Individual and Group Galaxies in Cnoc1 Clusters

Li, I. H.; Yee, H. K. C.; Ellingson, E.

doi:10.1088/0004-637x/698/1/83

Cited by 34 publications

(37 citation statements)

References 78 publications

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“…This method has been widely used to compute the luminosity function, e.g., Barkhouse et al (2007), and has been demonstrated numerically to be able to accurately recover the underlying luminosity function selected in three dimensions (Valotto et al 2001). We adopt the method to explore galaxy properties for photometric redshift samples, similar to the approach used in Loh et al (2008) and Li et al (2009). We stack galaxies around group centers within a redshift slice for which the redshift difference between galaxy and group has to be smaller than the photo-z accuracy, i.e., z z ) are galaxy redshift, group redshift, and photo-z accuracy, respectively.…”

Section: Background Subtractionmentioning

confidence: 99%

The Pan-STARRS1 Medium-deep Survey: Star Formation Quenching in Group and Cluster Environments

Jian

Lin

et al. 2017

ApJ

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Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. AbstractWe make use of a catalog of 1600 Pan-STARRS1 groups produced by the probability friends-of-friends algorithm to explore how the galaxy properties, i.e., the specific star formation rate (SSFR) and quiescent fraction, depend on stellar mass and group-centric radius. The work is the extension of Lin et al. In this work, powered by a stacking technique plus a background subtraction for contamination removal, a finer correction and more precise results are obtained than in our previous work. We find that while the quiescent fraction increases with decreasing groupcentric radius, the median SSFRs of star-forming galaxies in groups at fixed stellar mass drop slightly from the field toward the group center. This suggests that the main quenching process in groups is likely a fast mechanism. On the other hand, a reduction in SSFRs by∼0.2 dex is seen inside clusters as opposed to the field galaxies. If the reduction is attributed to the slow quenching effect, the slow quenching process acts dominantly in clusters. In addition, we also examine the density-color relation, where the density is defined by using a sixth-nearest-neighbor approach. Comparing the quiescent fractions contributed from the density and radial effect, we find that the density effect dominates the massive group or cluster galaxies, and the radial effect becomes more effective in less massive galaxies. The results support mergers and/or starvation as the main quenching mechanisms in the group environment, while harassment and/or starvation dominate in clusters.

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Section: Background Subtractionmentioning

confidence: 99%

The Pan-STARRS1 Medium-deep Survey: Star Formation Quenching in Group and Cluster Environments

Jian

Lin

et al. 2017

ApJ

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“…In a complementary analysis, Li, Yee & Ellingson (2009) observed that the fraction of blue galaxies increases faster with redshift in groups associated with Canadian Network for Observational Cosmology (CNOC1) clusters (Yee, Ellingson & Carlberg 1996) than in the clusters themselves. Finally, Tanaka et al (2007, 2009) have shown evidence of newly formed red galaxies with residual star formation in the large‐scale structure around clusters, indicating that these systems may be very effective in transforming galaxies over cosmic time.…”

Section: Introductionmentioning

confidence: 99%

The Cosmic Web and galaxy evolution around the most luminous X-ray cluster: RX J1347.5−1145

Verdugo¹,

Lerchster²,

Böhringer³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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In this paper we study large‐scale structures and their galaxy content around the most X‐ray luminous cluster known, RX J1347.5−1145 at z= 0.45. We make use of u*g′r′i′z′ Canada–France–Hawaii Telescope (CFHT) MegaCam photometry together with VIsible MultiObject Spectrograph (VIMOS) Very Large Telescope (VLT) spectroscopy to identify structures around RX J1347 on a scale of ∼20 × 20 Mpc2. We construct maps of the galaxy distribution and the fraction of blue galaxies. We study the photometric galaxy properties as a function of the environment traced by the galaxy density. We identify group candidates based on galaxy overdensities and study their galaxy content. We also use available Galaxy Evolution Explorer (GALEX) near‐ultraviolet imaging to identify strong unobscured star‐forming galaxies. We find that the large‐scale structure around RX J1347 extends in the north‐east–south‐west direction for at least 20 Mpc, over a region in which most of the group candidates are located, some of which show X‐ray emission in archival XMM–Newton observations. As in other studies, we find that the fraction of blue galaxies (Fblue) is a function of galaxy number density, but the bulk of the trend is due to galaxies belonging to massive systems. The fraction of ultraviolet‐ (UV‐) bright galaxies is also a function of environment, but their relative number compared with the blue population seems to be constant regardless of the environment. These UV emitters also have similar properties at all galaxy densities, indicating that the transition between galaxy types occurs over short time‐scales. Candidate galaxy groups show a large variation in their galaxy content and Fblue in those groups displays little dependence on galaxy number density. This may indicate possible differences in their evolutionary status, or suggest that the processes acting in groups are different from those in clusters. The large‐scale structure around rich clusters provides a dynamic environment for galaxy evolution. In the case of RX J1347, the transformation may start within infalling groups and finish with the removal of the cold gas once galaxies are accreted into massive systems.

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“…The currently favoured explanation for these observed trends is that infalling field galaxies are processed physically as they travel from the field, through the cluster outskirts and virialize in the central cluster region (Berrier et al 2009). However, the extent to which cluster galaxies were ‘pre‐processed’ by physical effects occurring during an earlier residence in a galaxy group 1 remains contested (Li, Yee & Ellingson 2009). Numerous physical processes have been suggested as the agents of this apparent transformation of galaxy populations.…”

Section: Introductionmentioning

confidence: 99%

An environmental Butcher-Oemler effect in intermediate-redshift X-ray clusters★

Urquhart

Willis

Hoekstra

et al. 2010

Monthly Notices of the Royal Astronomical Society

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We present uniform Canada–France–Hawaii Telescope (CFHT) Megacam g and r photometry for 34 X‐ray‐selected galaxy clusters drawn from the X‐ray Multi‐Mirror (XMM) Large Scale Structure (LSS) survey and the Canadian Cluster Comparison Project (CCCP). The clusters possess well‐determined X‐ray temperatures spanning the range 1 < kT(keV) < 12. In addition, the clusters occupy a relatively narrow redshift interval (0.15 < z < 0.41) in order to minimize any redshift‐dependent photometric effects. We investigate the colour bimodality of the cluster galaxy populations and compute blue fractions using criteria derived by Butcher & Oemler. We identify a trend to observe increasing blue fraction versus redshift in common with numerous previous studies of cluster galaxy populations. However, in addition we identify an environmental dependence of cluster blue fraction in that cool (low‐mass) clusters display higher blue fractions than hotter (higher mass) clusters. Finally, we tentatively identify a small excess population of extremely blue galaxies in the coolest X‐ray clusters (essentially massive groups) and note that these may be the signature of actively starbursting galaxies driven by galaxy–galaxy interactions in the group environment.

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Individual and Group Galaxies in Cnoc1 Clusters

Cited by 34 publications

References 78 publications

The Pan-STARRS1 Medium-deep Survey: Star Formation Quenching in Group and Cluster Environments

The Pan-STARRS1 Medium-deep Survey: Star Formation Quenching in Group and Cluster Environments

The Cosmic Web and galaxy evolution around the most luminous X-ray cluster: RX J1347.5−1145

An environmental Butcher-Oemler effect in intermediate-redshift X-ray clusters★

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