THE COLORS OF CENTRAL AND SATELLITE GALAXIES IN zCOSMOS OUT TO<i>z</i>≃ 0.8 AND IMPLICATIONS FOR QUENCHING

Knobel, C.; Lilly, S. J.; Kovač, K.; Peng, Yingjie; Bschorr, T. J.; Carollo, C. M.; Contini, T.; Kneib, Jean-Paul; Fèvre, O. Le; Mainieri, V.; Renzini, A.; Scodeggio, M.; Zamorani, G.; Bardelli, S.; Bolzonella, M.; Bongiorno, A.; Caputi, K.; Cucciati, O.; Torre, S. de la; Ravel, L. de; Franzetti, P.; Garilli, B.; Iovino, A.; Kampczyk, P.; Lamareille, F.; Borgne, J. F. Le; Brun, V. Le; Maier, C.; Mignoli, M.; Pelló, R.; Montero, E. Pérez; Presotto, V.; Silverman, John D.; Tanaka, Masayuki; Tasca, L.; Tresse, L.; Vergani, D.; Zucca, E.; Barnes, Luke A.; Bordoloi, Rongmon; Cappi, A.; Cimatti, A.; Coppa, G.; Koekemoer, Anton M.; López-Sanjuán, C.; McCracken, H. J.; Moresco, M.; Nair, Preethi; Pozzetti, L.; Welikala, N.

doi:10.1088/0004-637x/769/1/24

Cited by 51 publications

(68 citation statements)

References 51 publications

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“…This is consistent with what others have seen at this redshift (e.g. Gerke et al 2007;Knobel et al 2013;), and we show the Knobel et al (2013) results as the yellow shaded region for comparison. However, when we consider the full stellar mass range accessible to us, including the photometric redshift extension down to M star = 10 9.5 M , we find evidence that f convert decreases with decreasing stellar mass, becoming consistent with zero at the lowest masses.…”

Section: Pa S S I V E Ly E Vo Lv I N G G a L A X I E S I N G Ro U P Ssupporting

confidence: 93%

“…From these same surveys it is possible to learn something about the evolving role of environment from measurements of local density or group catalogues (e.g. Giodini et al 2009;George et al 2011a;Knobel et al 2013;Lin et al 2014). In the context of the halo model (e.g.…”

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confidence: 99%

“…Comparable work on more common, lower-mass haloes at z > 0.3 -the progenitors of today's massive clusters -is more difficult and hence more limited, but several studies have shown that group galaxies indeed evolve differently from the field, at least for z < 0.8 (e.g. Wilman et al 2005;Balogh et al 2007;Poggianti et al 2008;Rudnick et al 2009;McGee et al 2011;Knobel et al 2013). At z > 0.8, however, little is known about galaxy evolution in group and low-mass cluster haloes.…”

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confidence: 99%

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Evidence for a change in the dominant satellite galaxy quenching mechanism atz = 1

Balogh

McGee

Mok

et al. 2016

Mon. Not. R. Astron. Soc.

133

230

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Section: Pa S S I V E Ly E Vo Lv I N G G a L A X I E S I N G Ro U P Ssupporting

confidence: 93%

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confidence: 99%

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confidence: 99%

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Evidence for a change in the dominant satellite galaxy quenching mechanism atz = 1

Balogh

McGee

Mok

et al. 2016

Mon. Not. R. Astron. Soc.

133

230

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“…The observational situation is not clear, e.g. Knobel (2013) do not find any redshift evolution of the red central fraction at a given stellar mass, while Tal et al (2014) find a strong z-dependence for the cumulative red central fractions. To overcome some of the limitations of the "vdB" transition fractions, we have defined and estimated "refined" transition fractions f trans,ref that we detail in the following section.…”

Section: Guo Ftrans Vdb08mentioning

confidence: 94%

The influence of the environmental history on quenching star formation in a Λ cold dark matter universe

Hirschmann¹,

Lucia²,

Wilman³

et al. 2014

Monthly Notices of the Royal Astronomical Society

113

145

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We present a detailed analysis of the influence of the environment and of the environmental history on quenching star formation in central and satellite galaxies in the local Universe. We take advantage of publicly available galaxy catalogues obtained from applying a galaxy formation model to the Millennium simulation. In addition to halo mass, we consider the local density of galaxies within various fixed scales. Comparing our model predictions to observational data (SDSS), we demonstrate that the models are failing to reproduce the observed density dependence of the quiescent galaxy fraction in several aspects: for most of the stellar mass ranges and densities explored, models cannot reproduce the observed similar behaviour of centrals and satellites, they slightly under-estimate the quiescent fraction of centrals and significantly overestimate that of satellites. We show that in the models, the density dependence of the quiescent central galaxies is caused by a fraction of "backsplash" centrals which have been satellites in the past. The observed stronger density dependence on scales of 0.2 − 1 Mpc may, however, indicate additional environmental processes working on central galaxies. Turning to satellite galaxies, the density dependence of their quiescent fractions reflects a dependence on the time spent orbiting within a parent halo, correlating strongly with halo mass and distance from the halo centre. Comparisons with observational estimates suggest relatively long gas consumption time scales of roughly 5 Gyr in low mass satellite galaxies. The quenching time scales decrease with increasing satellite stellar mass. Overall, a change in modelling both internal processes and environmental processes is required for improving currently used galaxy formation models.

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“…The parent vs. satellite nature of a galaxy (cf. Berlind et al 2005;Tinker et al 2012) is envisioned to be key to explaining some critical observations (Peng et al 2012; Knobel et al 2013). However, disentangling the physics involved is complicated greatly by the different degrees to which environment correlates with various galaxy properties, such as morphology and color (Blanton et al 2003).…”

Section: Introductionmentioning

confidence: 99%

Giant disk galaxies : Where environment trumps mass in galaxy evolution

Courtois

2015

Proc. IAU

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We identify some of the most HI massive and fastest rotating disk galaxies in the local universe with the aim of probing the processes that drive the formation of these extreme disk galaxies. By combining data from the Cosmic Flows project, which has consistently reanalyzed archival galaxy HI profiles, and 3.6µm photometry obtained with the Spitzer Space Telescope, with which we can measure stellar mass, we use the baryonic Tully-Fisher (BTF) relationship to explore whether these massive galaxies are distinct. We discuss several results, but the most striking is the systematic offset of the HI-massive sample above the BTF. These galaxies have both more gas and more stars in their disks than the typical disk galaxy of similar rotational velocity. The "condensed" baryon fraction, f C , the fraction of the baryons in a dark matter halo that settle either as cold gas or stars into the disk, is twice as high in the HImassive sample than typical, and almost reaches the universal baryon fraction in some cases, suggesting that the most extreme of these galaxies have little in the way of a hot baryonic component or cold baryons distributed well outside the disk. In contrast, the star formation efficiency, measured as the ratio of the mass in stars to that in both stars and gas, shows no difference between the HI-massive sample and the typical disk galaxies. We conclude that the star formation efficiency is driven by an internal, self-regulating process, while f C is affected by external factors. Neither the morphology nor the star formation rate of these galaxies is primarily determined by either their dark or stellar mass. We also found that the most massive HI detected galaxies are located preferentially in filaments. We present the first evidence of an environmental effect on galaxy evolution using a dynamical definition of a filament.

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THE COLORS OF CENTRAL AND SATELLITE GALAXIES IN zCOSMOS OUT TOz≃ 0.8 AND IMPLICATIONS FOR QUENCHING

Cited by 51 publications

References 51 publications

Evidence for a change in the dominant satellite galaxy quenching mechanism atz = 1

Evidence for a change in the dominant satellite galaxy quenching mechanism atz = 1

The influence of the environmental history on quenching star formation in a Λ cold dark matter universe

Giant disk galaxies : Where environment trumps mass in galaxy evolution

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