world. Mojzsis, S. J. arXiv:2112.04309 [astro-ph], December, 2021. arXiv: 2112.04309
Paper abstract bibtex
Paper abstract bibtex Life on Earth emerged at the interface of the geosphere, hydrosphere and atmosphere. This setting serves as our basis for how biological systems originate on rocky planets. Often overlooked, however, is the fact that the chemical nature of a rocky planet is ultimately a product of galactic chemical evolution. Elemental abundances of the major rock-forming elements can be different for different stars and planets formed at different times in galactic history. These differences mean that we cannot expect small rocky exoplanets to be just like Earth. Furthermore, age of the system dictates starting nuclide inventory from galactic chemical evolution, and past, present and future mantle and crust thermal regimes. The bulk silicate mantle composition of a rocky planet modulates the kind of atmosphere and hydrosphere it possesses. Hence, the ingredients of a rocky planet are as important for its potential to host life as proximity to the so-called habitable zone around a star where liquid water is stable at the surface. To make sense of these variables, a new trans-disciplinary approach is warranted that fuses the disciplines of Geology and Astronomy into what is here termed, Geoastronomy.
@article{mojzsis_geoastronomy_2021,
title = {Geoastronomy: {Rocky} planets as the {Lavosier}-{Lomonosov} {Bridge} from the non-living to the living world},
shorttitle = {Geoastronomy},
url = {http://arxiv.org/abs/2112.04309},
abstract = {Life on Earth emerged at the interface of the geosphere, hydrosphere and atmosphere. This setting serves as our basis for how biological systems originate on rocky planets. Often overlooked, however, is the fact that the chemical nature of a rocky planet is ultimately a product of galactic chemical evolution. Elemental abundances of the major rock-forming elements can be different for different stars and planets formed at different times in galactic history. These differences mean that we cannot expect small rocky exoplanets to be just like Earth. Furthermore, age of the system dictates starting nuclide inventory from galactic chemical evolution, and past, present and future mantle and crust thermal regimes. The bulk silicate mantle composition of a rocky planet modulates the kind of atmosphere and hydrosphere it possesses. Hence, the ingredients of a rocky planet are as important for its potential to host life as proximity to the so-called habitable zone around a star where liquid water is stable at the surface. To make sense of these variables, a new trans-disciplinary approach is warranted that fuses the disciplines of Geology and Astronomy into what is here termed, Geoastronomy.},
urldate = {2021-12-17},
journal = {arXiv:2112.04309 [astro-ph]},
author = {Mojzsis, Stephen J.},
month = dec,
year = {2021},
note = {arXiv: 2112.04309},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics},
}[CII] line intensity mapping the epoch of reionization with the Prime-Cam on FYST. Karoumpis, C., Magnelli, B., Romano-Díaz, E., Haslbauer, M., & Bertoldi, F. arXiv:2111.12847 [astro-ph], November, 2021. arXiv: 2111.12847
Paper abstract bibtex
Paper abstract bibtex We predict the three-dimensional intensity power spectrum (PS) of the [CII] 158\${\textbackslash},{\textbackslash}mu\$m line throughout the epoch of (and post) reionization at redshifts from \${\textbackslash}approx\$ 3.5 to 8. We study the detectability of the PS in a line intensity mapping (LIM) survey with the Fred Young Submillimeter Telescope (FYST). We created mock [CII] tomographic scans in redshift bins at \$z{\textbackslash}approx\$ 3.7, 4.3, 5.8, and 7.4 using the Illustris TNG300-1 \${\textbackslash}Lambda\$CDM simulation and adopting a relation between the star formation activity and the [CII] luminosity (\$L_\{[CII]\}\$) of galaxies. A star formation rate (SFR) was assigned to a dark matter halo in the Illustris simulation in two ways: (i) we adopted the SFR computed in the Illustris simulation and, (ii) we matched the abundance of the halos with the SFR traced by the observed dust-corrected ultraviolet luminosity function of high-redshift galaxies. The \$L_\{[CII]\}\$ is related to the SFR from a semi-analytic model of galaxy formation, from a hydrodynamical simulation of a high-redshift galaxy, or from a high-redshift [CII] galaxy survey. The [CII] intensity PS was computed from mock tomographic scans to assess its detectability with the anticipated observational capability of the FYST. The amplitude of the predicted [CII] intensity power spectrum varies by more than a factor of 10, depending on the choice of the halo-to-galaxy SFR and the SFR-to-\$L_\{[CII]\}\$ relations. In the planned \$4{\textasciicircum}\{{\textbackslash}circ\} {\textbackslash}times 4{\textasciicircum}\{{\textbackslash}circ\}\$ FYST LIM survey, we expect a detection of the [CII] PS up to \$z {\textbackslash}approx\$ 5.8, and potentially even up to \$z {\textbackslash}approx \$ 7.4. The design of the envisioned FYST LIM survey enables a PS measurement not only in small (\textless10 Mpc) shot noise-dominated scales, but also in large (\textgreater50 Mpc) clustering-dominated scales making it the first LIM experiment that will place constraints on the SFR-to-\$L_\{[CII]\}\$ and the halo-to-galaxy SFR relations simultaneously.
@article{karoumpis_cii_2021,
title = {[{CII}] line intensity mapping the epoch of reionization with the {Prime}-{Cam} on {FYST}},
url = {http://arxiv.org/abs/2111.12847},
abstract = {We predict the three-dimensional intensity power spectrum (PS) of the [CII] 158\${\textbackslash},{\textbackslash}mu\$m line throughout the epoch of (and post) reionization at redshifts from \${\textbackslash}approx\$ 3.5 to 8. We study the detectability of the PS in a line intensity mapping (LIM) survey with the Fred Young Submillimeter Telescope (FYST). We created mock [CII] tomographic scans in redshift bins at \$z{\textbackslash}approx\$ 3.7, 4.3, 5.8, and 7.4 using the Illustris TNG300-1 \${\textbackslash}Lambda\$CDM simulation and adopting a relation between the star formation activity and the [CII] luminosity (\$L\_\{[CII]\}\$) of galaxies. A star formation rate (SFR) was assigned to a dark matter halo in the Illustris simulation in two ways: (i) we adopted the SFR computed in the Illustris simulation and, (ii) we matched the abundance of the halos with the SFR traced by the observed dust-corrected ultraviolet luminosity function of high-redshift galaxies. The \$L\_\{[CII]\}\$ is related to the SFR from a semi-analytic model of galaxy formation, from a hydrodynamical simulation of a high-redshift galaxy, or from a high-redshift [CII] galaxy survey. The [CII] intensity PS was computed from mock tomographic scans to assess its detectability with the anticipated observational capability of the FYST. The amplitude of the predicted [CII] intensity power spectrum varies by more than a factor of 10, depending on the choice of the halo-to-galaxy SFR and the SFR-to-\$L\_\{[CII]\}\$ relations. In the planned \$4{\textasciicircum}\{{\textbackslash}circ\} {\textbackslash}times 4{\textasciicircum}\{{\textbackslash}circ\}\$ FYST LIM survey, we expect a detection of the [CII] PS up to \$z {\textbackslash}approx\$ 5.8, and potentially even up to \$z {\textbackslash}approx \$ 7.4. The design of the envisioned FYST LIM survey enables a PS measurement not only in small ({\textless}10 Mpc) shot noise-dominated scales, but also in large ({\textgreater}50 Mpc) clustering-dominated scales making it the first LIM experiment that will place constraints on the SFR-to-\$L\_\{[CII]\}\$ and the halo-to-galaxy SFR relations simultaneously.},
urldate = {2021-12-17},
journal = {arXiv:2111.12847 [astro-ph]},
author = {Karoumpis, C. and Magnelli, B. and Romano-Díaz, E. and Haslbauer, M. and Bertoldi, F.},
month = nov,
year = {2021},
note = {arXiv: 2111.12847},
keywords = {Astrophysics - Astrophysics of Galaxies},
}Quasar UV Luminosity Function at \$3.5{\textless}z{\textless}5.0\$ from SDSS Deep Imaging Data. Pan, Z., Jiang, L., Fan, X., Wu, J., & Yang, J. arXiv:2112.07801 [astro-ph], December, 2021. arXiv: 2112.07801
Paper abstract bibtex
Paper abstract bibtex We present a well-designed sample of more than 1000 type 1 quasars at \$3.5{\textless}z{\textless}5\$ and derive UV quasar luminosity functions (QLFs) in this redshift range. These quasars were selected using the Sloan Digital Sky Survey (SDSS) imaging data in SDSS Stripe 82 and overlap regions with repeat imaging observations. They are about one magnitude fainter than those found using the SDSS single-epoch data. The spectroscopic observations were conducted by the SDSS-III Baryon Oscillation Spectroscopic Survey (BOSS) as one of the BOSS ancillary programs. This quasar sample reaches \$i{\textbackslash}sim21.5\$ mag and bridges previous samples from brighter surveys and deeper surveys. We use a \$1/V_{\textbackslash}mathrm\{a\}\$ method to derive binned QLFs at \$3.6{\textless}z{\textless}4.0\$, \$4.0{\textless}z{\textless}4.5\$, and \$4.5{\textless}z{\textless}4.9\$, and use a double-power law model to parameterize the QLFs. We also combine our data with those in the literature to better constrain the QLFs in the context of a much wider luminosity baseline. We find that the faint-end and bright-end slopes of the QLFs in this redshift range are around \$-1.7\$ and \$-3.7\$, respectively, with uncertainties from 0.2\$-\$0.3 to \${\textgreater}0.5\$. The evolution of the QLFs from \$z{\textbackslash}sim5\$ to \$3.5\$ can be described by a pure density evolution model (\${\textbackslash}propto10{\textasciicircum}\{kz\}\$) and the parameter \$k\$ is similar to that at \$5{\textless}z{\textless}7\$, suggesting a nearly uniform evolution of the quasar density at \$z=3.5-7\$.
@article{pan_quasar_2021,
title = {Quasar {UV} {Luminosity} {Function} at \$3.5{\textless}z{\textless}5.0\$ from {SDSS} {Deep} {Imaging} {Data}},
url = {http://arxiv.org/abs/2112.07801},
abstract = {We present a well-designed sample of more than 1000 type 1 quasars at \$3.5{\textless}z{\textless}5\$ and derive UV quasar luminosity functions (QLFs) in this redshift range. These quasars were selected using the Sloan Digital Sky Survey (SDSS) imaging data in SDSS Stripe 82 and overlap regions with repeat imaging observations. They are about one magnitude fainter than those found using the SDSS single-epoch data. The spectroscopic observations were conducted by the SDSS-III Baryon Oscillation Spectroscopic Survey (BOSS) as one of the BOSS ancillary programs. This quasar sample reaches \$i{\textbackslash}sim21.5\$ mag and bridges previous samples from brighter surveys and deeper surveys. We use a \$1/V\_{\textbackslash}mathrm\{a\}\$ method to derive binned QLFs at \$3.6{\textless}z{\textless}4.0\$, \$4.0{\textless}z{\textless}4.5\$, and \$4.5{\textless}z{\textless}4.9\$, and use a double-power law model to parameterize the QLFs. We also combine our data with those in the literature to better constrain the QLFs in the context of a much wider luminosity baseline. We find that the faint-end and bright-end slopes of the QLFs in this redshift range are around \$-1.7\$ and \$-3.7\$, respectively, with uncertainties from 0.2\$-\$0.3 to \${\textgreater}0.5\$. The evolution of the QLFs from \$z{\textbackslash}sim5\$ to \$3.5\$ can be described by a pure density evolution model (\${\textbackslash}propto10{\textasciicircum}\{kz\}\$) and the parameter \$k\$ is similar to that at \$5{\textless}z{\textless}7\$, suggesting a nearly uniform evolution of the quasar density at \$z=3.5-7\$.},
urldate = {2021-12-17},
journal = {arXiv:2112.07801 [astro-ph]},
author = {Pan, Zhiwei and Jiang, Linhua and Fan, Xiaohui and Wu, Jin and Yang, Jinyi},
month = dec,
year = {2021},
note = {arXiv: 2112.07801},
keywords = {Astrophysics - Astrophysics of Galaxies},
}Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs). XVI. 69 New Quasars at 5.8 \textless z \textless 7.0. Matsuoka, Y., Iwasawa, K., Onoue, M., Izumi, T., Kashikawa, N., Strauss, M. A., Imanishi, M., Nagao, T., Akiyama, M., Silverman, J. D., Asami, N., Bosch, J., Furusawa, H., Goto, T., Gunn, J. E., Harikane, Y., Ikeda, H., Ishimoto, R., Kawaguchi, T., Kato, N., Kikuta, S., Kohno, K., Komiyama, Y., Lee, C., Lupton, R. H., Minezaki, T., Miyazaki, S., Murayama, H., Nishizawa, A. J., Oguri, M., Ono, Y., Ouchi, M., Price, P. A., Sameshima, H., Sugiyama, N., Tait, P. J., Takada, M., Takahashi, A., Takata, T., Tanaka, M., Toba, Y., Utsumi, Y., Wang, S., & Yamashita, T. arXiv:2111.12766 [astro-ph], November, 2021. arXiv: 2111.12766
Paper abstract bibtex
Paper abstract bibtex We present the spectroscopic discovery of 69 quasars at 5.8 \textless z \textless 7.0, drawn from the Hyper Suprime-Cam (HSC) Subaru Strategic Program (SSP) imaging survey data. This is the 16th publication from the Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs) project, and completes identification of all but the faintest candidates (i.e., i-band dropouts with zAB \textless 24 and y-band detections, and z-band dropouts with yAB \textless 24) with Bayesian quasar probability Pq \textgreater 0.1 in the HSC-SSP third public data release (PDR3). The sample reported here also includes three quasars with Pq \textless 0.1 at z \textasciitilde 6.6, which we selected in an effort to completely cover the reddest point sources with simple color cuts. The number of high-z quasars discovered in SHELLQs has now grown to 162, including 23 type-II quasar candidates. This paper also presents identification of seven galaxies at 5.6 \textless z \textless 6.7, an [O III] emitter at z = 0.954, and 31 Galactic cool stars and brown dwarfs. High-z quasars and galaxies comprise 75 % and 16 % respectively of all the spectroscopic SHELLQs objects that pass our latest selection algorithm with the PDR3 photometry. That is, a total of 91 % of the objects lie at z \textgreater 5.6. This demonstrates that the algorithm has very high efficiency, even though we are probing an unprecedentedly low-luminosity population down to M1450 \textasciitilde -21 mag.
@article{matsuoka_subaru_2021,
title = {Subaru {High}-z {Exploration} of {Low}-{Luminosity} {Quasars} ({SHELLQs}). {XVI}. 69 {New} {Quasars} at 5.8 {\textless} z {\textless} 7.0},
url = {http://arxiv.org/abs/2111.12766},
abstract = {We present the spectroscopic discovery of 69 quasars at 5.8 {\textless} z {\textless} 7.0, drawn from the Hyper Suprime-Cam (HSC) Subaru Strategic Program (SSP) imaging survey data. This is the 16th publication from the Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs) project, and completes identification of all but the faintest candidates (i.e., i-band dropouts with zAB {\textless} 24 and y-band detections, and z-band dropouts with yAB {\textless} 24) with Bayesian quasar probability Pq {\textgreater} 0.1 in the HSC-SSP third public data release (PDR3). The sample reported here also includes three quasars with Pq {\textless} 0.1 at z {\textasciitilde} 6.6, which we selected in an effort to completely cover the reddest point sources with simple color cuts. The number of high-z quasars discovered in SHELLQs has now grown to 162, including 23 type-II quasar candidates. This paper also presents identification of seven galaxies at 5.6 {\textless} z {\textless} 6.7, an [O III] emitter at z = 0.954, and 31 Galactic cool stars and brown dwarfs. High-z quasars and galaxies comprise 75 \% and 16 \% respectively of all the spectroscopic SHELLQs objects that pass our latest selection algorithm with the PDR3 photometry. That is, a total of 91 \% of the objects lie at z {\textgreater} 5.6. This demonstrates that the algorithm has very high efficiency, even though we are probing an unprecedentedly low-luminosity population down to M1450 {\textasciitilde} -21 mag.},
urldate = {2021-12-17},
journal = {arXiv:2111.12766 [astro-ph]},
author = {Matsuoka, Yoshiki and Iwasawa, Kazushi and Onoue, Masafusa and Izumi, Takuma and Kashikawa, Nobunari and Strauss, Michael A. and Imanishi, Masatoshi and Nagao, Tohru and Akiyama, Masayuki and Silverman, John D. and Asami, Naoko and Bosch, James and Furusawa, Hisanori and Goto, Tomotsugu and Gunn, James E. and Harikane, Yuichi and Ikeda, Hiroyuki and Ishimoto, Rikako and Kawaguchi, Toshihiro and Kato, Nanako and Kikuta, Satoshi and Kohno, Kotaro and Komiyama, Yutaka and Lee, Chien-Hsiu and Lupton, Robert H. and Minezaki, Takeo and Miyazaki, Satoshi and Murayama, Hitoshi and Nishizawa, Atsushi J. and Oguri, Masamune and Ono, Yoshiaki and Ouchi, Masami and Price, Paul A. and Sameshima, Hiroaki and Sugiyama, Naoshi and Tait, Philip J. and Takada, Masahiro and Takahashi, Ayumi and Takata, Tadafumi and Tanaka, Masayuki and Toba, Yoshiki and Utsumi, Yousuke and Wang, Shiang-Yu and Yamashita, Takuji},
month = nov,
year = {2021},
note = {arXiv: 2111.12766},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
}The galaxy-halo size relation of low-mass galaxies in FIRE. Rohr, E., Feldmann, R., Bullock, J., Çatmabacak, O., Boylan-Kolchin, M., Faucher-Giguère, C., Kereš, D., Liang, L., Moreno, J., & Wetzel, A. arXiv:2112.05159 [astro-ph], December, 2021. arXiv: 2112.05159
Paper abstract bibtex
Paper abstract bibtex Galaxy sizes correlate closely with the sizes of their parent dark matter haloes, suggesting a link between halo formation and galaxy growth. However, the precise nature of this relation and its scatter remains to be understood fully, especially for low-mass galaxies. We analyse the galaxy-halo size relation for low-mass (\$M_{\textbackslash}star {\textbackslash}sim 10{\textasciicircum}\{7-9\} \{{\textbackslash}rm M_{\textbackslash}odot\}\$) central galaxies over the past 12.5 billion years with the help of cosmological volume simulations (FIREbox) from the Feedback in Realistic Environments (FIRE) project. We find a nearly linear relationship between the half-stellar mass galaxy size \$R_\{1/2\}\$ and the parent dark matter halo virial radius \$R_\{{\textbackslash}rm vir\}\$. This relation evolves only weakly since redshift \$z = 5\$: \$R_\{1/2\} \{{\textbackslash}rm kpc\} = (0.053{\textbackslash}pm0.002)(R_\{{\textbackslash}rm vir\}/35 \{{\textbackslash}rm kpc\}){\textasciicircum}\{0.934{\textbackslash}pm0.054\}\$, with a nearly constant scatter \${\textbackslash}langle {\textbackslash}sigma {\textbackslash}rangle = 0.084 [\{{\textbackslash}rm dex\}]\$. Whilst this ratio is similar to what is expected from models where galaxy disc sizes are set by halo angular momentum, the low-mass galaxies in our sample are not angular momentum supported, with stellar rotational to circular velocity ratios \$v_\{{\textbackslash}rm rot\} / v_\{{\textbackslash}rm circ\} {\textbackslash}sim 0.15\$. Introducing redshift as another parameter to the GHSR does not decrease the scatter. Furthermore, this scatter does not correlate with any of the halo properties we investigate – including spin and concentration – suggesting that baryonic processes and feedback physics are instead critical in setting the scatter in the galaxy-halo size relation. Given the relatively small scatter and the weak dependence of the galaxy-halo size relation on redshift and halo properties for these low-mass central galaxies, we propose using galaxy sizes as an independent method from stellar masses to infer halo masses.
@article{rohr_galaxy-halo_2021,
title = {The galaxy-halo size relation of low-mass galaxies in {FIRE}},
url = {http://arxiv.org/abs/2112.05159},
abstract = {Galaxy sizes correlate closely with the sizes of their parent dark matter haloes, suggesting a link between halo formation and galaxy growth. However, the precise nature of this relation and its scatter remains to be understood fully, especially for low-mass galaxies. We analyse the galaxy-halo size relation for low-mass (\$M\_{\textbackslash}star {\textbackslash}sim 10{\textasciicircum}\{7-9\} \{{\textbackslash}rm M\_{\textbackslash}odot\}\$) central galaxies over the past 12.5 billion years with the help of cosmological volume simulations (FIREbox) from the Feedback in Realistic Environments (FIRE) project. We find a nearly linear relationship between the half-stellar mass galaxy size \$R\_\{1/2\}\$ and the parent dark matter halo virial radius \$R\_\{{\textbackslash}rm vir\}\$. This relation evolves only weakly since redshift \$z = 5\$: \$R\_\{1/2\} \{{\textbackslash}rm kpc\} = (0.053{\textbackslash}pm0.002)(R\_\{{\textbackslash}rm vir\}/35 \{{\textbackslash}rm kpc\}){\textasciicircum}\{0.934{\textbackslash}pm0.054\}\$, with a nearly constant scatter \${\textbackslash}langle {\textbackslash}sigma {\textbackslash}rangle = 0.084 [\{{\textbackslash}rm dex\}]\$. Whilst this ratio is similar to what is expected from models where galaxy disc sizes are set by halo angular momentum, the low-mass galaxies in our sample are not angular momentum supported, with stellar rotational to circular velocity ratios \$v\_\{{\textbackslash}rm rot\} / v\_\{{\textbackslash}rm circ\} {\textbackslash}sim 0.15\$. Introducing redshift as another parameter to the GHSR does not decrease the scatter. Furthermore, this scatter does not correlate with any of the halo properties we investigate -- including spin and concentration -- suggesting that baryonic processes and feedback physics are instead critical in setting the scatter in the galaxy-halo size relation. Given the relatively small scatter and the weak dependence of the galaxy-halo size relation on redshift and halo properties for these low-mass central galaxies, we propose using galaxy sizes as an independent method from stellar masses to infer halo masses.},
urldate = {2021-12-17},
journal = {arXiv:2112.05159 [astro-ph]},
author = {Rohr, Eric and Feldmann, Robert and Bullock, James and Çatmabacak, Onur and Boylan-Kolchin, Michael and Faucher-Giguère, Claude-André and Kereš, Dušan and Liang, Lichen and Moreno, Jorge and Wetzel, Andrew},
month = dec,
year = {2021},
note = {arXiv: 2112.05159},
keywords = {Astrophysics - Astrophysics of Galaxies},
}2020 (13)
Endpoint of the up-down instability in precessing binary black holes. Mould, M. & Gerosa, D. Physical Review D, 101(12):124037, June, 2020.
doi bibtex
doi bibtex
@article{2020PhRvD.101l4037M,
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
adsurl = {https://ui.adsabs.harvard.edu/abs/2020PhRvD.101l4037M},
archiveprefix = {arXiv},
author = {{Mould}, Matthew and {Gerosa}, Davide},
doi = {10.1103/PhysRevD.101.124037},
eid = {124037},
eprint = {2003.02281},
journal = {Physical Review D},
keywords = {General Relativity and Quantum Cosmology, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena},
month = jun,
number = {12},
pages = {124037},
primaryclass = {gr-qc},
title = {{Endpoint of the up-down instability in precessing binary black holes}},
volume = {101},
year = 2020,
bdsk-url-1 = {https://doi.org/10.1103/PhysRevD.101.124037}}Milky Way Satellites Shining Bright in Gravitational Waves. Roebber, E., Buscicchio, R., Vecchio, A., Moore, C. J., Klein, A., Korol, V., Toonen, S., Gerosa, D., Goldstein, J., Gaebel, S. M., & Woods, T. E. Astrophysical Journal, 894(2):L15, May, 2020.
doi bibtex
doi bibtex
@article{2020ApJ...894L..15R,
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
adsurl = {https://ui.adsabs.harvard.edu/abs/2020ApJ...894L..15R},
archiveprefix = {arXiv},
author = {{Roebber}, Elinore and {Buscicchio}, Riccardo and {Vecchio}, Alberto and {Moore}, Christopher J. and {Klein}, Antoine and {Korol}, Valeriya and {Toonen}, Silvia and {Gerosa}, Davide and {Goldstein}, Janna and {Gaebel}, Sebastian M. and {Woods}, Tyrone E.},
doi = {10.3847/2041-8213/ab8ac9},
eid = {L15},
eprint = {2002.10465},
journal = {Astrophysical Journal},
keywords = {675, 1799, 990, 416, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics, General Relativity and Quantum Cosmology},
month = may,
number = {2},
pages = {L15},
primaryclass = {astro-ph.GA},
title = {{Milky Way Satellites Shining Bright in Gravitational Waves}},
volume = {894},
year = 2020,
bdsk-url-1 = {https://doi.org/10.3847/2041-8213/ab8ac9}}Populations of double white dwarfs in Milky Way satellites and their detectability with LISA. Korol, V., Toonen, S., Klein, A., Belokurov, V., Vincenzo, F., Buscicchio, R., Gerosa, D., Moore, C., Roebber, E., Rossi, E., & Vecchio, A. Astronomy & Astrophysics, 638:A153, June, 2020.
doi bibtex
doi bibtex
@article{2020A&A...638A.153K,
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
adsurl = {https://ui.adsabs.harvard.edu/abs/2020A&A...638A.153K},
archiveprefix = {arXiv},
author = {{Korol}, V. and {Toonen}, S. and {Klein}, A. and {Belokurov}, V. and {Vincenzo}, F. and {Buscicchio}, R. and {Gerosa}, D. and {Moore}, C.~J. and {Roebber}, E. and {Rossi}, E.~M. and {Vecchio}, A.},
doi = {10.1051/0004-6361/202037764},
eid = {A153},
eprint = {2002.10462},
journal = {Astronomy & Astrophysics},
keywords = {gravitational waves, binaries: close, white dwarfs, galaxies: dwarf, Local Group, Magellanic Clouds, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics, General Relativity and Quantum Cosmology},
month = jun,
pages = {A153},
primaryclass = {astro-ph.GA},
title = {{Populations of double white dwarfs in Milky Way satellites and their detectability with LISA}},
volume = {638},
year = 2020,
bdsk-url-1 = {https://doi.org/10.1051/0004-6361/202037764}}The Bardeen-Petterson effect in accreting supermassive black hole binaries: a systematic approach. Gerosa, D., Rosotti, G., & Barbieri, R. Monthly Notices of the Royal Astronomical Society, 496(3):3060-3075, August, 2020.
doi bibtex
doi bibtex
@article{2020MNRAS.496.3060G,
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
adsurl = {https://ui.adsabs.harvard.edu/abs/2020MNRAS.496.3060G},
archiveprefix = {arXiv},
author = {{Gerosa}, Davide and {Rosotti}, Giovanni and {Barbieri}, Riccardo},
doi = {10.1093/mnras/staa1693},
eprint = {2004.02894},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {accretion discs, Accretion, black hole mergers, Gravitational waves, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology},
month = aug,
number = {3},
pages = {3060-3075},
primaryclass = {astro-ph.GA},
title = {{The Bardeen-Petterson effect in accreting supermassive black hole binaries: a systematic approach}},
volume = {496},
year = 2020,
bdsk-url-1 = {https://doi.org/10.1093/mnras/staa1693}}Mapping the asymptotic inspiral of precessing binary black holes to their merger remnants. Reali, L., Mould, M., Gerosa, D., & Varma, V. Classical and Quantum Gravity, 37(22):225005, November, 2020.
doi bibtex
doi bibtex
@article{2020CQGra..37v5005R,
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
adsurl = {https://ui.adsabs.harvard.edu/abs/2020CQGra..37v5005R},
archiveprefix = {arXiv},
author = {{Reali}, Luca and {Mould}, Matthew and {Gerosa}, Davide and {Varma}, Vijay},
doi = {10.1088/1361-6382/abb639},
eid = {225005},
eprint = {2005.01747},
journal = {Classical and Quantum Gravity},
keywords = {black holes, gravitational waves, numerical relativity, relativistic astrophysics, General Relativity and Quantum Cosmology, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena},
month = nov,
number = {22},
pages = {225005},
primaryclass = {gr-qc},
title = {{Mapping the asymptotic inspiral of precessing binary black holes to their merger remnants}},
volume = {37},
year = 2020,
bdsk-url-1 = {https://doi.org/10.1088/1361-6382/abb639}}Considerations for the Observability of Kinematically Offset Binary AGN. Kelley, L. Z. arXiv:2005.10255 [astro-ph], May, 2020. arXiv: 2005.10255
Paper abstract bibtex
Paper abstract bibtex The gravitational waves from Massive black-hole (MBH) binaries are expected to be detected by pulsar timing arrays in the next few years. While they are a promising source for multimessenger observations as binary AGN, few convincing candidates have been identified in electromagnetic surveys. One approach to identifying candidates has been through spectroscopic surveys searching for offsets or time-dependent offsets of broad emission lines (BLs), which may be characteristic of Doppler shifts from binary orbital motion. In this study, we predict the parameter space of MBH binaries that should be kinematically detectable. There is a delicate trade-off between requiring binary separations to be large enough for BL regions to remain attached to one of the AGN, but also small enough such that their orbital velocity is detectable. We find that kinematic signatures are only observable for the lower-mass secondary AGN, for binaries with total-masses above about $10{\textasciicircum}8 M_{\}odot$, and separations between 0.1 and 1 pc. We motivate our usage of a kinematic-offset sensitivity of $10{\textasciicircum}3$ km/s, and a sensitivity to changing offsets of $10{\textasciicircum}2$ km/s. With these parameters, and an Eddington ratio of 0.1, we find that 0.5% of binaries have detectable offsets, and only 0.03% have detectable velocity changes. Overall, kinematic binary signatures should be expected in fewer than one in $10{\textasciicircum}4$ AGN. Better characterizing the intrinsic variability of BLs is crucial to understanding and vetting MBH binary candidates. This requires multi-epoch spectroscopy of large populations of AGN over a variety of timescales.
@article{kelley_considerations_2020,
title = {Considerations for the {Observability} of {Kinematically} {Offset} {Binary} {AGN}},
url = {http://arxiv.org/abs/2005.10255},
abstract = {The gravitational waves from Massive black-hole (MBH) binaries are expected to be detected by pulsar timing arrays in the next few years. While they are a promising source for multimessenger observations as binary AGN, few convincing candidates have been identified in electromagnetic surveys. One approach to identifying candidates has been through spectroscopic surveys searching for offsets or time-dependent offsets of broad emission lines (BLs), which may be characteristic of Doppler shifts from binary orbital motion. In this study, we predict the parameter space of MBH binaries that should be kinematically detectable. There is a delicate trade-off between requiring binary separations to be large enough for BL regions to remain attached to one of the AGN, but also small enough such that their orbital velocity is detectable. We find that kinematic signatures are only observable for the lower-mass secondary AGN, for binaries with total-masses above about \$10{\textasciicircum}8 M\_{\textbackslash}odot\$, and separations between 0.1 and 1 pc. We motivate our usage of a kinematic-offset sensitivity of \$10{\textasciicircum}3\$ km/s, and a sensitivity to changing offsets of \$10{\textasciicircum}2\$ km/s. With these parameters, and an Eddington ratio of 0.1, we find that 0.5\% of binaries have detectable offsets, and only 0.03\% have detectable velocity changes. Overall, kinematic binary signatures should be expected in fewer than one in \$10{\textasciicircum}4\$ AGN. Better characterizing the intrinsic variability of BLs is crucial to understanding and vetting MBH binary candidates. This requires multi-epoch spectroscopy of large populations of AGN over a variety of timescales.},
urldate = {2020-05-26},
journal = {arXiv:2005.10255 [astro-ph]},
author = {Kelley, Luke Zoltan},
month = may,
year = {2020},
note = {arXiv: 2005.10255},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena, mentions sympy},
}The halo of M105 and its group environment as traced by planetary nebula populations: I. Wide-field photometric survey of planetary nebulae in the Leo I group. Hartke, J., Arnaboldi, M., Gerhard, O., Coccato, L., Pulsoni, C., Freeman, K. C., Merrifield, M., Cortesi, A., & Kuijken, K. arXiv:2008.01696 [astro-ph], August, 2020. arXiv: 2008.01696
Paper abstract bibtex
Paper abstract bibtex M105 (NGC 3379) is an early-type galaxy in the Leo I group. This group is the nearest group that contains all main galaxy types and can thus be used as a benchmark to study the properties of the intra-group light (IGL) in low-mass groups. We use PNe as discrete stellar tracers of the diffuse light around M105. PNe were identified on the basis of their bright [OIII]5007 AA emission and the absence of a broad-band continuum. We compare the PN number density profile with the galaxy surface-brightness profile decomposed into metallicity components using published HST photometry in two halo fields. We identify 226 PNe candidates within a limiting magnitude of mlim = 28.1 from our Subaru-SuprimeCam imaging, covering 67.6 kpc along the major axis of M105 and the halos of NGC 3384 and NGC 3398. We find an excess of PNe at large radii compared to the stellar surface brightness profile from broad-band surveys. This excess is related to a variation in the luminosity-specific PN number ${\}alpha$ with radius. The ${\}alpha$-parameter value of the extended halo is more than 7 times higher than that of the inner halo. We also measure an increase in the slope of the PN luminosity function at fainter magnitudes with radius. We infer that the radial variation of the PN population properties is due to a diffuse population of metal-poor stars ([M/H] \textless -1.0) following an exponential profile, in addition to the M105 halo. The spatial coincidence between the number density profile of these metal-poor stars and the increase in the ${\}alpha$-parameter value with radius establishes the missing link between metallicity and the post-AGB phases of stellar evolution. We estimate that the total bolometric luminosity associated with the exponential IGL population is 2.04x10\textasciicircum9 Lsun as a lower limit, corresponding to an IGL fraction of 3.8%. This work sets the stage for kinematic studies of the IGL in low-mass groups.
@article{hartke_halo_2020,
title = {The halo of {M105} and its group environment as traced by planetary nebula populations: {I}. {Wide}-field photometric survey of planetary nebulae in the {Leo} {I} group},
shorttitle = {The halo of {M105} and its group environment as traced by planetary nebula populations},
url = {http://arxiv.org/abs/2008.01696},
abstract = {M105 (NGC 3379) is an early-type galaxy in the Leo I group. This group is the nearest group that contains all main galaxy types and can thus be used as a benchmark to study the properties of the intra-group light (IGL) in low-mass groups. We use PNe as discrete stellar tracers of the diffuse light around M105. PNe were identified on the basis of their bright [OIII]5007 AA emission and the absence of a broad-band continuum. We compare the PN number density profile with the galaxy surface-brightness profile decomposed into metallicity components using published HST photometry in two halo fields. We identify 226 PNe candidates within a limiting magnitude of mlim = 28.1 from our Subaru-SuprimeCam imaging, covering 67.6 kpc along the major axis of M105 and the halos of NGC 3384 and NGC 3398. We find an excess of PNe at large radii compared to the stellar surface brightness profile from broad-band surveys. This excess is related to a variation in the luminosity-specific PN number \${\textbackslash}alpha\$ with radius. The \${\textbackslash}alpha\$-parameter value of the extended halo is more than 7 times higher than that of the inner halo. We also measure an increase in the slope of the PN luminosity function at fainter magnitudes with radius. We infer that the radial variation of the PN population properties is due to a diffuse population of metal-poor stars ([M/H] {\textless} -1.0) following an exponential profile, in addition to the M105 halo. The spatial coincidence between the number density profile of these metal-poor stars and the increase in the \${\textbackslash}alpha\$-parameter value with radius establishes the missing link between metallicity and the post-AGB phases of stellar evolution. We estimate that the total bolometric luminosity associated with the exponential IGL population is 2.04x10{\textasciicircum}9 Lsun as a lower limit, corresponding to an IGL fraction of 3.8\%. This work sets the stage for kinematic studies of the IGL in low-mass groups.},
urldate = {2020-08-07},
journal = {arXiv:2008.01696 [astro-ph]},
author = {Hartke, J. and Arnaboldi, M. and Gerhard, O. and Coccato, L. and Pulsoni, C. and Freeman, K. C. and Merrifield, M. and Cortesi, A. and Kuijken, K.},
month = aug,
year = {2020},
note = {arXiv: 2008.01696},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics, astrophysics, mentions sympy},
}Magnetism Science with the Square Kilometre Array. Heald, G., Mao, S., Vacca, V., Akahori, T., Damas-Segovia, A., Gaensler, B., Hoeft, M., Agudo, I., Basu, A., Beck, R., Birkinshaw, M., Bonafede, A., Bourke, T., Bracco, A., Carretti, E., Feretti, L., Girart, J., Govoni, F., Green, J., Han, J., Haverkorn, M., Horellou, C., Johnston-Hollitt, M., Kothes, R., Landecker, T., Nikiel-Wroczyński, B., O'Sullivan, S., Padovani, M., Poidevin, F., Pratley, L., Regis, M., Riseley, C., Robishaw, T., Rudnick, L., Sobey, C., Stil, J., Sun, X., Sur, S., Taylor, A., Thomson, A., Van Eck, C., Vazza, F., West, J., & SKA Magnetism Science Working Group Galaxies, 8(3):53, July, 2020.
doi bibtex
doi bibtex
@ARTICLE{2020Galax...8...53H,
author = {{Heald}, George and {Mao}, Sui and {Vacca}, Valentina and {Akahori}, Takuya and {Damas-Segovia}, Ancor and {Gaensler}, Bryan and {Hoeft}, Matthias and {Agudo}, Ivan and {Basu}, Aritra and {Beck}, Rainer and {Birkinshaw}, Mark and {Bonafede}, Annalisa and {Bourke}, Tyler and {Bracco}, Andrea and {Carretti}, Ettore and {Feretti}, Luigina and {Girart}, J. and {Govoni}, Federica and {Green}, James and {Han}, JinLin and {Haverkorn}, Marijke and {Horellou}, Cathy and {Johnston-Hollitt}, Melanie and {Kothes}, Roland and {Landecker}, Tom and {Nikiel-Wroczy{\'n}ski}, B{\l}a{\.z}ej and {O'Sullivan}, Shane and {Padovani}, Marco and {Poidevin}, Fr{\'e}d{\'e}rick and {Pratley}, Luke and {Regis}, Marco and {Riseley}, Christopher and {Robishaw}, Tim and {Rudnick}, Lawrence and {Sobey}, Charlotte and {Stil}, Jeroen and {Sun}, Xiaohui and {Sur}, Sharanya and {Taylor}, A. and {Thomson}, Alec and {Van Eck}, Cameron and {Vazza}, Franco and {West}, Jennifer and {SKA Magnetism Science Working Group}},
title = "{Magnetism Science with the Square Kilometre Array}",
journal = {Galaxies},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics},
year = 2020,
month = jul,
volume = {8},
number = {3},
pages = {53},
doi = {10.3390/galaxies8030053},
archivePrefix = {arXiv},
eprint = {2006.03172},
primaryClass = {astro-ph.GA},
adsurl = {https://ui.adsabs.harvard.edu/abs/2020Galax...8...53H},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}Radial Star Formation Histories in 32 Nearby Galaxies. Dale, D. A., Anderson, K. R., Bran, L. M., Cox, I. S., Drake, C. L., Lee, N. J., Pilawa, J. D., Alexander Slane, F., Soto, S., Jensen, E. I., Sutter, J. S., Turner, J. A., & Kobulnicky, H. A. \aj, 159(5):195, May, 2020.
doi bibtex
doi bibtex
@ARTICLE{2020AJ....159..195D,
author = {{Dale}, Daniel A. and {Anderson}, Kristin R. and {Bran}, Louis M. and {Cox}, Isaiah S. and {Drake}, Carolyn L. and {Lee}, Nathan J. and {Pilawa}, Jacob D. and {Alexander Slane}, F. and {Soto}, Susana and {Jensen}, Emily I. and {Sutter}, Jessica S. and {Turner}, Jordan A. and {Kobulnicky}, Henry A.},
title = "{Radial Star Formation Histories in 32 Nearby Galaxies}",
journal = {\aj},
keywords = {576, 594, 598, Astrophysics - Astrophysics of Galaxies},
year = 2020,
month = may,
volume = {159},
number = {5},
eid = {195},
pages = {195},
doi = {10.3847/1538-3881/ab7eb2},
archivePrefix = {arXiv},
eprint = {2003.10260},
primaryClass = {astro-ph.GA},
adsurl = {https://ui.adsabs.harvard.edu/abs/2020AJ....159..195D},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}CS Cha B: A disc-obscured M-type star mimicking a polarised planetary companion. Haffert, S., van Holstein , R., Ginski, C., Brinchmann, J., Snellen, I., Milli, J., Stolker, T., Keller, C., & Girard, J. åp, 640:L12, August, 2020.
doi bibtex
doi bibtex
@ARTICLE{2020A&A...640L..12H,
author = {{Haffert}, S.~Y. and {van Holstein}, R.~G. and {Ginski}, C. and {Brinchmann}, J. and {Snellen}, I.~A.~G. and {Milli}, J. and {Stolker}, T. and {Keller}, C.~U. and {Girard}, J.},
title = "{CS Cha B: A disc-obscured M-type star mimicking a polarised planetary companion}",
journal = {\aap},
keywords = {planets and satellites: individual: CS Cha B, stars: low-mass, accretion, accretion disks, stars: winds, outflows, techniques: imaging spectroscopy, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics},
year = 2020,
month = aug,
volume = {640},
eid = {L12},
pages = {L12},
doi = {10.1051/0004-6361/202038706},
archivePrefix = {arXiv},
eprint = {2007.07831},
primaryClass = {astro-ph.EP},
adsurl = {https://ui.adsabs.harvard.edu/abs/2020A&A...640L..12H},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}Early formation and recent starburst activity in the nuclear disk of the Milky Way. Nogueras-Lara, F., Schödel, R., Gallego-Calvente, A. T., Gallego-Cano, E., Shahzamanian, B., Dong, H., Neumayer, N., Hilker, M., Najarro, F., Nishiyama, S., Feldmeier-Krause, A., Girard, J. H., & Cassisi, S. Nature Astronomy, 4:377-381, January, 2020.
doi bibtex
doi bibtex
@ARTICLE{2020NatAs...4..377N,
author = {{Nogueras-Lara}, Francisco and {Sch{\"o}del}, Rainer and {Gallego-Calvente}, Aurelia Teresa and {Gallego-Cano}, Eulalia and {Shahzamanian}, Banafsheh and {Dong}, Hui and {Neumayer}, Nadine and {Hilker}, Michael and {Najarro}, Francisco and {Nishiyama}, Shogo and {Feldmeier-Krause}, Anja and {Girard}, Julien H.~V. and {Cassisi}, Santi},
title = "{Early formation and recent starburst activity in the nuclear disk of the Milky Way}",
journal = {Nature Astronomy},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics},
year = 2020,
month = jan,
volume = {4},
pages = {377-381},
doi = {10.1038/s41550-019-0967-9},
archivePrefix = {arXiv},
eprint = {1910.06968},
primaryClass = {astro-ph.GA},
adsurl = {https://ui.adsabs.harvard.edu/abs/2020NatAs...4..377N},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}Debunking Generalization Error or: How I Learned to Stop Worrying and Love My Training Set. Acquaviva, V., Lovell, C., & Ishida, E. NeurIPS workshop `Machine Learning and the Physical Sciences', November, 2020.
Paper abstract bibtex
Paper abstract bibtex We aim to determine some physical properties of distant galaxies (for example, stellar mass, star formation history, or chemical enrichment history) from their observed spectra, using supervised machine learning methods. We know that different astrophysical processes leave their imprint in various regions of the spectra with characteristic signatures. Unfortunately, identifying a training set for this problem is very hard, because labels are not readily available - we have no way of knowing the true history of how galaxies have formed. One possible approach to this problem is to train machine learning models on state-of-the-art cosmological simulations. However, when algorithms are trained on the simulations, it is unclear how well they will perform once applied to real data. In this paper, we attempt to model the generalization error as a function of an appropriate measure of distance between the source domain and the application domain. Our goal is to obtain a reliable estimate of how a model trained on simulations might behave on data.
@article{acquaviva_debunking_2020,
title = {Debunking {Generalization} {Error} or: {How} {I} {Learned} to {Stop} {Worrying} and {Love} {My} {Training} {Set}},
shorttitle = {Debunking {Generalization} {Error}},
url = {http://adsabs.harvard.edu/abs/2020arXiv201200066A},
abstract = {We aim to determine some physical properties of distant galaxies (for
example, stellar mass, star formation history, or chemical enrichment
history) from their observed spectra, using supervised machine learning
methods. We know that different astrophysical processes leave their
imprint in various regions of the spectra with characteristic
signatures. Unfortunately, identifying a training set for this problem
is very hard, because labels are not readily available - we have no way
of knowing the true history of how galaxies have formed. One possible
approach to this problem is to train machine learning models on
state-of-the-art cosmological simulations. However, when algorithms are
trained on the simulations, it is unclear how well they will perform
once applied to real data. In this paper, we attempt to model the
generalization error as a function of an appropriate measure of distance
between the source domain and the application domain. Our goal is to
obtain a reliable estimate of how a model trained on simulations might
behave on data.},
urldate = {2020-12-02},
journal = {NeurIPS workshop `Machine Learning and the Physical Sciences'},
author = {Acquaviva, Viviana and Lovell, Chistopher and Ishida, Emille},
month = nov,
year = {2020},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics},
}Nebular-line emission during the Epoch of Reionization. Wilkins, S. M., Lovell, C. C., Fairhurst, C., Feng, Y., Matteo, T. D., Croft, R., Kuusisto, J., Vijayan, A. P., & Thomas, P. Monthly Notices of the Royal Astronomical Society, 493:6079–6094, March, 2020.
Paper doi abstract bibtex
Paper doi abstract bibtex Nebular emission lines associated with galactic H II regions carry information about both physical properties of the ionized gas and the source of ionizing photons as well as providing the opportunity of measuring accurate redshifts and thus distances once a cosmological model is assumed. While nebular-line emission has been extensively studied at lower redshift there are currently only few constraints within the epoch of reionization (EoR; z \textgreater 6), chiefly due to the lack of sensitive near-IR spectrographs. However, this will soon change with the arrival of the Webb Telescope providing sensitive near-IR spectroscopy covering the rest-frame UV and optical emission of galaxies in the EoR. In anticipation of Webb, we combine the large cosmological hydrodynamical simulation BlueTides with photoionization modelling to predict the nebular emission-line properties of galaxies at z = 8 → 13. We find good agreement with the, albeit limited, existing direct and indirect observational constraints on equivalent widths though poorer agreement with luminosity function constraints.
@article{wilkins_nebular-line_2020,
title = {Nebular-line emission during the {Epoch} of {Reionization}},
volume = {493},
issn = {0035-8711},
url = {http://adsabs.harvard.edu/abs/2020MNRAS.493.6079W},
doi = {10.1093/mnras/staa649},
abstract = {Nebular emission lines associated with galactic H II regions carry information about both physical properties of the ionized gas and the source of ionizing photons as well as providing the opportunity of measuring accurate redshifts and thus distances once a cosmological model is assumed. While nebular-line emission has been extensively studied at lower redshift there are currently only few constraints within the epoch of reionization (EoR; z {\textgreater} 6), chiefly due to the lack of sensitive near-IR spectrographs. However, this will soon change with the arrival of the Webb Telescope providing sensitive near-IR spectroscopy covering the rest-frame UV and optical emission of galaxies in the EoR. In anticipation of Webb, we combine the large cosmological hydrodynamical simulation BlueTides with photoionization modelling to predict the nebular emission-line properties of galaxies at z = 8 → 13. We find good agreement with the, albeit limited, existing direct and indirect observational constraints on equivalent widths though poorer agreement with luminosity function constraints.},
urldate = {2020-11-16},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Wilkins, Stephen M. and Lovell, Christopher C. and Fairhurst, Ciaran and Feng, Yu and Matteo, Tiziana Di and Croft, Rupert and Kuusisto, Jussi and Vijayan, Aswin P. and Thomas, Peter},
month = mar,
year = {2020},
keywords = {Astrophysics - Astrophysics of Galaxies, galaxies: high-redshift, galaxies: luminosity function, galaxies: photometry, mass function, methods: numerical},
pages = {6079--6094},
}2019 (9)
Wide nutation: binary black-hole spins repeatedly oscillating from full alignment to full anti-alignment. Gerosa, D., Lima, A., Berti, E., Sperhake, U., Kesden, M., & O'Shaughnessy, R. Classical and Quantum Gravity, 36(10):105003, May, 2019.
doi bibtex
doi bibtex
@article{2019CQGra..36j5003G,
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
adsurl = {https://ui.adsabs.harvard.edu/abs/2019CQGra..36j5003G},
archiveprefix = {arXiv},
author = {{Gerosa}, Davide and {Lima}, Alicia and {Berti}, Emanuele and {Sperhake}, Ulrich and {Kesden}, Michael and {O'Shaughnessy}, Richard},
doi = {10.1088/1361-6382/ab14ae},
eid = {105003},
eprint = {1811.05979},
journal = {Classical and Quantum Gravity},
keywords = {General Relativity and Quantum Cosmology, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena},
month = may,
number = {10},
pages = {105003},
primaryclass = {gr-qc},
title = {{Wide nutation: binary black-hole spins repeatedly oscillating from full alignment to full anti-alignment}},
volume = {36},
year = 2019,
bdsk-url-1 = {https://doi.org/10.1088/1361-6382/ab14ae}}Through thick or thin: multiple components of the magneto-ionic medium towards the nearby H II region Sharpless 2-27 revealed by Faraday tomography. Thomson, A. J., Landecker, T., Dickey, J. M., McClure-Griffiths, N., Wolleben, M., Carretti, E., Fletcher, A., Federrath, C., Hill, A., Mao, S., Gaensler, B., Haverkorn, M., Clark, S., Van Eck, C., & West, J. \mnras, 487(4):4751-4767, August, 2019.
doi bibtex
doi bibtex
@ARTICLE{2019MNRAS.487.4751T,
author = {{Thomson}, Alec J.~M. and {Landecker}, T.~L. and {Dickey}, John M. and {McClure-Griffiths}, N.~M. and {Wolleben}, M. and {Carretti}, E. and {Fletcher}, A. and {Federrath}, Christoph and {Hill}, A.~S. and {Mao}, S.~A. and {Gaensler}, B.~M. and {Haverkorn}, M. and {Clark}, S.~E. and {Van Eck}, C.~L. and {West}, J.~L.},
title = "{Through thick or thin: multiple components of the magneto-ionic medium towards the nearby H II region Sharpless 2-27 revealed by Faraday tomography}",
journal = {\mnras},
keywords = {polarization, H $\lt$sc$\gt$ii$\lt$/sc$\gt$ regions, ISM: magnetic fields, Astrophysics - Astrophysics of Galaxies},
year = 2019,
month = aug,
volume = {487},
number = {4},
pages = {4751-4767},
doi = {10.1093/mnras/stz1438},
archivePrefix = {arXiv},
eprint = {1905.09285},
primaryClass = {astro-ph.GA},
adsurl = {https://ui.adsabs.harvard.edu/abs/2019MNRAS.487.4751T},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}The Global Magneto-Ionic Medium Survey: Polarimetry of the Southern Sky from 300 to 480 MHz. Wolleben, M., Landecker, T., Carretti, E., Dickey, J., Fletcher, A., McClure-Griffiths, N., McConnell, D., Thomson, A., Hill, A., Gaensler, B., Han, J. -., Haverkorn, M., Leahy, J., Reich, W., & Taylor, A. \aj, 158(1):44, July, 2019.
doi bibtex
doi bibtex
@ARTICLE{2019AJ....158...44W,
author = {{Wolleben}, M. and {Landecker}, T.~L. and {Carretti}, E. and {Dickey}, J.~M. and {Fletcher}, A. and {McClure-Griffiths}, N.~M. and {McConnell}, D. and {Thomson}, A.~J.~M. and {Hill}, A.~S. and {Gaensler}, B.~M. and {Han}, J. -L. and {Haverkorn}, M. and {Leahy}, J.~P. and {Reich}, W. and {Taylor}, A.~R.},
title = "{The Global Magneto-Ionic Medium Survey: Polarimetry of the Southern Sky from 300 to 480 MHz}",
journal = {\aj},
keywords = {Galaxy: general, instrumentation: polarimeters, ISM: magnetic fields, radio continuum: ISM, surveys, techniques: polarimetric, Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics},
year = 2019,
month = jul,
volume = {158},
number = {1},
eid = {44},
pages = {44},
doi = {10.3847/1538-3881/ab22b0},
archivePrefix = {arXiv},
eprint = {1905.12685},
primaryClass = {astro-ph.GA},
adsurl = {https://ui.adsabs.harvard.edu/abs/2019AJ....158...44W},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}The Galactic Magneto-ionic Medium Survey: Moments of the Faraday Spectra. Dickey, J. M., Landecker, T., Thomson, A. J., Wolleben, M., Sun, X., Carretti, E., Douglas, K., Fletcher, A., Gaensler, B., Gray, A., Haverkorn, M., Hill, A., Mao, S., & McClure-Griffiths, N. \apj, 871(1):106, January, 2019.
doi bibtex
doi bibtex
@ARTICLE{2019ApJ...871..106D,
author = {{Dickey}, John M. and {Landecker}, T.~L. and {Thomson}, Alec J.~M. and {Wolleben}, M. and {Sun}, X. and {Carretti}, E. and {Douglas}, K. and {Fletcher}, A. and {Gaensler}, B.~M. and {Gray}, A. and {Haverkorn}, M. and {Hill}, A.~S. and {Mao}, S.~A. and {McClure-Griffiths}, N.~M.},
title = "{The Galactic Magneto-ionic Medium Survey: Moments of the Faraday Spectra}",
journal = {\apj},
keywords = {cosmic rays, ISM: magnetic fields, local interstellar matter, techniques: polarimetric, Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics},
year = 2019,
month = jan,
volume = {871},
number = {1},
eid = {106},
pages = {106},
doi = {10.3847/1538-4357/aaf85f},
archivePrefix = {arXiv},
eprint = {1812.05399},
primaryClass = {astro-ph.GA},
adsurl = {https://ui.adsabs.harvard.edu/abs/2019ApJ...871..106D},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}Census of the Local Universe (CLU) Narrowband Survey. I. Galaxy Catalogs from Preliminary Fields. Cook, D. O., Kasliwal, M. M., Van Sistine, A., Kaplan, D. L., Sutter, J. S., Kupfer, T., Shupe, D. L., Laher, R. R., Masci, F. J., Dale, D. A., Sesar, B., Brady, P. R., Yan, L., Ofek, E. O., Reitze, D. H., & Kulkarni, S. R. \apj, 880(1):7, July, 2019.
doi bibtex
doi bibtex
@ARTICLE{2019ApJ...880....7C,
author = {{Cook}, David O. and {Kasliwal}, Mansi M. and {Van Sistine}, Angela and {Kaplan}, David L. and {Sutter}, Jessica S. and {Kupfer}, Thomas and {Shupe}, David L. and {Laher}, Russ R. and {Masci}, Frank J. and {Dale}, Daniel A. and {Sesar}, Branimir and {Brady}, Patrick R. and {Yan}, Lin and {Ofek}, Eran O. and {Reitze}, David H. and {Kulkarni}, Shrinivas R.},
title = "{Census of the Local Universe (CLU) Narrowband Survey. I. Galaxy Catalogs from Preliminary Fields}",
journal = {\apj},
keywords = {galaxies: Seyfert, galaxies: starburst, gravitational waves, surveys, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics},
year = 2019,
month = jul,
volume = {880},
number = {1},
eid = {7},
pages = {7},
doi = {10.3847/1538-4357/ab2131},
archivePrefix = {arXiv},
eprint = {1710.05016},
primaryClass = {astro-ph.GA},
adsurl = {https://ui.adsabs.harvard.edu/abs/2019ApJ...880....7C},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}GALACTICNUCLEUS: A high-angular-resolution JHK$_{s}$ imaging survey of the Galactic centre. II. First data release of the catalogue and the most detailed CMDs of the GC. Nogueras-Lara, F., Schödel, R., Gallego-Calvente, A., Dong, H., Gallego-Cano, E., Shahzamanian, B., Girard, J., Nishiyama, S., Najarro, F., & Neumayer, N. åp, 631:A20, November, 2019.
doi bibtex
doi bibtex
@ARTICLE{2019A&A...631A..20N,
author = {{Nogueras-Lara}, F. and {Sch{\"o}del}, R. and {Gallego-Calvente}, A.~T. and {Dong}, H. and {Gallego-Cano}, E. and {Shahzamanian}, B. and {Girard}, J.~H.~V. and {Nishiyama}, S. and {Najarro}, F. and {Neumayer}, N.},
title = "{GALACTICNUCLEUS: A high-angular-resolution JHK$_{s}$ imaging survey of the Galactic centre. II. First data release of the catalogue and the most detailed CMDs of the GC}",
journal = {\aap},
keywords = {Galaxy: center, Galaxy: bulge, Galaxy: structure, stars: horizontal-branch, dust, extinction, Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Solar and Stellar Astrophysics},
year = 2019,
month = nov,
volume = {631},
eid = {A20},
pages = {A20},
doi = {10.1051/0004-6361/201936263},
archivePrefix = {arXiv},
eprint = {1908.10366},
primaryClass = {astro-ph.GA},
adsurl = {https://ui.adsabs.harvard.edu/abs/2019A&A...631A..20N},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}The Wide Field Infrared Survey Telescope: 100 Hubbles for the 2020s. Akeson, R., Armus, L., Bachelet, E., Bailey, V., Bartusek, L., Bellini, A., Benford, D., Bennett, D., Bhattacharya, A., Bohlin, R., Boyer, M., Bozza, V., Bryden, G., Calchi Novati, S., Carpenter, K., Casertano, S., Choi, A., Content, D., Dayal, P., Dressler, A., Doré, O., Fall, S. M., Fan, X., Fang, X., Filippenko, A., Finkelstein, S., Foley, R., Furlanetto, S., Kalirai, J., Gaudi, B. S., Gilbert, K., Girard, J., Grady, K., Greene, J., Guhathakurta, P., Heinrich, C., Hemmati, S., Hendel, D., Henderson, C., Henning, T., Hirata, C., Ho, S., Huff, E., Hutter, A., Jansen, R., Jha, S., Johnson, S., Jones, D., Kasdin, J., Kelly, P., Kirshner, R., Koekemoer, A., Kruk, J., Lewis, N., Macintosh, B., Madau, P., Malhotra, S., Mandel, K., Massara, E., Masters, D., McEnery, J., McQuinn, K., Melchior, P., Melton, M., Mennesson, B., Peeples, M., Penny, M., Perlmutter, S., Pisani, A., Plazas, A., Poleski, R., Postman, M., Ranc, C., Rauscher, B., Rest, A., Roberge, A., Robertson, B., Rodney, S., Rhoads, J., Rhodes, J., Ryan, R., Sahu, K., Sand, D., Scolnic, D., Seth, A., Shvartzvald, Y., Siellez, K., Smith, A., Spergel, D., Stassun, K., Street, R., Strolger, L., Szalay, A., Trauger, J., Troxel, M., Turnbull, M., van der Marel , R., von der Linden , A., Wang, Y., Weinberg, D., Williams, B., Windhorst, R., Wollack, E., Wu, H., Yee, J., & Zimmerman, N. arXiv e-prints, February, 2019.
bibtex
bibtex
@ARTICLE{2019arXiv190205569A,
author = {{Akeson}, Rachel and {Armus}, Lee and {Bachelet}, Etienne and {Bailey}, Vanessa and {Bartusek}, Lisa and {Bellini}, Andrea and {Benford}, Dominic and {Bennett}, David and {Bhattacharya}, Aparna and {Bohlin}, Ralph and {Boyer}, Martha and {Bozza}, Valerio and {Bryden}, Geoffrey and {Calchi Novati}, Sebastiano and {Carpenter}, Kenneth and {Casertano}, Stefano and {Choi}, Ami and {Content}, David and {Dayal}, Pratika and {Dressler}, Alan and {Dor{\'e}}, Olivier and {Fall}, S. Michael and {Fan}, Xiaohui and {Fang}, Xiao and {Filippenko}, Alexei and {Finkelstein}, Steven and {Foley}, Ryan and {Furlanetto}, Steven and {Kalirai}, Jason and {Gaudi}, B. Scott and {Gilbert}, Karoline and {Girard}, Julien and {Grady}, Kevin and {Greene}, Jenny and {Guhathakurta}, Puragra and {Heinrich}, Chen and {Hemmati}, Shoubaneh and {Hendel}, David and {Henderson}, Calen and {Henning}, Thomas and {Hirata}, Christopher and {Ho}, Shirley and {Huff}, Eric and {Hutter}, Anne and {Jansen}, Rolf and {Jha}, Saurabh and {Johnson}, Samson and {Jones}, David and {Kasdin}, Jeremy and {Kelly}, Patrick and {Kirshner}, Robert and {Koekemoer}, Anton and {Kruk}, Jeffrey and {Lewis}, Nikole and {Macintosh}, Bruce and {Madau}, Piero and {Malhotra}, Sangeeta and {Mandel}, Kaisey and {Massara}, Elena and {Masters}, Daniel and {McEnery}, Julie and {McQuinn}, Kristen and {Melchior}, Peter and {Melton}, Mark and {Mennesson}, Bertrand and {Peeples}, Molly and {Penny}, Matthew and {Perlmutter}, Saul and {Pisani}, Alice and {Plazas}, Andr{\'e}s and {Poleski}, Radek and {Postman}, Marc and {Ranc}, Cl{\'e}ment and {Rauscher}, Bernard and {Rest}, Armin and {Roberge}, Aki and {Robertson}, Brant and {Rodney}, Steven and {Rhoads}, James and {Rhodes}, Jason and {Ryan}, Russell, Jr. and {Sahu}, Kailash and {Sand}, David and {Scolnic}, Dan and {Seth}, Anil and {Shvartzvald}, Yossi and {Siellez}, Karelle and {Smith}, Arfon and {Spergel}, David and {Stassun}, Keivan and {Street}, Rachel and {Strolger}, Louis-Gregory and {Szalay}, Alexander and {Trauger}, John and {Troxel}, M.~A. and {Turnbull}, Margaret and {van der Marel}, Roeland and {von der Linden}, Anja and {Wang}, Yun and {Weinberg}, David and {Williams}, Benjamin and {Windhorst}, Rogier and {Wollack}, Edward and {Wu}, Hao-Yi and {Yee}, Jennifer and {Zimmerman}, Neil},
title = "{The Wide Field Infrared Survey Telescope: 100 Hubbles for the 2020s}",
journal = {arXiv e-prints},
keywords = {Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Astrophysics of Galaxies},
year = 2019,
month = feb,
eid = {arXiv:1902.05569},
pages = {arXiv:1902.05569},
archivePrefix = {arXiv},
eprint = {1902.05569},
primaryClass = {astro-ph.IM},
adsurl = {https://ui.adsabs.harvard.edu/abs/2019arXiv190205569A},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}Recalibrating the cosmic star formation history. Wilkins, S. M., Lovell, C. C., & Stanway, E. R. Monthly Notices of the Royal Astronomical Society, 490:5359–5365, December, 2019.
Paper doi abstract bibtex
Paper doi abstract bibtex The calibrations linking observed luminosities to the star formation rate (SFR) depend on the assumed stellar population synthesis model, initial mass function, star formation and metal enrichment history, and whether reprocessing by dust and gas is included. Consequently the shape and normalization of the inferred cosmic star formation history is sensitive to these assumptions. Using v2.2.1 of the Binary Population and Spectral Synthesis (BPASS) model we determine a new set of calibration coefficients for the ultraviolet, thermal infrared, and hydrogen recombination lines. These ultraviolet and thermal infrared coefficients are 0.15-0.2 dex higher than those widely utilized in the literature while the H α coefficient is ∼0.35 dex larger. These differences arise in part due to the inclusion binary evolution pathways but predominantly reflect an extension in the IMF to 300 M⊙ and a change in the choice of reference metallicity. We use these new coefficients to recalibrate the cosmic star formation history, and find improved agreement between the integrated cosmic star formation history and the in situ measured stellar mass density as a function of redshift. However, these coefficients produce new tension between SFR densities inferred from the ultraviolet and thermal infrared and those from H α.
@article{wilkins_recalibrating_2019,
title = {Recalibrating the cosmic star formation history},
volume = {490},
url = {http://adsabs.harvard.edu/abs/2019MNRAS.490.5359W},
doi = {10.1093/mnras/stz2894},
abstract = {The calibrations linking observed luminosities to the star formation rate (SFR) depend on the assumed stellar population synthesis model, initial mass function, star formation and metal enrichment history, and whether reprocessing by dust and gas is included. Consequently the shape and normalization of the inferred cosmic star formation history is sensitive to these assumptions. Using v2.2.1 of the Binary Population and Spectral Synthesis (BPASS) model we determine a new set of
calibration coefficients for the ultraviolet, thermal infrared, and hydrogen recombination lines. These ultraviolet and thermal infrared coefficients are 0.15-0.2 dex higher than those widely utilized in the literature while the H α coefficient is ∼0.35 dex larger.
These differences arise in part due to the inclusion binary evolution pathways but predominantly reflect an extension in the IMF to 300 M⊙ and a change in the choice of reference metallicity. We use these new coefficients to recalibrate the cosmic star formation history, and find improved agreement between the integrated cosmic star formation history and the in situ measured stellar mass density as a function of redshift. However, these coefficients produce new tension between SFR densities inferred from the ultraviolet and thermal infrared and those from H α.},
urldate = {2020-10-01},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Wilkins, Stephen M. and Lovell, Christopher C. and Stanway, Elizabeth R.},
month = dec,
year = {2019},
keywords = {Astrophysics - Astrophysics of Galaxies, galaxies: high-redshift, galaxies: luminosity function, galaxies: photometry, mass function, methods: numerical},
pages = {5359--5365},
}Spectroscopy with the JWST Advanced Deep Extragalactic Survey (JADES) – the NIRSpec/NIRCam GTO galaxy evolution project. Bunker, A. J. Proceedings of the International Astronomical Union, 15(S352):342–346, June, 2019. arXiv: 2112.15207
Paper doi abstract bibtex
Paper doi abstract bibtex I present an overview of the JWST Advanced Deep Extragalactic Survey (JADES), a joint program of the JWST/NIRCam and NIRSpec Guaranteed Time Observations (GTO) teams involving 950 hours of observation. We will target two well-studied fields with excellent supporting data (e.g., from HST-CANDELS): GOODS-North and South, including the Ultra Deep Field. The science goal of JADES is to chart galaxy evolution at z \textgreater 2, and potentially out to z \textgreater 10, using the rest-frame optical and near-IR though observations from \${\textbackslash}approx\$ 1 - 5 \${\textbackslash}mu\$m. Multi-colour NIRCam imaging with 9 filters will enable photometric redshifts and the application of the Lyman break technique out to unprecedented distances. NIRSpec spectroscopy (with spectral resolving powers of R = 100, 1000 & 2700) will measure secure spectroscopic redshifts of the photometrically-selected population, as well as stellar continuum slopes in the UV rest-frame, and hence study the role of dust, stellar population age, and other effects. Measuring emission lines can constrain the dust extinction, star formation rates, metallicity, chemical abundances, ionization and excitation mechanism in high redshift galaxies. Coupling NIRCam and NIRSpec observations will determine stellar populations (age, star formation histories, abundances) of galaxies and provide the information to correct their broad-band spectral energy distribution for likely line contamination. Potentially we can search for signatures of Population III stars such as HeII. We can address the contribution of star-forming galaxies at z \textgreater 7 to reionization by determining the faint end slope of the luminosity function and investigating the escape fraction of ionizing photons by comparing the UV stellar continuum with the Balmer-line fluxes.
@article{bunker_spectroscopy_2019,
title = {Spectroscopy with the {JWST} {Advanced} {Deep} {Extragalactic} {Survey} ({JADES}) -- the {NIRSpec}/{NIRCam} {GTO} galaxy evolution project},
volume = {15},
issn = {1743-9213, 1743-9221},
url = {http://arxiv.org/abs/2112.15207},
doi = {10.1017/S1743921319009463},
abstract = {I present an overview of the JWST Advanced Deep Extragalactic Survey (JADES), a joint program of the JWST/NIRCam and NIRSpec Guaranteed Time Observations (GTO) teams involving 950 hours of observation. We will target two well-studied fields with excellent supporting data (e.g., from HST-CANDELS): GOODS-North and South, including the Ultra Deep Field. The science goal of JADES is to chart galaxy evolution at z {\textgreater} 2, and potentially out to z {\textgreater} 10, using the rest-frame optical and near-IR though observations from \${\textbackslash}approx\$ 1 - 5 \${\textbackslash}mu\$m. Multi-colour NIRCam imaging with 9 filters will enable photometric redshifts and the application of the Lyman break technique out to unprecedented distances. NIRSpec spectroscopy (with spectral resolving powers of R = 100, 1000 \& 2700) will measure secure spectroscopic redshifts of the photometrically-selected population, as well as stellar continuum slopes in the UV rest-frame, and hence study the role of dust, stellar population age, and other effects. Measuring emission lines can constrain the dust extinction, star formation rates, metallicity, chemical abundances, ionization and excitation mechanism in high redshift galaxies. Coupling NIRCam and NIRSpec observations will determine stellar populations (age, star formation histories, abundances) of galaxies and provide the information to correct their broad-band spectral energy distribution for likely line contamination. Potentially we can search for signatures of Population III stars such as HeII. We can address the contribution of star-forming galaxies at z {\textgreater} 7 to reionization by determining the faint end slope of the luminosity function and investigating the escape fraction of ionizing photons by comparing the UV stellar continuum with the Balmer-line fluxes.},
number = {S352},
urldate = {2022-01-05},
journal = {Proceedings of the International Astronomical Union},
author = {Bunker, Andrew J.},
month = jun,
year = {2019},
note = {arXiv: 2112.15207},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics},
pages = {342--346},
}2018 (7)
Black-hole kicks from numerical-relativity surrogate models. Gerosa, D., Hébert, F., & Stein, L. C. Physical Review D, 97(10):104049, May, 2018.
doi bibtex
doi bibtex
@article{2018PhRvD..97j4049G,
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
adsurl = {https://ui.adsabs.harvard.edu/abs/2018PhRvD..97j4049G},
archiveprefix = {arXiv},
author = {{Gerosa}, Davide and {H{\'e}bert}, Fran{\c{c}}ois and {Stein}, Leo C.},
doi = {10.1103/PhysRevD.97.104049},
eid = {104049},
eprint = {1802.04276},
journal = {Physical Review D},
keywords = {General Relativity and Quantum Cosmology, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena},
month = may,
number = {10},
pages = {104049},
primaryclass = {gr-qc},
title = {{Black-hole kicks from numerical-relativity surrogate models}},
volume = {97},
year = 2018,
bdsk-url-1 = {https://doi.org/10.1103/PhysRevD.97.104049}}The NANOGrav 11-year Data Set: Pulsar-timing Constraints On The Stochastic Gravitational-wave Background. Arzoumanian, Z., Baker, P., Brazier, A., Burke-Spolaor, S., Chamberlin, S., Chatterjee, S., Christy, B., Cordes, J., Cornish, N., Crawford, F., Thankful Cromartie, H., Crowter, K., DeCesar, M., Demorest, P., Dolch, T., Ellis, J., Ferdman, R., Ferrara, E., Folkner, W., Fonseca, E., Garver-Daniels, N., Gentile, P., Haas, R., Hazboun, J., Huerta, E., Islo, K., Jenet, F., Jones, G., Jones, M., Kaplan, D., Kaspi, V., Lam, M., Lazio, T., Levin, L., Lommen, A., Lorimer, D., Luo, J., Lynch, R., Madison, D., McLaughlin, M., McWilliams, S., Mingarelli, C., Ng, C., Nice, D., Park, R., Pennucci, T., Pol, N., Ransom, S., Ray, P., Rasskazov, A., Siemens, X., Simon, J., Spiewak, R., Stairs, I., Stinebring, D., Stovall, K., Swiggum, J., Taylor, S., Vallisneri, M., Vigeland, S., & Zhu, W. ArXiv e-prints, January, 2018.
bibtex
bibtex
@ARTICLE{2018arXiv180102617A,
author = {{Arzoumanian}, Z. and {Baker}, P.~T. and {Brazier}, A. and {Burke-Spolaor}, S. and
{Chamberlin}, S.~J. and {Chatterjee}, S. and {Christy}, B. and
{Cordes}, J.~M. and {Cornish}, N.~J. and {Crawford}, F. and
{Thankful Cromartie}, H. and {Crowter}, K. and {DeCesar}, M. and
{Demorest}, P.~B. and {Dolch}, T. and {Ellis}, J.~A. and {Ferdman}, R.~D. and
{Ferrara}, E. and {Folkner}, W.~M. and {Fonseca}, E. and {Garver-Daniels}, N. and
{Gentile}, P.~A. and {Haas}, R. and {Hazboun}, J.~S. and {Huerta}, E.~A. and
{Islo}, K. and {Jenet}, F. and {Jones}, G. and {Jones}, M.~L. and
{Kaplan}, D.~L. and {Kaspi}, V.~M. and {Lam}, M.~T. and {Lazio}, T.~J.~W. and
{Levin}, L. and {Lommen}, A.~N. and {Lorimer}, D.~R. and {Luo}, J. and
{Lynch}, R.~S. and {Madison}, D.~R. and {McLaughlin}, M.~A. and
{McWilliams}, S.~T. and {Mingarelli}, C.~M.~F. and {Ng}, C. and
{Nice}, D.~J. and {Park}, R.~S. and {Pennucci}, T.~T. and {Pol}, N.~S. and
{Ransom}, S.~M. and {Ray}, P.~S. and {Rasskazov}, A. and {Siemens}, X. and
{Simon}, J. and {Spiewak}, R. and {Stairs}, I.~H. and {Stinebring}, D.~R. and
{Stovall}, K. and {Swiggum}, J. and {Taylor}, S.~R. and {Vallisneri}, M. and
{Vigeland}, S. and {Zhu}, W.~W.},
title = "{The NANOGrav 11-year Data Set: Pulsar-timing Constraints On The Stochastic Gravitational-wave Background}",
journal = {ArXiv e-prints},
archivePrefix = "arXiv",
eprint = {1801.02617},
primaryClass = "astro-ph.HE",
keywords = {Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies, General Relativity and Quantum Cosmology},
year = 2018,
month = jan,
adsurl = {http://adsabs.harvard.edu/abs/2018arXiv180102617A},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}Ghost of a shell: magnetic fields of Galactic supershell GSH 006 - 15 + 7. Thomson, A. J., McClure-Griffiths, N., Federrath, C., Dickey, J. M., Carretti, E., Gaensler, B., Haverkorn, M., Kesteven, M., & Staveley-Smith, L. \mnras, 479(4):5620-5637, October, 2018.
doi bibtex
doi bibtex
@ARTICLE{2018MNRAS.479.5620T,
author = {{Thomson}, Alec J.~M. and {McClure-Griffiths}, N.~M. and {Federrath}, Christoph and {Dickey}, John M. and {Carretti}, Ettore and {Gaensler}, B.~M. and {Haverkorn}, Marijke and {Kesteven}, M.~J. and {Staveley-Smith}, Lister},
title = "{Ghost of a shell: magnetic fields of Galactic supershell GSH 006 - 15 + 7}",
journal = {\mnras},
keywords = {polarization, ISM: bubbles, ISM: magnetic fields, Astrophysics - Astrophysics of Galaxies},
year = 2018,
month = oct,
volume = {479},
number = {4},
pages = {5620-5637},
doi = {10.1093/mnras/sty1865},
archivePrefix = {arXiv},
eprint = {1807.04759},
primaryClass = {astro-ph.GA},
adsurl = {https://ui.adsabs.harvard.edu/abs/2018MNRAS.479.5620T},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}Star formation history and metallicity in the Galactic inner bulge revealed by the red giant branch bump. Nogueras-Lara, F., Schödel, R., Dong, H., Najarro, F., Gallego-Calvente, A., Hilker, M., Gallego-Cano, E., Nishiyama, S., Neumayer, N., Feldmeier-Krause, A., Girard, J., Cassisi, S., & Pietrinferni, A. åp, 620:A83, December, 2018.
doi bibtex
doi bibtex
@ARTICLE{2018A&A...620A..83N,
author = {{Nogueras-Lara}, F. and {Sch{\"o}del}, R. and {Dong}, H. and {Najarro}, F. and {Gallego-Calvente}, A.~T. and {Hilker}, M. and {Gallego-Cano}, E. and {Nishiyama}, S. and {Neumayer}, N. and {Feldmeier-Krause}, A. and {Girard}, J.~H.~V. and {Cassisi}, S. and {Pietrinferni}, A.},
title = "{Star formation history and metallicity in the Galactic inner bulge revealed by the red giant branch bump}",
journal = {\aap},
keywords = {Galaxy: bulge, Galaxy: center, Galaxy: structure, stars: horizontal-branch, dust, extinction, Astrophysics - Astrophysics of Galaxies},
year = 2018,
month = dec,
volume = {620},
eid = {A83},
pages = {A83},
doi = {10.1051/0004-6361/201833518},
archivePrefix = {arXiv},
eprint = {1809.07627},
primaryClass = {astro-ph.GA},
adsurl = {https://ui.adsabs.harvard.edu/abs/2018A&A...620A..83N},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}GALACTICNUCLEUS: A high angular resolution JHK$_{s}$ imaging survey of the Galactic centre. I. Methodology, performance, and near-infrared extinction towards the Galactic centre. Nogueras-Lara, F., Gallego-Calvente, A., Dong, H., Gallego-Cano, E., Girard, J., Hilker, M., de Zeeuw , P., Feldmeier-Krause, A., Nishiyama, S., Najarro, F., Neumayer, N., & Schödel, R. åp, 610:A83, March, 2018.
doi bibtex
doi bibtex
@ARTICLE{2018A&A...610A..83N,
author = {{Nogueras-Lara}, F. and {Gallego-Calvente}, A.~T. and {Dong}, H. and {Gallego-Cano}, E. and {Girard}, J.~H.~V. and {Hilker}, M. and {de Zeeuw}, P.~T. and {Feldmeier-Krause}, A. and {Nishiyama}, S. and {Najarro}, F. and {Neumayer}, N. and {Sch{\"o}del}, R.},
title = "{GALACTICNUCLEUS: A high angular resolution JHK$_{s}$ imaging survey of the Galactic centre. I. Methodology, performance, and near-infrared extinction towards the Galactic centre}",
journal = {\aap},
keywords = {Galaxy: nucleus, dust, extinction, Galaxy: center, stars: horizontal-branch, Astrophysics - Astrophysics of Galaxies},
year = 2018,
month = mar,
volume = {610},
eid = {A83},
pages = {A83},
doi = {10.1051/0004-6361/201732002},
archivePrefix = {arXiv},
eprint = {1709.09094},
primaryClass = {astro-ph.GA},
adsurl = {https://ui.adsabs.harvard.edu/abs/2018A&A...610A..83N},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}Dust-obscured star-forming galaxies in the early universe. Wilkins, S. M., Feng, Y., Di Matteo, T., Croft, R., Lovell, C. C., & Thomas, P. Monthly Notices of the Royal Astronomical Society, 473:5363–5369, February, 2018.
Paper doi abstract bibtex
Paper doi abstract bibtex Motivated by recent observational constraints on dust reprocessed emission in star-forming galaxies at z ∼ 6 and above, we use the very large cosmological hydrodynamical simulation BLUETIDES to explore predictions for the amount of dust-obscured star formation in the early Universe (z \textgreater 8). BLUETIDES matches current observational constraints on both the UV luminosity function and galaxy stellar mass function and predicts that approximately 90 per cent of the star formation in high-mass (M* \textgreater 1010 M⊙) galaxies at z = 8 is already obscured by dust. The relationship between dust attenuation and stellar mass predicted by BLUETIDES is consistent with that observed at lower redshift. However, observations of several individual objects at z \textgreater 6 are discrepant with the predictions, though it is possible that their uncertainties may have been underestimated. We find that the predicted surface density of z ≥ 8 submm sources is below that accessible to current Herschel, SCUBA-2 and Atacama Large Millimetre Array (ALMA) submm surveys. However, as ALMA continues to accrue an additional surface area the population of z \textgreater 8 dust-obscured galaxies may become accessible in the near future.
@article{wilkins_dust-obscured_2018,
title = {Dust-obscured star-forming galaxies in the early universe},
volume = {473},
issn = {0035-8711},
url = {http://adsabs.harvard.edu/abs/2018MNRAS.473.5363W},
doi = {10.1093/mnras/stx2588},
abstract = {Motivated by recent observational constraints on dust reprocessed emission in star-forming galaxies at z ∼ 6 and above, we use the very large cosmological hydrodynamical simulation BLUETIDES to explore predictions for the amount of dust-obscured star formation in the early Universe (z {\textgreater} 8). BLUETIDES matches current observational constraints on both the UV luminosity function and galaxy stellar mass function and predicts that approximately 90 per cent of the star formation in high-mass (M* {\textgreater} 1010 M⊙)
galaxies at z = 8 is already obscured by dust. The relationship between dust attenuation and stellar mass predicted by BLUETIDES is consistent with that observed at lower redshift. However, observations of several individual objects at z {\textgreater} 6 are discrepant with the predictions, though it is possible that their uncertainties may have been
underestimated. We find that the predicted surface density of z ≥ 8 submm sources is below that accessible to current Herschel, SCUBA-2 and Atacama Large Millimetre Array (ALMA) submm surveys. However, as ALMA continues to accrue an additional surface area the population of z {\textgreater} 8 dust-obscured galaxies may become accessible in the near future.},
urldate = {2020-03-26},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Wilkins, Stephen M. and Feng, Yu and Di Matteo, Tiziana and Croft, Rupert and Lovell, Christopher C. and Thomas, Peter},
month = feb,
year = {2018},
keywords = {Astrophysics - Astrophysics of Galaxies, galaxies: high-redshift, galaxies: luminosity function, galaxies: photometry, mass function, methods: numerical},
pages = {5363--5369},
}Characterising and identifying galaxy protoclusters. Lovell, C. C., Thomas, P. A., & Wilkins, S. M. Monthly Notices of the Royal Astronomical Society, 474:4612–4628, March, 2018.
Paper doi abstract bibtex 1 download
Paper doi abstract bibtex 1 download We study the characteristics of galaxy protoclusters using the latest L-GALAXIES semi-analytic model. Searching for protoclusters on a scale of ˜10 cMpc gives an excellent compromise between the completeness and purity of their galaxy populations, leads to high distinction from the field in overdensity space, and allows accurate determination of the descendant cluster mass. This scale is valid over a range of redshifts and selection criteria. We present a procedure for estimating, given a measured galaxy overdensity, the protocluster probability and its descendant cluster mass for a range of modelling assumptions, particularly taking into account the shape of the measurement aperture. This procedure produces lower protocluster probabilities compared to previous estimates using fixed size apertures. The relationship between active galactic nucleus (AGN) and protoclusters is also investigated and shows significant evolution with redshift; at z ˜ 2, the fraction of protoclusters traced by AGN is high, but the fraction of all AGNs in protoclusters is low, whereas at z ≥ 5 the fraction of protoclusters containing AGN is low, but most AGNs are in protoclusters. We also find indirect evidence for the emergence of a passive sequence in protoclusters at z ˜ 2, and note that a significant fraction of all galaxies reside in protoclusters at z ≥ 2, particularly the most massive.
@article{lovell_characterising_2018,
title = {Characterising and identifying galaxy protoclusters},
volume = {474},
issn = {0035-8711},
url = {http://adsabs.harvard.edu/abs/2018MNRAS.474.4612L},
doi = {10.1093/mnras/stx3090},
abstract = {We study the characteristics of galaxy protoclusters using the latest L-GALAXIES semi-analytic model. Searching for protoclusters on a scale of ˜10 cMpc gives an excellent compromise between the completeness and purity of their galaxy populations, leads to high distinction from the field in overdensity space, and allows accurate determination of the descendant cluster mass. This scale is valid over a range of redshifts and selection criteria. We present a procedure for estimating, given a measured galaxy overdensity, the protocluster probability and its descendant cluster mass for a range of modelling assumptions,
particularly taking into account the shape of the measurement aperture. This procedure produces lower protocluster probabilities compared to previous estimates using fixed size apertures. The relationship between active galactic nucleus (AGN) and protoclusters is also investigated and shows significant evolution with redshift; at z ˜ 2, the fraction of protoclusters traced by AGN is high, but the fraction of all AGNs in protoclusters is low, whereas at z ≥ 5 the fraction of protoclusters containing AGN is low, but most AGNs are in protoclusters. We also find indirect evidence for the emergence of a passive sequence in
protoclusters at z ˜ 2, and note that a significant fraction of
all galaxies reside in protoclusters at z ≥ 2, particularly the most massive.},
urldate = {2019-05-28},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Lovell, Christopher C. and Thomas, Peter A. and Wilkins, Stephen M.},
month = mar,
year = {2018},
keywords = {Astrophysics - Astrophysics of Galaxies, galaxies: clusters: general, galaxies: high-redshift, galaxies: statistics},
pages = {4612--4628},
}2017 (5)
FIRE-2 Simulations: Physics versus Numerics in Galaxy Formation. Hopkins, P. F, Wetzel, A., Keres, D., Faucher-Giguere, C., Quataert, E., Boylan-Kolchin, M., Murray, N., Hayward, C. C., Garrison-Kimmel, S., Hummels, C., Feldmann, R., Torrey, P., Ma, X., Angles-Alcazar, D., Su, K., Orr, M., Schmitz, D., Escala, I., Sanderson, R., Grudic, M. Y., Hafen, Z., Kim, J., Fitts, A., Bullock, J. S., Wheeler, C., Chan, T. K., Elbert, O. D., & Narananan, D. ArXiv e-prints, 1702:arXiv:1702.06148, February, 2017.
Paper abstract bibtex
Paper abstract bibtex The Feedback In Realistic Environments (FIRE) project explores the role of feedback in cosmological simulations of galaxy formation. Previous FIRE simulations used an identical source code (FIRE-1) for consistency. Now, motivated by the development of more accurate numerics (hydrodynamic solvers, gravitational softening, supernova coupling) and the exploration of new physics (e.g. magnetic fields), we introduce FIRE-2, an updated numerical implementation of FIRE physics for the GIZMO code. We run a suite of simulations and show FIRE-2 improvements do not qualitatively change galaxy-scale properties relative to FIRE-1. We then pursue an extensive study of numerics versus physics in galaxy simulations. Details of the star-formation (SF) algorithm, cooling physics, and chemistry have weak effects, provided that we include metal-line cooling and SF occurs at higher-than-mean densities. We present several new resolution criteria for high-resolution galaxy simulations. Most galaxy-scale properties are remarkably robust to the numerics that we test, provided that: (1) Toomre masses (cold disk scale heights) are resolved; (2) feedback coupling ensures conservation and isotropy, and (3) individual supernovae are time-resolved. As resolution increases, stellar masses and profiles converge first, followed by metal abundances and visual morphologies, then properties of winds and the circumgalactic medium. The central (\textasciitildekpc) mass concentration of massive (L*) galaxies is sensitive to numerics, particularly how winds ejected into hot halos are trapped, mixed, and recycled into the galaxy. Multiple feedback mechanisms are required to reproduce observations: SNe regulate stellar masses; OB/AGB mass loss fuels late-time SF; radiative feedback suppresses instantaneous SFRs and accretion onto dwarfs. We provide tables, initial conditions, and the numerical algorithms required to reproduce our simulations.
@article{hopkins_fire-2_2017,
title = {{FIRE}-2 {Simulations}: {Physics} versus {Numerics} in {Galaxy} {Formation}},
volume = {1702},
shorttitle = {{FIRE}-2 {Simulations}},
url = {http://adsabs.harvard.edu/abs/2017arXiv170206148H},
abstract = {The Feedback In Realistic Environments (FIRE) project explores the role of feedback in cosmological simulations of galaxy formation. Previous FIRE simulations used an identical source code (FIRE-1) for consistency. Now, motivated by the development of more accurate numerics
(hydrodynamic solvers, gravitational softening, supernova coupling) and the exploration of new physics (e.g. magnetic fields), we introduce FIRE-2, an updated numerical implementation of FIRE physics for the GIZMO code. We run a suite of simulations and show FIRE-2 improvements do not qualitatively change galaxy-scale properties relative to FIRE-1. We then pursue an extensive study of numerics versus physics in galaxy simulations. Details of the star-formation (SF) algorithm, cooling physics, and chemistry have weak effects, provided that we include metal-line cooling and SF occurs at higher-than-mean densities. We present several new resolution criteria for high-resolution galaxy simulations. Most galaxy-scale properties are remarkably robust to the numerics that we test, provided that: (1) Toomre masses (cold disk scale heights) are resolved; (2) feedback coupling ensures conservation and isotropy, and (3) individual supernovae are time-resolved. As resolution increases, stellar masses and profiles converge first, followed by metal abundances and visual morphologies, then properties of winds and the circumgalactic medium. The central ({\textasciitilde}kpc) mass concentration of massive (L*) galaxies is sensitive to numerics, particularly how winds ejected into hot halos are trapped, mixed, and recycled into the galaxy. Multiple feedback mechanisms are required to reproduce observations: SNe regulate stellar masses; OB/AGB mass loss fuels late-time SF; radiative feedback suppresses instantaneous SFRs and accretion onto dwarfs. We provide tables, initial conditions, and the numerical algorithms required to reproduce our simulations.},
urldate = {2017-03-09},
journal = {ArXiv e-prints},
author = {Hopkins, Philip F and Wetzel, Andrew and Keres, Dusan and Faucher-Giguere, Claude-Andre and Quataert, Eliot and Boylan-Kolchin, Michael and Murray, Norman and Hayward, Christopher C. and Garrison-Kimmel, Shea and Hummels, Cameron and Feldmann, Robert and Torrey, Paul and Ma, Xiangcheng and Angles-Alcazar, Daniel and Su, Kung-Yi and Orr, Matthew and Schmitz, Denise and Escala, Ivanna and Sanderson, Robyn and Grudic, Michael Y. and Hafen, Zachary and Kim, Ji-Hoon and Fitts, Alex and Bullock, James S. and Wheeler, Coral and Chan, T. K. and Elbert, Oliver D. and Narananan, Desika},
month = feb,
year = {2017},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics},
pages = {arXiv:1702.06148},
}First light: exploring the spectra of high-redshift galaxies in the Renaissance Simulations. Barrow, K. S. S., Wise, J. H., Norman, M. L., O'Shea, B. W., & Xu, H. Monthly Notices of the Royal Astronomical Society, 469:4863–4878, August, 2017.
Paper doi abstract bibtex
Paper doi abstract bibtex We present synthetic observations for the first generations of galaxies in the Universe and make predictions for future deep field observations for redshifts greater than 6. Due to the strong impact of nebular emission lines and the relatively compact scale of H II regions, high-resolution cosmological simulations and a robust suite of analysis tools are required to properly simulate spectra. We created a software pipeline consisting of fsps, hyperion, cloudy and our own tools to generate synthetic IR observations from a fully three-dimensional arrangement of gas, dust, and stars. Our prescription allows us to include emission lines for a complete chemical network and tackle the effect of dust extinction and scattering in the various lines of sight. We provide spectra, 2D binned photon imagery for both HST and JWST IR filters, luminosity relationships, and emission-line strengths for a large sample of high-redshift galaxies in the Renaissance Simulations. Our resulting synthetic spectra show high variability between galactic haloes with a strong dependence on stellar mass, metallicity, gas mass fraction, and formation history. Haloes with the lowest stellar mass have the greatest variability in [O III]/Hβ, [O III], and C III], while haloes with higher masses are seen to show consistency in their spectra and [O III] equivalent widths between 1 and 10 Å. Viewing angle accounted for threefold difference in flux due to the presence of ionized gas channels in a halo. Furthermore, JWST colour plots show a discernible relationship between redshift, colour, and mean stellar age.
@article{barrow_first_2017,
title = {First light: exploring the spectra of high-redshift galaxies in the {Renaissance} {Simulations}},
volume = {469},
issn = {0035-8711},
shorttitle = {First light},
url = {http://adsabs.harvard.edu/abs/2017MNRAS.469.4863B},
doi = {10.1093/mnras/stx1181},
abstract = {We present synthetic observations for the first generations of galaxies
in the Universe and make predictions for future deep field observations
for redshifts greater than 6. Due to the strong impact of nebular
emission lines and the relatively compact scale of H II regions,
high-resolution cosmological simulations and a robust suite of analysis
tools are required to properly simulate spectra. We created a software
pipeline consisting of fsps, hyperion, cloudy and our own tools to
generate synthetic IR observations from a fully three-dimensional
arrangement of gas, dust, and stars. Our prescription allows us to
include emission lines for a complete chemical network and tackle the
effect of dust extinction and scattering in the various lines of sight.
We provide spectra, 2D binned photon imagery for both HST and JWST IR
filters, luminosity relationships, and emission-line strengths for a
large sample of high-redshift galaxies in the Renaissance Simulations.
Our resulting synthetic spectra show high variability between galactic
haloes with a strong dependence on stellar mass, metallicity, gas mass
fraction, and formation history. Haloes with the lowest stellar mass
have the greatest variability in [O III]/Hβ, [O III], and C III],
while haloes with higher masses are seen to show consistency in their
spectra and [O III] equivalent widths between 1 and 10 Å. Viewing
angle accounted for threefold difference in flux due to the presence of
ionized gas channels in a halo. Furthermore, JWST colour plots show a
discernible relationship between redshift, colour, and mean stellar age.},
urldate = {2020-03-26},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Barrow, Kirk S. S. and Wise, John H. and Norman, Michael L. and O'Shea, Brian W. and Xu, Hao},
month = aug,
year = {2017},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics, dark ages, first stars, methods: numerical, methods: observational, radiative transfer, reionization, techniques: photometric, techniques: spectroscopic},
pages = {4863--4878},
}How similar are the properties of quasars with nearly identical ultraviolet spectra?. Rochais, T., Singh, V., Chick, W., Maithil, J., Sutter, J., Brotherton, M. S., & Shang, Z. \mnras, 464(1):553-563, January, 2017.
doi bibtex
doi bibtex
@ARTICLE{2017MNRAS.464..553R,
author = {{Rochais}, Thomas and {Singh}, Vikram and {Chick}, William and {Maithil}, Jaya and {Sutter}, Jessica and {Brotherton}, Michael S. and {Shang}, Zhaohui},
title = "{How similar are the properties of quasars with nearly identical ultraviolet spectra?}",
journal = {\mnras},
keywords = {galaxies: active, quasars: general, Astrophysics - Astrophysics of Galaxies},
year = 2017,
month = jan,
volume = {464},
number = {1},
pages = {553-563},
doi = {10.1093/mnras/stw2350},
archivePrefix = {arXiv},
eprint = {1609.08732},
primaryClass = {astro-ph.GA},
adsurl = {https://ui.adsabs.harvard.edu/abs/2017MNRAS.464..553R},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}On the equal-mass limit of precessing black-hole binaries. Gerosa, D., Sperhake, U., & Vošmera, J. Classical and Quantum Gravity, 34(6):064004, March, 2017.
doi bibtex
doi bibtex
@article{2017CQGra..34f4004G,
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
adsurl = {https://ui.adsabs.harvard.edu/abs/2017CQGra..34f4004G},
archiveprefix = {arXiv},
author = {{Gerosa}, Davide and {Sperhake}, Ulrich and {Vo{\v{s}}mera}, Jakub},
doi = {10.1088/1361-6382/aa5e58},
eid = {064004},
eprint = {1612.05263},
journal = {Classical and Quantum Gravity},
keywords = {General Relativity and Quantum Cosmology, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena},
month = mar,
number = {6},
pages = {064004},
primaryclass = {gr-qc},
title = {{On the equal-mass limit of precessing black-hole binaries}},
volume = {34},
year = 2017,
bdsk-url-1 = {https://doi.org/10.1088/1361-6382/aa5e58}}The properties of the first galaxies in the BlueTides simulation. Wilkins, S. M., Feng, Y., Di Matteo, T., Croft, R., Lovell, C. C., & Waters, D. Monthly Notices of the Royal Astronomical Society, 469:2517–2530, August, 2017.
Paper doi abstract bibtex
Paper doi abstract bibtex We employ the very large cosmological hydrodynamical simulation BlueTides to investigate the predicted properties of the galaxy population during the epoch of reionization (z \textgreater 8). BlueTides has a resolution and volume ((400/h ≈ 577)3 cMpc3) providing a population of galaxies that is well matched to depth and area of current observational surveys targeting the high-redshift Universe. At z = 8, BlueTides includes almost 160 000 galaxies with stellar masses \textgreater108 M⊙. The population of galaxies predicted by BlueTides closely matches observational constraints on both the galaxy stellar mass function and far-UV (150 nm) luminosity function. Galaxies in BlueTides are characterized by rapidly increasing star formation histories. Specific star formation rates decrease with redshift though remain largely insensitive to stellar mass. As a result of the enhanced surface density of metals, more massive galaxies are predicted to have higher dust attenuation resulting in a significant steepening of the observed far-UV luminosity function at high luminosities. The contribution of active supermassive black holes (SMBHs) to the UV luminosities of galaxies with stellar masses 109-10 M⊙ is around 3 per cent on average. Approximately 25 per cent of galaxies with M* ≈ 1010 M⊙ are predicted to have active SMBHs that contribute \textgreater10 per cent of the total UV luminosity.
@article{wilkins_properties_2017,
title = {The properties of the first galaxies in the {BlueTides} simulation},
volume = {469},
issn = {0035-8711},
url = {http://adsabs.harvard.edu/abs/2017MNRAS.469.2517W},
doi = {10.1093/mnras/stx841},
abstract = {We employ the very large cosmological hydrodynamical simulation BlueTides to investigate the predicted properties of the galaxy
population during the epoch of reionization (z {\textgreater} 8). BlueTides has a resolution and volume ((400/h ≈ 577)3 cMpc3) providing a population of galaxies that is well matched to depth and area of current observational surveys targeting the high-redshift Universe. At z = 8, BlueTides includes almost 160 000 galaxies with stellar masses {\textgreater}108 M⊙. The population of
galaxies predicted by BlueTides closely matches observational
constraints on both the galaxy stellar mass function and far-UV (150 nm) luminosity function. Galaxies in BlueTides are characterized by rapidly increasing star formation histories. Specific star formation rates decrease with redshift though remain largely insensitive to stellar mass. As a result of the enhanced surface density of metals, more massive galaxies are predicted to have higher dust attenuation resulting in a significant steepening of the observed far-UV luminosity function at high luminosities. The contribution of active supermassive black holes (SMBHs) to the UV luminosities of galaxies with stellar masses 109-10 M⊙ is around 3 per cent on average. Approximately 25 per cent of galaxies with M* ≈
1010 M⊙ are predicted to have active SMBHs that contribute {\textgreater}10 per cent of the total UV luminosity.},
urldate = {2020-03-26},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Wilkins, Stephen M. and Feng, Yu and Di Matteo, Tiziana and Croft, Rupert and Lovell, Christopher C. and Waters, Dacen},
month = aug,
year = {2017},
keywords = {Astrophysics - Astrophysics of Galaxies, galaxies: high-redshift, galaxies: luminosity function, galaxies: photometry, mass function, methods: numerical},
pages = {2517--2530},
}2016 (5)
Black Hole Kicks as New Gravitational Wave Observables. Gerosa, D. & Moore, C. J. Physical Review Letters, 117(1):011101, July, 2016.
doi bibtex
doi bibtex
@article{2016PhRvL.117a1101G,
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
adsurl = {https://ui.adsabs.harvard.edu/abs/2016PhRvL.117a1101G},
archiveprefix = {arXiv},
author = {{Gerosa}, Davide and {Moore}, Christopher J.},
doi = {10.1103/PhysRevLett.117.011101},
eid = {011101},
eprint = {1606.04226},
journal = {Physical Review Letters},
keywords = {General Relativity and Quantum Cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena},
month = jul,
number = {1},
pages = {011101},
primaryclass = {gr-qc},
title = {{Black Hole Kicks as New Gravitational Wave Observables}},
volume = {117},
year = 2016,
bdsk-url-1 = {https://doi.org/10.1103/PhysRevLett.117.011101}}precession: Dynamics of spinning black-hole binaries with python. Gerosa, D. & Kesden, M. Physical Review D, 93(12):124066, June, 2016.
doi bibtex
doi bibtex
@article{2016PhRvD..93l4066G,
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
adsurl = {https://ui.adsabs.harvard.edu/abs/2016PhRvD..93l4066G},
archiveprefix = {arXiv},
author = {{Gerosa}, Davide and {Kesden}, Michael},
doi = {10.1103/PhysRevD.93.124066},
eid = {124066},
eprint = {1605.01067},
journal = {Physical Review D},
keywords = {Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, General Relativity and Quantum Cosmology},
month = jun,
number = {12},
pages = {124066},
primaryclass = {astro-ph.HE},
title = {{precession: Dynamics of spinning black-hole binaries with python}},
volume = {93},
year = 2016,
bdsk-url-1 = {https://doi.org/10.1103/PhysRevD.93.124066}}The Preferential Tidal Stripping of Dark Matter versus Stars in Galaxies. Smith, R., Choi, H., Lee, J., Rhee, J., Sanchez-Janssen, R., & Yi, S. K. arXiv:1610.04264 [astro-ph], October, 2016. arXiv: 1610.04264
Paper abstract bibtex
Paper abstract bibtex Using high resolution hydrodynamical cosmological simulations, we conduct a comprehensive study of how tidal stripping removes dark matter and stars from galaxies. We find that dark matter is always stripped far more significantly than the stars – galaxies that lose \${\textbackslash}sim\$80\${\textbackslash}%\$ of their dark matter, typically lose only 10\${\textbackslash}%\$ of their stars. This is because the dark matter halo is initially much more extended than the stars. As such, we find the stellar-to-halo size-ratio (measured using r\$_\{{\textbackslash}rm\{eff\}\}\$/r\$_\{{\textbackslash}rm\{vir\}\}\$) is a key parameter controlling the relative amounts of dark matter and stellar stripping. We use simple fitting formulae to measure the relation between the fraction of bound dark matter and fraction of bound stars. We measure a negligible dependence on cluster mass or galaxy mass. Therefore these formulae have general applicability in cosmological simulations, and are ideal to improve stellar stripping recipes in semi-analytical models, and/or to estimate the impact that tidal stripping would have on galaxies when only their halo mass evolution is known.
@article{smith_preferential_2016,
title = {The {Preferential} {Tidal} {Stripping} of {Dark} {Matter} versus {Stars} in {Galaxies}},
url = {http://arxiv.org/abs/1610.04264},
abstract = {Using high resolution hydrodynamical cosmological simulations, we conduct a comprehensive study of how tidal stripping removes dark matter and stars from galaxies. We find that dark matter is always stripped far more significantly than the stars -- galaxies that lose \${\textbackslash}sim\$80\${\textbackslash}\%\$ of their dark matter, typically lose only 10\${\textbackslash}\%\$ of their stars. This is because the dark matter halo is initially much more extended than the stars. As such, we find the stellar-to-halo size-ratio (measured using r\$\_\{{\textbackslash}rm\{eff\}\}\$/r\$\_\{{\textbackslash}rm\{vir\}\}\$) is a key parameter controlling the relative amounts of dark matter and stellar stripping. We use simple fitting formulae to measure the relation between the fraction of bound dark matter and fraction of bound stars. We measure a negligible dependence on cluster mass or galaxy mass. Therefore these formulae have general applicability in cosmological simulations, and are ideal to improve stellar stripping recipes in semi-analytical models, and/or to estimate the impact that tidal stripping would have on galaxies when only their halo mass evolution is known.},
urldate = {2016-11-03},
journal = {arXiv:1610.04264 [astro-ph]},
author = {Smith, Rory and Choi, Hoseung and Lee, Jaehyun and Rhee, Jinsu and Sanchez-Janssen, Ruben and Yi, Sukyoung K.},
month = oct,
year = {2016},
note = {arXiv: 1610.04264},
keywords = {Astrophysics - Astrophysics of Galaxies},
}The stellar mass assembly of galaxies in the Illustris simulation: growth by mergers and the spatial distribution of accreted stars. Rodriguez-Gomez, V., Pillepich, A., Sales, L. V., Genel, S., Vogelsberger, M., Zhu, Q., Wellons, S., Nelson, D., Torrey, P., Springel, V., Ma, C., & Hernquist, L. Monthly Notices of the Royal Astronomical Society, 458(3):2371–2390, May, 2016. arXiv: 1511.08804
Paper doi abstract bibtex
Paper doi abstract bibtex We use the Illustris simulation to study the relative contributions of in situ star formation and stellar accretion to the build-up of galaxies over an unprecedentedly wide range of masses (\$M_\{{\textbackslash}ast\} = 10{\textasciicircum}9-10{\textasciicircum}\{12\} {\textbackslash}, \{{\textbackslash}rm M_\{{\textbackslash}odot\}\}\$), galaxy types, environments, and assembly histories. We find that the `two-phase' picture of galaxy formation predicted by some models is a good approximation only for the most massive galaxies in our simulation – namely, the stellar mass growth of galaxies below a few times \$10{\textasciicircum}\{11\} {\textbackslash}, \{{\textbackslash}rm M_\{{\textbackslash}odot\}\}\$ is dominated by in situ star formation at all redshifts. The fraction of the total stellar mass of galaxies at \$z=0\$ contributed by accreted stars shows a strong dependence on galaxy stellar mass, ranging from about 10 per cent for Milky Way-sized galaxies to over 80 per cent for \$M_\{{\textbackslash}ast\} {\textbackslash}approx 10{\textasciicircum}\{12\} {\textbackslash}, \{{\textbackslash}rm M_\{{\textbackslash}odot\}\}\$ objects, yet with a large galaxy-to-galaxy variation. At a fixed stellar mass, elliptical galaxies and those formed at the centres of younger haloes exhibit larger fractions of ex situ stars than disc-like galaxies and those formed in older haloes. On average, \${\textbackslash}sim\$50 per cent of the ex situ stellar mass comes from major mergers (stellar mass ratio \${\textbackslash}mu {\textgreater} 1/4\$), \${\textbackslash}sim\$20 per cent from minor mergers (\$1/10 {\textless} {\textbackslash}mu {\textless} 1/4\$), \${\textbackslash}sim\$20 per cent from very minor mergers (\${\textbackslash}mu {\textless} 1/10\$), and \${\textbackslash}sim\$10 per cent from stars that were stripped from surviving galaxies (e.g. flybys or ongoing mergers). These components are spatially segregated, with in situ stars dominating the innermost regions of galaxies, and ex situ stars being deposited at larger galactocentric distances in order of decreasing merger mass ratio.
@article{rodriguez-gomez_stellar_2016,
title = {The stellar mass assembly of galaxies in the {Illustris} simulation: growth by mergers and the spatial distribution of accreted stars},
volume = {458},
issn = {0035-8711, 1365-2966},
shorttitle = {The stellar mass assembly of galaxies in the {Illustris} simulation},
url = {http://arxiv.org/abs/1511.08804},
doi = {10.1093/mnras/stw456},
abstract = {We use the Illustris simulation to study the relative contributions of in situ star formation and stellar accretion to the build-up of galaxies over an unprecedentedly wide range of masses (\$M\_\{{\textbackslash}ast\} = 10{\textasciicircum}9-10{\textasciicircum}\{12\} {\textbackslash}, \{{\textbackslash}rm M\_\{{\textbackslash}odot\}\}\$), galaxy types, environments, and assembly histories. We find that the `two-phase' picture of galaxy formation predicted by some models is a good approximation only for the most massive galaxies in our simulation -- namely, the stellar mass growth of galaxies below a few times \$10{\textasciicircum}\{11\} {\textbackslash}, \{{\textbackslash}rm M\_\{{\textbackslash}odot\}\}\$ is dominated by in situ star formation at all redshifts. The fraction of the total stellar mass of galaxies at \$z=0\$ contributed by accreted stars shows a strong dependence on galaxy stellar mass, ranging from about 10 per cent for Milky Way-sized galaxies to over 80 per cent for \$M\_\{{\textbackslash}ast\} {\textbackslash}approx 10{\textasciicircum}\{12\} {\textbackslash}, \{{\textbackslash}rm M\_\{{\textbackslash}odot\}\}\$ objects, yet with a large galaxy-to-galaxy variation. At a fixed stellar mass, elliptical galaxies and those formed at the centres of younger haloes exhibit larger fractions of ex situ stars than disc-like galaxies and those formed in older haloes. On average, \${\textbackslash}sim\$50 per cent of the ex situ stellar mass comes from major mergers (stellar mass ratio \${\textbackslash}mu {\textgreater} 1/4\$), \${\textbackslash}sim\$20 per cent from minor mergers (\$1/10 {\textless} {\textbackslash}mu {\textless} 1/4\$), \${\textbackslash}sim\$20 per cent from very minor mergers (\${\textbackslash}mu {\textless} 1/10\$), and \${\textbackslash}sim\$10 per cent from stars that were stripped from surviving galaxies (e.g. flybys or ongoing mergers). These components are spatially segregated, with in situ stars dominating the innermost regions of galaxies, and ex situ stars being deposited at larger galactocentric distances in order of decreasing merger mass ratio.},
number = {3},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Rodriguez-Gomez, Vicente and Pillepich, Annalisa and Sales, Laura V. and Genel, Shy and Vogelsberger, Mark and Zhu, Qirong and Wellons, Sarah and Nelson, Dylan and Torrey, Paul and Springel, Volker and Ma, Chung-Pei and Hernquist, Lars},
month = may,
year = {2016},
note = {arXiv: 1511.08804},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
pages = {2371--2390},
}The photometric properties of galaxies in the early Universe. Wilkins, S. M., Feng, Y., Di-Matteo, T., Croft, R., Stanway, E. R., Bunker, A., Waters, D., & Lovell, C. Monthly Notices of the Royal Astronomical Society, 460:3170–3178, August, 2016.
Paper doi abstract bibtex 2 downloads
Paper doi abstract bibtex 2 downloads We use the large cosmological hydro-dynamic simulation BLUETIDES to predict the photometric properties of galaxies during the epoch of reionization (z = 8-15). These properties include the rest-frame UV to near-IR broad-band spectral energy distributions, the Lyman continuum (LyC) photon production, the UV star formation rate calibration, and intrinsic UV continuum slope. In particular we focus on exploring the effect of various modelling assumptions, including the assumed choice of stellar population synthesis (SPS) model, initial mass function, and the escape fraction of LyC photons, upon these quantities. We find that these modelling assumptions can have a dramatic effect on photometric properties leading to consequences for the accurate determination of physical properties from observations. For example, at z = 8 we predict that nebular emission can account for up to 50 per cent of the rest-frame R-band luminosity, while the choice of SPS model can change the LyC production rate up to a factor of ×2.
@article{wilkins_photometric_2016,
title = {The photometric properties of galaxies in the early {Universe}},
volume = {460},
issn = {0035-8711},
url = {http://adsabs.harvard.edu/abs/2016MNRAS.460.3170W},
doi = {10.1093/mnras/stw1154},
abstract = {We use the large cosmological hydro-dynamic simulation BLUETIDES to predict the photometric properties of galaxies during the epoch of reionization (z = 8-15). These properties include the rest-frame UV to near-IR broad-band spectral energy distributions, the Lyman continuum (LyC) photon production, the UV star formation rate calibration, and intrinsic UV continuum slope. In particular we focus on exploring the effect of various modelling assumptions, including the assumed choice of stellar population synthesis (SPS) model, initial mass function, and the escape fraction of LyC photons, upon these quantities. We find that these modelling assumptions can have a dramatic effect on photometric properties leading to consequences for the accurate determination of physical properties from observations. For example, at z = 8 we predict that nebular emission can account for up to 50 per cent of the
rest-frame R-band luminosity, while the choice of SPS model can change the LyC production rate up to a factor of ×2.},
urldate = {2020-03-26},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Wilkins, Stephen M. and Feng, Yu and Di-Matteo, Tiziana and Croft, Rupert and Stanway, Elizabeth R. and Bunker, Andrew and Waters, Dacen and Lovell, Christopher},
month = aug,
year = {2016},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, galaxies: high-redshift, galaxies: photometry, methods: numerical},
pages = {3170--3178},
}2015 (5)
Spin alignment and differential accretion in merging black hole binaries. Gerosa, D., Veronesi, B., Lodato, G., & Rosotti, G. Monthly Notices of the Royal Astronomical Society, 451(4):3941-3954, August, 2015.
doi bibtex
doi bibtex
@article{2015MNRAS.451.3941G,
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
adsurl = {https://ui.adsabs.harvard.edu/abs/2015MNRAS.451.3941G},
archiveprefix = {arXiv},
author = {{Gerosa}, D. and {Veronesi}, B. and {Lodato}, G. and {Rosotti}, G.},
doi = {10.1093/mnras/stv1214},
eprint = {1503.06807},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {accretion, accretion discs, black hole physics, galaxies: evolution, galaxies: nuclei, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology},
month = aug,
number = {4},
pages = {3941-3954},
primaryclass = {astro-ph.GA},
title = {{Spin alignment and differential accretion in merging black hole binaries}},
volume = {451},
year = 2015,
bdsk-url-1 = {https://doi.org/10.1093/mnras/stv1214}}Physical Models of Galaxy Formation in a Cosmological Framework. Somerville, R. S. & Davé, R. Annual Review of Astronomy and Astrophysics, 53(1):51–113, August, 2015. arXiv: 1412.2712
Paper doi abstract bibtex
Paper doi abstract bibtex Modeling galaxy formation in a cosmological context presents one of the greatest challenges in astrophysics today, due to the vast range of scales and numerous physical processes involved. Here we review the current status of models that employ two leading techniques to simulate the physics of galaxy formation: semi-analytic models and numerical hydrodynamic simulations. We focus on a set of observational targets that describe the evolution of the global and structural properties of galaxies from roughly Cosmic High Noon (\$z{\textbackslash}sim 2-3\$) to the present. Although minor discrepancies remain, overall, models show remarkable convergence between different methods and make predictions that are in qualitative agreement with observations. Modelers seem to have converged on a core set of physical processes that are critical for shaping galaxy properties. This core set includes cosmological accretion, strong stellar-driven winds that are more efficient at low masses, black hole feedback that preferentially suppresses star formation at high masses, and structural and morphological evolution through merging and environmental processes. However, all cosmological models currently adopt phenomenological implementations of many of these core processes, which must be tuned to observations. Many details of how these diverse processes interact within a hierarchical structure formation setting remain poorly understood. Emerging multi-scale simulations are helping to bridge the gap between stellar and cosmological scales, placing models on a firmer, more physically grounded footing. Concurrently, upcoming telescope facilities will provide new challenges and constraints for models, particularly by directly constraining inflows and outflows through observations of gas in and around galaxies.
@article{somerville_physical_2015,
title = {Physical {Models} of {Galaxy} {Formation} in a {Cosmological} {Framework}},
volume = {53},
issn = {0066-4146, 1545-4282},
url = {http://arxiv.org/abs/1412.2712},
doi = {10.1146/annurev-astro-082812-140951},
abstract = {Modeling galaxy formation in a cosmological context presents one of the greatest challenges in astrophysics today, due to the vast range of scales and numerous physical processes involved. Here we review the current status of models that employ two leading techniques to simulate the physics of galaxy formation: semi-analytic models and numerical hydrodynamic simulations. We focus on a set of observational targets that describe the evolution of the global and structural properties of galaxies from roughly Cosmic High Noon (\$z{\textbackslash}sim 2-3\$) to the present. Although minor discrepancies remain, overall, models show remarkable convergence between different methods and make predictions that are in qualitative agreement with observations. Modelers seem to have converged on a core set of physical processes that are critical for shaping galaxy properties. This core set includes cosmological accretion, strong stellar-driven winds that are more efficient at low masses, black hole feedback that preferentially suppresses star formation at high masses, and structural and morphological evolution through merging and environmental processes. However, all cosmological models currently adopt phenomenological implementations of many of these core processes, which must be tuned to observations. Many details of how these diverse processes interact within a hierarchical structure formation setting remain poorly understood. Emerging multi-scale simulations are helping to bridge the gap between stellar and cosmological scales, placing models on a firmer, more physically grounded footing. Concurrently, upcoming telescope facilities will provide new challenges and constraints for models, particularly by directly constraining inflows and outflows through observations of gas in and around galaxies.},
number = {1},
urldate = {2017-05-22},
journal = {Annual Review of Astronomy and Astrophysics},
author = {Somerville, Rachel S. and Davé, Romeel},
month = aug,
year = {2015},
note = {arXiv: 1412.2712},
keywords = {Astrophysics - Astrophysics of Galaxies},
pages = {51--113},
}Multi-timescale analysis of phase transitions in precessing black-hole binaries. Gerosa, D., Kesden, M., Sperhake, U., Berti, E., & O'Shaughnessy, R. Physical Review D, 92(6):064016, September, 2015.
doi bibtex
doi bibtex
@article{2015PhRvD..92f4016G,
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
adsurl = {https://ui.adsabs.harvard.edu/abs/2015PhRvD..92f4016G},
archiveprefix = {arXiv},
author = {{Gerosa}, Davide and {Kesden}, Michael and {Sperhake}, Ulrich and {Berti}, Emanuele and {O'Shaughnessy}, Richard},
doi = {10.1103/PhysRevD.92.064016},
eid = {064016},
eprint = {1506.03492},
journal = {Physical Review D},
keywords = {04.25.dg, 04.30.-w, 04.70.Bw, Numerical studies of black holes and black-hole binaries, Gravitational waves: theory, Classical black holes, General Relativity and Quantum Cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena},
month = sep,
number = {6},
pages = {064016},
primaryclass = {gr-qc},
title = {{Multi-timescale analysis of phase transitions in precessing black-hole binaries}},
volume = {92},
year = 2015,
bdsk-url-1 = {https://doi.org/10.1103/PhysRevD.92.064016}}Missing black holes in brightest cluster galaxies as evidence for the occurrence of superkicks in nature. Gerosa, D. & Sesana, A. Monthly Notices of the Royal Astronomical Society, 446(1):38-55, January, 2015.
doi bibtex
doi bibtex
@article{2015MNRAS.446...38G,
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
adsurl = {https://ui.adsabs.harvard.edu/abs/2015MNRAS.446...38G},
archiveprefix = {arXiv},
author = {{Gerosa}, Davide and {Sesana}, Alberto},
doi = {10.1093/mnras/stu2049},
eprint = {1405.2072},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {Black hole physics, gravitation, gravitational waves, galaxies: evolution, galaxies: interactions, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, General Relativity and Quantum Cosmology},
month = jan,
number = {1},
pages = {38-55},
primaryclass = {astro-ph.GA},
title = {{Missing black holes in brightest cluster galaxies as evidence for the occurrence of superkicks in nature}},
volume = {446},
year = 2015,
bdsk-url-1 = {https://doi.org/10.1093/mnras/stu2049}}An analysis of the evolving comoving number density of galaxies in hydrodynamical simulations. Torrey, P., Wellons, S., Machado, F., Griffen, B., Nelson, D., Rodriguez-Gomez, V., McKinnon, R., Pillepich, A., Ma, C., Vogelsberger, M., Springel, V., & Hernquist, L. Monthly Notices of the Royal Astronomical Society, 454(3):2770–2786, December, 2015. arXiv: 1507.01942
Paper doi abstract bibtex
Paper doi abstract bibtex The cumulative comoving number-density of galaxies as a function of stellar mass or central velocity dispersion is commonly used to link galaxy populations across different epochs. By assuming that galaxies preserve their number-density in time, one can infer the evolution of their properties, such as masses, sizes, and morphologies. However, this assumption does not hold in the presence of galaxy mergers or when rank ordering is broken owing to variable stellar growth rates. We present an analysis of the evolving comoving number density of galaxy populations found in the Illustris cosmological hydrodynamical simulation focused on the redshift range \$0{\textbackslash}leq z {\textbackslash}leq 3\$. Our primary results are as follows: 1) The inferred average stellar mass evolution obtained via a constant comoving number density assumption is systematically biased compared to the merger tree results at the factor of \${\textbackslash}sim\$2(4) level when tracking galaxies from redshift \$z=0\$ out to redshift \$z=2(3)\$; 2) The median number density evolution for galaxy populations tracked forward in time is shallower than for galaxy populations tracked backward in time; 3) A similar evolution in the median number density of tracked galaxy populations is found regardless of whether number density is assigned via stellar mass, stellar velocity dispersion, or dark matter halo mass; 4) Explicit tracking reveals a large diversity in galaxies' assembly histories that cannot be captured by constant number-density analyses; 5) The significant scatter in galaxy linking methods is only marginally reduced by considering a number of additional physical and observable galaxy properties as realized in our simulation. We provide fits for the forward and backward median evolution in stellar mass and number density and discuss implications of our analysis for interpreting multi-epoch galaxy property observations.
@article{torrey_analysis_2015,
title = {An analysis of the evolving comoving number density of galaxies in hydrodynamical simulations},
volume = {454},
issn = {0035-8711, 1365-2966},
url = {http://arxiv.org/abs/1507.01942},
doi = {10.1093/mnras/stv1986},
abstract = {The cumulative comoving number-density of galaxies as a function of stellar mass or central velocity dispersion is commonly used to link galaxy populations across different epochs. By assuming that galaxies preserve their number-density in time, one can infer the evolution of their properties, such as masses, sizes, and morphologies. However, this assumption does not hold in the presence of galaxy mergers or when rank ordering is broken owing to variable stellar growth rates. We present an analysis of the evolving comoving number density of galaxy populations found in the Illustris cosmological hydrodynamical simulation focused on the redshift range \$0{\textbackslash}leq z {\textbackslash}leq 3\$. Our primary results are as follows: 1) The inferred average stellar mass evolution obtained via a constant comoving number density assumption is systematically biased compared to the merger tree results at the factor of \${\textbackslash}sim\$2(4) level when tracking galaxies from redshift \$z=0\$ out to redshift \$z=2(3)\$; 2) The median number density evolution for galaxy populations tracked forward in time is shallower than for galaxy populations tracked backward in time; 3) A similar evolution in the median number density of tracked galaxy populations is found regardless of whether number density is assigned via stellar mass, stellar velocity dispersion, or dark matter halo mass; 4) Explicit tracking reveals a large diversity in galaxies' assembly histories that cannot be captured by constant number-density analyses; 5) The significant scatter in galaxy linking methods is only marginally reduced by considering a number of additional physical and observable galaxy properties as realized in our simulation. We provide fits for the forward and backward median evolution in stellar mass and number density and discuss implications of our analysis for interpreting multi-epoch galaxy property observations.},
number = {3},
urldate = {2016-08-23},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Torrey, Paul and Wellons, Sarah and Machado, Francisco and Griffen, Brendan and Nelson, Dylan and Rodriguez-Gomez, Vicente and McKinnon, Ryan and Pillepich, Annalisa and Ma, Chung-Pei and Vogelsberger, Mark and Springel, Volker and Hernquist, Lars},
month = dec,
year = {2015},
note = {arXiv: 1507.01942},
keywords = {Astrophysics - Astrophysics of Galaxies},
pages = {2770--2786},
}2013 (4)
Black hole mergers: do gas discs lead to spin alignment?. Lodato, G. & Gerosa, D. Monthly Notices of the Royal Astronomical Society, 429:L30-L34, February, 2013.
doi bibtex
doi bibtex
@article{2013MNRAS.429L..30L,
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
adsurl = {https://ui.adsabs.harvard.edu/abs/2013MNRAS.429L..30L},
archiveprefix = {arXiv},
author = {{Lodato}, G. and {Gerosa}, D.},
doi = {10.1093/mnrasl/sls018},
eprint = {1211.0284},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {accretion, accretion discs, black hole physics, galaxies: evolution, galaxies: nuclei, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology},
month = feb,
pages = {L30-L34},
primaryclass = {astro-ph.CO},
title = {{Black hole mergers: do gas discs lead to spin alignment?}},
volume = {429},
year = 2013,
bdsk-url-1 = {https://doi.org/10.1093/mnrasl/sls018}}A Multiplicity Census of Intermediate-mass Stars in Scorpius-Centaurus. Janson, M., Lafrenière, D., Jayawardhana, R., Bonavita, M., Girard, J. H., Brandeker, A., & Gizis, J. E. \apj, 773(2):170, August, 2013.
doi bibtex
doi bibtex
@ARTICLE{2013ApJ...773..170J,
author = {{Janson}, Markus and {Lafreni{\`e}re}, David and {Jayawardhana}, Ray and {Bonavita}, Mariangela and {Girard}, Julien H. and {Brandeker}, Alexis and {Gizis}, John E.},
title = "{A Multiplicity Census of Intermediate-mass Stars in Scorpius-Centaurus}",
journal = {\apj},
keywords = {binaries: general, brown dwarfs, planetary systems, Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies},
year = 2013,
month = aug,
volume = {773},
number = {2},
eid = {170},
pages = {170},
doi = {10.1088/0004-637X/773/2/170},
archivePrefix = {arXiv},
eprint = {1307.2243},
primaryClass = {astro-ph.SR},
adsurl = {https://ui.adsabs.harvard.edu/abs/2013ApJ...773..170J},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}Characterization of the nearby L/T Binary Brown Dwarf WISE J104915.57-531906.1 at 2 pc from the Sun. Kniazev, A., Vaisanen, P., Mužić, K., Mehner, A., Boffin, H., Kurtev, R., Melo, C., Ivanov, V., Girard, J., Mawet, D., Schmidtobreick, L., Huelamo, N., Borissova, J., Minniti, D., Ishibashi, K., Potter, S., Beletsky, Y., Buckley, D., Crawford, S., Gulbis, A., Kotze, P., Miszalski, B., Pickering, T., Romero Colmenero, E., & Williams, T. \apj, 770(2):124, June, 2013.
doi bibtex
doi bibtex
@ARTICLE{2013ApJ...770..124K,
author = {{Kniazev}, A.~Y. and {Vaisanen}, P. and {Mu{\v{z}}i{\'c}}, K. and {Mehner}, A. and {Boffin}, H.~M.~J. and {Kurtev}, R. and {Melo}, C. and {Ivanov}, V.~D. and {Girard}, J. and {Mawet}, D. and {Schmidtobreick}, L. and {Huelamo}, N. and {Borissova}, J. and {Minniti}, D. and {Ishibashi}, K. and {Potter}, S.~B. and {Beletsky}, Y. and {Buckley}, D.~A.~H. and {Crawford}, S. and {Gulbis}, A.~A.~S. and {Kotze}, P. and {Miszalski}, B. and {Pickering}, T.~E. and {Romero Colmenero}, E. and {Williams}, T.~B.},
title = "{Characterization of the nearby L/T Binary Brown Dwarf WISE J104915.57-531906.1 at 2 pc from the Sun}",
journal = {\apj},
keywords = {brown dwarfs, infrared: stars, solar neighborhood, stars: individual: G 171{\textendash}22 HD 55383 WISE J104915.57{\textendash}531906.1, stars: low-mass, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics},
year = 2013,
month = jun,
volume = {770},
number = {2},
eid = {124},
pages = {124},
doi = {10.1088/0004-637X/770/2/124},
archivePrefix = {arXiv},
eprint = {1303.7171},
primaryClass = {astro-ph.GA},
adsurl = {https://ui.adsabs.harvard.edu/abs/2013ApJ...770..124K},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}A Young Protoplanet Candidate Embedded in the Circumstellar Disk of HD 100546. Quanz, S. P., Amara, A., Meyer, M. R., Kenworthy, M. A., Kasper, M., & Girard, J. H. \apjl, 766(1):L1, March, 2013.
doi bibtex
doi bibtex
@ARTICLE{2013ApJ...766L...1Q,
author = {{Quanz}, Sascha P. and {Amara}, Adam and {Meyer}, Michael R. and {Kenworthy}, Matthew A. and {Kasper}, Markus and {Girard}, Julien H.},
title = "{A Young Protoplanet Candidate Embedded in the Circumstellar Disk of HD 100546}",
journal = {\apjl},
keywords = {planet-disk interactions, planets and satellites: formation, protoplanetary disks, stars: formation, stars: individual: HD 100546, Astrophysics - Astrophysics of Galaxies, Astrophysics - Earth and Planetary Astrophysics},
year = 2013,
month = mar,
volume = {766},
number = {1},
eid = {L1},
pages = {L1},
doi = {10.1088/2041-8205/766/1/L1},
archivePrefix = {arXiv},
eprint = {1302.7122},
primaryClass = {astro-ph.GA},
adsurl = {https://ui.adsabs.harvard.edu/abs/2013ApJ...766L...1Q},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}2011 (1)
Searching for Gas Giant Planets on Solar System Scales: VLT NACO/APP Observations of the Debris Disk Host Stars HD172555 and HD115892. Quanz, S. P., Kenworthy, M. A., Meyer, M. R., Girard, J. H., & Kasper, M. \apjl, 736(2):L32, August, 2011.
doi bibtex
doi bibtex
@ARTICLE{2011ApJ...736L..32Q,
author = {{Quanz}, Sascha P. and {Kenworthy}, Matthew A. and {Meyer}, Michael R. and {Girard}, Julien H.~V. and {Kasper}, Markus},
title = "{Searching for Gas Giant Planets on Solar System Scales: VLT NACO/APP Observations of the Debris Disk Host Stars HD172555 and HD115892}",
journal = {\apjl},
keywords = {planetary systems, planets and satellites: detection, planets and satellites: formation, stars: formation, stars: individual: HD172555 HD115892, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Astrophysics of Galaxies},
year = 2011,
month = aug,
volume = {736},
number = {2},
eid = {L32},
pages = {L32},
doi = {10.1088/2041-8205/736/2/L32},
archivePrefix = {arXiv},
eprint = {1106.4528},
primaryClass = {astro-ph.EP},
adsurl = {https://ui.adsabs.harvard.edu/abs/2011ApJ...736L..32Q},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}