THE EFFECTS OF THE LOCAL ENVIRONMENT AND STELLAR MASS ON GALAXY QUENCHING TO z ∼ 3

Darvish, Behnam; Mobasher, Bahram; Sobral, David; Rettura, Alessandro; Scoville, N. Z.; Faisst, Andreas L.; Capak, P.

doi:10.3847/0004-637x/825/2/113

Cited by 197 publications

(315 citation statements)

References 145 publications

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“…to z 1 (e.g., van der Burg et al 2013;Darvish et al 2016;Nantais et al 2016Nantais et al , 2017) is thus unlikely to be due to enhanced galaxy-galaxy merging, at least in the most massive cluster systems. This suggests that the driving forces in quenching cluster galaxies are more likely to be due to interactions within the intracluster medium (such as ram-pressure stripping), harassment, or mass-induced selfquenching (e.g., Peng et al 2010;Bialas et al 2015).…”

Section: Discussionmentioning

confidence: 99%

Galaxy Merger Candidates in High-redshift Cluster Environments

Delahaye

Webb

Nantais

et al. 2017

ApJ

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We compile a sample of spectroscopically and photometrically selected cluster galaxies from four high-redshift galaxy clusters ( z 1.59 1.71 < <) from the Spitzer Adaptation of the Red-Sequence Cluster Survey (SpARCS), and a comparison field sample selected from the UKIDSS Deep Survey. Using near-infrared imaging from the Hubble Space Telescope, we classify potential mergers involving massive (M M 3 10 10 * ´) cluster members by eye, based on morphological properties such as tidal distortions, double nuclei, and projected near neighbors within 20 kpc. With a catalog of 23 spectroscopic and 32 photometric massive cluster members across the four clusters and 65 spectroscopic and 26 photometric comparable field galaxies, we find that after taking into account contamination from interlopers, 11.0 % 5.6 7.0 -+ of the cluster members are involved in potential mergers, compared to 24.7 % 4.6 5.3 -+ of the field galaxies. We see no evidence of merger enhancement in the central cluster environment with respect to the field, suggesting that galaxy-galaxy merging is not a stronger source of galaxy evolution in cluster environments compared to the field at these redshifts.

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Section: Discussionmentioning

confidence: 99%

Galaxy Merger Candidates in High-redshift Cluster Environments

Delahaye

Webb

Nantais

et al. 2017

ApJ

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“…Thus far, there is little evidence for the change of the scatter of the main sequence in a different environment (e.g., Peng et al 2010;Koyama et al 2013;Darvish et al 2016), but recently, Hayashi et al (2016) reported a larger (upward) scatter of main-sequence galaxies in the low-mass galaxies (<  M 10 9.3 ) at the z=2.5 protocluster, which is in fact similarly seen in our sample (I. Tanaka et al 2017, in preparation; see Figure 1).…”

Section: Suggested Picture and Future Aspectsmentioning

confidence: 99%

A Radio-to-mm Census of Star-forming Galaxies in Protocluster 4C23.56 at Z = 2.5: Gas Mass and Its Fraction Revealed with ALMA

Lee

Tanaka

Kawabe

et al. 2017

ApJ

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A Radio-to-mm Census of Star-forming Galaxies in Protocluster 4C23.56 at Z = 2.5: Gas Mass and Its Fraction Revealed with ALMA Lee, Minju M.; Tanaka, Ichi; Kawabe, Ryohei; Kohno, Kotaro; Kodama, Tadayuki; Kajisawa, Masaru; Yun, Min S.; Nakanishi, Kouichiro; Iono, Daisuke; Tamura, Yoichi IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish to cite from it. Please check the document version below. Document VersionPublisher's PDF, also known as Version of record Publication date: 2017Link to publication in University of Groningen/UMCG research database Citation for published version (APA): Lee, M. M., Tanaka, I., Kawabe, R., Kohno, K., Kodama, T., Kajisawa, M., ... Ivison, R. J. (2017). A Radioto-mm Census of Star-forming Galaxies in Protocluster 4C23.56 at Z = 2.5: Gas Mass and Its Fraction Revealed with ALMA. The Astrophysical Journal, 842(1), [55]. DOI: 10.3847/1538-4357/aa74c2 Copyright Other than for strictly personal use, it is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), unless the work is under an open content license (like Creative Commons).Take-down policy If you believe that this document breaches copyright please contact us providing details, and we will remove access to the work immediately and investigate your claim.Downloaded from the University of Groningen/UMCG research database (Pure): http://www.rug.nl/research/portal. For technical reasons the number of authors shown on this cover page is limited to 10 maximum. AbstractWe investigate gas contents of star-forming galaxies associated with protocluster 4C23.56 at z=2.49by using the redshifted CO(3-2) and 1.1 mm dust continuum with the Atacama Large Millimeter/submillimeter Array. The observations unveil seven CO detections out of 22 targeted Hα emitters (HAEs)and four out of 19 in 1.1 mm dust continuum. They have high stellar mass (  >Ḿ 4 10 10 M e ) and exhibit aspecific star-formation rate typical of main-sequence star-forminggalaxies atz 2.5. Different gas-mass estimators from CO(3-2) and 1.1 mm yield consistent values for simultaneous detections. The gas mass (M gas ) and gas fraction ( f gas ) are comparable to those of field galaxies, with ))  M , where a CO is the CO-to-H 2 conversion factor and A(Z) is the additional correction factor for the metallicity dependence of a CO , and á ñ =  f 0.53 0.07 gas from CO(3-2). Our measurements place a constraint on the cosmic gas density of high-z protoclusters, indicating thatthe protocluster is characterized by a gas density higher than that of the general fields by an order of magnitude. We found r~´- ( ) H M 5 10 Mpc 2 9 3 with the CO(3-2) detections. The five ALMA CO detections occur in the region ofhighest galaxy surface density,where the density positively correlates with global star-forming efficiency (SFE) and stellar mass. Such correlations possibly indicate a critical role of theenvironment on early galaxy evolution at high-z protocluste...

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“…The fraction of star-forming galaxies in the field is typically ∼80% at z>1 (e.g., Darvish et al 2016). The fraction of starforming galaxies in clusters within a region of radius 0.5Mpc (∼1′) is typically ∼10%-20% and ∼40%-50% at 1z1.4 and z>1.4, respectively (e.g., Brodwin et al 2013).…”

Section: Appendix B Significance Of the Spectroscopic Confirmationsmentioning

confidence: 99%

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

Noirot

Stern

Mei

et al. 2018

ApJ

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109

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We report spectroscopic results from our 40-orbit Hubble Space Telescope slitless grism spectroscopy program observing the 20 densest Clusters Around Radio-Loud AGN (CARLA) candidate galaxy clusters at 1.4<z<2.8. These candidate rich structures, among the richest and most distant known, were identified on the basis of [3.6]-[4.5] color from a 408hr multi-cycle Spitzer program targeting 420 distant radio-loud AGN. We report the spectroscopic confirmation of 16 distant structures at 1.4<z<2.8 associated with the targeted powerful highredshift radio-loud AGN. We also report the serendipitous discovery and spectroscopic confirmation of seven additional structures at 0.87<z<2.12 not associated with the targeted radio-loud AGN. We find that 10 10 -10 11 M e member galaxies of our confirmed CARLA structures form significantly fewer stars than their field counterparts at all redshifts within 1.4z2. We also observe higher star-forming activity in the structure cores up to z=2, finding similar trends as cluster surveys at slightly lower redshifts (1.0 < z < 1.5). By design, our efficient strategy of obtaining just two grism orbits per field only obtains spectroscopic confirmation of emission line galaxies. Deeper spectroscopy will be required to study the population of evolved, massive galaxies in these (forming) clusters. Lacking multi-band coverage of the fields, we adopt a very conservative approach of calling all confirmations "structures," although we note that a number of features are consistent with some of them being bona fide galaxy clusters. Together this survey represents a unique and large homogenous sample of spectroscopically confirmed structures at high redshifts, potentially more than doubling the census of confirmed, massive clusters at z>1.4.

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THE EFFECTS OF THE LOCAL ENVIRONMENT AND STELLAR MASS ON GALAXY QUENCHING TO z ∼ 3

Cited by 197 publications

References 145 publications

Galaxy Merger Candidates in High-redshift Cluster Environments

Galaxy Merger Candidates in High-redshift Cluster Environments

A Radio-to-mm Census of Star-forming Galaxies in Protocluster 4C23.56 at Z = 2.5: Gas Mass and Its Fraction Revealed with ALMA

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

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