A TALE OF A RICH CLUSTER AT<i>z</i>∼ 0.8 AS SEEN BY THE STAR FORMATION HISTORIES OF ITS EARLY-TYPE GALAXIES

Ferré-Mateu, Anna; Sánchez‐Blázquez, P.; Vazdekis, Alexandre; Rosa, I. G. de la

doi:10.1088/0004-637x/797/2/136

Cited by 17 publications

(19 citation statements)

References 135 publications

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“…This suggests that whatever mechanisms cause quenching in a group will do so at the same rate in both the dense inner and sparse outer regions. This result contradicts the results of Rettura et al (2010Rettura et al ( , 2011Ferré-Mateu et al (2014) and Darvish et al (2016) who find that galaxies in denser environments quench more rapidly than those in less dense environments.…”

Section: Resultscontrasting

confidence: 90%

Galaxy Zoo: the interplay of quenching mechanisms in the group environment★

Smethurst

Lintott

Bamford

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Does the environment of a galaxy directly influence the quenching history of a galaxy? Here we investigate the detailed morphological structures and star formation histories of a sample of SDSS group galaxies with both classifications from Galaxy Zoo 2 and NUV detections in GALEX. We use the optical and NUV colours to infer the quenching time and rate describing a simple exponentially declining SFH for each galaxy, along with a control sample of field galaxies. We find that the time since quenching and the rate of quenching do not correlate with the relative velocity of a satellite but are correlated with the group potential. This quenching occurs within an average quenching timescale of ∼ 2.5 Gyr from star forming to complete quiescence, during an average infall time (from ∼ 10R 200 to 0.01R 200 ) of ∼ 2.6 Gyr. Our results suggest that the environment does play a direct role in galaxy quenching through quenching mechanisms which are correlated with the group potential, such as harassment, interactions or starvation. Environmental quenching mechanisms which are correlated with satellite velocity, such as ram pressure stripping, are not the main cause of quenching in the group environment. We find that no single mechanism dominates over another, except in the most extreme environments or masses. Instead an interplay of mergers, mass & morphological quenching and environment driven quenching mechanisms dependent on the group potential drive galaxy evolution in groups.

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Section: Resultscontrasting

confidence: 90%

Galaxy Zoo: the interplay of quenching mechanisms in the group environment★

Smethurst

Lintott

Bamford

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…The colour, slope and low scatter of the red sequence within clusters are consistent with early-type cluster galaxies forming concurrently in a short burst of star formation at high redshift (z > 2) and passively evolving thereafter (e.g. Bower, Lucey & Ellis 1992;Eisenhardt et al 2007), although there are indications that further star formation occurs within galaxies towards the outskirts of the cluster (Ferré-Mateu et al 2014).…”

Section: Introductionsupporting

confidence: 63%

The formation history of massive cluster galaxies as revealed by CARLA

Cooke

Hatch

Rettura

et al. 2015

Mon. Not. R. Astron. Soc.

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We use a sample of 37 of the densest clusters and protoclusters across 1.3 z 3.2 from the Clusters Around Radio-Loud AGN (CARLA) survey to study the formation of massive cluster galaxies. We use optical i -band and infrared 3.6 µm and 4.5 µm images to statistically select sources within these protoclusters and measure their median observed colours; i − [3.6] . We find the abundance of massive galaxies within the protoclusters increases with decreasing redshift, suggesting these objects may form an evolutionary sequence, with the lower redshift clusters in the sample having similar properties to the descendants of the high redshift protoclusters. We find that the protocluster galaxies have an approximately unevolving observed-frame i − [3.6] colour across the examined redshift range. We compare the evolution of the i − [3.6] colour of massive cluster galaxies with simplistic galaxy formation models. Taking the full cluster population into account, we show that the formation of stars within the majority of massive cluster galaxies occurs over at least 2 Gyr, and peaks at z ∼ 2-3. From the median i − [3.6] colours we cannot determine the star formation histories of individual galaxies, but their star formation must have been rapidly terminated to produce the observed red colours. Finally, we show that massive galaxies at z > 2 must have assembled within 0.5 Gyr of them forming a significant fraction of their stars. This means that few massive galaxies in z > 2 protoclusters could have formed via dry mergers.

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“…Thus, to safely interpret z 0 observations, it is crucial to understand the chemical evolution of galaxies since they were formed, and in particular, during the build-up of their chemical properties (Vazdekis et al 1996). In this sense, it has been shown (e.g., Ferreras et al 2009;Choi et al 2014;Ferré-Mateu et al 2014) that the chemical composition of massive galaxies has remained constant over the last ∼7 Gyr. If metallicity actually regulates the dwarf-to-giant ratio variations, it would imply that the IMF of massive objects was bottom-heavy at z 1 , as recently suggested by observations (Shetty & Cappellari 2014;Martín-Navarro et al 2015c), since no chemical evolution has happened since then.…”

Section: Metallicity As a Driver Of Imf Variationsmentioning

confidence: 99%

Imf–metallicity: A Tight Local Relation Revealed by the Califa Survey

Martín-Navarro

Vazdekis

Barbera

et al. 2015

ApJ

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Variations in the stellar initial mass function (IMF) have been invoked to explain the spectroscopic and dynamical properties of early-type galaxies (ETGs). However, no observations have yet been able to disentangle the physical driver. We analyze here a sample of 24 ETGs drawn from the CALIFA survey, deriving in a homogeneous way their stellar population and kinematic properties. We find that the local IMF is tightly related to the local metallicity, becoming more bottom-heavy toward metal-rich populations. Our result, combined with the galaxy mass-metallicity relation, naturally explains previous claims of a galaxy mass-IMF relation, derived from non-IFU spectra. If we assume that-within the star formation environment of ETGs-metallicity is the main driver of IMF variations, a significant revision of the interpretation of galaxy evolution observables is necessary.

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A TALE OF A RICH CLUSTER ATz∼ 0.8 AS SEEN BY THE STAR FORMATION HISTORIES OF ITS EARLY-TYPE GALAXIES

Cited by 17 publications

References 135 publications

Galaxy Zoo: the interplay of quenching mechanisms in the group environment★

Galaxy Zoo: the interplay of quenching mechanisms in the group environment★

The formation history of massive cluster galaxies as revealed by CARLA

Imf–metallicity: A Tight Local Relation Revealed by the Califa Survey

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