Search

Your search keyword '"Kocevski, D.D."' showing total 4 results
Start Over Author "Kocevski, D.D."
4 results on '"Kocevski, D.D."'

1. Mass assembly and morphological transformations since z? 3 from CANDELS

Author

Huertas-Company, M., Bernardi, M., Ashby, M.L.N., Barro, G., Conselice, Christopher J., Daddi, E., Dekel, A., Dimauro, P., Faber, S.M., Grogin, N.A., Kartaltepe, J.S., Kocevski, D.D., Koekemoer, A.M., Koo, D.C., Mei, S., and Shankar, F.

Subjects
galaxies: abundances, galaxies: evolution, galaxies: high-redshift, galaxies: structure, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We quantify the evolution of the stellar mass functions (SMFs) of star-forming and quiescent galaxies as a function of morphology from z ? 3 to the present. Our sample consists of ?50 000 galaxies in the CANDELS fields (?880 arcmin2), which we divide into four main morphological types, i.e. pure bulge-dominated systems, pure spiral disc-dominated, intermediate two-component bulge+disc systems and irregular disturbed galaxies. At z ? 2, 80 per cent of the stellarmass density of star-forming galaxies is in irregular systems. However, by z ? 0.5, irregular objects only dominate at stellar masses below 109M_. A majority of the star-forming irregulars present at z ? 2 undergo a gradual transformation from disturbed to normal spiral disc morphologies by z ? 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, because the fraction of bulge-dominated star-forming galaxies with M?/M_ > 1010.7 reaches 40 per cent at z < 1. Quenching implies the presence of a bulge: the abundance of massive red discs 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 aboveM ? is dominated by compact spheroids. Quenching at this early epoch destroys the disc and produces a compact remnant unless the star-forming progenitors at even higher redshifts are significantly more dense. At 1 < z

Published
2016

3. Mass assembly and morphological transformations since z∼ 3 from CANDELS

Author

Huertas-Company, M., Bernardi, M., Pérez-González, P.G., Ashby, M.L.N., Barro, G., Conselice, Christopher J., Daddi, E., Dekel, A., Dimauro, P., Faber, S.M., Grogin, N.A., Kartaltepe, J.S., Kocevski, D.D., Koekemoer, A.M., Koo, D.C., Mei, S., Shankar, F., Huertas-Company, M., Bernardi, M., Pérez-González, P.G., Ashby, M.L.N., Barro, G., Conselice, Christopher J., Daddi, E., Dekel, A., Dimauro, P., Faber, S.M., Grogin, N.A., Kartaltepe, J.S., Kocevski, D.D., Koekemoer, A.M., Koo, D.C., Mei, S., and Shankar, F.

Abstract

We quantify the evolution of the stellar mass functions (SMFs) of star-forming and quiescent galaxies as a function of morphology from z ∼ 3 to the present. Our sample consists of ∼50 000 galaxies in the CANDELS fields (∼880 arcmin2), which we divide into four main morphological types, i.e. pure bulge-dominated systems, pure spiral disc-dominated, intermediate two-component bulge+disc systems and irregular disturbed galaxies. At z ∼ 2, 80 per cent of the stellarmass density of star-forming galaxies is in irregular systems. However, by z ∼ 0.5, irregular objects only dominate at stellar masses below 109M_. A majority of the star-forming irregulars present at z ∼ 2 undergo a gradual transformation from disturbed to normal spiral disc morphologies by z ∼ 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, because the fraction of bulge-dominated star-forming galaxies with M∗/M_ > 1010.7 reaches 40 per cent at z < 1. Quenching implies the presence of a bulge: the abundance of massive red discs 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 aboveM ∗ is dominated by compact spheroids. Quenching at this early epoch destroys the disc and produces a compact remnant unless the star-forming progenitors at even higher redshifts are significantly more dense. At 1 < z<2, the majority of newly quenched galaxies are discs with a significant central bulge. This suggests that mass quenching at this epoch starts from the inner parts and preserves the disc. At z < 1, the high-mass end of the passive SMF is globally in place and the evolution mostly happens at stellar masses below 1010M_. These low-mass galaxies are compact, bulge-dominated systems, which were environmentally quenched: destruction of the disc through ram-pressure stripping is the likely process.

Full Text
View/download PDF

4. VIMOS Ultra-Deep Survey (VUDS): Witnessing the Assembly of a Massive Cluster at z~3.3

Author

R. Thomas, Andrea Grazian, Jean-Gabriel Cuby, Daniel Schaerer, S. de la Torre, E. Zucca, Laurence Tresse, Letizia P. Cassarà, Dale D. Kocevski, Marco Castellano, Olivier Ilbert, D. Maccagni, N. Z. Scoville, Ricardo Amorín, Andrea Cimatti, T. Sadibekova, Stéphane Paltani, V. Sommariva, Sotiria Fotopoulou, Lidia Tasca, Stephane Charlot, Thierry Contini, C. López-Sanjuan, A. Durkalec, Margherita Talia, Yannick Mellier, Bianca Garilli, G. Zamorani, S. Bardelli, Olga Cucciati, L. M. Lubin, Daniela Vergani, Adriano Fontana, M. Scodeggio, B. Ribeiro, M. Giavalisco, P. W. Wang, Laura Pentericci, Peter Capak, Nimish P. Hathi, Brian C. Lemaux, V. Le Brun, Paolo Cassata, Yoshiaki Taniguchi, Eros Vanzella, C. Moreau, O. Le Fèvre, Roy R. Gal, Mara Salvato, 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), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-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), 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), European Project: 268107,EC:FP7:ERC,ERC-2010-AdG_20100224,EARLY(2011), 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 National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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), 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), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Lemaux, B.C., Cucciati, O., Tasca, L.A.M., Le Fèvre, O., Zamorani, G., Cassata, P., Garilli, B., Le Brun, V., Maccagni, D., Pentericci, L., Thomas, R., Vanzella, E., Zucca, E., Amorín, R., Bardelli, S., Capak, P., Cassarà, L.P., Castellano, M., Cimatti, A., Cuby, J.G., De La Torre, S., Durkalec, A., Fontana, A., Giavalisco, M., Grazian, A., Hathi, N.P., Ilbert, O., Moreau, C., Paltani, S., Ribeiro, B., Salvato, M., Schaerer, D., Scodeggio, M., Sommariva, V., Talia, M., Taniguchi, Y., Tresse, L., Vergani, D., Wang, P.W., Charlot, S., Contini, T., Fotopoulou, S., Gal, R.R., Kocevski, D.D., López-Sanjuan, C., Lubin, L.M., Mellier, Y., Sadibekova, T., and Scoville, N.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, galaxies: active, FOS: Physical sciences, Astrophysics, Spectral line, techniques: photometric, galaxies: high-redshift, Coma Cluster, Galaxies: active, Galaxies: clusters: general, Galaxies: evolution, Galaxies: high-redshift, Techniques: photometric, Techniques: spectroscopic, Astronomy and Astrophysics, Space and Planetary Science, Photometric redshift, media_common, Physics, Star formation, Astronomy and Astrophysic, Redshift, Galaxy, Universe, galaxies: clusters: general, Halo, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], techniques: spectroscopic, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Using new spectroscopic observations obtained as part of the VIMOS Ultra-Deep Survey (VUDS), we perform a systematic search for overdense environments in the early universe ($z>2$) and report here on the discovery of Cl J0227-0421, a massive protocluster at $z=3.29$. This protocluster is characterized by both the large overdensity of spectroscopically confirmed members, $\delta_{gal}=10.5\pm2.8$, and a significant overdensity in photometric redshift members. The halo mass of this protocluster is estimated, by a variety of methods, to be roughly $3\times10^{14}$ $\mathcal{M}_{\odot}$ at $z\sim3.3$, which, evolved to $z=0$ results in a halo mass rivaling or exceeding that of the Coma cluster. The properties of 19 spectroscopically confirmed member galaxies are compared with a large sample of VUDS/VVDS galaxies in lower density field environments at similar redshifts. We find tentative evidence for an excess of redder, brighter, and more massive galaxies within the confines of the protocluster relative to the field population, which suggests that we may be observing the beginning of environmentally-induced quenching. The properties of these galaxies are investigated, including a discussion of the brightest protocluster galaxy which appears to be undergoing vigorous coeval nuclear and starburst activity. The remaining member galaxies appear to have characteristics which are largely similar to the field population. Though we find weaker evidence of the suppression of the median star formation rates amongst and differences in stacked spectra of member galaxies with respect to the field, we defer any conclusions of these trends to future work with the ensemble of protostructures that are found in the full VUDS sample., Comment: 23 pages, 15 figures, 3 tables, accepted for publication in A&A after minor changes, v3/v4 contains an additional online table and minor topical changes

Published
2014
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results