X-ray-emitting active galactic nuclei from<i>z</i>= 0.6 to 1.3 in the intermediate- and high-density environments of the ORELSE survey

Rumbaugh, N.; Lemaux, B. C.; Tomczak, Adam; Kocevski, Dale D.; Lubin, Lori M.; Wu, Po-Feng; Gal, R. R.; Shen, Lu; Fassnacht, C. D.; Squires, G.

doi:10.1093/mnras/stw3091

Cited by 16 publications

(43 citation statements)

References 128 publications

(170 reference statements)

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“…The only ORELSE field included in the sample presented in this paper that has not appeared in detail in previous ORELSE studies is Cl1137. The remainder of the fields as well as the associated observations on each field are discussed extensively in other ORELSE papers (e.g., Lemaux et al 2012Lemaux et al , 2017Rumbaugh et al 2017Rumbaugh et al , 2018Tomczak et al 2017Tomczak et al , 2019. The Cl1137 field is unique among the ORELSE sample as it is the only cluster selected at radio wavelengths.…”

Section: +3000mentioning

confidence: 99%

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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Section: +3000mentioning

confidence: 99%

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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“…We used the Imperial reduction pipeline, which is described in detail in Laird et al (2009) andNandra et al (2015). For a summary of this reduction process, see Rumbaugh et al (2017).…”

Section: Chandra Observationsmentioning

confidence: 99%

“…Twelve of the sixteen LSSs in the ORELSE survey have Chandra imaging of sufficient quality to study diffuse X-ray emission, each of which has been described in previous papers (see Rumbaugh et al 2012Rumbaugh et al , 2013Rumbaugh et al , 2017. We combine the X-ray data of these 12 LSSs, which are succinctly summarized in Table 1, with our extensive optical and nearinfrared (IR) imaging and spectroscopy, as well as spectral energy distribution (SED) fitting, to assemble 10 tests of virialization/substructure and to compare them to three scaling relations between galaxy cluster observables.…”

Section: Introductionmentioning

confidence: 99%

Evaluating tests of virialization and substructure using galaxy clusters in the ORELSE survey

Rumbaugh

Lemaux

Tomczak

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We evaluated the effectiveness of different indicators of cluster virialization using 12 large-scale structures in the ORELSE survey spanning from 0.7 < z < 1.3. We located diffuse X-ray emission from 16 galaxy clusters using Chandra observations. We studied the properties of these clusters and their members, using Chandra data in conjunction with optical and near-IR imaging and spectroscopy. We measured X-ray luminosities and gas temperatures of each cluster, as well as velocity dispersions of their member galaxies. We compared these results to scaling relations derived from virialized clusters, finding significant offsets of up to 3-4σ for some clusters, which could indicate they are disturbed or still forming. We explored if other properties of the clusters correlated with these offsets by performing a set of tests of virialization and substructure on our sample, including Dressler-Schectman tests, power ratios, analyses of the velocity distributions of galaxy populations, and centroiding differences. For comparison to a wide range of studies, we used two sets of tests: ones that did and did not use spectral energy distribution fitting to obtain rest-frame colours, stellar masses, and photometric redshifts of galaxies. Our results indicated that the difference between the stellar mass or light mean-weighted center and the X-ray center, as well as the projected offset of the most-massive/brightest cluster galaxy from other cluster centroids had the strongest correlations with scaling relation offsets, implying they are the most robust indicators of cluster virialization and can be used for this purpose when X-ray data is insufficiently deep for reliable L X and T X measurements.

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“…Quenching mechanisms like ram pressure stripping or galaxy-galaxy interactions (for an exhaustive review, see Boselli & Gavazzi 2006) are more likely to occur in overdense regions (each process in a typical environment and on typical timescales), while other processes (e.g., AGN feedback) seem to be independent of environment (at least in the VIPERS redshift range, see Rumbaugh et al 2017). Moreover, the latter should be dominant at high masses (e.g.…”

Section: Vipers In Contextmentioning

confidence: 99%

The VIMOS Public Extragalactic Redshift Survey (VIPERS)

Cucciati

Davidzon

Bolzonella

et al. 2017

A&A

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We use the final data of the VIMOS Public Extragalactic Redshift Survey (VIPERS) to investigate the effect of the environment on the evolution of galaxies between z = 0.5 and z = 0.9. We characterise local environment in terms of the density contrast smoothed over a cylindrical kernel, the scale of which is defined by the distance to the fifth nearest neighbour. This is performed by using a volume-limited sub-sample of galaxies complete up to z = 0.9, but allows us to attach a value of local density to all galaxies in the full VIPERS magnitude-limited sample to i < 22.5. We use this information to estimate how the distribution of galaxy stellar masses depends on environment. More massive galaxies tend to reside in higher-density environments over the full redshift range explored. Defining star-forming and passive galaxies through their (NUV−r) vs. (r − K) colours, we then quantify the fraction of star-forming over passive galaxies, f ap , as a function of environment at fixed stellar mass. f ap is higher in low-density regions for galaxies with masses ranging from log(M/M ) = 10.38 (the lowest value explored) to at least log(M/M ) ∼ 11.3, although with decreasing significance going from lower to higher masses. This is the first time that environmental effects on high-mass galaxies are clearly detected at redshifts as high as z ∼ 0.9. We compared these results to VIPERS-like galaxy mock catalogues based on a widely used galaxy formation model. The model correctly reproduces f ap in low-density environments, but underpredicts it at high densities. The discrepancy is particularly strong for the lowest-mass bins. We find that this discrepancy is driven by an excess of low-mass passive satellite galaxies in the model. In high-density regions, we obtain a better (although not perfect) agreement of the model f ap with observations by studying the accretion history of these model galaxies (that is, the times when they become satellites), by assuming either that a non-negligible fraction of satellites is destroyed, or that their quenching timescale is longer than ∼2 Gyr.

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X-ray-emitting active galactic nuclei fromz= 0.6 to 1.3 in the intermediate- and high-density environments of the ORELSE survey

Cited by 16 publications

References 128 publications

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

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

Evaluating tests of virialization and substructure using galaxy clusters in the ORELSE survey

The VIMOS Public Extragalactic Redshift Survey (VIPERS)

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