Both starvation and outflows drive galaxy quenching

Trussler, James; Maiolino, R.; Maraston, Claudia; Peng, Yingjie; Thomas, Daniel; Goddard, Daniel; Lian, Jianhui

doi:10.1093/mnras/stz3286

Cited by 154 publications

(199 citation statements)

References 168 publications

(275 reference statements)

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“…Within the framework of gas-regulated galaxy evolution, this implies an anticorrelation between the gas surface density or star formation rate surface density and the metallicity in the gas. Starvation has been suggested as a key component for determining the star-forming properties of galaxies today (Peng et al 2015;Trussler et al 2018), with environment appearing to play a role in instigating this process (von der Linden et al 2010; Davies et al 2016). Relationship between μ and O/H for satellites of low-mass (gray background with blue points indicating the medians) and high-mass (red contours with red points indicating the medians) centrals for PP04 O3N2 (top) and D16 N2S2Hα (bottom).…”

Section: Can Starvation Explain Our Results?mentioning

confidence: 99%

SDSS-IV MaNGA: Evidence for Enriched Accretion onto Satellite Galaxies in Dense Environments

Schaefer

Tremonti

Pace

et al. 2019

ApJ

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We investigate the environmental dependence of the local gas-phase metallicity in a sample of star-forming galaxies from the MaNGA survey. Satellite galaxies with stellar masses in the range ()  < < M M 9 log 10 * are found to be ∼0.05 dex higher in metallicity than centrals of similar stellar mass. Within the low-mass satellite population, we find that the interstellar medium (ISM) metallicity depends most strongly on the stellar mass of the galaxy that is central to the halo, though there is no obvious difference in the metallicity gradients. At fixed total stellar mass, the satellites of high-mass (M * > 10 10.5 M e) centrals are ∼0.1 dex more metal-rich than the satellites of low-mass (M * < 10 10 M e) centrals, controlling for local stellar mass surface density and gas fraction. Fitting a gas regulator model to the spaxel data, we are able to account for variations in the local gas fraction, stellar mass surface density, and local escape velocity-dependent outflows. We find that the best explanation for the metallicity differences is the variation in the average metallicity of accreted gas between different environments that depends on the stellar mass of the dominant galaxies in each halo. This is interpreted as evidence for the exchange of enriched gas between galaxies in dense environments that is predicted by recent simulations.

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Section: Can Starvation Explain Our Results?mentioning

confidence: 99%

SDSS-IV MaNGA: Evidence for Enriched Accretion onto Satellite Galaxies in Dense Environments

Schaefer

Tremonti

Pace

et al. 2019

ApJ

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“…Here we give a brief description of the sample of galaxies and galaxy parameters used in our analysis. We refer the reader to Trussler et al (2020) for a more thorough description of the data.…”

Section: Sample and Galaxy Parametersmentioning

confidence: 99%

“…In this paper we extend the analysis of Trussler et al (2020), who studied the role of stellar mass in galaxy quenching by investigating the stellar metallicities and ages of galaxies. Here we instead shift our attention to the role of environment in galaxy quenching, by studying the imprint of the environment on the stellar populations of galaxies.…”

Section: Introductionmentioning

confidence: 97%

“…Such comparisons have not been possible for gas-phase metallicities, as the nebular emission in passive galaxies is often too weak (due to the lack of gas) and because proper calibration of gas-phase metallicity diagnostics in non star-forming regions have only recently become available (Kumari et al 2019). Peng et al (2015) and Trussler et al (2020) studied the stellar metallicities of galaxies in the SDSS (z ∼ 0) and found that green valley and passive galaxies are significantly more metal-rich than star-forming galaxies of the same stellar mass, indicating that galaxies typically undergo significant chemical enrichment during the quenching phase. They argue that the stellar metallicity difference between star-forming and passive galaxies can be used to distinguish between different quenching mechanisms as the amount of chemical enrichment during the quenching phase depends on the mechanism.…”

Section: Introductionmentioning

confidence: 99%

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The weak imprint of environment on the stellar populations of galaxies

Trussler

Maiolino

Maraston

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We investigate the environmental dependence of the stellar populations of galaxies in SDSS DR7. Echoing earlier works, we find that satellites are both more metal-rich (<0.1 dex) and older (<2 Gyr) than centrals of the same stellar mass. However, after separating star-forming, green valley and passive galaxies, we find that the true environmental dependence of both stellar metallicity (<0.03 dex) and age (<0.5 Gyr) is in fact much weaker. We show that the strong environmental effects found when galaxies are not differentiated result from a combination of selection effects brought about by the environmental dependence of the quenched fraction of galaxies, and thus we strongly advocate for the separation of star-forming, green valley and passive galaxies when the environmental dependence of galaxy properties are investigated. We also study further environmental trends separately for both central and satellite galaxies. We find that star-forming galaxies show no environmental effects, neither for centrals nor for satellites. In contrast, the stellar metallicities of passive and green valley satellites increase weakly (<0.05 dex and <0.08 dex, respectively) with increasing halo mass, increasing local overdensity and decreasing projected distance from their central; this effect is interpreted in terms of moderate environmental starvation (‘strangulation’) contributing to the quenching of satellite galaxies. Finally, we find a unique feature in the stellar mass–stellar metallicity relation for passive centrals, where galaxies in more massive haloes have larger stellar mass (∼0.1 dex) at constant stellar metallicity; this effect is interpreted in terms of dry merging of passive central galaxies and/or progenitor bias.

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“…Simulations show that present-day rich clusters have collected their galaxies along filaments from regions with comoving radii at least 10 h −1 Mpc at redshift z = 1 (Chiang et al 2013;Overzier 2016). The formation of clusters is accompanied by the star-formation quenching of galaxies when they fall into clusters (Haines et al 2015;Einasto et al 2018c;Musso et al 2018;Kraljic et al 2019;Maier et al 2019;Trussler et al 2020). One result of galaxy quenching and morphological transformations is the large-scale morphological segregation of galaxies at low and high redshifts.…”

Section: Introductionmentioning

confidence: 99%

Multiscale cosmic web detachments, connectivity, and preprocessing in the supercluster SCl A2142 cocoon

Einasto

Deshev

Tenjes

et al. 2020

A&A

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Context. Superclusters of galaxies and their surrounding low-density regions (cocoons) represent dynamically evolving environments in which galaxies and their systems form and evolve. While evolutionary processes of galaxies in dense environments are extensively studied at present, galaxy evolution in low-density regions has received less attention. Aims. We study the properties, connectivity, and galaxy content of groups and filaments in the A2142 supercluster (SCl A2142) cocoon to understand the evolution of the supercluster with its surrounding structures and the galaxies within them. Methods. We calculated the luminosity-density field of SDSS galaxies and traced the SCl A2142 cocoon boundaries by the lowest luminosity-density regions that separate SCl A2142 from other superclusters. We determined galaxy filaments and groups in the cocoon and analysed the connectivity of groups, the high density core (HDC) of the supercluster, and the whole of the supercluster. We compared the distribution and properties of galaxies with different star-formation properties in the supercluster and in the cocoon. Results. The supercluster A2142 and the long filament that is connected to it forms the longest straight structure in the Universe detected so far, with a length of approximately 75 h −1 Mpc. The connectivity of the cluster A2142 and the whole supercluster is C = 6 − 7; poor groups exhibit C = 1 − 2. Long filaments around the supercluster's main body are detached from it at the turnaround region. Among various local and global environmental trends with regard to the properties of galaxies and groups, we find that galaxies with very old stellar populations lie in systems across a wide range of richness from the richest cluster to poorest groups and single galaxies. They lie even at local densities as low as D1 < 1 in the cocoon and up to D1 > 800 in the supercluster. Recently quenched galaxies lie in the cocoon mainly in one region and their properties are different in the cocoon and in the supercluster. The star-formation properties of single galaxies are similar across all environments. Conclusions. The collapsing main body of SCl A2142 with the detached long filaments near it are evidence of an important epoch in the supercluster evolution. There is a need for further studies to explore possible reasons behind the similarities between galaxies with very old stellar populations in extremely different environments, as well as mechanisms for galaxy quenching at very low densities. The presence of long, straight structures in the cosmic web may serve as a test for cosmological models.

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Both starvation and outflows drive galaxy quenching

Cited by 154 publications

References 168 publications

SDSS-IV MaNGA: Evidence for Enriched Accretion onto Satellite Galaxies in Dense Environments

SDSS-IV MaNGA: Evidence for Enriched Accretion onto Satellite Galaxies in Dense Environments

The weak imprint of environment on the stellar populations of galaxies

Multiscale cosmic web detachments, connectivity, and preprocessing in the supercluster SCl A2142 cocoon

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