Unveiling the important role of groups in the evolution of massive galaxies: Insights from an infrared passive sequence at intermediate redshift

D.J. Wilman; D. Pierini; K. Tyler; S.L. McGee; A. Oemler Jr.; S.L. Morris; M.L. Balogh; R.G. Bower; J.S. Mulchaey

doi:10.1086/587478

Unveiling the important role of groups in the evolution of massive galaxies: Insights from an infrared passive sequence at intermediate redshift

D.J. Wilman, D. Pierini, K. Tyler, S.L. McGee, A. Oemler Jr., S.L. Morris, M.L. Balogh, R.G. Bower, J.S. Mulchaey

Physics and Astronomy

Research output: Contribution to journal › Article › peer-review

38 Citations (Scopus)

Abstract

The most massive galaxies in the universe are also the oldest. To overturn this apparent contradiction with hierarchical growth models we focus on the group-scale halos that host most of these galaxies. Our z 0.4 group sample is selected in redshift space from the CNOC2 redshift survey. A stellar mass-selected M* ≳ 2 × 1010 M⊙ sample is constructed using IRAC observations. A sensitive mid-infrared (MIR) IRAC color is used to isolate passive galaxies. It produces a bimodal distribution, in which passive galaxies (highlighted by morphological early types) define a tight MIR color sequence (infrared passive sequence, IPS). This is due to stellar atmospheric emission from old stellar populations. Significantly offset from the IPS are galaxies where reemission by dust boosts emission at λobs = 8 μm. We term them infrared excess galaxies, whether star formation and/or AGN activity are present. They include all known. morphological late types. Comparison with EW[0 II] shows that MIR color is highly sensitive to low levels of activity and allows us to separate dusty active from passive galaxies at high stellar mass. The fraction of infrared excess galaxies, f(IRE), drops with M*, such that f(IRE) = 0.5 at a "crossover mass" of Mcr ≃ 1.3 × 10 11 Mo. Within our optically defined group sample there is a strong and consistent deficit in f(IRE) at all masses, but most clearly at M* ≳ 1011 M⊙. Suppression of star formation must mainly occur in groups. In particular, the observed trend of f(IRE) with M* can be explained if suppression of M* ≳ 1011 M⊙ galaxies occurs primarily in the group environment. This is confirmed using a mock galaxy catalog derived from the millenium simulation. In this way, the mass-dependent evolution in f(IRE) (downsizing) can be driven solely by structure growth in the universe, as more galaxies are accreted into group-sized halos with cosmic time. © 2008. The American Astronomical Society. All rights reserved.

Original language	English
Pages (from-to)	1009-1021
Number of pages	13
Journal	The Astrophysical Journal
Volume	680
Issue number	2
DOIs	https://doi.org/10.1086/587478
Publication status	Published - 2008

Bibliographical note

Export Date: 15 August 2017

Correspondence Address: Wilman, D. J.; Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstraße, D-85748 Garching, Germany

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Keywords

Galaxies: clusters: general
Galaxies: evolution
Galaxies: high-redshift
Galaxies: photometry
Galaxies: statistics
Infrared: galaxies

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10.1086/587478

https://www.scopus.com/inward/record.uri?eid=2-s2.0-46249133747&doi=10.1086%2f587478&partnerID=40&md5=73d0e974279690ef2467cb7ea48f4e06

Cite this

@article{5dcf8b140a5341d7a0c12a4361820660,

title = "Unveiling the important role of groups in the evolution of massive galaxies: Insights from an infrared passive sequence at intermediate redshift",

abstract = "The most massive galaxies in the universe are also the oldest. To overturn this apparent contradiction with hierarchical growth models we focus on the group-scale halos that host most of these galaxies. Our z 0.4 group sample is selected in redshift space from the CNOC2 redshift survey. A stellar mass-selected M* ≳ 2 × 1010 M⊙ sample is constructed using IRAC observations. A sensitive mid-infrared (MIR) IRAC color is used to isolate passive galaxies. It produces a bimodal distribution, in which passive galaxies (highlighted by morphological early types) define a tight MIR color sequence (infrared passive sequence, IPS). This is due to stellar atmospheric emission from old stellar populations. Significantly offset from the IPS are galaxies where reemission by dust boosts emission at λobs = 8 μm. We term them infrared excess galaxies, whether star formation and/or AGN activity are present. They include all known. morphological late types. Comparison with EW[0 II] shows that MIR color is highly sensitive to low levels of activity and allows us to separate dusty active from passive galaxies at high stellar mass. The fraction of infrared excess galaxies, f(IRE), drops with M*, such that f(IRE) = 0.5 at a {"}crossover mass{"} of Mcr ≃ 1.3 × 10 11 Mo. Within our optically defined group sample there is a strong and consistent deficit in f(IRE) at all masses, but most clearly at M* ≳ 1011 M⊙. Suppression of star formation must mainly occur in groups. In particular, the observed trend of f(IRE) with M* can be explained if suppression of M* ≳ 1011 M⊙ galaxies occurs primarily in the group environment. This is confirmed using a mock galaxy catalog derived from the millenium simulation. In this way, the mass-dependent evolution in f(IRE) (downsizing) can be driven solely by structure growth in the universe, as more galaxies are accreted into group-sized halos with cosmic time. {\textcopyright} 2008. The American Astronomical Society. All rights reserved.",

keywords = "Galaxies: clusters: general, Galaxies: evolution, Galaxies: high-redshift, Galaxies: photometry, Galaxies: statistics, Infrared: galaxies",

author = "D.J. Wilman and D. Pierini and K. Tyler and S.L. McGee and {Oemler Jr.}, A. and S.L. Morris and M.L. Balogh and R.G. Bower and J.S. Mulchaey",

note = "Export Date: 15 August 2017 Correspondence Address: Wilman, D. J.; Max-Planck-Institut f{\"u}r Extraterrestrische Physik, Giessenbachstra{\ss}e, D-85748 Garching, Germany References: Aaronson, M., Huchra, J., Mould, J., (1979) ApJ, 229, p. 1; Aitken, D.K., Roche, P.F., Allen, M.C., Phillips, M.M., (1982) MNRAS, 199. , 31P; Baldry, I.K., Balogh, M.L., Bower, R.G., Glazebrook, K., Nichol, R.C., Bamford, S.P., Budavari, T., (2006) MNRAS, 373, p. 469; Balogh, M., Bower, R.G., Small, I., Ziegler, B.L., Davies, R.L., Gaztelu, A., Fritz, A., (2002) MNRAS, 337, p. 256; Balogh, M.L., (2004) MNRAS, 348, p. 1355; Balogh, M.L., (2007) MNRAS, 374, p. 1169; Bell, E.F., de Jong, R.S., (2001) ApJ, 550, p. 212; Bell, E.F., (2005) ApJ, 625, p. 23; Bender, R., Saglia, R.P., Ziegler, B., Belloni, P., Greggio, L., Hopp, U., Bruzual, G., (1998) ApJ, 493, p. 529; Benson, A.J., Ellis, R.S., Menanteau, F., (2002) MNRAS, 336, p. 564; Berta, S., (2007) A&A, 467, p. 565; Bertin, E., Arnouts, S., (1996) A&AS, 117, p. 393; Best, P.N., von der Linden, A., Kauffmann, G., Heckman, T.M., Kaiser, C.R., (2007) MNRAS, 379, p. 894; Blanton, M.R., Roweis, S., (2007) AJ, 133, p. 734; Boselli, A., Lequeux, J., Gavazzi, G., (2004) A&A, 428, p. 409; Boselli, A., Sauvage, M., Lequeux, J., Donati, A., Gavazzi, G., (2003) A&A, 406, p. 867; Boselli, A., (1998) A&A, 335, p. 53; Bower, R.G., Benson, A.J., Malbon, R., Helly, J.C., Frenk, C.S., Baugh, C.M., Cole, S., Lacey, C.G., (2006) MNRAS, 370, p. 645; Bower, R.G., Lucey, J.R., Ellis, R.S., (1992) MNRAS, 254, p. 601; Bressan, A., et al, 2007, in ASP Conf. 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year = "2008",

doi = "10.1086/587478",

language = "English",

volume = "680",

pages = "1009--1021",

journal = "The Astrophysical Journal",

issn = "0004637X",

publisher = "Institute of Physics Publishing Ltd",

number = "2",

}

TY - JOUR

T1 - Unveiling the important role of groups in the evolution of massive galaxies: Insights from an infrared passive sequence at intermediate redshift

AU - Wilman, D.J.

AU - Pierini, D.

AU - Tyler, K.

AU - McGee, S.L.

AU - Oemler Jr., A.

AU - Morris, S.L.

AU - Balogh, M.L.

AU - Bower, R.G.

AU - Mulchaey, J.S.

N1 - Export Date: 15 August 2017 Correspondence Address: Wilman, D. 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PY - 2008

Y1 - 2008

N2 - The most massive galaxies in the universe are also the oldest. To overturn this apparent contradiction with hierarchical growth models we focus on the group-scale halos that host most of these galaxies. Our z 0.4 group sample is selected in redshift space from the CNOC2 redshift survey. A stellar mass-selected M* ≳ 2 × 1010 M⊙ sample is constructed using IRAC observations. A sensitive mid-infrared (MIR) IRAC color is used to isolate passive galaxies. It produces a bimodal distribution, in which passive galaxies (highlighted by morphological early types) define a tight MIR color sequence (infrared passive sequence, IPS). This is due to stellar atmospheric emission from old stellar populations. Significantly offset from the IPS are galaxies where reemission by dust boosts emission at λobs = 8 μm. We term them infrared excess galaxies, whether star formation and/or AGN activity are present. They include all known. morphological late types. Comparison with EW[0 II] shows that MIR color is highly sensitive to low levels of activity and allows us to separate dusty active from passive galaxies at high stellar mass. The fraction of infrared excess galaxies, f(IRE), drops with M*, such that f(IRE) = 0.5 at a "crossover mass" of Mcr ≃ 1.3 × 10 11 Mo. Within our optically defined group sample there is a strong and consistent deficit in f(IRE) at all masses, but most clearly at M* ≳ 1011 M⊙. Suppression of star formation must mainly occur in groups. In particular, the observed trend of f(IRE) with M* can be explained if suppression of M* ≳ 1011 M⊙ galaxies occurs primarily in the group environment. This is confirmed using a mock galaxy catalog derived from the millenium simulation. In this way, the mass-dependent evolution in f(IRE) (downsizing) can be driven solely by structure growth in the universe, as more galaxies are accreted into group-sized halos with cosmic time. © 2008. The American Astronomical Society. All rights reserved.

AB - The most massive galaxies in the universe are also the oldest. To overturn this apparent contradiction with hierarchical growth models we focus on the group-scale halos that host most of these galaxies. Our z 0.4 group sample is selected in redshift space from the CNOC2 redshift survey. A stellar mass-selected M* ≳ 2 × 1010 M⊙ sample is constructed using IRAC observations. A sensitive mid-infrared (MIR) IRAC color is used to isolate passive galaxies. It produces a bimodal distribution, in which passive galaxies (highlighted by morphological early types) define a tight MIR color sequence (infrared passive sequence, IPS). This is due to stellar atmospheric emission from old stellar populations. Significantly offset from the IPS are galaxies where reemission by dust boosts emission at λobs = 8 μm. We term them infrared excess galaxies, whether star formation and/or AGN activity are present. They include all known. morphological late types. Comparison with EW[0 II] shows that MIR color is highly sensitive to low levels of activity and allows us to separate dusty active from passive galaxies at high stellar mass. The fraction of infrared excess galaxies, f(IRE), drops with M*, such that f(IRE) = 0.5 at a "crossover mass" of Mcr ≃ 1.3 × 10 11 Mo. Within our optically defined group sample there is a strong and consistent deficit in f(IRE) at all masses, but most clearly at M* ≳ 1011 M⊙. Suppression of star formation must mainly occur in groups. In particular, the observed trend of f(IRE) with M* can be explained if suppression of M* ≳ 1011 M⊙ galaxies occurs primarily in the group environment. This is confirmed using a mock galaxy catalog derived from the millenium simulation. In this way, the mass-dependent evolution in f(IRE) (downsizing) can be driven solely by structure growth in the universe, as more galaxies are accreted into group-sized halos with cosmic time. © 2008. The American Astronomical Society. All rights reserved.

KW - Galaxies: clusters: general

KW - Galaxies: evolution

KW - Galaxies: high-redshift

KW - Galaxies: photometry

KW - Galaxies: statistics

KW - Infrared: galaxies

U2 - 10.1086/587478

DO - 10.1086/587478

M3 - Article

SN - 0004637X

VL - 680

SP - 1009

EP - 1021

JO - The Astrophysical Journal

JF - The Astrophysical Journal

IS - 2

ER -

Unveiling the important role of groups in the evolution of massive galaxies: Insights from an infrared passive sequence at intermediate redshift

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