Author: "Marc Huertas-Company" / Topic: 01 natural sciences - Searchworks@Jio Institute Digital Library Search Results

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1. Stellar masses of giant clumps in CANDELS and simulated galaxies using machine learning

Author: David C. Koo, Omri Ginzburg, Anton M. Koekemoer, Nir Mandelker, Yicheng Guo, Gregory F. Snyder, Joel R. Primack, Christoph T. Lee, Maxwell Metter, Marc Huertas-Company, Haowen Zhang, Mauro Giavalisco, Daniel Ceverino, Avishai Dekel, Sandra M. Faber, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Sciences, Philosophie, Histoire (SPHERE (UMR_7219)), and Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Disc galaxy, Vela, 01 natural sciences, 0103 physical sciences, Galaxy formation and evolution, galaxies: formation, Astrophysics::Solar and Stellar Astrophysics, galaxies: irregular, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Solar mass, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, methods: data analysis, Redshift, Galaxy, Gravitational lens, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: star formation, galaxies: structure, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: A significant fraction of high redshift star-forming disc galaxies are known to host giant clumps, whose nature and role in galaxy evolution are yet to be understood. In this work we first present a new method based on neural networks to detect clumps in galaxy images. We use this method to detect clumps in the rest-frame optical and UV images of a complete sample of $\sim1500$ star forming galaxies at $1, Comment: Accepted for publication in MNRAS - This is the final version
Published: 2020

2. The evolution of compact massive quiescent and star-forming galaxies derived from the R e– R h and M star– M h relations

Author: Lorenzo Zanisi, H. Fu, Fernando Buitrago, Aldo Rodríguez-Puebla, Paolo Saracco, Andreas L. Faisst, Vladimir Avila-Reese, Lumen Boco, Francesco Shankar, E. Daddi, Avishai Dekel, Annagrazia Puglisi, Mauro Giavalisco, Marc Huertas-Company, Andrea Lapi, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)
Subjects: Stellar mass, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Settore FIS/05 - Astronomia e Astrofisica, galaxies: high-redshift, 0103 physical sciences, Galaxy formation and evolution, 10. No inequality, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Effective radius, Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, Astronomy and Astrophysics, galaxies: fundamental parameters, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Dark matter halo, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: star formation, galaxies: abundances, Halo, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: The mean size ( effective radius $R_e$) of Massive Galaxies (MGs, $M_{\rm star}>10^{11.2}M_\odot$) is observed to increase steadily with cosmic time. It is still unclear whether this trend originates from the size growth of individual galaxies (via, e.g., mergers and/or AGN feedback) or from the inclusion of larger galaxies entering the selection at later epochs (progenitor bias). We here build a data-driven, flexible theoretical framework to probe the structural evolution of MGs. We assign galaxies to dark matter haloes via stellar mass-halo mass (SMHM) relations with varying high-mass slopes and scatters $\sigma_{\rm SMHM}$ in stellar mass at fixed halo mass, and assign sizes to galaxies using an empirically-motivated, constant and linear relationship between $R_e$ and the host dark matter halo radius $R_h$. We find that: 1) the fast mean size growth of MGs is well reproduced independently of the shape of the input SMHM relation; 2) the numbers of compact MGs grow steadily until $z\gtrsim2$ and fall off at lower redshifts, suggesting a lesser role of progenitor bias at later epochs; 3) a time-independent scatter $\sigma_{\rm SMHM}$ is consistent with a scenario in which compact starforming MGs transition into quiescent MGs in a few $10^8$yr with a negligible structural evolution during the compact phase, while a scatter increasing at high redshift implies significant size growth during the starforming phase. A robust measurement of the size function of MGs at high redshift can set strong constraints on the scatter of the SMHM relation and, by extension, on models of galaxy evolution., Comment: Accepted for publication in MNRAS. Comments still welcome
Published: 2021

3. The size function of massive satellites from the R$_e$– R$_h$ and M$_{star}$–M$_h$ relations: constraining the role of environment

Author: Lorenzo Zanisi, Marc Huertas-Company, Mariangela Bernardi, Francesco Shankar, Simona Mei, University of Southampton, Department of Physics and Astronomy [Philadelphia], University of Pennsylvania [Philadelphia], AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Instituto de Astrofisica de Canarias (IAC), University of Pennsylvania, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
Subjects: galaxies: spiral, Dark matter, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Star (graph theory), 01 natural sciences, cD, 0103 physical sciences, Satellite galaxy, Cluster (physics), Astrophysics::Solar and Stellar Astrophysics, galaxies: elliptical and lenticular, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Size function, Physics, [PHYS]Physics [physics], education.field_of_study, 010308 nuclear & particles physics, Astronomy and Astrophysics, galaxies: fundamental parameters, Astrophysics - Astrophysics of Galaxies, Galaxy, galaxies: haloes, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Physics::Space Physics, galaxies: abundances, Astrophysics::Earth and Planetary Astrophysics, Halo, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: In previous work we showed that a semi-empirical model in which galaxies in host dark matter haloes are assigned stellar masses via a stellar mass-halo mass (SMHM) relation and sizes ($R_e$) via a linear and tight $R_e-R_h$ relation, can faithfully reproduce the size function of local SDSS central galaxies and the strong size evolution of massive galaxies (MGs, $M_{\rm star}>10^{11.2}M_\odot$). In this third paper of the series, we focus on the population of satellite MGs. We find that without any additional calibration and irrespective of the exact SMHM relation, fraction of quenched galaxies or level of stellar stripping, the same model is able to reproduce the local size function of quiescent satellite MGs in SDSS. In addition, the same model can reproduce the puzzling weak dependence of mean size on host halo mass for both central and satellite galaxies. The model also matches the size function of starforming satellite MGs, after assuming that some of them transform into massive lenticulars in a few Gyr after infalling in the group/cluster environment. However, the vast majority of satellite lenticulars is predicted to form before infall. The $R_e-R_h$ appears to be fundamental to connect galaxies and their host haloes., Accepted for publication in MNRAS. 5 pages, 3 figures. Comments and suggestions still welcome
Published: 2021

4. Anomaly detection in Hyper Suprime-Cam galaxy images with generative adversarial networks

Author: J. Xavier Prochaska, Nesar Ramachandra, Yifei Luo, Francois Lanusse, Kate Storey-Fisher, Alexie Leauthaud, Song Huang, Marc Huertas-Company, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
Subjects: FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy merger, Astronomical survey, 01 natural sciences, 0103 physical sciences, Cluster analysis, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Dwarf galaxy, Physics, [PHYS]Physics [physics], methods: statistical, galaxies: individual: COSMOS 244571, 010308 nuclear & particles physics, business.industry, Astronomy and Astrophysics, Pattern recognition, galaxies: peculiar, Autoencoder, methods: data analysis, galaxies: general, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Anomaly detection, Artificial intelligence, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Anomaly (physics), business, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The problem of anomaly detection in astronomical surveys is becoming increasingly important as data sets grow in size. We present the results of an unsupervised anomaly detection method using a Wasserstein generative adversarial network (WGAN) on nearly one million optical galaxy images in the Hyper Suprime-Cam (HSC) survey. The WGAN learns to generate realistic HSC-like galaxies that follow the distribution of the data set; anomalous images are defined based on a poor reconstruction by the generator and outlying features learned by the discriminator. We find that the discriminator is more attuned to potentially interesting anomalies compared to the generator, and compared to a simpler autoencoder-based anomaly detection approach, so we use the discriminator-selected images to construct a high-anomaly sample of $\sim$13,000 objects. We propose a new approach to further characterize these anomalous images: we use a convolutional autoencoder to reduce the dimensionality of the residual differences between the real and WGAN-reconstructed images and perform UMAP clustering on these. We report detected anomalies of interest including galaxy mergers, tidal features, and extreme star-forming galaxies. A follow-up spectroscopic analysis of one of these anomalies is detailed in the Appendix; we find that it is an unusual system most likely to be a metal-poor dwarf galaxy with an extremely blue, higher-metallicity HII region. We have released a catalog with the WGAN anomaly scores; the code and catalog are available at https://github.com/kstoreyf/anomalies-GAN-HSC, and our interactive visualization tool for exploring the clustered data is at https://weirdgalaxi.es., Published in MNRAS
Published: 2021

5. A deep learning approach to test the small-scale galaxy morphology and its relationship with star formation activity in hydrodynamical simulations

Author: Connor Bottrell, Lars Hernquist, Marc Huertas-Company, Annalisa Pillepich, Dylan Nelson, Mark Vogelsberger, Vicente Rodriguez-Gomez, Lorenzo Zanisi, François Lanusse, Francesco Shankar, Joel R. Primack, Berta Margalef-Bentabol, Avishai Dekel, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)
Subjects: media_common.quotation_subject, Scale (descriptive set theory), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, methods: numerical, 0103 physical sciences, Galaxy formation and evolution, 010303 astronomy & astrophysics, Scaling, Astrophysics::Galaxy Astrophysics, media_common, Physics, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, galaxies: fundamental parameters, Galaxy, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Autoregressive model, Space and Planetary Science, Sky, methods: miscellaneous, galaxies: star formation, Metric (mathematics), galaxies: structure, galaxies: evolution
Abstract: Accepted for publication in MNRAS. Comments welcome; International audience; 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 small-scale morphological details of galaxies from the sky background. We are able to 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 mostly driven by small, more spheroidal, and quenched galaxies that 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 discy galaxies, may stem from a still too coarse numerical resolution, which struggles to properly capture the inner, dense regions of quenched spheroidal galaxies.
Published: 2021

6. Extending the evolution of the stellar mass-size relation at z < 2 to low stellar mass galaxies from HFF and CANDELS

Author: Mauro Stefanon, Thomas H. Puzia, Kalina V. Nedkova, P. Dimauro, Nicholas Martis, Elizabeth J. McGrath, Rosalind E. Skelton, Heath Shipley, Henry C. Ferguson, Gabriel B. Brammer, Yasna Ordenes-Briceño, Arjen van der Wel, B. Häußler, Jeyhan S. Kartaltepe, Pascal Oesch, Erin Kado-Fong, Katherine E. Whitaker, Marc Huertas-Company, Paul Eigenthaler, Adina D. Feinstein, Adam Muzzin, Danilo Marchesini, Daniel Lange-Vagle, Brooke Simmons, Evelyn J. Johnston, Ivo Labbé, Tufts University [Medford], European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Observatorio Nacional [Rio de Janeiro], IT University of Copenhagen, Cosmic Dawn Center (DAWN), Pontificia Universidad Católica de Chile (UC), University of Chicago, Space Telescope Science Institute (STSci), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Instituto de Astrofisica de Canarias (IAC), Universidad Diego Portales [Santiago] (UDP), Princeton University, Rochester Institute of Technology, Swinburne University of Technology (Hawthorn campus), Colby College, York University [Toronto], McGill University = Université McGill [Montréal, Canada], Lancaster University, South African Astronomical Observatory (SAAO), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Universiteit Gent = Ghent University [Belgium] (UGENT), University of Massachusetts [Amherst] (UMass Amherst), and University of Massachusetts System (UMASS)
Subjects: PASSIVE GALAXIES, Stellar mass, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics - astrophysics of galaxies, REDSHIFT, FOS: Physical sciences, DWARF ELLIPTIC GALAXIES, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Power law, STAR-FORMATION, structure -galaxies, high-redshift, Galaxies: structure, 0103 physical sciences, galaxies, Astrophysics::Solar and Stellar Astrophysics, COLOR, Fornax Cluster, 010303 astronomy & astrophysics, COMPACT, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Dwarf galaxy, Physics, [PHYS]Physics [physics], CLUSTER GALAXIES, 010308 nuclear & particles physics, Galaxies: high-redshift, Galaxies: evolution, Astronomy and Astrophysics, Radius, ENVIRONMENTAL DEPENDENCE, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, evolution -galaxies, ASSEMBLY GAMA, Physics and Astronomy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), structure [galaxies], QUIESCENT GALAXIES, Astrophysics::Earth and Planetary Astrophysics, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Low Mass, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], high-redshift [galaxies]
Abstract: We reliably extend the stellar mass-size relation over $0.2\leq z \leq2$ to low stellar mass galaxies by combining the depth of Hubble Frontier Fields (HFF) with the large volume covered by CANDELS. Galaxies are simultaneously modelled in multiple bands using the tools developed by the MegaMorph project, allowing robust size (i.e., half-light radius) estimates even for small, faint, and high redshift galaxies. We show that above 10$^7$M$_\odot$, star-forming galaxies are well represented by a single power law on the mass-size plane over our entire redshift range. Conversely, the stellar mass-size relation is steep for quiescent galaxies with stellar masses $\geq 10^{10.3}$M$_\odot$ and flattens at lower masses, regardless of whether quiescence is selected based on star-formation activity, rest-frame colours, or structural characteristics. This flattening occurs at sizes of $\sim1$kpc at $z\leq1$. As a result, a double power law is preferred for the stellar mass-size relation of quiescent galaxies, at least above 10$^7$M$_\odot$. We find no strong redshift dependence in the slope of the relation of star-forming galaxies as well as of high mass quiescent galaxies. We also show that star-forming galaxies with stellar masses $\geq$10$^{9.5}$M$_\odot$ and quiescent galaxies with stellar masses $\geq10^{10.3}$M$_\odot$ have undergone significant size growth since $z\sim2$, as expected; however, low mass galaxies have not. Finally, we supplement our data with predominantly quiescent dwarf galaxies from the core of the Fornax cluster, showing that the stellar mass-size relation is continuous below 10$^7$M$_\odot$, but a more complicated functional form is necessary to describe the relation., Comment: 30 pages, 19 figures, Accepted for publication in MNRAS
Published: 2021

7. Pushing automated morphological classifications to their limits with the Dark Energy Survey

Author: Mariangela Bernardi, E. Suchyta, J. Carretero, M. Carrasco Kind, Christopher J. Conselice, A. G. Kim, A. Carnero Rosell, Felipe Menanteau, Marc Huertas-Company, E. Bertin, W. G. Hartley, I. Ferrero, Matt J. Jarvis, David J. Brooks, Jesús Vega-Ferrero, Samuel Hinton, Josh Frieman, J. Gschwend, M. E. C. Swanson, M. Smith, G. Gutierrez, D. L. Hollowood, Pablo Fosalba, R. L. C. Ogando, S. Serrano, Santiago Avila, Daniel Gruen, Ramon Miquel, H. Domínguez Sánchez, V. Scarpine, A. Choi, I. Sevilla-Noarbe, K. Honscheid, N. Kuropatkin, T. N. Varga, S. Desai, David Bacon, L. N. da Costa, S. Allam, Marcos Lima, G. Tarle, Michael Schubnell, Robert A. Gruendl, Ben Hoyle, Maria E. S. Pereira, Chun-Hao To, E. J. Sanchez, Antonella Palmese, B. Margalef, M. A. G. Maia, Michel Aguena, Robert Morgan, F. Tarsitano, F. Paz-Chinchón, A. K. Romer, J. De Vicente, A. A. Plazas, Douglas L. Tucker, Kyler Kuehn, M. Costanzi, R. D. Wilkinson, Juan Garcia-Bellido, J. Annis, National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), European Commission, Generalitat de Catalunya, Instituto Nacional de Ciência e Tecnologia (Brasil), Vega-Ferrero, J., Domínguez Sánchez, H., Bernardi, M., Huertas-Company, M., Morgan, R., Margalef, B., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bertin, E., Brooks, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Choi, A., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Ferrero, I., Fosalba, P., Frieman, J., García-Bellido, J., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., Jarvis, M., Kim, A. G., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Tarsitano, F., To, C., Tucker, D. L., Varga, T. N., Wilkinson, R. D., Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), structure [Galaxies], FOS: Physical sciences, Classification scheme, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Convolutional neural network, Astrophysics - Astrophysics of Galaxie, 0103 physical sciences, observational [Methods], 010303 astronomy & astrophysics, Lenticular galaxy, catalogues, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, business.industry, Deep learning, Astronomy and Astrophysics, Pattern recognition, Catalogues, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Dark energy, galaxies: structure, Artificial intelligence, methods: observational, Astrophysics - Cosmology and Nongalactic Astrophysics, catalogue, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Data release
Abstract: Vega-Ferrero, J., et al., We present morphological classifications of ∼27 million galaxies from the Dark Energy Survey (DES) Data Release 1 (DR1) using a supervised deep learning algorithm. The classification scheme separates: (a) early-type galaxies (ETGs) from late-type galaxies (LTGs); and (b) face-on galaxies from edge-on. Our convolutional neural networks (CNNs) are trained on a small subset of DES objects with previously known classifications. These typically have mr ≲ 17.7 mag; we model fainter objects to mr < 21.5 mag by simulating what the brighter objects with well-determined classifications would look like if they were at higher redshifts. The CNNs reach 97 per cent accuracy to mr < 21.5 on their training sets, suggesting that they are able to recover features more accurately than the human eye. We then used the trained CNNs to classify the vast majority of the other DES images. The final catalogue comprises five independent CNN predictions for each classification scheme, helping to determine if the CNN predictions are robust or not. We obtain secure classifications for ∼87 per cent and 73 per cent of the catalogue for the ETG versus LTG and edge-on versus face-on models, respectively. Combining the two classifications (a) and (b) helps to increase the purity of the ETG sample and to identify edge-on lenticular galaxies (as ETGs with high ellipticity). Where a comparison is possible, our classifications correlate very well with Sérsic index (n), ellipticity (ϵ), and spectral type, even for the fainter galaxies. This is the largest multiband catalogue of automated galaxy morphologies to date., The DES data management system is supported by the National Science Foundation under grant numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract no. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2021

8. The Next Generation Virgo Cluster Survey (NGVS). XIV. The Discovery of Low-mass Galaxies and a New Galaxy Catalog in the Core of the Virgo Cluster

Author: Andrés Jordán, Michele Cantiello, Lauren A. MacArthur, Eric Emsellem, Laura Ferrarese, Stephen Gwyn, Alessandro Boselli, James E. Taylor, J. Christopher Mihos, Thomas H. Puzia, Joel Roediger, Giuseppe Gavazzi, Jean-Charles Cuillandre, Patrick Côté, John P. Blakeslee, Chengze Liu, Puragra Guhathakurta, David Schade, Thomas Erben, Rubén Sánchez-Janssen, Patrick R. Durrell, Ariane Lançon, Pierre-Alain Duc, Elisa Toloba, Eric W. Peng, Stéphane Courteau, Hong-Xin Zhang, Fred Boyer, Simona Mei, Matthew Santos, Marc Huertas-Company, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, and Université Paris sciences et lettres (PSL)
Subjects: Physics, galaxies: clusters: individual (Virgo), 010308 nuclear & particles physics, Astronomy, galaxies: fundamental parameters, Astronomy and Astrophysics, 01 natural sciences, Virgo Cluster, Galaxy, Core (optical fiber), Space and Planetary Science, [SDU]Sciences of the Universe [physics], 0103 physical sciences, galaxies: stellar content, galaxies: structure, galaxies: distances and redshifts, galaxies: nuclei, Space Science, Low Mass, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS
Abstract: The Next Generation Virgo Cluster Survey (NGVS) was designed to provide a deep census of baryonic structures in the Virgo cluster. The survey covers the 104 deg2 area from the core of Virgo out to one virial radius, in the u*griz bandpasses, to a point-source depth of g ∼ 25.9 mag (10σ) and a single pixel surface brightness limit of μg ∼ 29 mag arcsec-2 (2σ above the sky). Here we present the final catalog of 404 Virgo galaxies located within a 3.71 deg2 (0.3 Mpc2) region centered on M87, Virgo's dominant galaxy. Of these, 154 were previously uncataloged and span the range 17.8 mag < g < 23.7 mag (-13.4 mag < Mg < -7.4 mag at the 16.5 Mpc distance of Virgo). Extensive simulations show that the NGVS catalog is complete down to g = 18.6 mag (Mg = -12.5 mag, corresponding to a stellar mass ${ \mathcal M }\sim 1.6\times {10}^{7}{{ \mathcal M }}_{\odot }$ for an old stellar population), and 50% complete at g = 22.0 mag (Mg = -9.1 mag, ${ \mathcal M }\sim 6.2\times {10}^{5}{{ \mathcal M }}_{\odot }$ ). The NGVS 50% completeness limit is 3 mag deeper than that of the Virgo Cluster Catalog (VCC), which has served as Virgo's reference standard for over a quarter century, and 2 mag deeper than the VCC detection limit. We discuss the procedure adopted for the identification of objects and the criteria used to assess cluster membership. For each of the 404 galaxies in the NGVS Virgo Cluster core catalog, we present photometric and structural parameters based on a nonparametric curve-of-growth and isophotal analysis, as well as parametric (Sérsic, double-Sérsic, and/or core-Sérsic) fits to the one-dimensional surface brightness profiles and two-dimensional light distributions.
Published: 2020

9. Galaxy sizes and the galaxy-halo connection - I. The remarkable tightness of the size distributions

Author: Mariangela Bernardi, Lorenzo Zanisi, Nicola Menci, Philip J. Grylls, Andrea Lapi, Christopher Duckworth, Marc Huertas-Company, Paolo Salucci, Francesco Shankar, ITA, USA, GBR, and University of St Andrews. School of Physics and Astronomy
Subjects: galaxies: spiral, Angular momentum, Stellar mass, structure [Galaxies], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, disc [Galaxies], Disc galaxy, 01 natural sciences, Virial theorem, Settore FIS/05 - Astronomia e Astrofisica, galaxies: structure, galaxies: formation, galaxies: fundamental parameters, galaxies: kinematics and dynamics, Astrophysics - Astrophysics of Galaxies, 0103 physical sciences, Galaxy formation and evolution, QB Astronomy, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, QB, Physics, 010308 nuclear & particles physics, kinematics and dynamics [Galaxies], Astronomy and Astrophysics, 3rd-DAS, formation [Galaxies], Galaxy, Dark matter halo, QC Physics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), fundamental parameters [Galaxies], Halo, Astrophysics::Earth and Planetary Astrophysics
Abstract: The mass and structural assembly of galaxies is a matter of intense debate. Current theoretical models predict the existence of a linear relationship between galaxy size ($R_e$) and the host dark matter halo virial radius ($R_h$).\\ By making use of semi-empirical models compared to the size distributions of central galaxies from the Sloan Digital Sky Survey, we provide robust constraints on the normalization and scatter of the $R_e-R_h$ relation. We explore the parameter space of models in which the $R_e-R_h$ relation is mediated by either the spin parameter or the concentration of the host halo, or a simple constant the nature of which is in principle unknown. We find that the data require extremely tight relations for both early-type and late-type galaxies (ETGs,LTGs), especially for more massive galaxies. These constraints challenge models based solely on angular momentum conservation, which predict significantly wider distributions of galaxy sizes and no trend with stellar mass, if taken at face value. We discuss physically-motivated alterations to the original models that bring the predictions into better agreement with the data. We argue that the measured tight size distributions of SDSS disk galaxies can be reproduced by semi-empirical models in which the $R_e-R_h$ connection is mediated by the \emph{stellar} specific angular momenta $j_{star}.$ We find that current cosmological models of galaxy formation broadly agree with our constraints for LTGs, and justify the strong link between $R_e$ and $j_{star}$ that we propose, however the tightness of the $R_e-R_h$ relation found in such ab-initio theoretical models for ETGs is in tension with our semi-empirical findings., 22 pages, 14 figures
Published: 2020

10. The bivariate gas–stellar mass distributions and the mass functions of early- and late-type galaxies at

Author: Aldo Rodríguez-Puebla, A. R. Calette, Vicente Rodriguez-Gomez, Marc Huertas-Company, and Vladimir Avila-Reese
Subjects: Physics, Stellar mass, Mass distribution, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Redshift, Galaxy, Baryon, Stars, Space and Planetary Science, 0103 physical sciences, Galaxy formation and evolution, Surface brightness, 010303 astronomy & astrophysics
Abstract: We report the bivariate $\rm HI$ - and $\rm H_{2}$ -stellar mass distributions of local galaxies in addition of an inventory of galaxy mass functions, MFs, for $\rm HI$ , $\rm H_{2}$ , cold gas, and baryonic mass, separately into early- and late-type galaxies. The MFs are determined using the $\rm HI$ and $\rm H_{2}$ conditional distributions and the galaxy stellar mass function (GSMF). For the conditional distributions we use the results from the compilation presented in Calette et al. [(2018) RMxAA, 54, 443.]. For determining the GSMF from $M_{*}\sim3\times10^{7}$ to $3\times10^{12}\ \text{M}_{\odot}$ , we combine two spectroscopic samples from the Sloan Digital Sky Survey at the redshift range $0.0033 . We find that the low-mass end slope of the GSMF, after correcting from surface brightness incompleteness, is $\alpha\approx-1.4$ , consistent with previous determinations. The obtained $\rm HI\,$ MFs agree with radio blind surveys. Similarly, the $\rm H_{2}\,$ MFs are consistent with CO follow-up optically-selected samples. We estimate the impact of systematics due to mass-to-light ratios and find that our MFs are robust against systematic errors. We deconvolve our MFs from random errors to obtain the intrinsic MFs. Using the MFs, we calculate cosmic density parameters of all the baryonic components. Baryons locked inside galaxies represent 5.4% of the universal baryon content, while $\sim\! 96\%$ of the $\rm HI$ and $\rm H_{2}$ mass inside galaxies reside in late-type morphologies. Our results imply cosmic depletion times of $\rm H_{2}$ and total neutral H in late-type galaxies of $\sim\!1.3$ and 7.2 Gyr, respectively, which shows that late type galaxies are on average inefficient in converting $\rm H_{2}$ into stars and in transforming $\rm HI$ gas into $\rm H_{2}$ . Our results provide a fully self-consistent empirical description of galaxy demographics in terms of the bivariate gas–stellar mass distribution and their projections, the MFs. This description is ideal to compare and/or to constrain galaxy formation models.
Published: 2020

11. The nature of giant clumps in high-z discs: a deep-learning comparison of simulations and observations

Author: Nir Mandelker, Omri Ginzburg, Marc Huertas-Company, Joel R. Primack, Daniel Ceverino, Gregory F. Snyder, Avishai Dekel, UAM. Departamento de Física Teórica, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)
Subjects: Galaxies: Structure, Population, FOS: Physical sciences, Star Formation [Galaxies], Formation [Galaxies], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Disc galaxy, Vela, 01 natural sciences, Evolution [Galaxies], 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, education, Galaxies: Star Formation, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Galaxies:Evolution, Physics, [PHYS]Physics [physics], education.field_of_study, 010308 nuclear & particles physics, Galaxies: Formation, Galaxies: Irregular, Física, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Supernova, Irregular [Galaxies], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), High mass, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Structure [Galaxies]
Abstract: We use deep learning to explore the nature of observed giant clumps in high-redshift disc galaxies, based on their identification and classification in cosmological simulations. Simulated clumps are detected using the 3D gas and stellar densities in the VELA zoom-in cosmological simulation suite, with $\sim \!\! 25\ \!\rm{pc}$ maximum resolution, targeting main sequence galaxies at $1\!, Comment: 17 pages, 13 figures. Accepted for publication in MNRAS
Published: 2020
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12. Beyond the Hubble Sequence -- Exploring Galaxy Morphology with Unsupervised Machine Learning

Author: Marc Huertas-Company, Nesar Ramachandra, Brant Robertson, Christopher J. Conselice, Alfonso Aragón-Salamanca, Ting-Yun Cheng, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)
Subjects: Feature extraction, FOS: Physical sciences, techniques: image processing, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Hubble sequence, symbols.namesake, 0103 physical sciences, 10. No inequality, Cluster analysis, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, business.industry, Astronomy and Astrophysics, Pattern recognition, Astrophysics - Astrophysics of Galaxies, Autoencoder, galaxies: general, methods: data analysis, Galaxy, Hierarchical clustering, Binary classification, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), symbols, Unsupervised learning, Artificial intelligence, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We explore unsupervised machine learning for galaxy morphology analyses using a combination of feature extraction with a vector-quantised variational autoencoder (VQ-VAE) and hierarchical clustering (HC). We propose a new methodology that includes: (1) consideration of the clustering performance simultaneously when learning features from images; (2) allowing for various distance thresholds within the HC algorithm; (3) using the galaxy orientation to determine the number of clusters. This setup provides 27 clusters created with this unsupervised learning which we show are well separated based on galaxy shape and structure (e.g., S\'ersic index, concentration, asymmetry, Gini coefficient). These resulting clusters also correlate well with physical properties such as the colour-magnitude diagram, and span the range of scaling-relations such as mass vs. size amongst the different machine-defined clusters. When we merge these multiple clusters into two large preliminary clusters to provide a binary classification, an accuracy of $\sim87\%$ is reached using an imbalanced dataset, matching real galaxy distributions, which includes 22.7\% early-type galaxies and 77.3\% late-type galaxies. Comparing the given clusters with classic Hubble types (ellipticals, lenticulars, early spirals, late spirals, and irregulars), we show that there is an intrinsic vagueness in visual classification systems, in particular galaxies with transitional features such as lenticulars and early spirals. Based on this, the main result in this work is not how well our unsupervised method matches visual classifications and physical properties, but that the method provides an independent classification that may be more physically meaningful than any visually based ones., Comment: 22 pages, 18 figures. Accepted by MNRAS
Published: 2020
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13. Photometry of high-redshift blended galaxies using deep learning

Author: Nima Sedaghat, A. M. M. Trindade, A. Boucaud, Ben Moews, Caroline Heneka, Marc Huertas-Company, Emiliano Merlin, Madhura Killedar, Valerio Roscani, Emille E. O. Ishida, Marco Castellano, Andrea Tramacere, H. Dole, Rafael S. de Souza, AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Observatoire de Paris, PSL Research University (PSL), Instituto de Astrofisica de Canarias (IAC), Université Blaise Pascal - Clermont-Ferrand 2 (UBP), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)
Subjects: FOS: Physical sciences, Astrophysics, 01 natural sciences, Photometry (optics), Spitzer Space Telescope, 0103 physical sciences, Monochrome, Projection (set theory), Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, [PHYS]Physics [physics], Physics, 010308 nuclear & particles physics, business.industry, Deep learning, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Data set, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Artificial intelligence, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], business
Abstract: The new generation of deep photometric surveys requires unprecedentedly precise shape and photometry measurements of billions of galaxies to achieve their main science goals. At such depths, one major limiting factor is the blending of galaxies due to line-of-sight projection, with an expected fraction of blended galaxies of up to 50%. Current deblending approaches are in most cases either too slow or not accurate enough to reach the level of requirements. This work explores the use of deep neural networks to estimate the photometry of blended pairs of galaxies in monochrome space images, similar to the ones that will be delivered by the Euclid space telescope. Using a clean sample of isolated galaxies from the CANDELS survey, we artificially blend them and train two different network models to recover the photometry of the two galaxies. We show that our approach can recover the original photometry of the galaxies before being blended with $\sim$7% accuracy without any human intervention and without any assumption on the galaxy shape. This represents an improvement of at least a factor of 4 compared to the classical SExtractor approach. We also show that forcing the network to simultaneously estimate a binary segmentation map results in a slightly improved photometry. All data products and codes will be made public to ease the comparison with other approaches on a common data set., Comment: 16 pages, 12 figures, submitted to MNRAS, comments welcome
Published: 2019

14. Stellar mass functions and implications for a variable IMF

Author: Ravi K. Sheth, J. L. Fischer, Vinu Vikram, A. Meert, Mariangela Bernardi, Francesco Shankar, H. Domínguez-Sánchez, Marc Huertas-Company, Kyu-Hyun Chae, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Initial mass function, Stellar mass, Stellar population, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, 0103 physical sciences, 010303 astronomy & astrophysics, galaxies: kinematics and dynamics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astronomy, Velocity dispersion, galaxies: fundamental parameters, Astronomy and Astrophysics, Virial mass, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, galaxies: luminosity function, mass function, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: structure, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Fundamental plane (elliptical galaxies), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Spatially resolved kinematics of nearby galaxies has shown that the ratio of dynamical- to stellar population-based estimates of the mass of a galaxy ($M_*^{\rm JAM}/M_*$) correlates with $\sigma_e$, if $M_*$ is estimated using the same IMF for all galaxies and the stellar M/L ratio within each galaxy is constant. This correlation may indicate that, in fact, the IMF is more dwarf-rich for galaxies with large $\sigma$. We use this correlation to estimate a dynamical or IMF-corrected stellar mass, $M_*^{\rm \alpha_{JAM}}$, from $M_{*}$ and $\sigma_e$ for a sample of $6 \times 10^5$ SDSS galaxies for which spatially resolved kinematics is not available. We also compute the `virial' mass estimate $k(n,R)\,R_e\,\sigma_R^2/G$, where $n$ is the Sersic index, in the SDSS and ATLAS$^{\rm 3D}$ samples. We show that an $n$-dependent correction must be applied to the $k(n,R)$ values provided by Prugniel & Simien (1997). Our analysis also shows that the shape of the velocity dispersion profile in the ATLAS$^{\rm 3D}$ sample varies weakly with $n$: $(\sigma_R/\sigma_e) = (R/R_e)^{-\gamma(n)}$. The resulting stellar mass functions, based on $M_*^{\rm \alpha_{JAM}}$ and the recalibrated virial mass, are in good agreement. If the $M_*^{\rm \alpha_{JAM}}/M_* - \sigma_e$ correlation is indeed due to the IMF, and stellar M/L gradients can be ignored, then our $\phi(M_*^{\rm \alpha_{JAM}})$ is an estimate of the stellar mass function in which $\sigma_e$-dependent variations in the IMF across the population have been accounted for. Using a Fundamental Plane based observational proxy for $\sigma_e$ produces comparable results. By demonstrating that cheaper proxies are sufficiently accurate, our analysis should enable a more reliable census of the mass in stars for large galaxy samples, at a fraction of the cost. Our results are provided in tabular form., Comment: 17 pages, 19 figures, 4 tables. Accepted for publication by MNRAS. Tables 1, C1 and C2 are provided as ancillary files
Published: 2017

15. A Duality in the Origin of Bulges and Spheroidal Galaxies

Author: Marc Huertas-Company, Antonio Hernán-Caballero, Giulia Rodighiero, Anton M. Koekemoer, P. Dimauro, Helena Domínguez-Sánchez, Jairo Méndez-Abreu, Emanuele Daddi, Fernando Buitrago, Daniel Ceverino, Belén Alcalde-Pampliega, Pablo G. Pérez-González, Néstor Espino-Briones, L. Costantin, Constantin, L. [0000-0001-6820-0015], Pérez González, P. G. [0000-0003-4528-5639], Méndez Abreu, J. [0000-0002-8766-2597], Huertas Company, M. [0000-0002-1416-8483], Dimauro, P. [0000-0001-7399-2854], Alcalde Pampliega, B. [0000-0002-4140-0428], Buitrago, F. [0000-0002-2861-9812], Caverino, D. [0000-0002-8680-248X], Daddi, E. [0000-0002-3331-9590], Domínguez Sánchez, H. [0000-0002-9013-1316], Espino Briones, N. [0000-0001-6426-3844], Hernán Caballero, A. [0000-0002-4237-5500], Koekemoer, A. M. [0000-0002-6610-2048], and Rodighiero, G. [0000-0002-9415-2296]
Subjects: Astrofísica, Galaxy structure, 010504 meteorology & atmospheric sciences, Stellar population, media_common.quotation_subject, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy properties, 01 natural sciences, Galaxy spheroids, Bulge, Galaxy evolution, 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, Galaxy disks, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Galaxy bulges, 0105 earth and related environmental sciences, media_common, Physics, Galaxy formation, Galaxy ages, Star formation, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Universe, Redshift, Astronomía, Galaxy stellar content, Galaxy quenching, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics
Abstract: Studying the resolved stellar populations of the different structural components which build massive galaxies directly unveils their assembly history. We aim at characterizing the stellar population properties of a representative sample of bulges and pure spheroids in massive galaxies ($M_{\star}>10^{10}$ M$_{\odot}$) in the GOODS-N field. We take advantage of the spectral and spatial information provided by SHARDS and HST data to perform the multi-image spectro-photometrical decoupling of the galaxy light. We derive the spectral energy distribution separately for bulges and disks in the redshift range $0.14, Comment: Accepted for publication in ApJ. 27 pages, 18 figures
Published: 2021

16. Quenching as a Contest between Galaxy Halos and their Central Black Holes

Author: Sandro Tacchella, Fengshan Liu, Dale D. Kocevski, Fangzhou Jiang, Bryan A. Terrazas, Mauro Giavalisco, Jerome J. Fang, Viraj Pandya, S. M. Faber, Zhijian Luo, Guillermo Barro, A. van der Wel, Samir Salim, Chenggang Shu, Marc Huertas-Company, Aldo Rodríguez-Puebla, David C. Koo, Lin Lin, Henry C. Ferguson, Joel R. Primack, Rachel S. Somerville, Joanna Woo, Camilla Pacifici, Avishai Dekel, Zhu Chen, Eric F. Bell, Susan A. Kassin, Hassen M. Yesuf, Yicheng Guo, and Yifei Luo
Subjects: Physics, Supermassive black hole, 010504 meteorology & atmospheric sciences, Stellar mass, Star formation, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, Physical cosmology, Black hole, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Galaxy formation and evolution, Halo, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract: Existing models of galaxy formation have not yet explained striking correlations between structure and star-formation activity in galaxies, notably the sloped and moving boundaries that divide star-forming from quenched galaxies in key structural diagrams. This paper uses these and other relations to ``reverse-engineer'' the quenching process for central galaxies. The basic idea is that star-forming galaxies with larger radii (at a given stellar mass) have lower black-hole masses due to lower central densities. Galaxies cross into the green valley when the cumulative effective energy radiated by their black hole equals $\sim4\times$ their halo-gas binding energy. Since larger-radii galaxies have smaller black holes, one finds they must evolve to higher stellar masses in order to meet this halo-energy criterion, which explains the sloping boundaries. A possible cause of radii differences among star-forming galaxies is halo concentration. The evolutionary tracks of star-forming galaxies are nearly parallel to the green-valley boundaries, and it is mainly the sideways motions of these boundaries with cosmic time that cause galaxies to quench. BH-scaling laws for star-forming, quenched, and green-valley galaxies are different, and most BH mass growth takes place in the green valley. Implications include: the radii of star-forming galaxies are an important second parameter in shaping their black holes; black holes are connected to their halos but in different ways for star-forming, quenched, and green-valley galaxies; and the same BH-halo quenching mechanism has been in place since $z \sim 3$. We conclude with a discussion of black hole-galaxy co-evolution, the origin and interpretation of BH scaling laws., 45 pages, 20 figures, 2 tables, accepted for publication in ApJ
Published: 2019

17. The Hubble Sequence at $z\sim0$ in the IllustrisTNG simulation with deep learning

Author: Dylan Nelson, Vicente Rodriguez-Gomez, Connor Bottrell, Marc Huertas-Company, Mariangela Bernardi, Annalisa Pillepich, Mark Vogelsberger, Helena Domínguez-Sánchez, Gregory F. Snyder, Shy Genel, Ruediger Pakmor, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)
Subjects: Normalization (statistics), Stellar mass, media_common.quotation_subject, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Convolutional neural network, Hubble sequence, symbols.namesake, 0103 physical sciences, Radiative transfer, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, media_common, [PHYS]Physics [physics], Physics, Artificial neural network, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), symbols, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We analyze the optical morphologies of galaxies in the IllustrisTNG simulation at $z\sim0$ with a Convolutional Neural Network trained on visual morphologies in the Sloan Digital Sky Survey. We generate mock SDSS images of a mass complete sample of $\sim12,000$ galaxies in the simulation using the radiative transfer code SKIRT and include PSF and noise to match the SDSS r-band properties. The images are then processed through the exact same neural network used to estimate SDSS morphologies to classify simulated galaxies in four morphological classes (E, S0/a, Sab, Scd). The CNN model finds that $\sim95\%$ of the simulated galaxies fall in one the four main classes with high confidence. The mass-size relations of the simulated galaxies divided by morphological type also reproduce well the slope and the normalization of observed relations which confirms the realism of optical morphologies in the TNG suite. However, the Stellar Mass Functions decomposed into different morphologies still show significant discrepancies with observations both at the low and high mass end. We find that the high mass end of the SMF is dominated in TNG by massive disk galaxies while early-type galaxies dominate in the observations according to the CNN classifications. The present work highlights the importance of detailed comparisons between observations and simulations in comparable conditions., Comment: submitted to MNRAS, comments welcome
Published: 2019
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18. Structural and Stellar Population Properties vs. Bulge Types in Sloan Digital Sky Survey Central Galaxies

Author: Aldo Rodríguez-Puebla, Hassen M. Yesuf, Viraj Pandya, Joanna Woo, Yicheng Guo, Marc Huertas-Company, Guillermo Barro, David C. Koo, Shude Mao, Jerome J. Fang, Zhu Chen, Lin Lin, S. M. Faber, Yifei Luo, Joel R. Primack, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS]Physics [physics], Physics, Stellar population, 010308 nuclear & particles physics, media_common.quotation_subject, Sigma, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Galaxy, Large sample, Space and Planetary Science, Bulge, Sky, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common
Abstract: This paper studies pseudo-bulges (P-bulges) and classical bulges (C-bulges) in Sloan Digital Sky Survey central galaxies using the new bulge indicator $\Delta\Sigma_1$, which measures relative central stellar-mass surface density within 1 kpc. We compare $\Delta\Sigma_1$ to the established bulge-type indicator $\Delta\langle\mu_e\rangle$ from Gadotti (2009) and show that classifying by $\Delta\Sigma_1$ agrees well with $\Delta\langle\mu_e\rangle$. $\Delta\Sigma_1$ requires no bulge-disk decomposition and can be measured on SDSS images out to $z = 0.07$. Bulge types using it are mapped onto twenty different structural and stellar-population properties for 12,000 SDSS central galaxies with masses 10.0 < log $M_*$/$M_{\odot}$ < 10.4. New trends emerge from this large sample. Structural parameters show fairly linear log-log relations vs. $\Delta\Sigma_1$ and $\Delta\langle\mu_e\rangle$ with only moderate scatter, while stellar-population parameters show a highly non-linear "elbow" in which specific star-formation rate remains roughly flat with increasing central density and then falls rapidly at the elbow, where galaxies begin to quench. P-bulges occupy the low-density end of the horizontal arm of the elbow and are universally star-forming, while C-bulges occupy the elbow and the vertical branch and exhibit a wide range of star-formation rates at fixed density. The non-linear relation between central density and star-formation rate has been seen before, but this mapping onto bulge class is new. The wide range of star-formation rates in C-bulges helps to explain why bulge classifications using different parameters have sometimes disagreed in the past. The elbow-shaped relation between density and stellar indices suggests that central structure and stellar-populations evolve at different rates as galaxies begin to quench., Comment: 23 pages, 17 figures, published in MNRAS
Published: 2019
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19. The structural properties of classical bulges and discs from z ∼ 2

Author: Anton M. Koekemoer, Dale D. Kocevski, Pablo G. Pérez-González, Francesco Shankar, Joel R. Primack, Paola Dimauro, Aldo Rodríguez-Puebla, Ulrike Kuchner, Sandra M. Faber, Fernando Buitrago, Marc Huertas-Company, Simona Mei, David C. Koo, A. Cattaneo, Mariangela Bernardi, B. Häußler, Guillermo Barro, Fernando Caro, Emanuele Daddi, Mara Salvato, Reynier Peletier, D. Tuccillo, Salvato, M. [https://orcid.org/0000-0001-7116-9303], Buitrago, F. [https://orcid.org/0000-0002-2861-9812], Daddi, E. [https://orcid.org/0000-0002-3331-9590], Peletier, R. [https://orcid.org/0000-0001-7621-947X], Huertas Company, M. [https://orcid.org/0000-0002-1416-8483], Spanish Government, AYA2015-63650-P, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Ministerio de Economía y Competitividad (MINECO), Ministerio de Economía y Competitividad (España), and Leverhulme Trust
Subjects: Physics, 010308 nuclear & particles physics, Star formation, structure [Galaxies], FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Redshift, Galaxy, Space and Planetary Science, Bulge, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics
Abstract: We study the rest-frame optical mass–size relation of bulges and discs from z ∼ 2 to z ∼ 0 for a complete sample of massive galaxies in the CANDELS fields using two-component Sérsic models. Discs and star-forming galaxies follow similar mass–size relations. The mass–size relation of bulges is less steep than the one of quiescent galaxies (best-fitting slope of 0.7 for quiescent galaxies against 0.4 for bulges). We find little dependence of the structural properties of massive bulges and discs with the global morphology of galaxies (disc versus bulge dominated) and the star formation activity (star-forming versus quiescent). This result suggests similar bulge formation mechanisms for most massive galaxies and also that the formation of the bulge component does not significantly affect the disc structure. Our results pose a challenge to current cosmological models that predict distinct structural properties for stellar bulges arising from mergers and disc instabilities., This work has been essentially funded by to a French national PhD scholarship. MHC is also thankful to Google for their unrestricted gift to explore deep-learning techniques for galaxy evolution. PGP-G acknowledges support from the Spanish Government grant AYA2015-63650-P. FS acknowledges partial support from a Leverhulme Trust Research Fellowship.
Published: 2019

20. The Strong Gravitational Lens Finding Challenge

Author: Eric Jullo, Manuel Blanco Valentin, Crescenzo Tortora, Alessandro Sonnenfeld, Emmanuel Bertin, F. Bellagamba, Chun-Liang Li, N. J. Jackson, Remi A. Cabanac, Francois Lanusse, G. A. Verdoes Kleijn, Frederic Courbin, Stephen Serjeant, Massimo Meneghetti, Raphael Gavazzi, Clecio R. Bom, Santiago Velasco-Forero, Quanbin Ma, G. Vernardos, Jean-Paul Kneib, Marc Huertas-Company, D. Tuccillo, Etienne Decencière, Mario Geiger, Martin Makler, R. B. Metcalf, Rémi Flamary, Camille Avestruz, Nan Li, Luitje Koopmans, A. Davies, Christoph Schäfer, P. Hartley, C. Jacobs, C. E. Petrillo, M. Lightman, Amitpal S. Tagore, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Centre de Morphologie Mathématique (CMM), Mines Paris - PSL (École nationale supérieure des mines de Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Astronomy, Discrete Technology and Production Automation, Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), École des Mines de Paris, Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France-Centre National de la Recherche Scientifique (CNRS), Metcalf, R. B., Meneghetti, M., Avestruz, C., Bellagamba, F., Bom, C. R., Bertin, E., Cabanac, R., Courbin, F., Davies, A., Decencière, E., Flamary, R., Gavazzi, R., Geiger, M., Hartley, P., Huertas-Company, M., Jackson, N., Jacobs, C., Jullo, E., Kneib, J.-P., Koopmans, L. V. E., Lanusse, F., Li, C.-L., Ma, Q., Makler, M., Li, N., Lightman, M., Petrillo, C. E., Serjeant, S., Schäfer, C., Sonnenfeld, A., Tagore, A., Tortora, C., Tuccillo, D., Valentín, M. B., Velasco-Forero, S., Verdoes Kleijn, G. A., Vernardos, G., Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Convolutional neural network, law.invention, gravitational lensing: strong – methods: data analysis, law, 0103 physical sciences, Computer vision, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, business.industry, gravitational lensing: strong, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, methods: data analysis, Lens (optics), Data flow diagram, Support vector machine, Identification (information), Gravitational lens, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Noise (video), Artificial intelligence, business, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Test data, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Large scale imaging surveys will increase the number of galaxy-scale strong lensing candidates by maybe three orders of magnitudes beyond the number known today. Finding these rare objects will require picking them out of at least tens of millions of images and deriving scientific results from them will require quantifying the efficiency and bias of any search method. To achieve these objectives automated methods must be developed. Because gravitational lenses are rare objects reducing false positives will be particularly important. We present a description and results of an open gravitational lens finding challenge. Participants were asked to classify 100,000 candidate objects as to whether they were gravitational lenses or not with the goal of developing better automated methods for finding lenses in large data sets. A variety of methods were used including visual inspection, arc and ring finders, support vector machines (SVM) and convolutional neural networks (CNN). We find that many of the methods will be easily fast enough to analyse the anticipated data flow. In test data, several methods are able to identify upwards of half the lenses after applying some thresholds on the lens characteristics such as lensed image brightness, size or contrast with the lens galaxy without making a single false-positive identification. This is significantly better than direct inspection by humans was able to do. (abridged), 22 pages, 16 figures, 4 tables, accepted version for A&A
Published: 2019

21. Transfer learning for galaxy morphology from one survey to another

Author: V. Scarpine, Michael Schubnell, Mariangela Bernardi, E. Suchyta, August E. Evrard, T. M. C. Abbott, N. Kuropatkin, L. N. da Costa, A. Carnero Rosell, M. E. C. Swanson, E. J. Sanchez, Peter Doel, Kyler Kuehn, R. H. Schindler, Ben Hoyle, Santiago Avila, Sugata Kaviraj, Carlos E. Cunha, K. Honscheid, Ofer Lahav, Joshua A. Frieman, G. Tarle, Joe Zuntz, J. Annis, Peter Melchior, Brian Nord, David J. Brooks, David J. James, Felipe Menanteau, Pablo Fosalba, Marc Huertas-Company, M. Carrasco Kind, Alistair R. Walker, H. Doḿinguez Sanchez, Marcelle Soares-Santos, Filipe B. Abdalla, Ramon Miquel, M. A. G. Maia, A. A. Plazas, G. Gutierrez, D. L. Hollowood, C. Davis, C. B. D'Andrea, J. Gschwend, Enrique Gaztanaga, W. G. Hartley, Flavia Sobreira, Robert A. Gruendl, M. Smith, D. W. Gerdes, J. L. Fischer, Daniel Gruen, M. March, Daniel Thomas, E. Buckley-Geer, J. De Vicente, Juan Garcia-Bellido, J. Carretero, R. C. Smith, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Paris Diderot - Paris 7 (UPD7), DES, Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)
Subjects: structure [Galaxies], astro-ph.GA, FOS: Physical sciences, Morphology (biology), photometric [Methods], Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, 01 natural sciences, surveys, methods: photometric, 0103 physical sciences, observational [Methods], 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Methods observational, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: structure, methods: observational, Transfer of learning, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Deep Learning (DL) algorithms for morphological classification of galaxies have proven very successful, mimicking (or even improving) visual classifications. However, these algorithms rely on large training samples of labelled galaxies (typically thousands of them). A key question for using DL classifications in future Big Data surveys is how much of the knowledge acquired from an existing survey can be exported to a new dataset, i.e. if the features learned by the machines are meaningful for different data. We test the performance of DL models, trained with Sloan Digital Sky Survey (SDSS) data, on Dark Energy survey (DES) using images for a sample of $\sim$5000 galaxies with a similar redshift distribution to SDSS. Applying the models directly to DES data provides a reasonable global accuracy ($\sim$ 90%), but small completeness and purity values. A fast domain adaptation step, consisting in a further training with a small DES sample of galaxies ($\sim$500-300), is enough for obtaining an accuracy > 95% and a significant improvement in the completeness and purity values. This demonstrates that, once trained with a particular dataset, machines can quickly adapt to new instrument characteristics (e.g., PSF, seeing, depth), reducing by almost one order of magnitude the necessary training sample for morphological classification. Redshift evolution effects or significant depth differences are not taken into account in this study., Accepted for publication in MNRAS
Published: 2019

22. Multiband galaxy morphologies for CLASH: a convolutional neural network transferred from CANDELS

Author: Monserrat Martinez-Marín, Ricardo Demarco, Marc Huertas-Company, Julio Godoy, P. Cerulo, G. Cabrera-Vives, M. Pérez-Carrasco, Pavlos Protopapas, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)
Subjects: 010504 meteorology & atmospheric sciences, Computer science, Point source, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Convolutional neural network, Set (abstract data type), 0103 physical sciences, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, [PHYS]Physics [physics], business.industry, Astronomy and Astrophysics, Pattern recognition, Filter (signal processing), Collision, Galaxy, Supernova, Space and Planetary Science, Test set, Artificial intelligence, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], business, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We present visual-like morphologies over 16 photometric bands, from ultra-violet to near infrared, for 8,412 galaxies in the Cluster Lensing And Supernova survey with Hubble (CLASH) obtained by a convolutional neural network (CNN) model. Our model follows the CANDELS main morphological classification scheme, obtaining the probability for each galaxy at each CLASH band of being spheroid, disk, irregular, point source, or unclassifiable. Our catalog contains morphologies for each galaxy with Hmag < 24.5 in every filter where the galaxy is observed. We trained an initial CNN model using approximately 7,500 expert eyeball labels from The Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey (CANDELS). We created eyeball labels for 100 randomly selected galaxies per each of the 16-filters set of CLASH (1,600 galaxy images in total), where each image was classified by at least five of us. We use these labels to fine-tune the network in order to accurately predict labels for the CLASH data and to evaluate the performance of our model. We achieve a root-mean-square error of 0.0991 on the test set. We show that our proposed fine-tuning technique reduces the number of labeled images needed for training, as compared to directly training over the CLASH data, and achieves a better performance. This approach is very useful to minimize eyeball labeling efforts when classifying unlabeled data from new surveys. This will become particularly useful for massive datasets such as the ones coming from near future surveys such as EUCLID or the LSST. Our catalog consists of prediction of probabilities for each galaxy by morphology in their different bands and is made publicly available at http://www.inf.udec.cl/~guille/data/Deep-CLASH.csv., 11 pages, 11 figures, submitted to Publications of the Astronomical Society of the Pacific
Published: 2018

23. On the Transition of the Galaxy Quenching Mode at 0.5 < z < 1 in CANDELS

Author: Hassen M. Yesuf, Anton M. Koekemoer, Dale D. Kocevski, S. M. Faber, Lu Liu, Darren J. Croton, Yicheng Guo, Marc Huertas-Company, Dongfei Jiang, Weichen Wang, Guillermo Barro, Xian-Min Meng, David C. Koo, Meng Jia, Eric F. Bell, Nimish P. Hathi, F. S. Liu, Wei Tong, Pablo G. Pérez-González, X. Z. Zheng, Avishai Dekel, Jerome J. Fang, Space Telescope Science Institute (STSci), Racah Institute of Physics (Racah Institute of Physics), The Hebrew University of Jerusalem (HUJ)-Racah Institute of Physics, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Communication et Sociétés (ComSocs), Université Clermont Auvergne [2017-2020] (UCA [2017-2020]), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)
Subjects: Physics, Quenching, Astrofísica, [PHYS]Physics [physics], geography, geography.geographical_feature_category, Stellar mass, 010308 nuclear & particles physics, Star formation, Mode (statistics), Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Astronomía, Space and Planetary Science, Ridge, 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS
Abstract: We investigate the galaxy quenching process at intermediate redshift using a sample of $\sim4400$ galaxies with $M_{\ast} > 10^{9}M_{\odot}$ between redshift 0.5 and 1.0 in all five CANDELS fields. We divide this sample, using the integrated specific star formation rate (sSFR), into four sub-groups: star-forming galaxies (SFGs) above and below the ridge of the star-forming main sequence (SFMS), transition galaxies and quiescent galaxies. We study their $UVI$ ($U-V$ versus $V-I$) color gradients to infer their sSFR gradients out to twice effective radii. We show that on average both star-forming and transition galaxies at all masses are not fully quenched at any radii, whereas quiescent galaxies are fully quenched at all radii. We find that at low masses ($M_{\ast} = 10^{9}-10^{10}M_{\odot}$) SFGs both above and below the SFMS ridge generally have flat sSFR profiles, whereas the transition galaxies at the same masses generally have sSFRs that are more suppressed in their outskirts. In contrast, at high masses ($M_{\ast} > 10^{10.5}M_{\odot}$), SFGs above and below the SFMS ridge and transition galaxies generally have varying degrees of more centrally-suppressed sSFRs relative to their outskirts. These findings indicate that at $z\sim~0.5-1.0$ the main galaxy quenching mode depends on its already formed stellar mass, exhibiting a transition from "the outside-in" at $M_{\ast} \leq 10^{10}M_{\odot}$ to "the inside-out" at $M_{\ast} > 10^{10.5}M_{\odot}$. In other words, our findings support that internal processes dominate the quenching of massive galaxies, whereas external processes dominate the quenching of low-mass galaxies., Comment: 19 pages, 12 figures, 2 tables, accepted for publication in ApJ
Published: 2018

24. Deep Learning Identifies High- z Galaxies in a Central Blue Nugget Phase in a Characteristic Mass Range

Author: Berta Margalef-Bentabol, H. Domínguez-Sánchez, Sharon Lapiner, Joel R. Primack, Zhu Chen, Mariangela Bernardi, Marc Huertas-Company, David C. Koo, Daniel Ceverino, C. T. Lee, D. Tuccillo, Gregory F. Snyder, Avishai Dekel, Raymond C. Simons, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Racah Institute of Physics, The Hebrew University of Jerusalem (HUJ), Department of Physics and Astronomy [Philadelphia], University of Pennsylvania [Philadelphia], Fudan University [Shanghai], Jet Propulsion Laboratory (JPL), and NASA-California Institute of Technology (CALTECH)
Subjects: Stellar mass, Phase (waves), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Convolutional neural network, Luminosity, 0103 physical sciences, Range (statistics), 10. No inequality, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, business.industry, Deep learning, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Artificial intelligence, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We use machine learning to identify in color images of high-redshift galaxies an astrophysical phenomenon predicted by cosmological simulations. This phenomenon, called the blue nugget (BN) phase, is the compact star-forming phase in the central regions of many growing galaxies that follows an earlier phase of gas compaction and is followed by a central quenching phase. We train a Convolutional Neural Network (CNN) with mock "observed" images of simulated galaxies at three phases of evolution: pre-BN, BN and post-BN, and demonstrate that the CNN successfully retrieves the three phases in other simulated galaxies. We show that BNs are identified by the CNN within a time window of $\sim0.15$ Hubble times. When the trained CNN is applied to observed galaxies from the CANDELS survey at $z=1-3$, it successfully identifies galaxies at the three phases. We find that the observed BNs are preferentially found in galaxies at a characteristic stellar mass range, $10^{9.2-10.3} M_\odot$ at all redshifts. This is consistent with the characteristic galaxy mass for BNs as detected in the simulations, and is meaningful because it is revealed in the observations when the direct information concerning the total galaxy luminosity has been eliminated from the training set. This technique can be applied to the classification of other astrophysical phenomena for improved comparison of theory and observations in the era of large imaging surveys and cosmological simulations., Comment: Accepted for publication in ApJ
Published: 2018

25. Revisiting the bulge–halo conspiracy – II. Towards explaining its puzzling dependence on redshift

Author: Stewart Buchan, Philip J. Grylls, Alessandro Sonnenfeld, Kyu-Hyun Chae, Lorenzo Zanisi, Francesco Shankar, Mariangela Bernardi, Gary A. Mamon, Marc Huertas-Company, Carlo Nipoti, C. E. Petrillo, Shankar, Francesco, Sonnenfeld, Alessandro, Grylls, Philip, Zanisi, Lorenzo, Nipoti, Carlo, Chae, Kyu-Hyun, Bernardi, Mariangela, Petrillo, Carlo Enrico, Huertas-Company, Marc, Mamon, Gary A, Buchan, Stewart, Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Astronomy, Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), and Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Initial mass function, Stellar mass, INITIAL MASS FUNCTION, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, SIMILAR-TO 1, 01 natural sciences, DARK-MATTER FRACTION, galaxies: evolution, galaxies: fundamental parameters, cosmology: theory, ELLIPTIC GALAXIES, Bulge, cosmology: theory, 0103 physical sciences, EARLY-TYPE GALAXIES, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Effective radius, 010308 nuclear & particles physics, LENS ACS SURVEY, Astronomy, Astronomy and Astrophysics, galaxies: fundamental parameters, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, BRIGHTEST CLUSTER GALAXIES, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FUNDAMENTAL PLANE, DIGITAL SKY SURVEY, Astrophysics::Earth and Planetary Astrophysics, STELLAR MASS, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Fundamental plane (elliptical galaxies), galaxies: evolution, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We carry out a systematic investigation of the total mass density profile of massive (Mstar~3e11 Msun) early-type galaxies and its dependence on redshift, specifically in the range 0, Comment: 14 pages, 8 figures. MNRAS, accepted. Main result of the paper in Figure 2
Published: 2018

26. A catalog of polychromatic bulge-disk decompositions of ~ 17.600 galaxies in CANDELS

Author: Paola Dimauro, D. Tuccillo, David C. Koo, B. Häußler, Mariangela Bernardi, A. Cattaneo, Dale D. Kocevski, Helena Domínguez-Sánchez, Guillermo Barro, Fernando Buitrago, Marc Huertas-Company, Sandra M. Faber, Emanuele Daddi, Fernando Caro, Aldo Rodríguez-Puebla, Mara Salvato, Francesco Shankar, Joel R. Primack, Anton M. Koekemoer, Christoph T. Lee, Simona Mei, Berta Margalef-Bentabol, Pablo G. Pérez-González, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Department of Physics and Astronomy [Philadelphia], University of Pennsylvania [Philadelphia], Galaxies, Etoiles, Physique, Instrumentation (GEPI), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Department of Physics, University of California [Santa Cruz] (UCSC), University of California-University of California, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Max-Planck-Institut für Astrophysik (MPA), École des Mines de Paris, Space Telescope Science Institute (STSci), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), University of Pennsylvania, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), University of California [Santa Cruz] (UC Santa Cruz), University of California (UC)-University of California (UC), Centre de Morphologie Mathématique (CMM), and Mines Paris - PSL (École nationale supérieure des mines de Paris)
Subjects: Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, galaxies: fundamental parameters, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, galaxies: bulges, Redshift, Galaxy, Large sample, Space and Planetary Science, Bulge, galaxies: high-redshift, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Surface brightness, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Understanding how bulges grow in galaxies is critical step towards unveiling the link between galaxy morphology and star-formation. To do so, it is necessary to decompose large sample of galaxies at different epochs into their main components (bulges and disks). This is particularly challenging, especially at high redshifts, where galaxies are poorly resolved. This work presents a catalog of bulge-disk decompositions of the surface brightness profiles of ~17.600 H-band selected galaxies in the CANDELS fields (F160W, Comment: 18 pages, 18 figures, 3 table, submitted to MNRAS after the first referee's report
Published: 2018
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27. $M_*/L$ gradients driven by IMF variation: Large impact on dynamical stellar mass estimates

Author: Ravi K. Sheth, J. L. Fischer, Kyu-Hyun Chae, Francesco Shankar, Mariangela Bernardi, H. Domínguez-Sánchez, Marc Huertas-Company, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation ( GEPI ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Initial mass function, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Stellar population, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Adiabatic process, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, galaxies: kinematics and dynamics, Physics, 010308 nuclear & particles physics, Velocity dispersion, Astronomy and Astrophysics, galaxies: fundamental parameters, Astrophysics - Astrophysics of Galaxies, Galaxy, Stars, galaxies: luminosity function, Space and Planetary Science, mass function, Astrophysics of Galaxies (astro-ph.GA), galaxies: structure, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Within a galaxy the stellar mass-to-light ratio $\Upsilon_*$ is not constant. Spatially resolved kinematics of nearby early-type galaxies suggest that allowing for a variable initial mass function (IMF) returns significantly larger $\Upsilon_*$ gradients than if the IMF is held fixed. If $\Upsilon_*$ is greater in the central regions, then ignoring the IMF-driven gradient can overestimate $M_*^{\rm dyn}$ by as much as a factor of two for the most massive galaxies, though stellar population estimates $M_*^{\rm SP}$ are also affected. Large $\Upsilon_*$-gradients have four main consequences: First, $M_*^{\rm dyn}$ cannot be estimated independently of stellar population synthesis models. Second, if there is a lower limit to $\Upsilon_*$ and gradients are unknown, then requiring $M_*^{\rm dyn}=M_*^{\rm SP}$ constrains them. Third, if gradients are stronger in more massive galaxies, then $M_*^{\rm dyn}$ and $M_*^{\rm SP}$ can be brought into agreement, not by shifting $M_*^{\rm SP}$ upwards by invoking constant bottom-heavy IMFs, as advocated by a number of recent studies, but by revising $M_*^{\rm dyn}$ estimates in the literature downwards. Fourth, accounting for $\Upsilon_*$ gradients changes the high-mass slope of the stellar mass function $\phi(M_*^{\rm dyn})$, and reduces the associated stellar mass density. These conclusions potentially impact estimates of the need for feedback and adiabatic contraction, so our results highlight the importance of measuring $\Upsilon_*$ gradients in larger samples., Comment: 13 pages, 7 figures, MNRAS in press
Published: 2018

28. The morphological transformation of red sequence galaxies in clusters since z ∼ 1

Author: P. Cerulo, R. Munoz, Marc Huertas-Company, Rubén Sánchez-Janssen, L. F. Barrientos, S. Mei, C. Lidman, R. Demarco, Warrick J. Couch, AUTRES, Departamento de Industrias, Universidad Técnica Federico Santa María, Av. España 1680, Valparaíso, Chile, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Dirección de Monitoreo Atmosférico, Gobierno del Distrito Federal, and École normale supérieure - Paris (ENS-PSL)
Subjects: Radio galaxy, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Peculiar galaxy, Galaxy group, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Brightest cluster galaxy, Disc, 010303 astronomy & astrophysics, Lenticular galaxy, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, Luminous infrared galaxy, [PHYS]Physics [physics], 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Elliptical galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: The study of galaxy morphology is fundamental to understand the physical processes driving the structural evolution of galaxies. It has long been known that dense environments host high fractions of early-type galaxies and low fractions of late-type galaxies, indicating that the environment affects the structural evolution of galaxies. In this paper we present an analysis of the morphological composition of red sequence galaxies in a sample of 9 galaxy clusters at $0.8, Comment: 21 pages, 6 figures, 5 tables, 1 appendix, accepted by MNRAS
Published: 2017

29. Improving galaxy morphologies for SDSS with Deep Learning

Author: D Tuccillo, H. Domínguez Sánchez, Mariangela Bernardi, J. L. Fischer, Marc Huertas-Company, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Department of Physics and Astronomy [Philadelphia], and University of Pennsylvania [Philadelphia]
Subjects: media_common.quotation_subject, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Convolutional neural network, Hubble sequence, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, Bulge, 0103 physical sciences, 010303 astronomy & astrophysics, catalogues, Astrophysics::Galaxy Astrophysics, media_common, Physics, 010308 nuclear & particles physics, business.industry, Deep learning, Astronomy and Astrophysics, Pattern recognition, Astrophysics - Astrophysics of Galaxies, Galaxy, Support vector machine, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), symbols, galaxies: structure, Artificial intelligence, methods: observational, Precision and recall, business
Abstract: We present a morphological catalogue for $\sim$ 670,000 galaxies in the Sloan Digital Sky Survey in two flavours: T-Type, related to the Hubble sequence, and Galaxy Zoo 2 (GZ2 hereafter) classification scheme. By combining accurate existing visual classification catalogues with machine learning, we provide the largest and most accurate morphological catalogue up to date. The classifications are obtained with Deep Learning algorithms using Convolutional Neural Networks (CNNs). We use two visual classification catalogues, GZ2 and Nair & Abraham (2010), for training CNNs with colour images in order to obtain T-Types and a series of GZ2 type questions (disk/features, edge-on galaxies, bar signature, bulge prominence, roundness and mergers). We also provide an additional probability enabling a separation between pure elliptical (E) from S0, where the T-Type model is not so efficient. For the T-Type, our results show smaller offset and scatter than previous models trained with support vector machines. For the GZ2 type questions, our models have large accuracy (> 97\%), precision and recall values (> 90\%) when applied to a test sample with the same characteristics as the one used for training. The catalogue is publicly released with the paper., 18 pages, 21 figures; Accepted for publication in MNRAS
Published: 2017

30. SHARDS Frontier Fields: Physical Properties of a Low-mass Lyα Emitter at z=5.75

Author: Helmut Dannerbauer, Helena Domínguez-Sánchez, Pablo G. Pérez-González, Daniel Rosa González, Jose M. Diego, Daniel Schaerer, Jose Miguel Rodriguez Espinosa, P. Esquej, David J. Lagattuta, Ismael Perez-Fournon, Belén Alcalde-Pampliega, Panos Sklias, Marc Huertas-Company, T. D. Rawle, Rui Marques-Chaves, Almudena Alonso-Herrero, Johan Richard, Carmen Eliche-Moral, Antonio Hernán-Caballero, Christopher J. Conselice, Raffaella Anna Marino, Antonio Cava, Wiphu Rujopakarn, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Institut für Astronomie [Wien], Universität Wien, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, Université Paris sciences et lettres (PSL), Swiss National Science Foundation, European Research Council, European Commission, Ministerio de Economía y Competitividad (España), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and École normale supérieure - Paris (ENS-PSL)
Subjects: Astrofísica, Stellar population, Gravitational lensing: strong, Population, Early universe, FOS: Physical sciences, Astrophysics, strong [Gravitational lensing], 01 natural sciences, high-redshift [Galaxies], Dark ages, reionization, first stars, 0103 physical sciences, education, 010303 astronomy & astrophysics, Reionization, ComputingMilieux_MISCELLANEOUS, Physics, [PHYS]Physics [physics], education.field_of_study, Spectral index, 010308 nuclear & particles physics, Star formation, Galaxies: high-redshift, Galaxies: evolution, Astronomy and Astrophysics, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, Galaxy, Astronomía, starburst [Galaxies], 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Spectral energy distribution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Equivalent width, Galaxies: starburst
Abstract: arXiv:1710.00826v1, We analyze the properties of a multiply imaged Lyα (Lyα) emitter at z = 5.75 identified through SHARDS Frontier Fields intermediate-band imaging of the Hubble Frontier Fields (HFF) cluster Abell 370. The source, A370-L57, has low intrinsic luminosity (M ∼ -16.5), steep UV spectral index (β = -2.4 ± 0.1), and extreme rest-frame equivalent width of Lyα. Two different gravitational lens models predict high magnification (μ ∼ 10-16) for the two detected counterimages, separated by 7″, while a predicted third counterimage (μ ∼ 3-4) is undetected. We find differences of ∼50% in magnification between the two lens models, quantifying our current systematic uncertainties. Integral field spectroscopy of A370-L57 with MUSE shows a narrow (FWHM = 204 ± 10 km s) and asymmetric Lyα profile with an integrated luminosity L(Lyα) ∼ 10 erg s. The morphology in the Hubble Space Telescope bands comprises a compact clump (r < 100 pc) that dominates the Lyα and continuum emission and several fainter clumps at projected distances ≲1 kpc that coincide with an extension of the Lyα emission in the SHARDS F823W17 and MUSE observations. The latter could be part of the same galaxy or an interacting companion. We find no evidence of a contribution from active galactic nuclei to the Lyα emission. Fitting of the spectral energy distribution with stellar population models favors a very young (t < 10 Myr), low-mass (), and metal-poor (Z ≲ 4 10) stellar population. Its modest star formation rate (SFR ∼ 1.0 yr) implies high specific SFR (sSFR ∼ 2.5 10 yr) and SFR density ( yr kpc). The properties of A370-L57 make it a good representative of the population of galaxies responsible for cosmic reionization., A.H.-C. and P.G.P.-G. acknowledge funding by the Spanish Ministry of Economy and Competitiveness (MINECO) under grants AYA2012-31277, AYA2015-70815-ERC, and AYA2015-63650-P. J.M.D. acknowledges support of the projects AYA2015-64508-P (MINECO/FEDER, UE), AYA2012-39475-C02-01, and the consolider project CSD2010-00064 funded by MINECO. D.J.L. and J.R. acknowledge support from the ERC starting grant 336736-CALENDS. R.A.M. acknowledges support by the Swiss National Science Foundation. A.A.-H. acknowledges funding by the MINECO grant AYA2015-64346-C2-1-P, which is partly funded by the FEDER program. H.D.S. acknowledges funding from the program ANR-T-ERC ASTROBRAIN. P.S. acknowledges funding from the Swiss National Science Foundation under grant P2GEP2_165426. J.M.R.E. acknowledges funding by the MINECO grant AYA2015-70498-C2-1-R. H.D. acknowledges financial support from the Spanish 2014 Ramón y Cajal program MINECO RYC-2014-15686.
Published: 2017

31. Comparing PyMorph and SDSS photometry. II.: The differences are more than semantics and are not dominated by intracluster light

Author: Vinu Vikram, Francesco Shankar, Mariangela Bernardi, A. Meert, Marc Huertas-Company, J. L. Fischer, Ravi K. Sheth, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Université Paris Diderot - Paris 7 (UPD7), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation ( GEPI ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), and Université Paris Diderot - Paris 7 ( UPD7 )
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxies: clusters: intracluster medium, Stellar mass, media_common.quotation_subject, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Photometry (optics), 0103 physical sciences, galaxies: formation, Astrophysics::Solar and Stellar Astrophysics, Surface brightness, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, 010308 nuclear & particles physics, Star formation, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, galaxies: fundamental parameters, Full sample, Astrophysics - Astrophysics of Galaxies, Galaxy, galaxies: photometry, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), Halo, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Sloan Digital Sky Survey pipeline photometry underestimates the brightnesses of the most luminous galaxies. This is mainly because (i) the SDSS overestimates the sky background and (ii) single or two-component Sersic-based models better fit the surface brightness profile of galaxies, especially at high luminosities, than does the de Vaucouleurs model used by the SDSS pipeline. We use the PyMorph photometric reductions to isolate effect (ii) and show that it is the same in the full sample as in small group environments, and for satellites in the most massive clusters as well. None of these are expected to be significantly affected by intracluster light (ICL). We only see an additional effect for centrals in the most massive halos, but we argue that even this is not dominated by ICL. Hence, for the vast majority of galaxies, the differences between PyMorph and SDSS pipeline photometry cannot be ascribed to the semantics of whether or not one includes the ICL when describing the stellar mass of massive galaxies. Rather, they likely reflect differences in star formation or assembly histories. Failure to account for the SDSS underestimate has significantly biased most previous estimates of the SDSS luminosity and stellar mass functions, and therefore Halo Model estimates of the z ~ 0.1 relation between the mass of a halo and that of the galaxy at its center. We also show that when one studies correlations, at fixed group mass, with a quantity which was not used to define the groups, then selection effects appear. We show why such effects arise, and should not be mistaken for physical effects., 15 pages, 17 figures, accepted for publication in MNRAS. The PyMorph luminosities and stellar masses are available at https://www.physics.upenn.edu/~ameert/SDSS_PhotDec/
Published: 2017

32. Revisiting the bulge-halo conspiracy I: dependence on galaxy properties and halo mass

Author: Francesco Shankar, Gary A. Mamon, Ravi K. Sheth, Stewart Buchan, Carlo Nipoti, Tommaso Treu, Marc Huertas-Company, Alessandro Sonnenfeld, Kyu-Hyun Chae, Raphael Gavazzi, Mariangela Bernardi, Benedikt Diemer, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris - Site de Paris (OP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Université Paris Diderot - Paris 7 (UPD7), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Observatoire de Paris - Site de Paris ( OP ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Centre National de la Recherche Scientifique ( CNRS ), Université Paris Diderot - Paris 7 ( UPD7 ), Shankar, Francesco, Sonnenfeld, Alessandro, Mamon, Gary A., Chae, Kyu-Hyun, Gavazzi, Raphael, Treu, Tommaso, Diemer, Benedikt, Nipoti, Carlo, Buchan, Stewart, Bernardi, Mariangela, Sheth, Ravi, Huertas-Company, Marc, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Initial mass function, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Star (game theory), Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, Bulge, cosmology: theory, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, galaxies: statistics, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, cosmology: theory – galaxies: evolution – galaxies: statistics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Halo, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics, Dimensionless quantity
Abstract: We carry out a systematic investigation of the total mass density profile of massive (Mstar>2e11 Msun) early-type galaxies and its dependence on galactic properties and host halo mass with the aid of a variety of lensing/dynamical data and large mock galaxy catalogs. The latter are produced via semi-empirical models that, by design, are based on just a few basic input assumptions. Galaxies, with measured stellar masses, effective radii and S��rsic indices, are assigned, via abundance matching relations, host dark matter halos characterized by a typical LCDM profile. Our main results are as follows: (i) In line with observational evidence, our semi-empirical models naturally predict that the total, mass-weighted density slope at the effective radius gamma' is not universal, steepening for more compact and/or massive galaxies, but flattening with increasing host halo mass. (ii) Models characterized by a Salpeter or variable initial mass function and uncontracted dark matter profiles are in good agreement with the data, while a Chabrier initial mass function and/or adiabatic contractions/expansions of the dark matter halos are highly disfavored. (iii) Currently available data on the mass density profiles of very massive galaxies (Mstar>1e12 Msun), with Mhalo>3e14 Msun, favor instead models with a stellar profile flatter than a S��rsic one in the very inner regions (r, 23 pages, 10 figures, 3 Appendices (with an extra 7 figures). ApJ, accepted. Main results in Figures 3, 5, 6, 8
Published: 2017

33. Deep learning for galaxy surface brightness profile fitting

Author: P. Dimauro, H. Domínguez Sánchez, Santiago Velasco-Forero, Marc Huertas-Company, D. Tuccillo, Etienne Decencière, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Centre de Morphologie Mathématique (CMM), MINES ParisTech - École nationale supérieure des mines de Paris, and Decencière, Etienne
Subjects: Domain adaptation, media_common.quotation_subject, Big data, FOS: Physical sciences, Astrophysics, 01 natural sciences, Convolutional neural network, galaxies: high-redshift, 0103 physical sciences, Surface brightness, 010303 astronomy & astrophysics, catalogues, media_common, Physics, Effective radius, 010308 nuclear & particles physics, business.industry, Deep learning, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, methods: data analysis, Galaxy, [INFO.INFO-TI] Computer Science [cs]/Image Processing [eess.IV], Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), [INFO.INFO-TI]Computer Science [cs]/Image Processing [eess.IV], galaxies: structure, Artificial intelligence, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Algorithm
Abstract: Numerous ongoing and future large area surveys (e.g. DES, EUCLID, LSST, WFIRST), will increase by several orders of magnitude the volume of data that can be exploited for galaxy morphology studies. The full potential of these surveys can only be unlocked with the development of automated, fast and reliable analysis methods. In this paper we present DeepLeGATo, a new method for two-dimensional photometric galaxy profile modeling, based on convolutional neural networks. Our code is trained and validated on analytic profiles (HST/CANDELS F160W filter) and it is able to retrieve the full set of parameters of one- component S\'ersic models: total magnitude, effective radius, S\'ersic index, axis ratio. We show detailed comparisons between our code and GALFIT. On simulated data, our method is more accurate than GALFIT and 3000 time faster on GPU (50 times when run on the same CPU). On real data, DeepLeGATo trained on simulations behaves similarly to GALFIT on isolated galaxies. With a fast domain adaptation step made with the 0.1 - 0.8 per cent the size of the training set, our code is easily capable to reproduce the results obtained with GALFIT even on crowded regions. DeepLeGATo does not require any human intervention beyond the training step, rendering it much automated than traditional profiling methods. The development of this method for more complex models (two-component galaxies, variable PSF, dense sky regions) could constitute a fundamental tool in the era of big data in astronomy., Comment: 17 pages, 9 figures
Published: 2017

34. The abundance of compact quiescent galaxies since $z\sim0.6$

Author: Maria E. S. Pereira, Emmanuel Galliano, Huanyuan Shan, Thiago S. Gonçalves, Thomas Erben, Aldée Charbonnier, Kevin Bundy, Bruno Moraes, Martin Makler, L. Riguccini, Hendrik Hildebrandt, Karín Menéndez-Delmestre, Marco Grossi, G. B. Caminha, Marc Huertas-Company, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique ( LERMA ), École normale supérieure - Paris ( ENS Paris ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université de Cergy Pontoise ( UCP ), and Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique ( CNRS )
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Measure (mathematics), law.invention, cD, Telescope, surveys, law, Abundance (ecology), 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, galaxies: formation, galaxies: elliptical and lenticular, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, catalogues, media_common, Physics, Number density, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Cosmic variance, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), galaxies: structure, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We set out to quantify the number density of quiescent massive compact galaxies at intermediate redshifts. We determine structural parameters based on i-band imaging using the CFHT equatorial SDSS Stripe 82 (CS82) survey (~170 sq. degrees) taking advantage of an exquisite median seeing of ~0.6''. We select compact massive (M > 5x10^10 M_sun) galaxies within the redshift range of 0.210. We systematically measure a factor of ~5 more compacts at the same redshift than what was previously reported on smaller fields with HST imaging, which are more affected by cosmic variance. This means that the decrease in number density from z ~ 1.5 to z ~ 0.2 might be only of a factor of ~2-5, significantly smaller than what previously reported. This supports progenitor bias as the main contributor to the size evolution. This milder decrease is roughly compatible with the predictions from recent numerical simulations. Only the most extreme compact galaxies, with Reff < 1.5x( M/10^11 M_sun)^0.75 and M > 10^10.7 M_sun, appear to drop in number by a factor of ~20 and hence likely experience a noticeable size evolution., Comment: 15 pages, 16 figures, accepted for publication in MNRAS
Published: 2017

35. Mass assembly and morphological transformations since z~3 from CANDELS

Author: David C. Koo, Pablo G. Pérez-González, Emanuele Daddi, Dale D. Kocevski, M. L. N. Ashby, Francesco Shankar, S. M. Faber, Guillermo Barro, Jeyhan S. Kartaltepe, Marc Huertas-Company, Anton M. Koekemoer, P. Dimauro, Norman A. Grogin, Simona Mei, Mariangela Bernardi, Avishai Dekel, Christopher J. Conselice, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Philadelphia], University of Pennsylvania, DLO Winand Staring Centre, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Racah Institute of Physics, The Hebrew University of Jerusalem (HUJ), National Optical Astronomy Observatory (NOAO), GSFC Laboratory for High Energy Astrophysics (LHEA), NASA Goddard Space Flight Center (GSFC), Space Telescope Science Institute (STSci), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), University of Pennsylvania [Philadelphia], and École normale supérieure - Paris (ENS Paris)
Subjects: Astrofísica, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Disc galaxy, 01 natural sciences, Peculiar galaxy, Bulge, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Disc, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Luminous infrared galaxy, Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Astronomía, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Elliptical galaxy, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: [abridged] We quantify the evolution of the stellar mass functions of star-forming and quiescent galaxies as a function of morphology from $z\sim 3$ to the present. Our sample consists of ~50,000 galaxies in the CANDELS fields ($\sim880$ $arcmin^2$), which we divide into four main morphological types, i.e. pure bulge dominated systems, pure spiral disk dominated, intermediate 2-component bulge+disk systems and irregular disturbed galaxies. Our main results are: Star-formation: At $z\sim 2$, 80\% of the stellar mass density of star-forming galaxies is in irregular systems. However, by $z\sim 0.5$, irregular objects only dominate at stellar masses below $10^9M\odot$. A majority of the star-forming irregulars present at $z\sim 2$ undergo a gradual transformation from disturbed to normal spiral disk morphologies by $z\sim 1$ without significant interruption to their star-formation. Rejuvenation after a quenching event does not seem to be common except perhaps for the most massive objects. Quenching: We confirm that galaxies reaching a stellar mass of $M_*\sim10^{10.8}M_\odot$ ($M^*$) tend to quench. Also, quenching implies the presence of a bulge: the abundance of massive red disks is negligible at all redshifts over 2~dex in stellar mass. However the dominant quenching mechanism evolves. At $z>2$, the SMF of quiescent galaxies above $M^*$ is dominated by compact spheroids. Quenching at this early epoch destroys the disk and produces a compact remnant unless the star-forming progenitors at even higher redshifts are significantly more dense. At $1, Comment: resubmitted to MNRAS after addressing minor comments from the referee
Published: 2016

36. The Next Generation Virgo Cluster Survey. XX. RedGOLD Background Galaxy Cluster Detections

Author: Roberto Munoz, Thomas H. Puzia, Marc Huertas-Company, Laura Ferrarese, Thomas Erben, Ariane Lançon, Stephen D. J. Gwyn, Ludovic Van Waerbeke, Carolina Parroni, Anand Raichoor, Hendrik Hildebrandt, Rossella Licitra, Simona Mei, Pierre-Alain Duc, Jean-Charles Cuillandre, Patrick Côté, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Argelander-Institut für Astronomie (AlfA), Rheinische Friedrich-Wilhelms-Universität Bonn, Centro de Investigacion y de Estudios Avanzados del Instituto Politécnico Nacional (CINVESTAV), National Research Council of Canada (NRC), Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, Université Paris sciences et lettres (PSL), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Pontificia Universidad Católica de Chile (UC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), and Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS]Physics [physics], Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Virgo Cluster, Galaxy, law.invention, Red shift, Telescope, Space and Planetary Science, law, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Cluster (physics), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Galaxy cluster, Astrophysics - Cosmology and Nongalactic Astrophysics, Photometric redshift
Abstract: We build a background cluster candidate catalog from the Next Generation Virgo Cluster Survey, using our detection algorithm RedGOLD. The NGVS covers 104$deg^2$ of the Virgo cluster in the $u^*,g,r,i,z$-bandpasses to a depth of $ g \sim 25.7$~mag (5$\sigma$). Part of the survey was not covered or has shallow observations in the $r$--band. We build two cluster catalogs: one using all bandpasses, for the fields with deep $r$--band observations ($\sim 20 \ deg^2$), and the other using four bandpasses ($u^*,g,i,z$) for the entire NGVS area. Based on our previous CFHT-LS W1 studies, we estimate that both of our catalogs are $\sim100\%$($\sim70\%$) complete and $\sim80\%$ pure, at $z\le 0.6$($z\lesssim1$), for galaxy clusters with masses of $M\gtrsim10^{14}\ M_{\odot}$. We show that when using four bandpasses, though the photometric redshift accuracy is lower, RedGOLD detects massive galaxy clusters up to $z\sim 1$ with completeness and purity similar to the five-band case. This is achieved when taking into account the bias in the richness estimation, which is $\sim40\%$ lower at $0.5\le z 1.4 \times 10^{14} \rm M_{\odot}$ and $0.08, Comment: Licitra e al. 2016, ApJ, 829, 44 Our catalogs are planned to be available on ADS
Published: 2016

37. The Accelerated Build-up of the Red Sequence in High Redshift Galaxy Clusters

Author: L. F. Barrientos, Roberto Munoz, C. Lidman, Warrick J. Couch, P. Cerulo, Ruben Sanchez-Janssen, R. Demarco, Marc Huertas-Company, Simona Mei, AUTRES, Departamento de Industrias, Universidad Técnica Federico Santa María, Av. España 1680, Valparaíso, Chile, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Dirección de Monitoreo Atmosférico, Gobierno del Distrito Federal, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and École normale supérieure - Paris (ENS-PSL)
Subjects: FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, Galaxy groups and clusters, 0103 physical sciences, Cluster (physics), Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Galaxy cluster, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Halo, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We analyse the evolution of the red sequence in a sample of galaxy clusters at redshifts $0.8 11.5$) red sequence galaxies in the WINGS clusters, which do not include only the brightest cluster galaxies and which are not present in the HCS clusters, suggesting that they formed at epochs later than $z=0.8$. The comparison with the luminosity distribution of a sample of passive red sequence galaxies drawn from the COSMOS/UltraVISTA field in the photometric redshift range $0.8, Comment: 28 pages, 9 figures, 8 tables, accepted for publication in MNRAS
Published: 2016
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38. The massive end of the luminosity and stellar mass functions and clustering from CMASS to SDSS: evidence for and against passive evolution

Author: Mariangela Bernardi, Francesco Shankar, A. Meert, Marc Huertas-Company, Claudia Maraston, Ravi K. Sheth, Vinu Vikram, Department of Physics and Astronomy [Philadelphia], University of Pennsylvania [Philadelphia], University of Illinois at Urbana Champaign (UIUC), University of Illinois at Urbana-Champaign [Urbana], University of Illinois System-University of Illinois System, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institute of Cosmology and Gravitation [Portsmouth] (ICG), and University of Portsmouth
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, media_common.quotation_subject, astro-ph.GA, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Photometry (optics), 0103 physical sciences, abundances [galaxies], Astrophysics::Solar and Stellar Astrophysics, education, Cluster analysis, 010303 astronomy & astrophysics, evolution [galaxies], STFC, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, media_common, galaxies, luminosity function, Physics, Luminous infrared galaxy, [PHYS]Physics [physics], education.field_of_study, 010308 nuclear & particles physics, Astronomy, RCUK, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, Sky, mass function, Astrophysics of Galaxies (astro-ph.GA), astro-ph.CO, photometry [galaxies], Halo, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We describe the luminosity function, based on Sersic fits to the light profiles, of CMASS galaxies at z ~ 0.55. Compared to previous estimates, our Sersic-based reductions imply more luminous, massive galaxies, consistent with the effects of Sersic- rather than Petrosian or de Vaucouleur-based photometry on the Sloan Digital Sky Survey (SDSS) main galaxy sample at z ~ 0.1. This implies a significant revision of the high mass end of the correlation between stellar and halo mass. Inferences about the evolution of the luminosity and stellar mass functions depend strongly on the assumed, and uncertain, k+e corrections. In turn, these depend on the assumed age of the population. Applying k+e corrections taken from fitting the models of Maraston et al. (2009) to the colors of both SDSS and CMASS galaxies, the evolution of the luminosity and stellar mass functions appears impressively passive, provided that the fits are required to return old ages. However, when matched in comoving number- or luminosity-density, the SDSS galaxies are less strongly clustered compared to their counterparts in CMASS. This rules out the passive evolution scenario, and, indeed, any minor merger scenarios which preserve the rank ordering in stellar mass of the population. Potential incompletenesses in the CMASS sample would further enhance this mismatch. Our analysis highlights the virtue of combining clustering measurements with number counts., Accepted for publication in MNRAS, 15 pages, 12 figures
Published: 2015

39. A robust morphological classification of high-redshift galaxies using support vector machines on seeing limited images

Author: Marc Huertas-Company, Lidia Tasca, O. Le Fèvre, G. Soucail, D. Rouan, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Departement de recherche SPAtiale (DESPA), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Observatoire de Paris - Site de Paris (OP), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), and Université Fédérale Toulouse Midi-Pyrénées
Subjects: Physics, 010308 nuclear & particles physics, Generalization, Astrophysics (astro-ph), FOS: Physical sciences, galaxies: fundamental parameters, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, methods: data analysis, 01 natural sciences, Sample (graphics), Galaxy, Redshift, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Support vector machine, galaxies: high-redshift, Space and Planetary Science, 0103 physical sciences, Limit (mathematics), Completeness (statistics), 010303 astronomy & astrophysics, Algorithm
Abstract: We present a new non-parametric method to quantify morphologies of galaxies based on a particular family of learning machines called support vector machines. The method, that can be seen as a generalization of the classical CAS classification but with an unlimited number of dimensions and non-linear boundaries between decision regions, is fully automated and thus particularly well adapted to large cosmological surveys. The source code is available for download at http://www.lesia.obspm.fr/~huertas/galsvm.html To test the method, we use a seeing limited near-infrared ($K_s$ band, $2,16\mu m$) sample observed with WIRCam at CFHT at a median redshift of $z\sim0.8$. The machine is trained with a simulated sample built from a local visually classified sample from the SDSS chosen in the high-redshift sample's rest-frame (i band, $0.77\mu m$) and artificially redshifted to match the observing conditions. We use a 12-dimensional volume, including 5 morphological parameters and other caracteristics of galaxies such as luminosity and redshift. We show that a qualitative separation in two main morphological types (late type and early type) can be obtained with an error lower than 20% up to the completeness limit of the sample ($KAB\sim 22$) which is more than 2 times better that what would be obtained with a classical C/A classification on the same sample and indeed comparable to space data. The method is optimized to solve a specific problem, offering an objective and automated estimate of errors that enables a straightforward comparison with other surveys., Comment: 11 pages, 7 figures, 3 tables. Submitted to A&A. High resolution images are available on request
Published: 2007

40. THE MORPHOLOGIES OF MASSIVE GALAXIES FROM z ∼ 3—WITNESSING THE TWO CHANNELS OF BULGE GROWTH

Author: Simona Mei, Guillermo Barro, P. Dimauro, Mariangela Bernardi, Marc Huertas-Company, Romaric Gravet, Pablo G. Pérez-González, Francesco Shankar, Andrea Cattaneo, G. Cabrera-Vives, Emanuele Daddi, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Antarctic Research a European Network for Astrophysics (ARENA), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)
Subjects: Physics, Astrofísica, [PHYS]Physics [physics], Morphology (linguistics), 010308 nuclear & particles physics, Star formation, Mass growth, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Structural evolution, Galaxy, Morphological transformation, Astronomía, Space and Planetary Science, Bulge, Phase (matter), 0103 physical sciences, 10. No inequality, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS
Abstract: We quantify the morphological evolution of z ~ 0 massive galaxies (M_*/M_∼ ∼10^11.2 +/- 0.3) from z ~ 3 in the 5 CANDELS fields. The progenitors are selected using abundance matching techniques to account for the mass growth. At z < 1, the population matches the massive end of the Hubble sequence, with 30% of pure spheroids, 50% of galaxies with equally dominant disk and bulge components, and 20% of disks. At z ~ 2-3 however, there is a majority of irregular systems (~ 60%-70%) with still 30% of pure spheroids. We then analyze the stellar populations, star formation rates (SFRs), gas fractions, and structural properties for the different morphologies independently. Our results suggest two distinct channels for the growth of bulges in massive galaxies. Around ~ 30%-40% were already bulges at z ~ 2.5, with low average SFRs and gas fractions (10%-15%), high Sersic indices (n > 3-4), and small effective radii (R_e ∼1 kpc), pointing toward an even earlier formation through gas-rich mergers or violent disk instabilities. Between z ~ 2.5 and z ~ 0, they rapidly increase their size by a factor of ~ 4-5, are quenched, and slightly increase their Sersic indices (n ~ 5) but their global morphology remains unaltered. The structural evolution is independent of the gas fractions, suggesting that it is driven by ex situ events. The remaining 60% experience a gradual morphological transformation, from clumpy disks to more regular bulge +disk systems, essentially happening at z > 1. This results in the growth of a significant bulge component (n ~ 3) for 2/3 of the systems, possibly through the migration of clumps, while the remaining 1/3 retain a rather small bulge (n ~ 1.5-2). The transition phase between disturbed and relaxed systems and the emergence of the bulge is correlated with a decrease in the star formation activity and the gas fractions, suggesting a morphological quenching process as a plausible mechanism for the formation of these bulges.
Published: 2015

41. Star-forming Blue ETGs in Two Newly Discovered Galaxy Overdensities in the HUDF at z=1.84 and 1.9: Unveiling the Progenitors of Passive ETGs in Cluster Cores

Author: Simona Mei, Steven L. Finkelstein, Casey Papovich, Anton M. Koekemoer, Jeffrey A. Newman, Benjamin J. Weiner, Marc Rafelski, Matthew L. N. Ashby, Laura Pentericci, Harry I. Tepliz, Claudia Scarlata, Norman A. Grogin, Audrey Galametz, Ray A. Lucas, Caterina Lani, C. J. Conselice, Marc Huertas-Company, Marco Castellano, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), AUTRES, INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Space Telescope Science Institute (STSci), Observatoire de Paris, and Université Paris sciences et lettres (PSL)
Subjects: Physics, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star (game theory), Population, FOS: Physical sciences, Velocity dispersion, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Instability, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Space and Planetary Science, galaxies: clusters: general, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), Hubble space telescope, 0103 physical sciences, Cluster (physics), education, galaxies: evolution, 010303 astronomy & astrophysics
Abstract: We present the discovery of two galaxy overdensities in the Hubble Space Telescope UDF: a proto-cluster, HUDFJ0332.4-2746.6 at $z = 1.84 \pm 0.01$, and a group, HUDFJ0332.5-2747.3 at $z =1.90 \pm 0.01$. Assuming viralization, the velocity dispersion of HUDFJ0332.4-2746.6 implies a mass of $M_{200}= (2.2 \pm 1.8) \times 10^{14} M_{\odot}$, consistent with the lack of extended X-ray emission. Neither overdensity shows evidence of a red sequence. About $50\%$ of their members show interactions and/or disturbed morphologies, which are signatures of merger remnants or disk instability. Most of their ETGs have blue colors and show recent star-formation. These observations reveal for the first time large fractions of spectroscopically confirmed star-forming blue ETGs in proto-clusters at $z\approx 2$. These star-forming ETGs are most likely among the progenitors of the quiescent population in clusters at more recent epochs. Their mass-size relation is consistent with that of passive ETGs in clusters at $z\sim0.7-1.5$. If these galaxies are the progenitors of cluster ETGs at these lower redshifts, their size would evolve according to a similar mass-size relation. It is noteworthy that quiescent ETGs in clusters at $z=1.8-2$ also do not show any significant size evolution over this redshift range, contrary to field ETGs. The ETG fraction is $\lesssim 50\%$, compared to the typical quiescent ETG fraction of $\approx 80\%$ in cluster cores at $z< 1$. The fraction, masses, and colors of the newly discovered ETGs imply that other cluster ETGs will be formed/accreted at a later time., 33 pages, 13 figures. ApJ, in press
Published: 2015

42. Avoiding progenitor bias: The structural and mass evolution of Brightest Group and Cluster Galaxies in Hierarchical models since z~1

Author: Vincent Bouillot, Ravi K. Sheth, Simona Mei, Lauriane Delaye, Rossella Licitra, Begoña Ascaso, Marc Huertas-Company, Stewart Buchan, Alessandro Rettura, Anand Raichoor, Jorge Moreno, Mariangela Bernardi, Francesco Shankar, Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), Cosmologie: Origine et Structures, Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Department of Physics and Astronomy [Victoria], University of Victoria [Canada] (UVIC), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Philadelphia], University of Pennsylvania [Philadelphia], Observatoire de Paris, Université Paris sciences et lettres (PSL), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), and PSL Research University (PSL)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, media_common.quotation_subject, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, cosmology: theory, 0103 physical sciences, Galaxy formation and evolution, 010303 astronomy & astrophysics, galaxies: statistics, Astrophysics::Galaxy Astrophysics, media_common, Physics, Effective radius, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), Halo, galaxies: evolution, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The mass and structural evolution of massive galaxies is one of the hottest topics in galaxy formation. This is because it may reveal invaluable insights into the still debated evolutionary processes governing the growth and assembly of spheroids. However, direct comparison between models and observations is usually prevented by the so-called "progenitor bias", i.e., new galaxies entering the observational selection at later epochs, thus eluding a precise study of how pre-existing galaxies actually evolve in size. To limit this effect, we here gather data on high-redshift brightest group and cluster galaxies, evolve their (mean) host halo masses down to z=0 along their main progenitors, and assign as their "descendants" local SDSS central galaxies matched in host halo mass. At face value, the comparison between high redshift and local data suggests a noticeable increase in stellar mass of a factor of >2 since z~1, and of >2.5 in mean effective radius. We then compare the inferred stellar mass and size growth with those predicted by hierarchical models for central galaxies, selected at high redshifts to closely match the halo and stellar mass bins as in the data. Only hierarchical models characterized by very limited satellite stellar stripping and parabolic orbits are capable of broadly reproducing the stellar mass and size increase of a factor ~2-4 observed in cluster galaxies since z ~1. The predicted, average (major) merger rate since z~1 is in good agreement with the latest observational estimates., 9 pages, 5 figures. ApJ, in press. Additional (minor) editing included in text and figure captions
Published: 2015
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43. The high mass end of the stellar mass function: Dependence on stellar population models and agreement between fits to the light profile

Author: Vinu Vikram, Francesco Shankar, J. L. Fischer, A. Meert, Marc Huertas-Company, Ravi K. Sheth, Claudia Maraston, Mariangela Bernardi, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation ( GEPI ), and Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS )
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Stellar population, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], media_common.quotation_subject, Dark matter, FOS: Physical sciences, Astrophysics, 01 natural sciences, Photometry (optics), 0103 physical sciences, fundamental parameters [galaxies], 010303 astronomy & astrophysics, luminosity function [galaxies], media_common, Physics, Number density, 010308 nuclear & particles physics, Astronomy, galaxies: fundamental parameters, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, galaxies: photometry, galaxies: luminosity function, mass function, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), photometry [galaxies], High mass, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We quantify the systematic effects on the stellar mass function which arise from assumptions about the stellar population, as well as how one fits the light profiles of the most luminous galaxies at z ~ 0.1. When comparing results from the literature, we are careful to separate out these effects. Our analysis shows that while systematics in the estimated comoving number density which arise from different treatments of the stellar population remain of order < 0.5 dex, systematics in photometry are now about 0.1 dex, despite recent claims in the literature. Compared to these more recent analyses, previous work based on Sloan Digital Sky Survey (SDSS) pipeline photometry leads to underestimates of rho_*(> M_*) by factors of 3-10 in the mass range 10^11 - 10^11.6 M_Sun, but up to a factor of 100 at higher stellar masses. This impacts studies which match massive galaxies to dark matter halos. Although systematics which arise from different treatments of the stellar population remain of order < 0.5 dex, our finding that systematics in photometry now amount to only about 0.1 dex in the stellar mass density is a significant improvement with respect to a decade ago. Our results highlight the importance of using the same stellar population and photometric models whenever low and high redshift samples are compared., 18 pages, 17 figures, accepted for publication in MNRAS. The PyMorph luminosities and stellar masses are available at https://www.physics.upenn.edu/~ameert/SDSS_PhotDec/
Published: 2017

44. On the intermediate-redshift central stellar mass-halo mass relation, and implications for the evolution of the most massive galaxies since z~1

Author: Vinu Vikram, Danilo Marchesini, Diego Capozzi, Claudia Maraston, Roy R. Gal, Marcella Carollo, Zheng Zheng, Alessandro Rettura, Vincent Bouillot, Francesco Shankar, Ravi K. Sheth, A. Meert, Marc Huertas-Company, Peter Behroozi, Begoña Ascaso, Hong Guo, Brian C. Lemaux, Mariangela Bernardi, Christopher J. Conselice, Lori M. Lubin, Andrey V. Kravtsov, Andrea Cattaneo, and Stewart Buchan
Subjects: Systematic error, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, media_common.quotation_subject, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, 10. No inequality, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Universe, Galaxy, Redshift, Space and Planetary Science, Mass relation, Halo, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The stellar mass-halo mass relation is a key constraint in all semi-analytic, numerical, and semi-empirical models of galaxy formation and evolution. However, its exact shape and redshift dependence remain debated. Several recent works support a relation in the local Universe steeper than previously thought. Based on the comparisons with a variety of data on massive central galaxies, we show that this steepening holds up to z~1, for stellar masses Mstar>2e11 Msun. Specifically, we find significant evidence for a high-mass end slope of ��>0.35-0.70, instead of the usual ��~0.20-0.30 reported by a number of previous results. When including the independent constraints from the recent BOSS clustering measurements, the data, independent of any systematic errors in stellar masses, tend to favor a model with a very small scatter (< 0.15 dex) in stellar mass at fixed halo mass, in the redshift range z < 0.8 and for Mstar>3e11 Msun, suggesting a close connection between massive galaxies and host halos even at relatively recent epochs. We discuss the implications of our results with respect to the evolution of the most massive galaxies since z~1., 6 pages, 4 figures. ApJ Letters, accepted
Published: 2014

45. Systematic effects on the size–luminosity relations of early- and late-type galaxies: dependence on model fitting and morphology

Author: Vinu Vikram, Francesco Shankar, Mariangela Bernardi, A. Meert, Marc Huertas-Company, Ravi K. Sheth, Simona Mei, Institut de recherches sur la catalyse et l'environnement de Lyon (IRCELYON), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), University of Illinois at Urbana Champaign (UIUC), University of Illinois at Urbana-Champaign [Urbana], and University of Illinois System-University of Illinois System
Subjects: Luminous infrared galaxy, Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, Radio galaxy, Astronomy, Astronomy and Astrophysics, Astrophysics, Disc galaxy, 01 natural sciences, Peculiar galaxy, Space and Planetary Science, Bulge, 0103 physical sciences, Elliptical galaxy, Disc, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Sersic profile, ComputingMilieux_MISCELLANEOUS
Abstract: We quantify the systematics in the size–luminosity relation of galaxies in the Sloan Digital Sky Survey main sample (i.e. at z ∼ 0.1) which arise from fitting different one- and two-component model profiles to the r-band images. For objects brighter than L_*, fitting a single Sersic profile to what is really a two-component SerExp system leads to biases: the half-light radius is increasingly overestimated as n of the fitted single component increases; it is also overestimated at B/T ∼ 0.6. For such objects, the assumption of a single Sersic component is particularly misleading. However, the net effect on the R-L relation is small, except for the most luminous tail. We then study how this relation depends on morphology. Our analysis is one of the first to use Bayesian-classifier-derived weights, rather than hard cuts, to define morphology. For the R-L relation Es, S0s and Sas are early types, whereas Sbs and Scds are late, although S0s tend to be 15 per cent smaller than Es of the same luminosity, and faint Sbs are more than 25 per cent smaller than faint Scds. Neither the early- nor the late-type relations are pure power laws: both show significant curvature, which we quantify. This curvature confirms that two mass scales are special for both early- and late-type galaxies: M_* ∼ 3 × 10^10 and 2 × 10^11 M_⊙. Also, although the R_disc-L_disc and R_disc-M_*disc relations of discs of disc-dominated galaxies run parallel to the corresponding relations for the total light in late types (i.e. they are significantly curved), R_bulge-L_bulge and R_bulge-M_*bulge for bulge-dominated systems show almost no curvature (i.e. unlike for the total light of early-type galaxies). Finally, the intrinsic scatter in the R-L relation decreases at large L and/or M_* and should provide additional constraints on models of how the most massive galaxies formed.
Published: 2014

46. Environmental dependence of bulge-dominated galaxy sizes in hierarchical models of galaxy formation. Comparison with the local Universe

Author: Ravi K. Sheth, L. Delaye, Andrea Cattaneo, Pierluigi Monaco, Simona Mei, Anand Raichoor, Francesco Shankar, Rossella Licitra, F. Fontanot, Jorge Moreno, Mariangela Bernardi, Marc Huertas-Company, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Victoria], University of Victoria [Canada] (UVIC), Heidelberger Institut für Theoretische Studien (H-ITS), Dipartimento di Fisica, Università degli Studi di Trieste, Università degli studi di Trieste, Department of Physics and Astronomy [Philadelphia], University of Pennsylvania [Philadelphia], Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), F., Shankar, S., Mei, M., Huertas Company, J., Moreno, F., Fontanot, Monaco, Pierluigi, M., Bernardi, A., Cattaneo, R., Sheth, R., Licitra, L., Delaye, A., Raichoor, Università degli studi di Trieste = University of Trieste, University of Pennsylvania, and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy merger, galaxies: bulges, 01 natural sciences, Peculiar galaxy, cosmology: theory, Galaxy group, 0103 physical sciences, Galaxy formation and evolution, Satellite galaxy, statistic [galaxies], Brightest cluster galaxy, 010303 astronomy & astrophysics, Lenticular galaxy, galaxies: statistics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Physics, [PHYS]Physics [physics], theory [cosmology], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Galaxy, galaxies: evolution, galaxies: structure, Space and Planetary Science, bulge [galaxies], structure [galaxies], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We compare state-of-the-art semi-analytic models of galaxy formation as well as advanced sub-halo abundance matching models with a large sample of early-type galaxies from SDSS at z < 0.3. We focus our attention on the dependence of median sizes of central galaxies on host halo mass. The data do not show any difference in the structural properties of early-type galaxies with environment, at fixed stellar mass. All hierarchical models considered in this work instead tend to predict a moderate to strong environmental dependence, with the median size increasing by a factor of about 1.5-3 when moving from low to high mass host haloes. At face value the discrepancy with the data is highly significant, especially at the cluster scale, for haloes above log Mhalo > 14. The convolution with (correlated) observational errors reduces some of the tension. Despite the observational uncertainties, the data tend to disfavour hierarchical models characterized by a relevant contribution of disc instabilities to the formation of spheroids, strong gas dissipation in (major) mergers, short dynamical friction timescales, and very short quenching timescales in infalling satellites. We also discuss a variety of additional related issues, such as the slope and scatter in the local size-stellar mass relation, the fraction of gas in local early-type galaxies, and the general predictions on satellite galaxies., 27 pages, 14 figures, 2 tables. MNRAS, in press
Published: 2014

47. THE NEXT GENERATION VIRGO CLUSTER SURVEY-INFRARED (NGVS-IR). I. A NEW NEAR-ULTRAVIOLET, OPTICAL, AND NEAR-INFRARED GLOBULAR CLUSTER SELECTION TOOL

Author: Eric W. Peng, Matthew A. Taylor, Rossella Licitra, Michael L. Balogh, Andrés Jordán, Chengze Liu, Jean-Charles Cuillandre, Ariane Lançon, Laura Ferrarese, Stephen Gwyn, Thomas H. Puzia, Alan W. McConnachie, Chien Y. Peng, H. J. McCracken, Lauren A. MacArthur, R. Brent Tully, Patrick Côté, Marc Huertas-Company, Alessandro Boselli, Patrick R. Durrell, Stéphane Courteau, Frédéric Bournaud, Pierre-Alain Duc, Scott Chapman, Raymond G. Carlberg, Hongxin Zhang, Anand Raichoor, Simona Mei, Paul Eigenthaler, Roberto Munoz, Olivier Ilbert, Giuseppe Gavazzi, John P. Blakeslee, P. Hudelot, John L. Tonry, Ronald Läsker, Yannick Mellier, Eric Emsellem, Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), Services communs OMP (UMS 831), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), University of Waterloo [Waterloo], Leiden Observatory [Leiden], Universiteit Leiden, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Dalhousie University [Halifax], Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB), Pontificia Universidad Católica de Chile (UC), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Research Center for Eco-Environmental Sciences, Chinese Academy of Sciences [Changchun Branch] (CAS), Services communs OMP - UMS 831 (UMS 831), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Universiteit Leiden [Leiden], Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Universitá degli Studi di Milano-Bicocca, Universitá degli Studi di Milan-Bocca, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Muñoz, R, Puzia, T, Lançon, A, Peng, E, Côté, P, Ferrarese, L, Blakeslee, J, Mei, S, Cuillandre, J, Hudelot, P, Courteau, S, Duc, P, Balogh, M, Boselli, A, Bournaud, F, Carlberg, R, Chapman, S, Durrell, P, Eigenthaler, P, Emsellem, E, Gavazzi, G, Gwyn, S, Huertas Company, M, Ilbert, O, Jordán, A, Läsker, R, Licitra, R, Liu, C, Macarthur, L, Mcconnachie, A, Mccracken, H, Mellier, Y, Peng, C, Raichoor, A, Taylor, M, Tonry, J, Tully, R, Zhang, H, Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Università degli Studi di Milano-Bicocca [Milano] (UNIMIB), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), and Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: galaxies: clusters: individual (Virgo), 010504 meteorology & atmospheric sciences, Point source, Astrophysics, 01 natural sciences, law.invention, Telescope, Sky brightness, law, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, [PHYS]Physics [physics], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy and Astrophysics, Virgo Cluster, Galaxy, galaxies: distances and redshift, galaxies: photometry, Star cluster, Space and Planetary Science, Limiting magnitude, Globular cluster, galaxies: luminosity function, mass function, galaxies: star clusters: general
Abstract: International audience; The NGVS-IR project (Next Generation Virgo Cluster Survey-Infrared) is a contiguous, near-infrared imaging survey of the Virgo cluster of galaxies. It complements the optical wide-field survey of Virgo (NGVS). In its current state, NGVS-IR consists of K-s-band imaging of 4 deg(2) centered on M87 and J- and K-s-band imaging of similar to 16 deg(2) covering the region between M49 and M87. We present observations of the central 4 deg(2) centered on Virgo's core region. The data were acquired with WIRCam on the Canada-France-Hawaii Telescope, and the total integration time was 41 hr distributed over 34 contiguous tiles. A survey-specific strategy was designed to account for extended galaxies while still measuring accurate sky brightness within the survey area. The average 5s limiting magnitude is K-s = 24.4 AB mag, and the 50% completeness limit is K-s = 23.75 AB mag for point-source detections, when using only images with better than 0.” 7 seeing (median seeing 0.” 54). Star clusters are marginally resolved in these image stacks, and Virgo galaxies with mu(Ks) similar or equal to 24.4 AB mag arcsec(-2) are detected. Combining the K-s data with optical and ultraviolet data, we build the uiK(s) color-color diagram, which allows a very clean color-based selection of globular clusters in Virgo. This diagnostic plot will provide reliable globular cluster candidates for spectroscopic follow-up campaigns, needed to continue the exploration of Virgo's photometric and kinematic substructures, and will help the design of future searches for globular clusters in extragalactic systems. We show that the new uiK(s) diagram displays significantly clearer substructure in the distribution of stars, globular clusters, and galaxies than the gzK(s) diagram-the NGVS + NGVS-IR equivalent of the BzK diagram that is widely used in cosmological surveys. Equipped with this powerful new tool, future NGVS-IR investigations based on the uiK(s) diagram will address the mapping and analysis of extended structures and compact stellar systems in and around Virgo galaxies.
Published: 2014

48. The Morphological Transformation of Red-Sequence Galaxies in the Distant Cluster XMMU J1229+0151

Author: P. Cerulo, Lauriane Delaye, Rubén Sánchez-Janssen, C. Lidman, Warrick J. Couch, Marc Huertas-Company, Simona Mei, R. Demarco, Centre for Astrophysics and Supercomputing [Swinburne] (CAS), Swinburne University of Technology [Melbourne], Anglo-Australian Observatory (AAO), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Departamento de Industrias, Universidad Técnica Federico Santa María, Av. España 1680, Valparaíso, Chile, European Southern Observatory [Santiago] (ESO), and European Southern Observatory (ESO)
Subjects: galaxies: high redshift, galaxies: spiral, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Disc galaxy, 01 natural sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Brightest cluster galaxy, education, 010303 astronomy & astrophysics, Galaxy cluster, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Luminous infrared galaxy, Physics, [PHYS]Physics [physics], education.field_of_study, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, galaxies: clusters: individual: XMMU J1229+0151, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: elliptical and lenticular, cD, Elliptical galaxy, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the results of a detailed analysis of galaxy properties along the red sequence in XMMU J1229+0151, an X-ray selected cluster at $z=0.98$ drawn from the HAWK-I Cluster Survey (HCS). Taking advantage of the broad photometric coverage and the availability of 77 spectra in the cluster field, we fit synthetic spectral energy distributions, and estimate stellar masses and photometric redshifts, which we use to determine the cluster membership. We investigate morphological and structural properties of red sequence galaxies and find that elliptical galaxies populate the bright end, while S0 galaxies represent the predominant population at intermediate luminosities, with their fraction decreasing at fainter magnitudes. A comparison with the low-redshift sample of the WINGS cluster survey reveals that at $z\sim1$ the bright end of the red sequence of XMMU J1229+0151 is richer in S0 galaxies. The faint end of the red sequence in XMMUJ1229+0151 appears rich in disc-dominated galaxies, which are rarer in the low redshift comparison sample at the same luminosities. Despite these differences between the morphological composition of the red sequence in XMMUJ1229+0151 and in low redshift samples, we find that to within the uncertainties, no such difference exists in the ratio of luminous to faint galaxies along the red sequence., Comment: 25 pages, 13 figures, accepted for publication in MNRAS
Published: 2014
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49. Larger sizes of massive quiescent early-type galaxies in clusters than in the field at 0.8 < z < 1.5

Author: A. Raichoor, P. Cerulo, Roberto Munoz, C. Lidman, Warrick J. Couch, R. Demarco, Francesco Shankar, Mariangela Bernardi, Ruben Sanchez-Janssen, R. Licitra, Masayuki Tanaka, Marc Huertas-Company, F. Barrientos, Andrew B. Newman, Lauriane Delaye, Simona Mei, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Service d'Expertise Nucléaire en Assainissement et Conception (SENAC), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Australian Astronomical Observatory, Cahill Center for Astronomy and Astrophysics, California Institute of Technology (CALTECH), Département de Physique des Particules (ex SPP) (DPP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Instituto de Astrofisica [Santiago], Pontificia Universidad Católica de Chile (UC), Department of Physics and Astronomy [Philadelphia], University of Pennsylvania [Philadelphia], Centre for Astrophysics and Supercomputing [Swinburne] (CAS), Swinburne University of Technology [Melbourne], Universidad de Concepción [Chile], European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), National Astronomical Observatory of Japan (NAOJ), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Département de Physique des Particules (ex SPP) (DPhP), University of Pennsylvania, and Universidad de Concepción - University of Concepcion [Chile]
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Field (physics), media_common.quotation_subject, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, 0103 physical sciences, Cluster (physics), 10. No inequality, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Accretion (astrophysics), Galaxy, Universe, Redshift, Early type, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: [abridged] The mass-size relation of early-type galaxies (ETGs) has been largely studied in the last years to probe the mass assembly of the most massive objects in the Universe. In this paper, we focus on the mass-size relation of quiescent massive ETGs (Mstar/Msol > 3*10^10) living in massive clusters (M200 ~ 10^14 Mstar) at 0.8< z, submitted to MNRAS
Published: 2014

50. NO EVIDENCE FOR A DEPENDENCE OF THE MASS-SIZE RELATION OF EARLY-TYPE GALAXIES ON ENVIRONMENT IN THE LOCAL UNIVERSE

Author: Francesco Shankar, J. A. L. Aguerri, Vinu Vikram, A. Meert, Marc Huertas-Company, Mariangela Bernardi, Simona Mei, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Institut de recherches sur la catalyse et l'environnement de Lyon (IRCELYON), Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Field (physics), Stellar mass, media_common.quotation_subject, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, 10. No inequality, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, media_common, Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Redshift, Galaxy, Universe, Space and Planetary Science, Sky, Halo, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The early--type galaxy (ETG) mass--size relation has been largely studied to understand how these galaxies have assembled their mass. One key observational result of the last years is that massive galaxies increased their size by a factor of a few at fixed stellar mass from $z\sim2$. Hierarchical models favor minor mergers as a plausible driver of this size growth. Some of these models, predict a significant environmental dependence in the sense that galaxies residing in more massive halos tend to be larger than galaxies in lower mass halos, at fixed stellar mass and redshift. At present, observational results of this environmental dependence have been contradictory. In this paper we revisit this issue in the local Universe, by investigating how the sizes of massive ETGs depend on large-scale environment using an updated and accurate sample of ETGs in different environments - field, group, clusters - from the Sloan Digital Sky Survey DR7. Our analysis does not show any significant environmental dependence of the sizes of central and satellites ETGs at fixed stellar mass at $z\sim0$. The size-mass relation of early-type galaxies at $z\sim0$ seems to be universal, i.e., independent of the mass of the host halo and of the position of the galaxy in that halo (central or satellite). The result is robust to different galaxy selections based on star formation, morphology or central density. In fact, considering our observational errors and the size of the sample, any size ratio larger than $30-40%$ between massive galaxies ($log(M_*/M_\odot)>11$) living in clusters and in the field can be ruled out at $3\sigma$ level., Comment: accepted for publication in ApJ
Published: 2013

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