On the fast quenching of young low-mass galaxies up to z ∼ 0.6: new spotlight on the lead role of environment

Moutard, T.; Sawicki, Marcin; Arnouts, S.; Golob, Anneya; Malavasi, Nicola; Adami, C.; Coupon, J.; Ilbert, O.

doi:10.1093/mnras/sty1543

Cited by 47 publications

(40 citation statements)

References 93 publications

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“…As we found that a large fraction of groups not located at the nodes of the reconstructed cosmic web are in fact inside filaments (80% of groups at d skel < 1 cMpc), we postulated that this pre-processing could occur in galaxy groups during the hierarchical growth of structures in agreement with previously proposed quenching models (e.g. Wetzel et al 2013;Moutard et al 2018).…”

Section: Discussionsupporting

confidence: 90%

Pre-processing of galaxies in cosmic filaments around AMASCFI clusters in the CFHTLS

Sarron

Adami

Durret

et al. 2019

A&A

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Context. Galaxy clusters and groups are thought to accrete material along the preferred direction of cosmic filaments. Yet these structures have proven difficult to detect due to their low contrast with few studies focusing on cluster infall regions. Aims. In this work, we detected cosmic filaments around galaxy clusters using photometric redshifts in the range 0.15 < z < 0.7. We characterised galaxy populations in these structures to study the influence of "pre-processing" by cosmic filaments and galaxy groups on star-formation quenching. Methods. The cosmic filament detection was performed using the AMASCFI Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) T0007 cluster sample ). The filament reconstruction was done with the DISPERSE algorithm in photometric redshift slices. We showed that this reconstruction is reliable for a CFHTLS-like survey at 0.15 < z < 0.7 using a mock galaxy catalogue. We split our galaxy catalogue in two populations (passive and star-forming) using the LePhare SED fitting algorithm and worked with two redshift bins (0.15 < z ≤ 0.4 and 0.4 < z < 0.7). Results. We showed that the AMASCFI cluster connectivity (i.e. the number of filaments connecting to a cluster) increases with cluster mass M200. Filament galaxies outside R200 are found to be closer to clusters at low redshift, whatever the galaxy type. Passive galaxies in filaments are closer to clusters than star-forming galaxies in the low redshift bin only. The passive fraction of galaxies decreases with increasing clustercentric distance up to d ∼ 5 cMpc. Galaxy groups/clusters that are not located at nodes of our reconstruction are mainly found inside cosmic filaments. Conclusions. These results give clues for "pre-processing" in cosmic filaments, that could be due to smaller galaxy groups. This trend could be further explored by applying this method to larger photometric surveys such as HSC-SPP or Euclid.

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Section: Discussionsupporting

confidence: 90%

Pre-processing of galaxies in cosmic filaments around AMASCFI clusters in the CFHTLS

Sarron

Adami

Durret

et al. 2019

A&A

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“…Though not plotted, the high value of the environmental quenching efficiency observed for low-M * galaxies in our lowest redshift bin is broadly consistent with the strong signatures of environmentally-driven quenching seen in the VIPERS Multi-Lambda Survey (Moutard et al 2016a) for similar galaxies at similar redshifts (Moutard et al 2018). In that study, the authors constrain the quenching timescales for such galaxies and settle on "delayed-then-rapid" picture of quenching similar to that presented in §3.3 in our study.…”

Section: Environmental Quenching Efficiencysupporting

confidence: 82%

“…In that study, the authors constrain the quenching timescales for such galaxies and settle on "delayed-then-rapid" picture of quenching similar to that presented in §3.3 in our study. Further, it appears that such a quenching channel, while perhaps not the dominant channel for the full population of higher stellar mass galaxies at lower redshifts (Moutard et al 2018), appears dominant for galaxies of these stellar masses which inhabit clusters and groups at all redshifts studied here (see §3.3 for more discussion). However, that study lacked the redshift baseline to observe the precipitous drop of environmental quenching efficiency for galaxies log(M * /M ⊙ ) < 10.4.…”

Section: Environmental Quenching Efficiencymentioning

confidence: 79%

Persistence of the colour–density relation and efficient environmental quenching to z ∼ 1.4

Lemaux

Tomczak

Lubin

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Using ∼5000 spectroscopically-confirmed galaxies drawn from the Observations of Redshift Evolution in Large Scale Environments (ORELSE) survey we investigate the relationship between color and galaxy density for galaxy populations of various stellar masses in the redshift range 0.55 ≤ z ≤ 1.4. The fraction of galaxies with colors consistent with no ongoing star formation ( f q ) is broadly observed to increase with increasing stellar mass, increasing galaxy density, and decreasing redshift, with clear differences observed in f q between field and group/cluster galaxies at the highest redshifts studied. We use a semi-empirical model to generate a suite of mock group/cluster galaxies unaffected by environmentally-specific processes and compare these galaxies at fixed stellar mass and redshift to observed populations to constrain the efficiency of environmentally-driven quenching (Ψ convert ). High-density environments from 0.55 ≤ z ≤ 1.4 appear capable of efficiently quenching galaxies with log(M * /M ⊙ ) > 10.45. Lower stellar mass galaxies also appear efficiently quenched at the lowest redshifts studied here, but this quenching efficiency is seen to drop precipitously with increasing redshift. Quenching efficiencies, combined with simulated group/cluster accretion histories and results on the star formation rate-density relation from a companion ORELSE study, are used to constrain the average time from group/cluster accretion to quiescence and the elapsed time between accretion and the inception of the quenching event. These timescales were constrained to be t convert = 2.4 ± 0.3 and t delay = 1.3 ± 0.4 Gyr, respectively, for galaxies with log(M * /M ⊙ ) > 10.45 and t convert = 3.3 ± 0.3 and t delay = 2.2 ± 0.4 Gyr for lower stellar mass galaxies. These quenching efficiencies and associated timescales are used to rule out certain environmental mechanisms as being the primary processes responsible for transforming the star-formation properties of galaxies over this 4 Gyr window in cosmic time.

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“…Several studies at high redshift show that massive passive galaxies are already in place at z = 2 (van der Wel et al 2008;Bamford et al 2009;Baldry et al 2012). In contrast, the observed number of quenched low-mass galaxies increases towards the present day (Drory et al 2009;Baldry et al 2012;Moutard et al 2016Moutard et al , 2018. This downsizing in the passive population is generally associated with environmental quenching, and has been measured up to z ∼ 1 (Muzzin et al 2013;Tomczak et al 2014;Socolovsky et al 2018).…”

Section: Introductionmentioning

confidence: 92%

Compact star-forming galaxies preferentially quenched to become PSBs inz< 1 clusters

Socolovsky

Maltby

Hatch

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We analyse the structure of galaxies with high specific star formation rate (SSFR) in cluster and field environments in the redshift range 0.5 < z < 1.0. Recent studies have shown that these galaxies are strongly depleted in dense environments due to rapid environmental quenching, giving rise to post-starburst galaxies (PSBs). We use effective radii and Sérsic indices as tracers of galaxy structure, determined using imaging from the UKIDSS Ultra Deep Survey (UDS). We find that the high-SSFR galaxies that survive into the cluster environment have, on average, larger effective radii than those in the field. We suggest that this trend is likely to be driven by the most compact star-forming galaxies being preferentially quenched in dense environments. We also show that the PSBs in clusters have stellar masses and effective radii that are similar to the missing compact star-forming population, suggesting that these PSBs are the result of size-dependent quenching. We propose that both strong stellar feedback and the stripping of the extended halo act together to preferentially and rapidly quench the compact and low-mass star-forming systems in clusters to produce PSBs. We test this scenario using the stacked spectra of 124 high-SSFR galaxies, showing that more compact galaxies are more likely to host outflows. We conclude that a combination of environmental and secular processes is the most likely explanation for the appearance of PSBs in galaxy clusters.

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On the fast quenching of young low-mass galaxies up to z ∼ 0.6: new spotlight on the lead role of environment

Cited by 47 publications

References 93 publications

Pre-processing of galaxies in cosmic filaments around AMASCFI clusters in the CFHTLS

Pre-processing of galaxies in cosmic filaments around AMASCFI clusters in the CFHTLS

Persistence of the colour–density relation and efficient environmental quenching to z ∼ 1.4

Compact star-forming galaxies preferentially quenched to become PSBs inz< 1 clusters

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