HST Grism Confirmation of 16 Structures at 1.4 &lt; z &lt; 2.8 from the Clusters Around Radio-Loud AGN (CARLA) Survey

Noirot, Gaël; Stern, Daniel; Mei, S.; Wylezalek, Dominika; Cooke, Elizabeth A.; Breuck, C. De; Galametz, A.; Hatch, N. A.; Vernet, J.; Brodwin, M.; Eisenhardt, Peter; Gonzalez, Anthony H.; Jarvis, Matt J.; Rettura, Alessandro; Seymour, N.; Stanford, S. A.

doi:10.3847/1538-4357/aabadb

Cited by 55 publications

(120 citation statements)

References 137 publications

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“…In this study, we identify an environmental dependence on the star-forming galaxy main sequence at 1.0 < z < 1.5, where cluster galaxies have lower log ∆SFR MS at fixed stellar mass than their counterparts in the field by a factor of 1.4, with a significance in log ∆SFR MS of ∼ 3.3σ across all stellar masses, but strongest at lower stellar masses ( Figure 5). Our findings are in good agreement with those of Noirot et al (2018), who find a significant suppression in the main sequence of the CARLA cluster sample, relative to the field sample of Whitaker et al (2014) at z ∼ 1.5. However, our results appear to differ somewhat from some other studies at a comparable redshift.…”

Section: Environmental Dependence Of the Star-forming Main Sequencesupporting

confidence: 91%

The GOGREEN survey: the environmental dependence of the star-forming galaxy main sequence at 1.0 < z < 1.5

Old

Balogh

Burg

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present results on the environmental dependence of the star-forming galaxy main sequence in 11 galaxy cluster fields at 1.0 < z < 1.5 from the Gemini Observations of Galaxies in Rich Early Environments Survey (GOGREEN) survey. We use a homogeneously selected sample of field and cluster galaxies whose membership is derived from dynamical analysis. Using [O ii]-derived star formation rates (SFRs), we find that cluster galaxies have suppressed SFRs at fixed stellar mass in comparison to their field counterparts by a factor of 1.4 ± 0.1 (∼ 3.3σ) across the stellar mass range: 9.0 < log(M * /M ) < 11.2. We also find that this modest suppression in the cluster galaxy star-forming main sequence is mass and redshift dependent: the difference between cluster and field increases towards lower stellar masses and lower redshift. When comparing the distribution of cluster and field galaxy SFRs to the star-forming main sequence, we find an overall shift towards lower SFRs in the cluster population, and note the absence of a tail of high SFR galaxies as seen in the field. Given this observed suppression in the cluster galaxy star-forming main sequence, we explore the implications for several scenarios such as formation time differences between cluster and field galaxies, and environmentally-induced star formation quenching and associated timescales.

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Section: Environmental Dependence Of the Star-forming Main Sequencesupporting

confidence: 91%

The GOGREEN survey: the environmental dependence of the star-forming galaxy main sequence at 1.0 < z < 1.5

Old

Balogh

Burg

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…To the best of our knowledge this proto-cluster candidate has never been reported in previous work. If confirmed spectroscopically, it will be one of the most distant proto-clusters discovered around radio galaxies (see also e.g., Noirot et al 2016Noirot et al , 2018. Castignani et al (2014a) searched for overdensities associated with z > 1 COSMOS-FRI radio galaxies within the proto-cluster catalog of Diener et al (2013), which was constructed using spectroscopic redshift information from the zCOSMOS-deep survey (Lilly et al 2007, Lilly et al, in prep.).…”

Section: Low-richness Structuresmentioning

confidence: 99%

Molecular gas in radio galaxies in dense megaparsec-scale environments at z = 0.4–2.6

Castignani

Combes

Salomé

et al. 2019

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Context. Low luminosity radio galaxies (LLRGs) typically reside in dense megaparsec-scale environments and are often associated with brightest cluster galaxies (BCGs). They are an excellent tool to study the evolution of molecular gas reservoirs in giant ellipticals, even close to the active galactic nucleus. Aims. We investigate the role of dense megaparsec-scale environment in processing molecular gas in LLRGs in the cores of galaxy (proto-)clusters. To this aim we selected within the COSMOS and DES surveys a sample of five LLRGs at z = 0.4 − 2.6 that show evidence of ongoing star formation on the basis of their far-infrared (FIR) emission. Methods. We assembled and modeled the FIR-to-UV spectral energy distributions (SEDs) of the five radio sources to characterize their host galaxies in terms of stellar mass and star formation rate. We observed the LLRGs with the IRAM-30m telescope to search for CO emission. We then searched for dense megaparsec-scale overdensities associated with the LLRGs using photometric redshifts of galaxies and the Poisson Probability Method, which we have upgraded using an approach based on the wavelet-transform (wPPM), to ultimately characterize the overdensity in the projected space and estimate the radio galaxy miscentering. Color-color and colormagnitude plots were then derived for the fiducial cluster members, selected using photometric redshifts. Results. Our IRAM-30m observations yielded upper limits to the CO emission of the LLRGs, at z = 0.39, 0.61, 0.91, 0.97, and 2.6. For the most distant radio source, COSMOS-FRI 70 at z = 2.6, a hint of CO(7→6) emission is found at 2.2σ. The upper limits found for the molecular gas content M(H 2 )/M <0.11, 0.09, 1.8, 1.5, and 0.29, respectively, and depletion time τ dep (0.2 − 7) Gyr of the five LLRGs are overall consistent with the corresponding values of main sequence field galaxies. Our SED modeling implies large stellar-mass estimates in the range log(M /M ) = 10.9 − 11.5, typical for giant ellipticals. Both our wPPM analysis and the cross-matching of the LLRGs with existing cluster/group catalogs suggest that the megaparsec-scale overdensities around our LLRGs are rich ( 10 14 M ) groups and show a complex morphology. The color-color and color-magnitude plots suggest that the LLRGs are consistent with being star forming and on the high-luminosity tail of the red sequence. The present study thus increases the still limited statistics of distant cluster core galaxies with CO observations. Conclusions. The radio galaxies of this work are excellent targets for ALMA as well as next-generation telescopes such as the James Webb Space Telescope.

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“…At z 1.5 several studies targeting galaxy overdensities have found evidence for cases where the SFRs of member galaxies are comparable or enhanced relative to field galaxies (e.g., Tran et al 2010;Strazzullo et al 2013;Santos et al 2015;Webb et al 2015;Wang et al 2016) indicating that environment did not always strictly act to quench star-formation. These observations mainly pertain to cluster cores, in other works cluster members have shown systematically lower SFRs than similar mass counterparts among field galaxies at these redshifts (Noirot et al 2018). Unfortunately, however, understanding the nature of a transition in the SFR-density relation and the exact epoch at which it occurs is still debated with some studies finding positive correlations, some finding negative correlations, and others no significant correlation at intervening redshifts (e.g., Elbaz et al 2007;Cooper et al 2008;Popesso et al 2011;Patel et al 2011;Grützbauch et al 2011;Muzzin et al 2012;Koyama et al 2013;Ziparo et al 2014;Lin et al 2014;Darvish et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Conditional quenching: a detailed look at the SFR−density relation at $z$ ∼ 0.9 from ORELSE

Tomczak

Lemaux

Lubin

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present a study of the star-formation rate (SFR)-density relation at z ∼ 0.9 using data drawn from the Observations of Redshift Evolution in Large Scale Environments (ORELSE) survey. We find that SFR does depend on environment, but only for intermediate-stellar mass galaxies (10 10.1 < M * /M < 10 10.8 ) wherein the median SFR at the highest densities is 0.2 − 0.3 dex less than at lower densities at a significance of 4σ. Interestingly, mass does not drive SFR; galaxies that are more/less massive have SFRs that vary at most by ≈ 20% across all environments showing no statistically significant dependence. We further split galaxies into low-redshift (z ∼ 0.8) and high-redshift (z ∼ 1.05) subsamples and observe nearly identical behavior. We devise a simple toy model to explore possible star-formation histories (SFHs) for galaxies evolving between these redshifts. The key assumption in this model is that star-forming galaxies in a given environment-stellar mass bin can be described as a superposition of two exponential timescales (SFR ∝ e −t/τ ): a long−τ timescale with τ = 4 Gyr to simulate "normal" star-forming galaxies, and a short−τ timescale with free τ (between 0.3 ≤ τ/Gyr ≤ 2) to simulate galaxies on a quenching trajectory. In general we find that galaxies residing in low/high environmental densities are more heavily weighted to the long−τ/short−τ pathways respectively, which we argue is a signature of environmental quenching. Furthermore, for intermediate-stellar mass galaxies this transition begins at intermediate-density environments suggesting that environmental quenching is relevant in group-like halos and/or cluster infall regions. formation in galaxies and how this changes over cosmic history. Efforts over the past several decades have found that there is no simple solution to these questions, but have instead revealed that there are many nuances that govern this aspect of galaxy evolution. This has led many investigators to take a reductionist approach to the subject by studying

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HST Grism Confirmation of 16 Structures at 1.4 < z < 2.8 from the Clusters Around Radio-Loud AGN (CARLA) Survey

Cited by 55 publications

References 137 publications

The GOGREEN survey: the environmental dependence of the star-forming galaxy main sequence at 1.0 < z < 1.5

The GOGREEN survey: the environmental dependence of the star-forming galaxy main sequence at 1.0 < z < 1.5

Molecular gas in radio galaxies in dense megaparsec-scale environments at z = 0.4–2.6

Conditional quenching: a detailed look at the SFR−density relation at $z$ ∼ 0.9 from ORELSE

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HST Grism Confirmation of 16 Structures at 1.4 < z < 2.8 from the Clusters Around Radio-Loud AGN (CARLA) Survey

Cited by 55 publications

References 137 publications

The GOGREEN survey: the environmental dependence of the star-forming galaxy main sequence at 1.0 &lt; z &lt; 1.5

The GOGREEN survey: the environmental dependence of the star-forming galaxy main sequence at 1.0 &lt; z &lt; 1.5

Molecular gas in radio galaxies in dense megaparsec-scale environments at z = 0.4–2.6

Conditional quenching: a detailed look at the SFR−density relation at $z$ ∼ 0.9 from ORELSE

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The GOGREEN survey: the environmental dependence of the star-forming galaxy main sequence at 1.0 < z < 1.5

The GOGREEN survey: the environmental dependence of the star-forming galaxy main sequence at 1.0 < z < 1.5