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

Lemaux, B. C.; Tomczak, Adam; Lubin, Lori M.; Gal, R. R.; Shen, Lu; Pelliccia, Debora; Wu, Po-Feng; Hung, Denise; Mei, S.; Fèvre, O. Le; Rumbaugh, N.; Kocevski, Dale D.; Squires, G.

doi:10.1093/mnras/stz2661

Cited by 61 publications

(72 citation statements)

References 214 publications

(357 reference statements)

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“…This overall effect on the median sSFR can be linked to the results on the quenched fraction ( f Q ) shown in PA18, where we find that at high stellar masses (>10 11 M ) there is no dependence effect on f Q , while at lower stellar masses there is an increase from intermediate-to high-density regions (see also e.g. Lemaux et al 2019). An increase of the quenched fraction (from ∼10% to ∼50% of the sample from low-and intermediate-to high-density regions, see Table A.1) results in a lower median sSFR value for the population.…”

Section: Environmental Effects On Star Formationsupporting

confidence: 71%

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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Section: Environmental Effects On Star Formationsupporting

confidence: 71%

VIS³COS

Paulino-Afonso

Sobral

Darvish

et al. 2020

A&A

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“…In this study, we use both spectroscopic and photometric galaxies and account for their associated z phot to mitigate this selection effect. In addition, the high-priority targets (red sequence cluster members) are always subdominant in our observations (Lemaux et al 2019), and the resultant spectral galaxy sample is mostly representative of the underlying galaxy population at these redshifts (Shen et al 2017;Lemaux et al 2019). We expect high completeness and purity of the ERAGN sample.…”

Section: Radio Observations and Sample Selectionmentioning

confidence: 80%

“…The spectroscopic redshift catalogs are extracted and assessed primarily on observations from the DEep Imaging and Multi-Object Spectrograph (DEIMOS; Faber et al 2003) equipped on Keck II. Complementary spectroscopy is obtained in the literature (Oke et al 1998;Gal & Lubin 2004;Gioia et al 2004;Tanaka et al 2008), and the different facilities utilized therein are detailed in Lemaux et al (2012Lemaux et al ( , 2019.…”

Section: The Orelse Survey and Available Datamentioning

confidence: 99%

“…Considering our local overdensity footprints (see Section 2.4), the completeness/representativeness of our spectroscopic catalogs, and consistencies with previous radio galaxy studies in ORELSE, we require host galaxies to have 0.55 z 1.35, ¢   i z 18.5 24.5, and  M M 10 10 *  (Shen et al 2017;Lemaux et al 2019). As a result, we have a total sample of 50 ERAGN (Table 1) of which 24 have spectroscopically confirmed redshifts (hereafter ERAGN-spec) Note.…”

Section: Radio Observations and Sample Selectionmentioning

confidence: 99%

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Extended Radio AGN at z ∼ 1 in the ORELSE Survey: The Confining Effect of Dense Environments

Shen

Liu

Zhang

et al. 2020

ApJ

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Recent hydrodynamic simulations and observations of radio jets have shown that the surrounding environment has a large effect on their resulting morphology. To investigate this, we use a sample of 50 Extended Radio Active Galactic Nuclei (ERAGN) detected in the Observations of Redshift Evolution in Large-Scale Environments survey. These sources are all successfully cross-identified to galaxies within a redshift range of 0.55z1.35, either through spectroscopic redshifts or accurate photometric redshifts. We find that ERAGN are more compact in high-density environments than those in low-density environments at a significance level of 4.5σ. Among a series of internal properties under our scrutiny, only the radio power demonstrates a positive correlation with their spatial extent. After removing the possible radio power effect, the difference of size in low-and high-density environments persists. In the global environment analyses, the majority (86%) of high-density ERAGN reside in the cluster/group environment. In addition, ERAGN in the cluster/group central regions are preferentially compact with a small scatter in size, compared to those in the cluster/group intermediate regions and fields. In conclusion, our data appear to support the interpretation that the dense intracluster gas in the central regions of galaxy clusters plays a major role in confining the spatial extent of radio jets. Unified Astronomy Thesaurus concepts: Radio active galactic nuclei (2134); Radio galaxies (1343); Galaxy clusters (584); Radio jets (1347)

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“…At redshifts z < 1.5 galaxy cluster cores are dominated by red, quenched, early-type galaxies, while blue, star-forming, latetype galaxies are mostly found in the field (e.g., Dressler 1980;Balogh et al 1998Balogh et al , 2004Postman et al 2005;Mei et al 2009;Rettura et al 2011;Lemaux et al 2012Lemaux et al , 2019Wagner et al 2015;Tomczak et al 2019). At higher redshifts, the results are somewhat conflicting, as it also becomes more difficult to Lee et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Massive molecular gas reservoir around the central AGN in the CARLA J1103 + 3449 cluster at z = 1.44

Markov

Mei

Salomé

et al. 2020

A&A

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Passive early-type galaxies dominate cluster cores at z ≲ 1.5. At higher redshift, cluster core galaxies are observed to have on-going star-formation, which is fueled by cold molecular gas. We measured the molecular gas reservoir of the central region around the radio-loud active galactic nucleus (AGN) in the cluster CARLA J1103 + 3449 at z = 1.44 using NOEMA. The AGN synchrotron emission dominates the continuum emission at 94.48 GHz, and we measured its flux at the AGN position and at the position of two radio jets. Combining our measurements with published results over the range 4.71–94.5 GHz, and assuming Ssynch ∝ ν−α, we obtain a flat spectral index of α = 0.14 ± 0.03 for the AGN core emission, and a steeper index of α = 1.43 ± 0.04 and α = 1.15 ± 0.04 at positions close to the western and eastern lobes, respectively. The total spectral index is α = 0.92 ± 0.02 over the range 73.8 MHz–94.5 GHz. We detect two CO(2–1) emission lines, both blueshifted with respect to the AGN. Their emission corresponds to two regions, ~17 kpc southeast and ~14 kpc southwest of the AGN, not associated with galaxies. In these two regions, we find a total massive molecular gas reservoir of Mgastot = 3.9 ± 0.4 × 1010 M⊙, which dominates (≳60%) the central total molecular gas reservoir. These results can be explained by massive cool gas flows in the center of the cluster. The AGN early-type host is not yet quenched; its star formation rate is consistent with being on the main sequence of star-forming galaxies in the field (star formation rate ~30–140 M⊙ yr−1), and the cluster core molecular gas reservoir is expected to feed the AGN and the host star formation before quiescence. The other confirmed cluster members show star formation rates at ~2σ below the field main sequence at similar redshifts and do not have molecular gas masses larger than galaxies of similar stellar mass in the field.

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

Cited by 61 publications

References 214 publications

VIS³COS

VIS³COS

Extended Radio AGN at z ∼ 1 in the ORELSE Survey: The Confining Effect of Dense Environments

Massive molecular gas reservoir around the central AGN in the CARLA J1103 + 3449 cluster at z = 1.44

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