High‐redshift elliptical galaxies: are they (all) really compact?
Identifieur interne : 000017 ( France/Analysis ); précédent : 000016; suivant : 000018High‐redshift elliptical galaxies: are they (all) really compact?
Auteurs : C. Mancini [Italie] ; E. Daddi [France] ; A. Renzini [Italie] ; F. Salmi [France] ; H. J. Mccracken [France] ; A. Cimatti [Italie] ; M. Onodera [France] ; M. Salvato [États-Unis] ; A. M. Koekemoer [États-Unis] ; H. Aussel [France] ; E. Le Floc'H [France, États-Unis] ; C. Willott [Canada] ; P. Capak [États-Unis]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2010-01-11.
English descriptors
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Abstract
We investigate the properties of 12 ultramassive passively evolving early‐type galaxies (ETGs) at zphot > 1.4 in the COSMOS 2 deg2 field. These 12 ETGs were selected as pBzKs, have accurate 1.4 ≲zphot≲ 1.7, high Sérsic index profiles typical of ellipticals, no detection at 24 μm, resulting in a complete ETG sample at M* > 2.5 × 1011 M⊙ (Chabrier initial mass function). Contrary to the previous claims, the half‐light radii estimated in very high signal‐to‐noise ratio imaging data from Hubble Space Telescope+Advanced Camera for Surveys (ACS) are found to be large for most of the sample, consistent with local ellipticals. If the high‐redshift ETGs with M* < 2.5 × 1011 M⊙ are really small in size and compact as reported in the previous studies, our result may suggest a ‘downsizing’ scenario, whereby the most massive ETGs reach their final structure earlier and faster than the lower mass ones. However, simulating galaxies with morphological properties fixed to those of local ETGs with the same stellar mass show that the few compact galaxies that we still recover in our sample can be understood in terms of fluctuations due to noise preventing the recovery of the extended low surface brightness haloes in the light profile. Such haloes, typical of Sérsic profiles, extending even up to 40 kpc, are indeed seen in our sample.
Url:
DOI: 10.1111/j.1365-2966.2009.15728.x
Affiliations:
- Canada, France, Italie, États-Unis
- Émilie-Romagne, Île-de-France
- Bologne, Gif‐Sur Yvette, Paris
- Université Pierre-et-Marie-Curie, Université de Bologne
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ISTEX:918CBB6CA945F7DB9EF655A1A6A5E925C978D4DDLe document en format XML
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Cimatti</name><affiliation wicri:level="4"><country xml:lang="fr">Italie</country><wicri:regionArea>Dipartimento di Astronomia, Università di Bologna, via Ranzani 1, I‐40127 Bologna</wicri:regionArea><orgName type="university">Université de Bologne</orgName><placeName><settlement type="city">Bologne</settlement><region nuts="2" type="region">Émilie-Romagne</region></placeName></affiliation></author><author><name sortKey="Onodera, M" sort="Onodera, M" uniqKey="Onodera M" first="M." last="Onodera">M. Onodera</name><affiliation wicri:level="3"><country xml:lang="fr">France</country><wicri:regionArea>CEA‐Saclay, DSM/DAPNIA/Service d'Astrophysique, 91191 Gif‐Sur Yvette Cedex</wicri:regionArea><placeName><region type="region" nuts="2">Île-de-France</region><settlement type="city">Gif‐Sur Yvette</settlement></placeName></affiliation></author><author><name sortKey="Salvato, M" sort="Salvato, M" uniqKey="Salvato M" first="M." last="Salvato">M. 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Willott</name><affiliation wicri:level="1"><country xml:lang="fr">Canada</country><wicri:regionArea>Herzberg Institute of Astrophysics, National Research Council, 5071 West Saanich Rd, Victoria, BC V9E 2E7</wicri:regionArea><wicri:noRegion>BC V9E 2E7</wicri:noRegion></affiliation></author><author><name sortKey="Capak, P" sort="Capak, P" uniqKey="Capak P" first="P." last="Capak">P. Capak</name><affiliation wicri:level="1"><country xml:lang="fr">États-Unis</country><wicri:regionArea>Spitzer Science Center, 314‐6 Caltech, Pasadena, CA 91125</wicri:regionArea><wicri:noRegion>CA 91125</wicri:noRegion></affiliation><affiliation wicri:level="1"><country xml:lang="fr">États-Unis</country><wicri:regionArea>California Institute of Technology, MS 104‐25 Pasadena, CA 91125</wicri:regionArea><wicri:noRegion>CA 91125</wicri:noRegion></affiliation></author></analytic><monogr></monogr><series><title level="j">Monthly Notices of the Royal Astronomical Society</title><idno type="ISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><imprint><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2010-01-11">2010-01-11</date><biblScope unit="volume">401</biblScope><biblScope unit="issue">2</biblScope><biblScope unit="page" from="933">933</biblScope><biblScope unit="page" to="940">940</biblScope></imprint><idno type="ISSN">0035-8711</idno></series><idno type="istex">918CBB6CA945F7DB9EF655A1A6A5E925C978D4DD</idno><idno type="DOI">10.1111/j.1365-2966.2009.15728.x</idno><idno type="ArticleID">MNR15728</idno></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>galaxies: elliptical and lenticular, cD</term><term>galaxies: evolution</term><term>galaxies: formation</term><term>galaxies: high‐redshift</term></keywords></textClass><langUsage><language ident="en">en</language></langUsage></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We investigate the properties of 12 ultramassive passively evolving early‐type galaxies (ETGs) at zphot > 1.4 in the COSMOS 2 deg2 field. These 12 ETGs were selected as pBzKs, have accurate 1.4 ≲zphot≲ 1.7, high Sérsic index profiles typical of ellipticals, no detection at 24 μm, resulting in a complete ETG sample at M* > 2.5 × 1011 M⊙ (Chabrier initial mass function). Contrary to the previous claims, the half‐light radii estimated in very high signal‐to‐noise ratio imaging data from Hubble Space Telescope+Advanced Camera for Surveys (ACS) are found to be large for most of the sample, consistent with local ellipticals. If the high‐redshift ETGs with M* < 2.5 × 1011 M⊙ are really small in size and compact as reported in the previous studies, our result may suggest a ‘downsizing’ scenario, whereby the most massive ETGs reach their final structure earlier and faster than the lower mass ones. However, simulating galaxies with morphological properties fixed to those of local ETGs with the same stellar mass show that the few compact galaxies that we still recover in our sample can be understood in terms of fluctuations due to noise preventing the recovery of the extended low surface brightness haloes in the light profile. Such haloes, typical of Sérsic profiles, extending even up to 40 kpc, are indeed seen in our sample.</div></front></TEI><affiliations><list><country><li>Canada</li><li>France</li><li>Italie</li><li>États-Unis</li></country><region><li>Émilie-Romagne</li><li>Île-de-France</li></region><settlement><li>Bologne</li><li>Gif‐Sur Yvette</li><li>Paris</li></settlement><orgName><li>Université Pierre-et-Marie-Curie</li><li>Université de Bologne</li></orgName></list><tree><country name="Italie"><noRegion><name sortKey="Mancini, C" sort="Mancini, C" uniqKey="Mancini C" first="C." last="Mancini">C. Mancini</name></noRegion><name sortKey="Cimatti, A" sort="Cimatti, A" uniqKey="Cimatti A" first="A." last="Cimatti">A. Cimatti</name><name sortKey="Renzini, A" sort="Renzini, A" uniqKey="Renzini A" first="A." last="Renzini">A. Renzini</name></country><country name="France"><region name="Île-de-France"><name sortKey="Daddi, E" sort="Daddi, E" uniqKey="Daddi E" first="E." last="Daddi">E. Daddi</name></region><name sortKey="Aussel, H" sort="Aussel, H" uniqKey="Aussel H" first="H." last="Aussel">H. Aussel</name><name sortKey="Floc H, E Le" sort="Floc H, E Le" uniqKey="Floc H E" first="E. Le" last="Floc'H">E. Le Floc'H</name><name sortKey="Mccracken, H J" sort="Mccracken, H J" uniqKey="Mccracken H" first="H. J." last="Mccracken">H. J. Mccracken</name><name sortKey="Onodera, M" sort="Onodera, M" uniqKey="Onodera M" first="M." last="Onodera">M. Onodera</name><name sortKey="Salmi, F" sort="Salmi, F" uniqKey="Salmi F" first="F." last="Salmi">F. 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