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3. The hidden side of cosmic star formation at z > 3: Bridging optically-dark and Lyman break galaxies with GOODS-ALMA

Author

M.-Y. Xiao, D. Elbaz, C. Gómez-Guijarro, L. Leroy, L.-J. Bing, E. Daddi, B. Magnelli, M. Franco, L. Zhou, M. Dickinson, T. Wang, W. Rujopakarn, G. E. Magdis, E. Treister, H. Inami, R. Demarco, M. T. Sargent, X. Shu, J. S. Kartaltepe, D. M. Alexander, M. Béthermin, F. Bournaud, L. Ciesla, H. C. Ferguson, S. L. Finkelstein, M. Giavalisco, Q.-S. Gu, D. Iono, S. Juneau, G. Lagache, R. Leiton, H. Messias, K. Motohara, J. Mullaney, N. Nagar, M. Pannella, C. Papovich, A. Pope, C. Schreiber, and J. Silverman

Subjects
high-redshift [Galaxies], galaxies [Submillimeter], Space and Planetary Science, photometry [Galaxies], Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, star formation [Galaxies]
Abstract

Our current understanding of the cosmic star formation history at z>3 is primarily based on UV-selected galaxies (i.e., LBGs). Recent studies of H-dropouts have revealed that we may be missing a large proportion of star formation that is taking place in massive galaxies at z>3. In this work, we extend the H-dropout criterion to lower masses to select optically dark/faint galaxies (OFGs), in order to complete the census between LBGs and H-dropouts. Our criterion (H> 26.5 mag & [4.5] < 25 mag) combined with a de-blending technique is designed to select not only extremely dust-obscured massive galaxies but also normal star-forming galaxies. In total, we identified 27 OFGs at z_phot > 3 (z_med=4.1) in the GOODS-ALMA field, covering a wide distribution of stellar masses with log($M_{\star}$/$M_{\odot}$) = 9.4-11.1. We find that up to 75% of the OFGs with log($M_{\star}$/$M_{\odot}$) = 9.5-10.5 were neglected by previous LBGs and H-dropout selection techniques. After performing stacking analyses, the OFGs exhibit shorter gas depletion timescales, slightly lower gas fractions, and lower dust temperatures than typical star-forming galaxies. Their SFR_tot (SFR_ IR+SFR_UV) is much larger than SFR_UVcorr (corrected for dust extinction), with SFR_tot/SFR_UVcorr = $8\pm1$, suggesting the presence of hidden dust regions in the OFGs that absorb all UV photons. The average dust size measured by a circular Gaussian model fit is R_e(1.13 mm)=1.01$\pm$0.05 kpc. We find that the cosmic SFRD at z>3 contributed by massive OFGs is at least two orders of magnitude higher than the one contributed by equivalently massive LBGs. Finally, we calculate the combined contribution of OFGs and LBGs to the cosmic SFRD at z=4-5 to be 4 $\times$ 10$^{-2}$ $M_{\odot}$ yr$^{-1}$Mpc$^{-3}$, which is about 0.15 dex (43%) higher than the SFRD derived from UV-selected samples alone at the same redshift., 26 pages, 14 figures, 8 tables. Accepted for publication in A&A

Published
2022
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4. A super-linear 'radio-AGN main sequence' links mean radio-AGN power and galaxy stellar mass since z$\sim$3

Author

I. Delvecchio, E. Daddi, M. T. Sargent, J. Aird, J. R. Mullaney, B. Magnelli, D. Elbaz, L. Bisigello, L. Ceraj, S. Jin, B. S. Kalita, D. Liu, M. Novak, I. Prandoni, J. F. Radcliffe, C. Spingola, G. Zamorani, V. Allevato, G. Rodighiero, and V. Smolčić

Subjects
galaxies: nuclei, radio continuum: galaxies, galaxies: luminosity function, mass function, galaxies: active, galaxies: evolution, Astrophysics - Astrophysics of Galaxies, active [Galaxies], Space and Planetary Science, astro-ph.GA, nuclei [Galaxies], Mass function, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, galaxies [Radio continuum], evolution [Galaxies], luminosity function [Galaxies]
Abstract

Mapping the average AGN luminosity across galaxy populations and over time encapsulates important clues on the interplay between supermassive black hole (SMBH) and galaxy growth. This paper presents the demography, mean power and cosmic evolution of radio AGN across star-forming galaxies (SFGs) of different stellar masses (${M_{*}}$). We exploit deep VLA-COSMOS 3 GHz data to build the rest-frame 1.4 GHz AGN luminosity functions at 0.1$\leq$$z$$\leq$4.5 hosted in SFGs. Splitting the AGN luminosity function into different ${M_{*}}$ bins reveals that, at all redshifts, radio AGN are both more frequent and more luminous in higher ${M_*}$ than in lower ${M_*}$ galaxies. The cumulative kinetic luminosity density exerted by radio AGN in SFGs peaks at $z$$\sim$2, and it is mostly driven by galaxies with 10.5$\leq$$\log$(${M_{*}}$/${M_{\odot}}$)$, Comment: Accepted for publication in A&A. 20 pages + Appendices

Published
2022
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5. GOODS-ALMA 2.0:Starbursts in the main sequence reveal compact star formation regulating galaxy evolution prequenching

Author

C. Gómez-Guijarro, D. Elbaz, M. Xiao, V. I. Kokorev, G. E. Magdis, B. Magnelli, E. Daddi, F. Valentino, M. T. Sargent, M. Dickinson, M. Béthermin, M. Franco, A. Pope, B. S. Kalita, L. Ciesla, R. Demarco, H. Inami, W. Rujopakarn, X. Shu, T. Wang, L. Zhou, D. M. Alexander, F. Bournaud, R. Chary, H. C. Ferguson, S. L. Finkelstein, M. Giavalisco, D. Iono, S. Juneau, J. S. Kartaltepe, G. Lagache, E. Le Floc’h, R. Leiton, L. Leroy, L. Lin, K. Motohara, J. Mullaney, K. Okumura, M. Pannella, C. Papovich, E. Treister, 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), University of Copenhagen = Københavns Universitet (UCPH), Danmarks Tekniske Universitet = Technical University of Denmark (DTU), University of Sussex, Community Science and Data Center, 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), University of Hertfordshire [Hatfield] (UH), University of Massachusetts [Amherst] (UMass Amherst), University of Massachusetts System (UMASS), Universidad de Concepción - University of Concepcion [Chile], Hiroshima University, Chulalongkorn University [Bangkok], Anhui Normal University, Nanjing University (NJU), Durham University, California Institute of Technology (CALTECH), Space Telescope Science Institute (STSci), University of Texas at Austin [Austin], National Astronomical Observatory of Japan (NAOJ), Rochester Institute of Technology, Academia Sinica, The University of Tokyo (UTokyo), University of Sheffield [Sheffield], Università degli studi di Trieste = University of Trieste, Texas A&M University [College Station], and Pontificia Universidad Católica de Chile (UC)

Subjects
submillimeter: galaxies, SPECTROSCOPIC SURVEY, Cosmology and Nongalactic Astrophysics (astro-ph.CO), SIMILAR-TO 3, MASS-METALLICITY RELATION, INFRARED-EMISSION, structure [Galaxies], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, star formation [Galaxies], star formation, high-redshift, high-redshift [Galaxies], galaxies [Submillimeter], galaxies: high-redshift, galaxies, evolution, DUST TEMPERATURES, Astrophysics::Solar and Stellar Astrophysics, submillimeter, structure, Astrophysics::Galaxy Astrophysics, FORMING GALAXIES, SUBMILLIMETER GALAXIES, galaxies: fundamental parameters, Astronomy and Astrophysics, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, ORIGINS DEEP SURVEY, MOLECULAR GAS FRACTIONS, Space and Planetary Science, galaxies: star formation, Astrophysics of Galaxies (astro-ph.GA), fundamental parameters [Galaxies], galaxies: structure, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], fundamental parameters, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Compact star formation appears to be generally common in dusty star-forming galaxies (SFGs). However, its role in the framework set by the scaling relations in galaxy evolution remains to be understood. In this work we follow up on the galaxy sample from the GOODS-ALMA 2.0 survey, an ALMA blind survey at 1.1mm covering a continuous area of 72.42arcmin$^2$ using two array configurations. We derived physical properties, such as star formation rates, gas fractions, depletion timescales, and dust temperatures for the galaxy sample built from the survey. There exists a subset of galaxies that exhibit starburst-like short depletion timescales, but they are located within the scatter of the so-called main sequence of SFGs. These are dubbed starbursts in the main sequence and display the most compact star formation and they are characterized by the shortest depletion timescales, lowest gas fractions, and highest dust temperatures of the galaxy sample, compared to typical SFGs at the same stellar mass and redshift. They are also very massive, accounting for $\sim 60\%$ of the most massive galaxies in the sample ($\log (M_{\rm{*}}/M_{\odot}) > 11.0$). We find trends between the areas of the ongoing star formation regions and the derived physical properties for the sample, unveiling the role of compact star formation as a physical driver of these properties. Starbursts in the main sequence appear to be the extreme cases of these trends. We discuss possible scenarios of galaxy evolution to explain the results drawn from our galaxy sample. Our findings suggest that the star formation rate is sustained in SFGs by gas and star formation compression, keeping them within the main sequence even when their gas fractions are low and they are presumably on the way to quiescence., Accepted by A&A. 26 pages, 13 figures

Published
2022
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6. The environmental effect on galaxy evolution: Cl J1449 + 0856 at z = 1.99

Author

R. Coogan, Raphael Gobat, M. T. Sargent, and E. Daddi

Subjects
Physics, Environmental effect, Space and Planetary Science, Star formation, Galaxy formation and evolution, Astronomy and Astrophysics, Astrophysics, Redshift, Galaxy, Galaxy cluster
Abstract

This work focuses on understanding the formation of the first massive, passive galaxies in clusters, as a first step to the development of environmental trends seen at low redshift. Cl J1449 + 0856 is an excellent case to study this - a galaxy cluster at redshift z = 1.99 that already shows evidence of a virialised atmosphere. Here we highlight two recent results: the discovery of merger-driven star formation and highly-excited molecular gas in galaxies at the core of Cl J1449, along with the lowest-mass Sunyaev-Zel’dovich detection to date.

Published
2020
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7. The infrared-radio correlation of star-forming galaxies is strongly M⋆-dependent but nearly redshift-invariant since z ∼ 4

Author

I. Delvecchio, E. Daddi, M. T. Sargent, M. J. Jarvis, D. Elbaz, S. Jin, D. Liu, I. H. Whittam, H. Algera, R. Carraro, C. D’Eugenio, J. Delhaize, B. S. Kalita, S. Leslie, D. Cs. Molnár, M. Novak, I. Prandoni, V. Smolčić, Y. Ao, M. Aravena, F. Bournaud, J. D. Collier, S. M. Randriamampandry, Z. Randriamanakoto, G. Rodighiero, J. Schober, S. V. White, G. Zamorani, 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), INAF - Osservatorio Astronomico di Milano (OAM), Istituto Nazionale di Astrofisica (INAF), Astronomy Centre, University of Sussex, Oxford Astrophysics, University of Oxford [Oxford], University of the Western Cape, Instituto de Astrofisica de Canarias (IAC), Departamento de Astrofísica [La laguna], Universidad de La Laguna [Tenerife - SP] (ULL), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Universidad de Valparaiso [Chile], University of Cape Town, INAF - Osservatorio Astronomico di Cagliari (OAC), Istituto di Radioastronomia [Bologna] (IRA), University of Zagreb, Universita degli Studi di Padova, EPFL Laboratoire d’astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL), Rhodes University, Grahamstown, INAF - Osservatorio Astronomico di Bologna (OABO), European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 788679, European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 694343), Support from the ERC Advanced Grant 740246 (Cosmic Gas), National Research Foundation (NRF), 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), University of Oxford, University of the Western Cape (UWC), Universiteit Leiden, and Università degli Studi di Padova = University of Padua (Unipd)

Subjects
Field (physics), Stellar mass, Infrared, galaxies: star formation, radio continuum: galaxies, infrared: galaxies, galaxies: active, galaxies: evolution, Astrophysics - Astrophysics of Galaxies, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics - astrophysics of galaxies, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Luminous infrared galaxy, 010308 nuclear & particles physics, Spectral density, Astronomy and Astrophysics, Galaxy, Redshift, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Several works in the past decade have used the ratio between total (rest 8-1000$\mu$m) infrared and radio (rest 1.4~GHz) luminosity in star-forming galaxies (q$_{IR}$), often referred to as the "infrared-radio correlation" (IRRC), to calibrate radio emission as a star formation rate (SFR) indicator. Previous studies constrained the evolution of q$_{IR}$ with redshift, finding a mild but significant decline, that is yet to be understood. For the first time, we calibrate q$_{IR}$ as a function of \textit{both} stellar mass (M$_{\star}$) and redshift, starting from an M$_{\star}$-selected sample of $>$400,000 star-forming galaxies in the COSMOS field, identified via (NUV-r)/(r-J) colours, at redshifts 0.1$, Comment: Accepted for publication in A&A. 22 pages + Appendices. 24 figures, 4 tables

Published
2021
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8. The Main Sequence at z ∼ 1.3 Contains a Sizable Fraction of Galaxies with Compact Star Formation Sizes: A New Population of Early Post-starbursts?

Author

E. Daddi, M. T. Sargent, Lorenzo Zanisi, John D. Silverman, D. Elbaz, Manuel Aravena, Dominik Riechers, G. Rodighiero, Yang Gao, Georgios E. Magdis, Chiara Mancini, Shuowen Jin, C. Circosta, Anna Cibinel, Daizhong Liu, E. Le Floc'h, Francesco Valentino, Helmut Dannerbauer, Alfio Puglisi, Raphael Gobat, A. Calabrò, F. Bournaud, and I. Delvecchio

Subjects
010504 meteorology & atmospheric sciences, Stellar mass, Population, FOS: Physical sciences, interactions [Galaxies], Astrophysics, Compact star, Lambda, star formation [Galaxies], 01 natural sciences, high-redshift [Galaxies], galaxies: high-redshift, ISM [Galaxies], 0103 physical sciences, galaxies: interactions, Poor correlation, 10. No inequality, education, 010303 astronomy & astrophysics, QB, 0105 earth and related environmental sciences, Physics, education.field_of_study, Astronomy and Astrophysics, evolution [Galaxies], New population, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: star formation, galaxies: evolution, galaxies: ISM
Abstract

ALMA measurements for 93 $Herschel$-selected galaxies at $1.1 \leqslant z \leqslant 1.7$ in COSMOS reveal a sizable ($>29$\%) population with compact star formation (SF) sizes, lying on average $> \times 3.6$ below the optical stellar mass ($M_{\star}$)-size relation of disks. This sample widely spans the star-forming Main Sequence (MS), having $10^{8} \leqslant M_{\star} \leqslant 10^{11.5} \ M_{\odot}$ and $20 \leqslant SFR \leqslant 680 \ M_{\odot} \rm yr^{-1}$. The 32 size measurements and 61 upper limits are measured on ALMA images that combine observations of CO(5-4), CO(4-3), CO(2-1) and $��_{\rm obs} \sim 1.1-1.3 \ \rm mm$ continuum, all tracing the star-forming molecular gas. These compact galaxies have instead normally extended $K_{band}$ sizes, suggesting strong specific $SFR$ gradients. Compact galaxies comprise the $50\pm18 \%$ of MS galaxies at $M_{\star} > 10^{11} M_{\odot}$. This is not expected in standard bi-modal scenarios where MS galaxies are mostly steadily-growing extended disks. We suggest that compact MS objects are early post-starburst galaxies in which the merger-driven boost of SF has subsided. They retain their compact SF size until either further gas accretion restores pre-merger galaxy-wide SF, or until becoming quenched. The fraction of merger-affected SF inside the MS seems thus larger than anticipated and might reach $\sim 50$\% at the highest $M_{\star}$. The presence of large galaxies above the MS demonstrates an overall poor correlation between galaxy SF size and specific $SFR$., 7 pages, 5 figures. Accepted for publication in ApJ Letters

Published
2019
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9. Deciphering the Activity and Quiescence of High-redshift Cluster Environments: ALMA Observations of Cl J1449+0856 at z = 2

Author

Masato Onodera, E. Daddi, Francesco Valentino, Maurilio Pannella, Daizhong Liu, A. Cimatti, Raphael Gobat, A. Finoguenov, Alvio Renzini, Nobuo Arimoto, V. Strazzullo, M. T. Sargent, R. Coogan, Helmut Dannerbauer, Mark Dickinson, M. Bethermin, Department of Physics, Ludwig-Maximilians-Universität München (LMU), 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), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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), National Optical Astronomy Observatory (NOAO), Max-Planck-Institut für Extraterrestrische Physik (MPE), National Astronomical Observatory of Japan (NAOJ), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Astronomy Centre [Brighton], University of Sussex, Département d'Astrophysique (ex SAP) (DAP), 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, 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), Pontificia Universidad Católica de Valparaíso (PUCV), Dark Cosmology Centre (DARK), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Seoul National University [Seoul] (SNU), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Instituto de Astrofisica de Canarias (IAC), Max Planck Institute for Astronomy (MPIA), 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), Strazzullo, V., Coogan, R. T., Daddi, E., Sargent, M. T., Gobat, R., Valentino, F., Bethermin, M., Pannella, M., Dickinson, M., Renzini, A., Arimoto, N., Cimatti, A., Dannerbauer, H., Finoguenov, A., Liu, D., Onodera, M., University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Università degli Studi di Bologna, NOAO, and Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)

Subjects
galaxies: clusters: individual, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Population, FOS: Physical sciences, Astrophysics, 01 natural sciences, galaxies: clusters: individual: Cl J1449+0856, galaxies: evolution, galaxies: high-redshift, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxie, Z=1.46, 0103 physical sciences, STAR-FORMING GALAXIES, Continuum (set theory), Brightest cluster galaxy, RED-SEQUENCE, education, 010303 astronomy & astrophysics, evolution [galaxies], QB, Line (formation), Physics, education.field_of_study, PROTOCLUSTER, 010308 nuclear & particles physics, Star formation, Center (category theory), STARBURST GALAXIES, Astronomy and Astrophysics, Astronomy and Astrophysic, ALPHA EMITTERS, 115 Astronomy, Space science, Galaxy, Redshift, DENSE ENVIRONMENTS, EVOLUTION, galaxies: clusters: individual ( ClJ1449+0856), [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, LUMINOSITY FUNCTION, Astrophysics of Galaxies (astro-ph.GA), MOLECULAR GAS-RESERVOIRS, clusters: individual: Cl J1449+0856 [galaxies], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], high-redshift [galaxies]
Abstract

We present ALMA observations of the 870$\mu$m continuum and CO(4-3) line emission in the core of the galaxy cluster ClJ1449+0856 at z=2, a NIR-selected, X-ray detected system in the mass range of typical progenitors of today's massive clusters. The 870$\mu$m map reveals six F$_{870\mu m}$ > 0.5 mJy sources spread over an area of 0.07 arcmin$^2$, giving an overdensity of a factor ~10 (6) with respect to blank field counts down to F$_{870\mu m}$ > 1 (0.5) mJy. On the other hand, deep CO(4-3) follow-up confirms membership of three of these sources, but suggests that the remaining three, including the brightest 870$\mu$m sources in the field (F$_{870\mu m}\gtrsim$2 mJy), are likely interlopers. The measurement of 870$\mu$m continuum and CO(4-3) line fluxes at the positions of previously-known cluster members provides a deep probe of dusty star formation occurring in the core of this high-redshift structure, adding up to a total SFR~700$\pm$100 M$_{\odot}$/yr and yielding an integrated star formation rate density of ~10$^4$ M$_{\odot}$/yr/Mpc$^3$, five orders of magnitude larger than in the field at the same epoch, due to the concentration of star-forming galaxies in the small volume of the dense cluster core. The combination of these observations with previously available HST imaging highlights the presence in this same volume of a population of galaxies with already suppressed star formation. This diverse composition of galaxy populations in ClJ1449+0856 is especially highlighted at the very cluster center, where a complex assembly of quiescent and star-forming sources is likely forming the future Brightest Cluster Galaxy., Comment: 11 pages, 6 figures, ApJ in press

Published
2018
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10. GOODS-Herschel: the far-infrared view of star formation in active galactic nucleus host galaxies since z ≈ 3

Author

David M. Alexander, Benjamin Magnelli, Frederic Bournaud, Rob Ivison, Roger Leiton, Maurilio Pannella, James Mullaney, Emanuele Daddi, Mark Dickinson, Ho Seong Hwang, D. Elbaz, Douglas Scott, W. N. Brandt, Franz E. Bauer, Ivan Valtchanov, P. Popesso, M. T. Sargent, Bruno Altieri, Kalliopi Dasyra, Ryan C. Hickox, Bin Luo, Georgios E. Magdis, D. J. Hanish, Dieter Lutz, Helmut Dannerbauer, A. Del Moro, D. Coia, Yongquan Xue, J. Kartaltepe, Stéphanie Juneau, and H. Aussel

Subjects
Physics, Luminous infrared galaxy, Active galactic nucleus, 010308 nuclear & particles physics, Radio galaxy, Star formation, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Disc galaxy, 01 natural sciences, Galaxy, Space and Planetary Science, 0103 physical sciences, Elliptical galaxy, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Lenticular galaxy, Astrophysics::Galaxy Astrophysics
Abstract

We present a study of the infrared properties of X-ray selected, moderate-luminosity (i.e. L_X= 10^(42)–10^(44) erg s^(−1)) active galactic nuclei (AGNs) up to z ≈ 3, in order to explore the links between star formation in galaxies and accretion on to their central black holes. We use 100 and 160 μ m fluxes from GOODS-Herschel – the deepest survey yet undertaken by the Herschel telescope – and show that in the vast majority of cases (i.e. >94 per cent) these fluxes are dominated by emission from the host galaxy. As such, these far-infrared bands provide an uncontaminated view of star formation in the AGN host galaxies. We find no evidence of any correlation between the X-ray and infrared luminosities of moderate AGNs at any redshift, suggesting that global star formation is decoupled from nuclear (i.e. AGN) activity in these galaxies. On the other hand, we confirm that the star formation rates of AGN hosts increase strongly with redshift, by a factor of 43^(+27)_(−18) from z < 0.1 to z = 2–3 for AGNs with the same range of X-ray luminosities. This increase is entirely consistent with the factor of 25–50 increase in the specific star formation rates (SSFRs) of normal, star-forming (i.e. main-sequence) galaxies over the same redshift range. Indeed, the average SSFRs of AGN hosts are only marginally (i.e. ≈20 per cent) lower than those of main-sequence galaxies at all surveyed redshifts, with this small deficit being due to a fraction of AGNs residing in quiescent (i.e. low SSFR) galaxies. We estimate that 79 ± 10 per cent of moderate-luminosity AGNs are hosted in main-sequence galaxies, 15 ± 7 per cent in quiescent galaxies and

Published
2011
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11. SPITZER70 AND 160 μm OBSERVATIONS OF THE COSMOS FIELD

Author

Patrick L. Shopbell, David L. Shupe, George Helou, Nick Scoville, O. Ilbert, Peter Capak, Bidushi Bhattacharya, Kartik Sheth, Jason Surace, N. Lee, Hai Fu, D. B. Sanders, Lin Yan, J. Kartaltepe, A. Afonso-Luis, Mara Salvato, Anton M. Koekemoer, H. Aussel, David T. Frayer, Minh Huynh, E. Le Floc'h, Eric J. Murphy, Eva Schinnerer, D. Fadda, and M. T. Sargent

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Field (physics), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Space and Planetary Science, medicine, Calibration, Source counts, medicine.symptom, Noise level, Astrophysics - Cosmology and Nongalactic Astrophysics, Confusion
Abstract

We present Spitzer 70 and 160 micron observations of the COSMOS Spitzer survey (S-COSMOS). The data processing techniques are discussed for the publicly released products consisting of images and source catalogs. We present accurate 70 and 160 micron source counts of the COSMOS field and find reasonable agreement with measurements in other fields and with model predictions. The previously reported counts for GOODS-North and the extragalactic First Look Survey are updated with the latest calibration, and counts are measured based on the large area SWIRE survey to constrain the bright source counts. We measure an extragalactic confusion noise level of sigma_c = 9.4+/-3.3 mJy (q=5) for the MIPS 160-micron band based on the deep S-COSMOS data and report an updated confusion noise level of sigma_c = 0.35+/-0.15 mJy (q=5) for the MIPS 70-micron band., Comment: Accepted AJ, 15 Aug. 2009. Data available at http://spider.ipac.caltech.edu/staff/frayer/mycosmos/ until released by IRSA

Published
2009
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12. The Dependence of Star Formation Activity on Stellar Mass Surface Density and Sersic Index in zCOSMOS Galaxies at 0.5 <z <0.9 Compared with SDSS Galaxies at 0.04 <z <0.08

Author

M. T. Sargent, D. Bottini, Daniela Vergani, P. Franzetti, Olga Cucciati, Andrea Cimatti, A. Iovino, Simon J. Lilly, Christian Maier, A. Cappi, J. F. Le Borgne, S. de la Torre, Christian Marinoni, Karina Caputi, C. Knobel, U. Abbas, L. de Ravel, Y. Peng, E. Ricciardelli, Alvio Renzini, C. Halliday, M. Scodeggio, Claudia Scarlata, V. Le Brun, M. Mignoli, Angela Bongiorno, Anton M. Koekemoer, Pascal Oesch, A. Leauthaud, S. Bardelli, Cristiano Porciani, P. Kampczyk, Laurence Tresse, Lidia Tasca, Thierry Contini, B. Meneux, Paolo Cassata, Masayuki Tanaka, Bianca Garilli, P. Memeo, V. Mainieri, Roser Pello, Lucia Pozzetti, C. M. Carollo, O. Le Fèvre, M. Bolzonella, G. Zamorani, John D. Silverman, Jean-Paul Kneib, E. Perez Montero, H. J. McCracken, Graziano Coppa, D. Maccagni, E. Zucca, Luigi Guzzo, F. Lamareille, M. Fumana, Roberto Scaramella, K. Kovac, INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Laboratoire Astrophysique de Toulouse-Tarbes (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), 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), Centre de Physique Théorique - UMR 6207 (CPT), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), 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 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), 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), Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astronomy, Maier C., Lilly S. J., Zamorani G., Scodeggio M., Lamareille F., Contini T., Sargent M. T., Scarlata C., Oesch P., Carollo C. M., Le Fèvre O., Renzini A., Kneib J.-P., Mainieri V., Bardelli S., Bolzonella M., Bongiorno A., Caputi K., Coppa G., Cucciati O., de la Torre S., de Ravel L., Franzetti P., Garilli B., Iovino A., Kampczyk P., Knobel C., Kova&#269, K., Le Borgne J.-F., Le Brun V., Mignoli M., Pello R., Peng Y., Montero E. Perez, Ricciardelli E., Silverman J. D., Tanaka M., Tasca L., Tresse L., Vergani D., Zucca E., Abbas U., Bottini D., Cappi A., Cassata P., Cimatti A., Fumana M., Guzzo L., Halliday C., Koekemoer A. M., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Porciani C., Pozzetti L., and Scaramella R.

Subjects
Surface (mathematics), 010504 meteorology & atmospheric sciences, Stellar mass, Population, PHYSICAL-PROPERTIES, POPULATION SYNTHESIS, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, galaxies: high-redshift, 0103 physical sciences, Galaxy formation and evolution, 10. No inequality, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, LOCAL UNIVERSE, Physics, EVOLUTION SURVEY COSMOS, REDSHIFT SURVEY, education.field_of_study, Galaxies: evolution, Galaxies: high-redshift, Astronomy and Astrophysics, Space and Planetary Science, FORMING GALAXIES, Star formation, ASSEMBLY HISTORY, DISK GALAXIES, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, LUMINOSITY FUNCTION, DIGITAL SKY SURVEY, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], galaxies: evolution, Surface mass, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

One of the key unanswered questions in the study of galaxy evolution is what physical processes inside galaxies drive the changes in the SFRs in individual galaxies that, taken together, produce the large decline in the global star-formation rate density (SFRD) to redshifts since z~2. Many studies of the SFR at intermediate redshifts have been made as a function of the integrated stellar mass of galaxies but these did not use information on the internal structural properties of the galaxies. In this paper we present a comparative study of the dependence of SFRs on the average surface mass densities (SigmaM) of galaxies of different morphological types up to z~1 using the zCOSMOS and SDSS surveys. The main findings about the evolution of these relatively massive galaxies are: 1) There is evidence that, for both SDSS ans zCOSMOS galaxies, the mean specific SFR within a given population (either disk-dominated or bulge-dominated) is independent of SigmaM; 2) The observed SSFR - SigmaM step-function relation is due, at all investigated redshifts, to the changing mix of disk-dominated and bulge-dominated galaxies as surface density increases and the strong difference in the average SSFR between disks and bulges. We also find a modest differential evolution in the size-mass relations of disk and spheroid galaxies; 3) The shape of the median SSFR - SigmaM relation is similar, but with median SSFR values that are about 5-6 times higher in zCOSMOS galaxies than for SDSS, across the whole range of SigmaM, and in both spheroid and disk galaxies. This increase matches that of the global SFRD of the Universe as a whole, emphasizing that galaxies of all types are contributing, proportionally, to the global increase in SFRD in the Universe back to these redshifts (abridged)., Comment: Published 2009 in ApJ, 694, 1099

Published
2009
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13. COSMOS Morphological Classification with the Zurich Estimator of Structural Types (ZEST) and the Evolution Since z = 1 of the Luminosity Function of Early, Disk, and Irregular Galaxies

Author

A. Leauthaud, Christian Maier, Yasuhiro Shioya, Cristiano Porciani, Masaru Ajiki, Herve Aussel, Nick Scoville, Kartik Sheth, M. T. Sargent, Richard Massey, P. Kampczyk, C. M. Carollo, Robert Feldmann, Jean-Paul Kneib, H. J. McCracken, Anton M. Koekemoer, D. Thompson, Simon J. Lilly, Yoshiaki Taniguchi, L. A. M. Tasca, Peter Capak, D. B. Sanders, Claudia Scarlata, T. Murayama, Alvio Renzini, S. S. Sasaki, Jason Rhodes, Bahram Mobasher, M. I. Takahashi, 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), Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Zest, Cosmology: Dark Matter, Galaxies: Formation, Dark matter, Astrophysics::Instrumentation and Methods for Astrophysics, Estimator, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Surveys, Cosmology: Observations, Galaxy, Redshift, Cosmology: Large-Scale Structure of Universe, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Galaxies: Evolution, Galaxy formation and evolution, Surface brightness, Irregular galaxy, Astrophysics::Galaxy Astrophysics
Abstract

International audience; Motivated by the desire to reliably and automatically classify structure of thousands of COSMOS galaxies, we present ZEST, the Zurich Estimator of Structural Types. To classify galaxy structure, ZEST uses (1) five nonparametric diagnostics: asymmetry, concentration, Gini coefficient, second-order moment of the brightest 20% of galaxy pixels, and ellipticity; and (2) the exponent n of single-Sérsic fits to the two-dimensional surface brightness distributions. To fully exploit the wealth of information while reducing the redundancy present in these diagnostics, ZEST performs a principal component (PC) analysis. We use a sample of ~56,000 IAB1, PC2, and PC3. We demonstrate the robustness of the ZEST grid on the z=0 sample of Frei et al. The ZEST classification breaks most of the degeneracy between different galaxy populations that affects morphological classifications based on only some of the diagnostics included in ZEST. As a first application, we present the evolution since z~1 of the luminosity functions (LFs) of COSMOS galaxies of early, disk, and irregular galaxies and, for disk galaxies, of different bulge-to-disk ratios. Overall, we find that the LF up to a redshift z=1 is consistent with a pure luminosity evolution (of about 0.95 mag at z~0.7). We highlight, however, two trends that are in general agreement with a downsizing scenario for galaxy formation, i.e., (1) a deficit of a factor of about 2 at z~0.7 of MB>-20.5 structurally classified early-type galaxies and (2) an excess of a factor of about 3, at a similar redshift, of irregular galaxies. Based on observations with the NASA/ESA Hubble Space Telescope , obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under NASA contract NAS 5-26555 also based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory, and the National Optical Astronomy Observatory, which are operated by AURA, Inc., under cooperative agreement with the National Science Foundation; and the Canada-France-Hawaii Telescope operated by the National Research Council of Canada, the Centre National de la Recherche Scientifique de France, and the University of Hawaii.

Published
2007
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14. A higher efficiency of converting gas to stars push galaxies at z ~ 1.6 well above the star-forming main sequence

Author

E. Daddi, Daizhong Liu, Anton M. Koekemoer, M. Bethermin, Chiara Feruglio, D. Lutz, Masato Onodera, D. B. Sanders, Nobuo Arimoto, M. T. Sargent, Georgios E. Magdis, G. Rodighiero, Tohru Nagao, J. S. Kartaltepe, G. Zamorani, John D. Silverman, Chiara Mancini, S. Berta, W. Rujopakarn, Daichi Kashino, and Alvio Renzini

Subjects
Physics, galaxies: high-redshift, galaxies: ISM, galaxies: star formation, galaxies: starburst, Astronomy and Astrophysics, Space and Planetary Science, Stellar mass, Star formation, Plateau de Bure Interferometer, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy merger, Astrophysics - Astrophysics of Galaxies, Galaxy, Interstellar medium, Stars, Astrophysics of Galaxies (astro-ph.GA), Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Local starbursts have a higher efficiency of converting gas into stars, as compared to typical star-forming galaxies at a given stellar mass, possibly indicative of different modes of star formation. With the peak epoch of galaxy formation occurring at z > 1, it remains to be established whether such an efficient mode of star formation is occurring at high-redshift. To address this issue, we measure the molecular gas content of seven high-redshift (z ~ 1.6) starburst galaxies with the Atacama Large (sub-)Millimeter Array and IRAM/Plateau de Bure Interferometer. Our targets are selected from the sample of Herschel far-infrared detected galaxies having star formation rates (~300-800 Msolar/yr) elevated (>4x) above the star-forming `main sequence', and included in the FMOS-COSMOS near-infrared spectroscopic survey of star-forming galaxies at z ~ 1.6 with Subaru. We detect CO emission in all cases at high levels of significance, indicative of high gas fractions (~30-50%). Even more compelling, we firmly establish with a clean and systematic selection that starbursts, identified as main-sequence outliers, at high redshift generally have a lower ratio of CO to total infrared luminosity as compared to typical main-sequence star-forming galaxies, although with a smaller offset than expected based on past studies of local starbursts. We put forward a hypothesis that there exists a continuous increase in star formation efficiency with elevation from the main sequence with galaxy mergers as a possible physical driver. Along with a heightened star formation efficiency, our high-redshift sample is similar in other respects to local starbursts such as being metal rich and having a higher ionization state of the interstellar medium., Published in ApJ Letters; 6 pages, 4 figures

Published
2015

15. Erratum: The Herschel PEP/HerMES Luminosity Function - I. Probing the Evolution of PACS selected Galaxies to z = 4

Author

P. Chania, G. Mainetti, M. Bethermin, I. Ṕerez-Fournon, Matthew Joseph Griffin, L. Vigroux, H. Aussel, J. J. Bock, Andreas Papageorgiou, Vincenzo Mainieri, Anthony J. Smith, A. Conley, Benjamin Magnelli, Bruno Altieri, Asantha Cooray, Marcella Carollo, Raanan Nordon, V. Buat, Linda J. Tacconi, V. Arumugam, B. O'Halloran, E. Ibar, Alberto Franceschini, Alexandre Amblard, Francesca Pozzi, S. Bardelli, David J. Rosario, Bruno Maffei, Dimitra Rigopoulou, Mattia Vaccari, G. Wright, K. G. Isaak, Simon J. Lilly, Lucia Marchetti, Dieter Lutz, S. Berta, Ángel Bongiovanni, Albrecht Poglitsch, Michael Rowan-Robinson, I. Valtchanov, Alvaro Iribarrem, E. Zucca, Michael Pohlen, C. K. Xu, Marco Scodeggio, P. Popesso, Guilaine Lagache, G. Rodighiero, Thierry Contini, M. J. Page, Emanuele Daddi, Eckhard Sturm, Roberto Maiolino, S. C. Madden, N. M. Förster Schreiber, Jason Glenn, E. Le Floc'h, David L. Shupe, Lucia Pozzetti, Michael Zemcov, Alvio Renzini, M. Magliocchetti, Eli Dwek, N. Castro-Rodŕlguez, Douglas Scott, Louis Levenson, C. D. Dowell, R. Genzel, D. Elbaz, Nick Seymour, Rob Ivison, Jamie Stevens, Andrea Cimatti, Antonio Cava, Evanthia Hatziminaoglou, H. T. Nguyen, Nanyao Y. Lu, M. Symeonidis, Paola Andreani, Alessandro Boselli, O. Le Fevre, K. E. Tugwell, L. Riguccini, P. Panuzzo, A. Ṕerez Garćla, G. Zamorani, Chris Pearson, M. Sánchez-Portal, David L. Clements, Steve Eales, Denis Burgarella, L. Monaco, Ivan Delvecchio, J. Cepa, H. Doḿlnguez-Śanchez, M. T. Sargent, Benjamin L. Schulz, S. J. Oliver, Lian-Tao Wang, Carlotta Gruppioni, Isaac Roseboom, Markos Trichas, and O. Ilbert

Subjects
Luminous infrared galaxy, Physics, Radio galaxy, Física atmosférica, Astronomy, Astronomy and Astrophysics, Astrophysics, Disc galaxy, Galaxy, Space and Planetary Science, Galaxy group, Galaxy formation and evolution, Elliptical galaxy, Luminosity function (astronomy)
Abstract

This is an erratum to the paper ‘The Herschel PEP/HerMES Luminosity Function – I: Probing the Evolution of PACS selected Galaxies to z ≃ 4’, by Gruppioni et al., published in MNRAS, 432, 23 (2013).

Published
2013

16. ENVIRONMENTAL EFFECTS IN THE INTERACTION AND MERGING OF GALAXIES IN zCOSMOS

Author

P. Kampczyk, S. J. Lilly, L. de Ravel, O. Le Fèvre, M. Bolzonella, C. M. Carollo, C. Diener, C. Knobel, K. Kovač, C. Maier, A. Renzini, M. T. Sargent, D. Vergani, U. Abbas, S. Bardelli, A. Bongiorno, R. Bordoloi, K. Caputi, T. Contini, G. Coppa, O. Cucciati, S. de la Torre, P. Franzetti, B. Garilli, A. Iovino, J.-P. Kneib, A. M. Koekemoer, F. Lamareille, J.-F. Le Borgne, V. Le Brun, A. Leauthaud, V. Mainieri, M. Mignoli, R. Pello, Y. Peng, E. Perez Montero, E. Ricciardelli, M. Scodeggio, J. D. Silverman, M. Tanaka, L. Tasca, L. Tresse, G. Zamorani, E. Zucca, D. Bottini, A. Cappi, P. Cassata, A. Cimatti, M. Fumana, L. Guzzo, J. Kartaltepe, C. Marinoni, H. J. McCracken, P. Memeo, B. Meneux, P. Oesch, C. Porciani, L. Pozzetti, R. Scaramella, AUTRES, Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), 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), University of Chicago, Laboratoire Léon Brillouin (LLB - UMR 12), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astrofisico di Torino (OATo), College of Computing (GATECH), Georgia Institute of Technology [Atlanta], 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), Dipartimento di Fisica, Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), Ecole Polytechnique Fédérale de Lausanne (EPFL), Institut de recherche en astrophysique et planétologie (IRAP), California Institute of Technology (CALTECH), European Southern Observatory (ESO), Hunan Normal University (HNU), 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), National Optical Astronomy Observatory (NOAO), Centre de Physique Théorique - UMR 6207 (CPT), Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-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), Astronomy, 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), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay, 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), Université Fédérale Toulouse Midi-Pyrénées, Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI), 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), 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), Hunan Normal University, 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, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Kampczyk P., Lilly S. J., de Ravel L., Le Fèvre O., Bolzonella M., Carollo C. M., Diener C., Knobel C., Kovac K., Maier C., Renzini A., Sargent M. T., Vergani D., Abbas U., Bardelli S., Bongiorno A., Bordoloi R., Caputi K., Contini T., Coppa G., Cucciati O., de la Torre S., Franzetti P., Garilli B., Iovino A., Kneib J.-P., Koekemoer A. M., Lamareille F., Le Borgne J.-F., Le Brun V., Leauthaud A., Mainieri V., Mignoli M., Pello R., Peng Y., Perez Montero E., Ricciardelli E., Scodeggio M., Silverman J. D., Tanaka M., Tasca L., Tresse L., Zamorani G., Zucca E., Bottini D., Cappi A., Cassata P., Cimatti A., Fumana M., Guzzo L., Kartaltepe J., Marinoni C., McCracken H. J., Memeo P., Meneux B., Oesch P., Porciani C., Pozzetti L., and Scaramella R.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Population, FOS: Physical sciences, galaxies: starburst, MORPHOLOGICAL TRANSFORMATION, Astrophysics, Kinematics, Astrophysics::Cosmology and Extragalactic Astrophysics, STAR-FORMATION RATES, MERGER RATE EVOLUTION, 01 natural sciences, SIMILAR-TO 1, galaxies: evolution, galaxies: general, galaxies: interactions, Astronomy and Astrophysics, Space and Planetary Science, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Fraction (mathematics), education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, QB, Physics, education.field_of_study, FORMATION HISTORY, Star formation, CLOSE PAIRS, Cosmology: observations, Galaxies: high-redshift, Galaxies: statistics, Large-scale structure of Universe, CNOC2 REDSHIFT SURVEY, DISK GALAXIES, Environmental variation, Galaxy, Redshift, COSMOS FIELD, DIGITAL SKY SURVEY, Irregular galaxy, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

(Abridged) We analyze the environments and galactic properties (morphologies and star-formation histories) of a sample of 153 close kinematic pairs in the redshift range 0.2 < z < 1 identified in the zCOSMOS-bright 10k spectroscopic sample of galaxies. Correcting for projection effects, the fraction of close kinematic pairs is three times higher in the top density quartile than in the lowest one. This translates to a three times higher merger rate because the merger timescales are shown, from mock catalogues based on the Millennium simulation, to be largely independent of environment once the same corrections for projection is applied. We then examine the morphologies and stellar populations of galaxies in the pairs, comparing them to control samples that are carefully matched in environment so as to remove as much as possible the well-known effects of environment on the properties of the parent population of galaxies. Once the environment is properly taken into account in this way, we find that the early-late morphology mix is the same as for the parent population, but that the fraction of irregular galaxies is boosted by 50-75%, with a disproportionate increase in the number of irregular-irregular pairs (factor of 4-8 times), due to the disturbance of disk galaxies. Future dry-mergers, involving elliptical galaxies comprise less than 5% of all close kinematic pairs. In the closest pairs, there is a boost in the specific star-formation rates of star-forming galaxies of a factor of 2-4, and there is also evidence for an increased incidence of post star-burst galaxies. Although significant for the galaxies involved, the "excess" star-formation associated with pairs represents only about 5% of the integrated star-formation activity in the parent sample. Although most pair galaxies are in dense environments, the effects of interaction appear to be largest in the lower density environments., 38 pages, 17 figures, submitted to ApJ

Published
2013
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17. Spectral Energy Distributions of Type 1 Active Galactic Nuclei in the COSMOS Survey. I. The XMM-COSMOS Sample

Author

Y. Taniguchi, M. Zatloukal, John P. Huchra, Francesca Civano, C. M. Urry, Luis C. Ho, Chris Impey, Dave Frayer, G. Hasinger, John D. Silverman, Mara Salvato, S. J. Lilly, Mauricio Cisternas, Peter Capak, Giorgio Lanzuisi, Knud Jahnke, Eva Schinnerer, Andrea Comastri, Nick Scoville, D. B. Sanders, Andrea Merloni, M. T. Sargent, David Schiminovich, H. J. McCracken, Jonathan R. Trump, Patrick J. McCarthy, Roberto Gilli, Elisabeta Lusso, Angela Bongiorno, Yuan Liu, E. Le Floc'h, Anton M. Koekemoer, Vincenzo Mainieri, Nico Cappelluti, H. J. Roeser, G. Zamorani, Cristian Vignali, H. Hao, H. Aussel, M. Zamojski, Martin Elvis, and Marcella Brusa

Subjects
Physics, Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, galaxies: evolution, quasars: general, surveys, Spectral density, Astrophysics::Solar and Stellar Astrophysics, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Sample (graphics), Cosmos, Astrophysics::Galaxy Astrophysics
Abstract

The "Cosmic Evolution Survey" (COSMOS) enables the study of the spectral energy distributions (SEDs) of active galactic nuclei (AGNs) because of the deep coverage and rich sampling of frequencies from X-ray to radio. Here we present an SED catalog of 413 X-ray (XMM-Newton)-selected type 1 (emission line FWHM > 2000 km s^(–1)) AGNs with Magellan, SDSS, or VLT spectrum. The SEDs are corrected for Galactic extinction, broad emission line contributions, constrained variability, and host galaxy contribution. We present the mean SED and the dispersion SEDs after the above corrections in the rest-frame 1.4 GHz to 40 keV, and show examples of the variety of SEDs encountered. In the near-infrared to optical (rest frame ~8 μm-4000 Å), the photometry is complete for the whole sample and the mean SED is derived from detections only. Reddening and host galaxy contamination could account for a large fraction of the observed SED variety. The SEDs are all available online.

Published
2012

18. The Molecular Gas Content of Z = 3 Lyman Break Galaxies: Evidence of a Non-Evolving Gas Fraction in Main-Sequence Galaxies At Z > 2

Author

Chiara Feruglio, Georgios E. Magdis, Helmut Dannerbauer, Mark Dickinson, Raphael Gobat, Emanuele Daddi, Qinghua Tan, Vassilis Charmandaris, M. T. Sargent, D. Rigopoulou, N. Reddy, D. Elbaz, Herve Aussel, Department of Physics [Oxford], University of Oxford [Oxford], 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), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Space Science and Technology Department [Didcot] (RAL Space), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC)-Science and Technology Facilities Council (STFC), IESL, National Optical Astronomy Observatory (NOAO), Department of Physics and Astronomy [Riverside], University of California [Riverside] (UCR), University of California-University of California, UPGAL, ANR-08-JCJC-0008,UPGAL(2008), European Project: 240039,EC:FP7:ERC,ERC-2009-StG,UPGAL(2009), Department of Physics, NOAO, University of Oxford, 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), University of California [Riverside] (UC Riverside), and University of California (UC)-University of California (UC)

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Infrared, Star formation, FOS: Physical sciences, Plateau de Bure Interferometer, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Mass ratio, Plateau (mathematics), 01 natural sciences, Redshift, Flattening, Galaxy, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 13. Climate action, Space and Planetary Science, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present observations of the CO[3-2] emission towards two massive and infrared luminous Lyman Break Galaxies at z = 3.21 and z = 2.92, using the IRAM Plateau de Bure Interferometer, placing first constraints on the molecular gas masses (Mgas) of non-lensed LBGs. Their overall properties are consistent with those of typical (Main-Sequence) galaxies at their redshifts, with specific star formation rates ~1.6 and ~2.2 Gyr^(-1), despite their large infrared luminosities L_IR ~2-3 x 10^12 Lsun derived from Herschel. With one plausible CO detection (spurious detection probability of 10^(-3)) and one upper limit, we investigate the evolution of the molecular gas-to-stellar mass ratio (Mgas/M*) with redshift. Our data suggest that the steep evolution of Mgas/M* of normal galaxies up to z~2 is followed by a flattening at higher redshifts, providing supporting evidence for the existence of a plateau in the evolution of the specific star formation rate at z > 2.5., Accepted for publication in ApJL

Published
2012
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19. GOODS-Herschel~: Gas-to-dust mass ratios and CO-to-H_2 conversion factors in normal and starbursting galaxies at high-z

Author

Dominik A. Riechers, Georgios E. Magdis, D. Rigopoulou, Ho Seong Hwang, E. Elbaz, Maurilio Pannella, M. T. Sargent, Helmut Dannerbauer, Fabian Walter, James Mullaney, Chris Carilli, Roger Leiton, Emanuele Daddi, J. A. Hodge, Mark Dickinson, Douglas Scott, H. Aussel, Vassilis Charmandaris, 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), National Optical Astronomy Observatory (NOAO), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Institute of Theoretical and Computational Physics [Heraklion], University of Crete [Heraklion] (UOC), IESL, Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), Department of Physics [Oxford], University of Oxford [Oxford], National Radio Astronomy Observatory [Socorro] (NRAO), National Radio Astronomy Observatory (NRAO), Department of Physics and Astrononomy, University of British Columbia (UBC), ANR-08-JCJC-0008,UPGAL(2008), European Project: 240039,EC:FP7:ERC,ERC-2009-StG,UPGAL(2009), 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), University of Oxford, 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), Department of Physics, NOAO, Department of Physics, ICTP, UPGAL, and European Project

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Field (physics), 010308 nuclear & particles physics, Star formation, Infrared, Metallicity, Star (game theory), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Mass ratio, 01 natural sciences, Galaxy, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Body function, Space and Planetary Science, 0103 physical sciences, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We explore the gas-to-dust mass ratio (G/D) and the CO luminosity-to-Mgas conversion factor (a_co) of two well studied galaxies in the GOODS-N field, that are expected to have different star forming modes, the starburst GN20 at z=4.05 and the normal star-forming galaxy BzK-21000 at z=1.52. Detailed sampling is available for their Rayleigh-Jeans emission via ground based mm interferometry (1.1-6.6mm) along with Herschel, PACS and SPIRE data that probe the peak of their infrared emission. Using the physically motivated Draine & Li (2007) models, as well as a modified black body function, we measure the dust mass (Md) of the sources and find 2.0^{+0.7}_{-0.6} x 10^{9} Msun for GN20 and 8.6^{+0.6}_{-0.9} x 10^{8} Msun for BzK-21000. The addition of mm data reduces the uncertainties of the derived Md by a factor of ~2, allowing the use of the local G\D vs metallicity relation to place constraints on the a_co values of the two sources. For GN20 we derive a conversion factor of a_co < 1.0 Msun pc^{-2}(K km s^{-1})^{-1}, consistent with that of local ULIRGs, while for BzK-21000 we find a considerably higher value, a_co ~4.0 Msun pc^{-2}(K km s^{-1})^{-1}, in agreement with an independent kinematic derivation reported previously. The implied star formation efficiency is ~25 Lsun/Msun for BzK-21000, a factor of ~5-10 lower than that of GN20. The findings for these two sources support the existence of different disk-like and starburst star-formation modes in distant galaxies, although a larger sample is required to draw statistically robust results, Accepted for publication in ApJ

Published
2011
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20. The buildup of the Hubble sequence in the cosmos field

Author

Anton M. Koekemoer, Claudia Scarlata, C. M. Carollo, Jason Rhodes, Mara Salvato, Richard Massey, S. J. Lilly, Kevin Bundy, T. J. Bschorr, Y. Taniguchi, H. Aussel, Nick Scoville, Alvio Renzini, Kartik Sheth, A. Leauthaud, Oliver Hahn, M. Bolzonella, H. J. McCracken, Peter Capak, David R. Thompson, Lucia Pozzetti, E. Le Floc'h, D. B. Sanders, Robert Feldmann, O. Ilbert, Katarina Kovac, Monique Aller, Pascal Oesch, M. T. Sargent, J. P. Kneib, Laboratoire d'Astrophysique de Marseille (LAM), 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), Field (physics), Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Hubble sequence, symbols.namesake, Bulge, 0103 physical sciences, Mass scale, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QB, Physics, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Secular evolution, Astronomy and Astrophysics, Galaxy, Space and Planetary Science, symbols, Irregular galaxy, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We use ~8,600 >5e10 Msol COSMOS galaxies to study how the morphological mix of massive ellipticals, bulge-dominated disks, intermediate-bulge disks, bulge-less disks and irregular galaxies evolves from z=0.2 to z=1. The morphological evolution depends strongly on mass. At M>3e11 Msol, no evolution is detected in the morphological mix: ellipticals dominate since z=1, and the Hubble sequence has quantitatively settled down by this epoch. At the 1e11 Msol mass scale, little evolution is detected, which can be entirely explained with major mergers. Most of the morphological evolution from z=1 to z=0.2 takes place at masses 5e10 - 1e11 Msol, where: (i) The fraction of spirals substantially drops and the contribution of early-types increases. This increase is mostly produced by the growth of bulge-dominated disks, which vary their contribution from ~10% at z=1 to >30% at z=0.2 (cf. the elliptical fraction grows from ~15% to ~20%). Thus, at these masses, transformations from late- to early-types result in disk-less elliptical morphologies with a statistical frequency of only 30% - 40%. Otherwise, the processes which are responsible for the transformations either retain or produce a non-negligible disk component. (ii) The bulge-less disk galaxies, which contribute ~15% to the intermediate-mass galaxy population at z=1, virtually disappear by z=0.2. The merger rate since z=1 is too low to account for the disappearance of these massive bulge-less disks, which most likely grow a bulge via secular evolution., 5 pages, 3 figures, submitted to ApJL

Published
2010
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21. The X-ray to optical-UV luminosity ratio of X-ray selected Type 1 AGN in XMM-COSMOS

Author

O. Le Fèvre, Andrea Comastri, Anton M. Koekemoer, Jean-Paul Kneib, Eva Schinnerer, M. Scodeggio, Fabrizio Fiore, Francesca Civano, K. Iwasawa, M. Mignoli, John D. Silverman, Mara Salvato, Roberto Gilli, F. Lamareille, D. Vergani, G. Zamorani, Jonathan R. Trump, Nico Cappelluti, Knud Jahnke, Simon J. Lilly, V. Mainieri, Bianca Garilli, Andrea Merloni, M. T. Sargent, Elisabeta Lusso, Angela Bongiorno, Cristian Vignali, Martin Elvis, Marcella Brusa, Micol Bolzonella, E. Le Floc'h, A. Iovino, 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), Lusso E., Comastri A., Vignali C., Zamorani G., Brusa M., Gilli R., Iwasawa K., Salvato M., Civano F., Elvis M., Merloni A., Bongiorno A., Trump J.R., Koekemoer A.M., Schinnerer E., Le Floch E., Cappelluti N., Jahnke K., Sargent M., Silverman J., Mainieri V., Fiore F., Bolzonella M., Le Fevre O., Garilli B., Iovino A., Kneib J.P., Lamareille F., Lilly S., Mignoli M., Scodeggio M., and Vergani D.

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Galaxies: active, Galaxy: evolution, Methods: statistical, Quasars: general, Astronomy and Astrophysics, Space and Planetary Science, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Spectral density, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Type (model theory), 01 natural sciences, Redshift, Luminosity, Black hole, galaxies: active – Galaxy: evolution – quasars: general – methods: statistical, 0103 physical sciences, Spectral slope, Bolometric correction, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Photometric redshift, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a study of the X-ray to optical properties of a sample of 545 X-ray selected Type 1 AGN, from the XMM-COSMOS survey, over a wide range of redshifts ($0.04, Comment: 14 pages, 15 figures, to appear in A&A

Published
2009
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22. The Redshift Evolution of Early-Type Galaxies in COSMOS: Do Massive Early-Type Galaxies Form by Dry Mergers?

Author

Shunji S. Sasaki, J. P. Kneib, C. M. Carollo, P. Kampczyk, Alvio Renzini, Richard Massey, Anton M. Koekemoer, Claudia Scarlata, Robert Feldmann, T. Murayama, Jason Rhodes, Nick Scoville, Emanuele Daddi, Capak, H. J. McCracken, A. Leauthaud, D. B. Sanders, Y. Shioya, C. Halliday, Masaru Ajiki, Yoshiaki Taniguchi, S. J. Lilly, M. I. Takahashi, L. A. M. Tasca, M. T. Sargent, Andrea Cimatti, Bahram Mobasher, David R. Thompson, H. Aussel, Scarlata C., Carollo C. M., Lilly S. J., Feldmann R., Kampczyk P., Renzini A., Cimatti A., Halliday C., Daddi E., Sargent M. T., Koekemoer A., Scoville N., Kneib J.-P., Leauthaud A., Massey R., Rhodes J., Tasca L., Capak P., McCracken H. J., Mobasher B., Taniguchi Y., Thompson D., Ajiki M., Aussel H., Murayama T., Sanders D. B., Sasaki S., Shioya Y., Takahashi M., Services communs OMP (UMS 831), 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), 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), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire de Physique Statistique de l'ENS (LPS), Université Paris Diderot - Paris 7 (UPD7)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-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), 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), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, COSMIC cancer database, 010308 nuclear & particles physics, Star formation, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Cosmic variance, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Redshift, Galaxy, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Fundamental plane (elliptical galaxies), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy)
Abstract

ABRIDGED: We study the evolution since z~1 of the rest-frame B luminosity function of the early-type galaxies (ETGs) in ~0.7 deg^2 in the COSMOS field. In order to identify ALL progenitors of local ETGs we construct the sample of high-z galaxies using two complementary criteria: (i) A morphological selection based on the Zurich Estimator of Structural Types, and (ii) A photometric selection based on the galaxy properties in the (U-V)-M_V color-magnitude diagram. We furthermore constrain both samples so as to ensure that the selected progenitors of ETGs are compatible with evolving into systems which obey the mu_B-r_{hl} Kormendy relation. Assuming the luminosity evolution derived from studies of the fundamental plane for high-z ETGs, our analysis shows no evidence for a decrease in the number density of the most massive ETGs out to z~ 0.7: Both the morphologically- and the photometrically-selected sub-samples show no evolution in the number density of bright (~L>2.5L*) ETGs. Allowing for different star formation histories, and cosmic variance, we estimate a maximum decrease in the number density of massive galaxies at that redshift of ~30%. We observe, however, in both the photometrical and morphological samples, a deficit of up to ~2-3 of fainter ETGs over the same cosmic period. Our results argue against a significant contribution of recent dissipationless ``dry'' mergers to the formation of the most massive ETGs. We suggest that the mass growth in low luminosity ETGs can be explained with a conversion from z~0.7 to z=0 of blue, irregular and disk galaxies into low- and intermediate-mass ``red'' ETGs, possibly also through gas rich mergers., Replaced with accepted version (ApJ COSMOS special issue)

Published
2007

23. The evolution of the number density of large disk galaxies in COSMOS

Author

Claudia Scarlata, A. Leauthaud, H. J. McCracken, Peter Capak, Y. Taniguchi, Nick Scoville, Anton M. Koekemoer, Kartik Sheth, Alvio Renzini, Richard Massey, Jason Rhodes, P. Kampczyk, C. M. Carollo, David Thompson, S. J. Lilly, Robert Feldmann, L. A. M. Tasca, Jean-Paul Kneib, M. T. Sargent, Cristiano Porciani, 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), Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Stellar mass, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, Cosmology: Observations, Bulge, Galaxies: Evolution, education, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, Number density, Astrophysics (astro-ph), Galaxies: Formation, Astrophysics::Instrumentation and Methods for Astrophysics, Secular evolution, Astronomy and Astrophysics, Galaxy, Cosmology: Large-Scale Structure of Universe, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Cosmos (category theory), Astrophysics::Earth and Planetary Astrophysics
Abstract

We study a sample of approximately 16,500 galaxies with I_AB 7 kpc) decreases by a factor of about two out to z~1. (iii) There is a constancy in the number density of large bulgeless disks out to z~1; the deficit of large disks at early epochs seems to arise from a smaller number of bulged disks. Our results indicate that the bulk of the large disk galaxy population has completed its growth by z~1, and support the hypothesis that secular evolution processes produce - or at least add stellar mass to - the bulge components of disk galaxies., Accepted for publication in the ApJ COSMOS special issue. A version with figures in higher resolution is available at http://www.exp-astro.phys.ethz.ch/sargent/manuscripts/ApJS_sizes.pdf

Published
2006
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24. 9-cis retinoic acid antagonizes the stimulatory effect of 1,25 dihydroxyvitamin D3 on chondrogenesis of chick limb bud mesenchymal cells: interactions of their receptors

Author

P A, Tsonis, M T, Sargent, K, Del Rio-Tsonis, and J C, Jung

Subjects
Chloramphenicol O-Acetyltransferase, Histocytochemistry, Receptors, Retinoic Acid, Gene Expression Regulation, Developmental, Cell Differentiation, Extremities, Tretinoin, Chick Embryo, Transfection, Models, Biological, Mesoderm, Cartilage, Calcitriol, Animals, Receptors, Calcitriol, Dimerization, Alitretinoin, Cell Division, Cells, Cultured
Abstract

Retinoids or vitamin D have been found to profoundly affect pattern formation and chondrogenesis in the developing limb. These substances mediate their actions through their nuclear receptors. In the present investigation, we present data showing that 9-cis RA, the ligand for RXR can stimulate chondrogenesis of chick limb bud mesenchymal cells, however, in combination, it antagonizes the stimulatory effect of vitamin D in the same system. The receptors for 9-cis RA (RXR) and vitamin D (VDR) were also shown to be present in the mesenchymal cells and to form heterodimers. These results implicate these receptors in cartilage differentiation during limb development.

Published
1996

25. THE HIDDEN 'AGN MAIN SEQUENCE': EVIDENCE FOR A UNIVERSAL BLACK HOLE ACCRETION TO STAR FORMATION RATE RATIO SINCE z ∼ 2 PRODUCING AN M BH - M * RELATION

Author

E. Daddi, M. Bethermin, Ryan C. Hickox, D. Elbaz, Maurilio Pannella, M. T. Sargent, D. M. Alexander, Stéphanie Juneau, and James Mullaney

Subjects
Physics, Supermassive black hole, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, 010308 nuclear & particles physics, Star formation, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Redshift, Galaxy, Accretion (astrophysics), Black hole, Space and Planetary Science, Bulge, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Using X-ray stacking analyses we estimate the average amounts of supermassive black hole (SMBH) growth taking place in star-forming galaxies (SFGs) at z~1 and z~2 as a function of galaxy stellar mass (M*). We find the average SMBH growth rate follows remarkably similar trends with M* and redshift as the average star-formation rates (SFRs) of their host galaxies (i.e., (i.e., dM_BH/dt ~ M*^(0.86+/-0.39) for the z~1 sample and dM_BH/dt ~ M*^(1.05+/-0.36) for the z~2 sample). It follows that the ratio of SMBH growth rate to SFR is (a) flat with respect to M* (b) not evolving with redshift and (c) close to the ratio required to maintain/establish a SMBH to M* ratio of ~10^{-3} as also inferred from today's M_BH-M_bulge relationship. We interpret this as evidence that SMBHs have, on average, grown in-step with their host galaxies since at least z~2, irrespective of host galaxy mass and AGN triggering mechanism. As such, we suggest that the same secular processes that drive the bulk of star formation are also responsible for the majority of SMBH growth. From this, we speculate that it is the availability of gas reservoirs that regulate both cosmological SMBH growth and star formation., Comment: 6 Pages, 3 Figures, ApJL accepted after minor changes

Published
2012
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26. Deciphering the Activity and Quiescence of High-redshift Cluster Environments: ALMA Observations of Cl J1449+0856 at z = 2.

Author

V. Strazzullo, R. T. Coogan, E. Daddi, M. T. Sargent, R. Gobat, F. Valentino, M. Bethermin, M. Pannella, M. Dickinson, A. Renzini, N. Arimoto, A. Cimatti, H. Dannerbauer, A. Finoguenov, D. Liu, and M. Onodera

Subjects
GALACTIC redshift, GALAXY clusters, ASTRONOMICAL observations, SUPERGIANT stars
Abstract

We present Atacama Large Millimeter/submillimeter Array observations of the 870 μm continuum and CO(4–3) line emission in the core of the galaxy cluster Cl J1449+0856 at z = 2, a near-IR-selected, X-ray-detected system in the mass range of typical progenitors of today’s massive clusters. The 870 μm map reveals six F870μm > 0.5 mJy sources spread over an area of 0.07 arcmin2, giving an overdensity of a factor of ∼10 (6) with respect to blank-field counts down to F870μm > 1 mJy (>0.5 mJy). On the other hand, deep CO(4–3) follow-up confirms membership of three of these sources but suggests that the remaining three, including the brightest 870 μm sources in the field (F870μm ≳ 2 mJy), are likely interlopers. The measurement of 870 μm continuum and CO(4–3) line fluxes at the positions of previously known cluster members provides a deep probe of dusty star formation occurring in the core of this high-redshift structure, adding up to a total star formation rate of ∼700 ± 100 M⊙ yr−1 and yielding an integrated star formation rate density of ∼104M⊙ yr−1 Mpc−3, five orders of magnitude larger than in the field at the same epoch, due to the concentration of star-forming galaxies in the small volume of the dense cluster core. The combination of these observations with previously available Hubble Space Telescope imaging highlights the presence in this same volume of a population of galaxies with already suppressed star formation. This diverse composition of galaxy populations in Cl J1449+0856 is especially highlighted at the very cluster center, where a complex assembly of quiescent and star-forming sources is likely forming the future brightest cluster galaxy. [ABSTRACT FROM AUTHOR]

Published
2018
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29. GAS FRACTION AND DEPLETION TIME OF MASSIVE STAR-FORMING GALAXIES AT z ∼ 3.2: NO CHANGE IN GLOBAL STAR FORMATION PROCESS OUT TO z > 3.

Author

E. Schinnerer, B. Groves, M. T. Sargent, A. Karim, P. A. Oesch, B. Magnelli, O. LeFevre, L. Tasca, F. Civano, P. Cassata, and V. Smolčić

Subjects
GALAXIES, STAR formation, STELLAR luminosity function, LUMINOSITY, STELLAR mass
Abstract

The observed evolution of the gas fraction and its associated depletion time in main-sequence (MS) galaxies provides insights on how star formation proceeds over cosmic time. We report ALMA detections of the rest-frame ∼300 μm continuum observed at 240 GHz for 45 massive (), normal star-forming (), i.e., MS, galaxies at in the COSMOS field. From an empirical calibration between cold neutral, i.e., molecular and atomic, gas mass and monochromatic (rest-frame) infrared luminosity, the gas mass for this sample is derived. Combined with stellar mass and star formation rate (SFR) estimates (from MagPhys fits) we obtain a median gas fraction of and a median gas depletion time correction for the location on the MS will only slightly change the values. The reported uncertainties are the error on the median. Our results are fully consistent with the expected flattening of the redshift evolution from the 2-SFM (2 star formation mode) framework which empirically prescribes the evolution assuming a universal, log-linear relation between SFR and gas mass coupled to the redshift evolution of the specific star formation rate (sSFR) of MS galaxies. While shows only a mild dependence on location within the MS, a clear trend of increasing across the MS is observed (as known from previous studies). Further, we comment on trends within the MS and (in)consistencies with other studies. [ABSTRACT FROM AUTHOR]

Published
2016
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