Stellar Mass Profiles of Quiescent Galaxies in Different Environments at z ∼ 0

Mosleh, Moein; Tavasoli, Saeed; Tacchella, Sandro

doi:10.3847/1538-4357/aac5e6

Cited by 11 publications

(14 citation statements)

References 143 publications

(197 reference statements)

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“…This evidence contrasts with the scenario recently proposed by Matharu et al (2019) in which compact cluster spheroids should disappear over time 5 to justify the observed negligible difference between the mean size of cluster and field spheroids (e.g. Weinmann et al 2009;Maltby et al 2010;Cappellari et al 2013;Fernández Lorenzo et al 2013;Huertas-Company et al 2013b;Cebrián & Trujillo 2014;Kelkar et al 2015;Sweet et al 2017;Saracco et al 2017;Mosleh et al 2018, but see also Raichoor et al (2012); Strazzullo et al (2013); Andreon (2018), for a different result). It is worth to note that galaxies younger than 7 Gyr in the Coma cluster (cyan symbols, see §4.3) are offset with respect to high redshift galaxies, having preferentially larger Re and lower σ at fixed mass.…”

Section: The Evolution Of Cluster Spheroidscontrasting

confidence: 88%

The Fundamental Plane of cluster spheroidal galaxies at z ∼ 1.3: evidence for mass-dependent evolution

Saracco

Gargiulo

Barbera

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present spectroscopic observations obtained at the Large Binocular Telescope in the field of the cluster XLSSJ0223-0436 at z = 1.22. We confirm 12 spheroids cluster members and determine stellar velocity dispersion for 7 of them. We combine these data with those in the literature for clusters RXJ0848+4453 at z = 1.27 (8 galaxies) and XMMJ2235-2557 at z = 1.39 (7 galaxies) to determine the Fundamental Plane of cluster spheroids. We find that the FP at z ∼ 1.3 is offset and rotated (∼ 3σ) with respect to the local FP. The offset corresponds to a mean evolution ∆log(M dyn /L B )=(-0.5±0.1)z. High-redshift galaxies follow a steeper mass-dependenthigher-mass galaxies (log(M dyn /M ⊙ )≥11.5) have a higher-formation redshift (z f ≥6.5) than lower-mass ones (z f ≤2 for log(M dyn /M ⊙ ≤10)), with a median z f ≃ 2.5 for the whole sample. Also, galaxies with higher stellar mass density host stellar populations formed earlier than those in lower density galaxies. At fixed IMF, M dyn /M * varies systematically with mass and mass density. It follows that the evolution of the stellar populations (M * /L B ) accounts for the observed evolution of M dyn /L B for M dyn > 10 11 M ⊙ galaxies, while accounts for ∼85% of the evolution at M dyn < 10 11 M ⊙ . We find no evidence in favour of structural evolution of individual galaxies, while we find evidences that spheroids later added to the population may account for the observed discrepancy between ∆log(M dyn /L B ) and ∆ log(M * /L B ) at masses < 10 11 M ⊙ . Thus, the evolution of the FP of cluster spheroids is consistent with the mass-dependent and mass density-dependent evolution of their stellar populations superimposed to a minor contribution of spheroids joining the population at later times.

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Section: The Evolution Of Cluster Spheroidscontrasting

confidence: 88%

The Fundamental Plane of cluster spheroidal galaxies at z ∼ 1.3: evidence for mass-dependent evolution

Saracco

Gargiulo

Barbera

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…3.3), we find that quenched galaxies in the densest regions are much older (assuming an SSP, ∼2.2 +0.1 −0.4 Gyr) than those in the field (∼0.54 +0.09 −0.07 Gyr). These differences among quiescent galaxies depending on the environment are not found by Muzzin et al (2012) or Mosleh et al (2018). We note that the quiescent samples in low-and high-density regions have similar stellar mass distributions, therefore we should not expect this to be a simple consequence of an underlying mass-metallicity relation.…”

Section: Star Formation Activity In Different Environmentsmentioning

confidence: 53%

VIS³COS

Paulino-Afonso

Sobral

Darvish

et al. 2020

A&A

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We present spectroscopic observations of 466 galaxies in and around a superstructure at z ∼ 0.84 targeted by the VIMOS Spectroscopic Survey of a Supercluster in the COSMOS field (VIS3COS). We use [OII]λ3727, Hδ, and Dn4000 to trace recent, medium-, and long-term star formation histories and investigate the effect of stellar mass and local environment on them. By studying trends in individual and composite galaxy spectra, we find that stellar mass and environment play a role in the observed galactic properties. Galaxies with low stellar mass (10 < log10(M⋆/M⊙) < 10.5) in the field show the strongest Hδ absorption. Similarly, the massive population (log10(M⋆/M⊙) > 11) shows an increase in Hδ absorption strengths in intermediate-density environments (e.g. filaments). Galaxies with intermediate stellar mass (10.5 < log10(M⋆/M⊙) < 11) have similar Hδ absorption profiles in all environments, but show an indication of enhanced [OII] emission in intermediate-density environments. This indicates that field galaxies with low stellar mass and filament galaxies with high stellar mass are more likely to have experienced a recent burst of star formation, while galaxies of the intermediate stellar-mass show an increase of star formation at filament-like densities. We also find that the median [OII] equivalent width (|EW[OII]|) decreases from 27 ± 2 Å to 2.0+0.5−0.4 Å and Dn4000 increases from 1.09 ± 0.01 to 1.56 ± 0.03 with increasing stellar mass (from ∼109.25 to ∼1011.35 M⊙). For the dependence on the environment, we find that at fixed stellar mass, |EW[OII]| is tentatively lower in environments with higher density. We find for Dn4000 that the increase with stellar mass is sharper in denser environments, which indicates that these environments may accelerate galaxy evolution. Moreover, we find higher Dn4000 values in denser environments at fixed stellar mass, suggesting that galaxies are on average older and/or more metal rich in these dense environments. This set of tracers depicts a scenario where the most massive galaxies have, on average, the lowest specific star formation rates and the oldest stellar populations (age ≳ 1 Gyr, showing a mass-downsizing effect). We also hypothesize that the observed increase in star formation (higher EW[OII]|, higher specific star formation rate) at intermediate densities may lead to quenching because we find that the quenched fraction increases sharply from the filament to cluster-like regions at similar stellar masses.

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“…This catalog consists of 1014 void galaxies, brighter than M r = −19 with the redshift range 0.01 < z < 0.055. Mosleh et al (2018) divided galaxies in this catalog into star-forming and quiescent ones by using the urz color criteria and quiescent galaxies are crossmatched with the groups catalog of Tempel et al (2014). Then quenched void galaxies with more than one companion are removed which reduced the number of galaxies in void sub-sample to 147.…”

Section: Data and Sample Selectionmentioning

confidence: 99%

“…Then quenched void galaxies with more than one companion are removed which reduced the number of galaxies in void sub-sample to 147. Mosleh et al (2018) did so to ensure that galaxies in their sub-sample are isolated void galaxies, which magnify any variation between galaxy parameters at low-and high-density environments.…”

Section: Data and Sample Selectionmentioning

confidence: 99%

Comparing IMF-sensitive indices of intermediate-mass quiescent galaxies in various environments

Eftekhari

Mosleh

Vazdekis

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Using samples drawn from the Sloan Digital Sky Survey, we study for the first time the relation between large-scale environments (Clusters, Groups and Voids) and the stellar Initial Mass Function (IMF). We perform an observational approach based on the comparison of IMF-sensitive indices of quiescent galaxies with similar mass in varying environments. These galaxies are selected within a narrow redshift interval (0.020 < z < 0.055) and spanning a range in velocity dispersion from 100 to 200 km s −1 . The results of this paper are based upon analysis of composite spectra created by stacking the spectra of galaxies, binned by their velocity dispersion and redshift. The trends of spectral indices as measured from the stacked spectra, with respect to velocity dispersion, are compared in different environments. We find a lack of dependence of the IMF on the environment for intermediate-mass galaxy regime. We verify this finding by providing a more quantitative measurement of the IMF variations among galactic environments using MILES stellar population models with a precision of ∆Γ b ∼ 0.2.

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Stellar Mass Profiles of Quiescent Galaxies in Different Environments at z ∼ 0

Cited by 11 publications

References 143 publications

The Fundamental Plane of cluster spheroidal galaxies at z ∼ 1.3: evidence for mass-dependent evolution

The Fundamental Plane of cluster spheroidal galaxies at z ∼ 1.3: evidence for mass-dependent evolution

VIS³COS

Comparing IMF-sensitive indices of intermediate-mass quiescent galaxies in various environments

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