STAR-FORMING BRIGHTEST CLUSTER GALAXIES AT 0.25 &lt; z &lt; 1.25: A TRANSITIONING FUEL SUPPLY

McDonald, Michael; Stalder, B.; Bayliss, M.; Allen, S. W.; Applegate, Douglas; Ashby, M. L. N.; Bautz, Marshall W.; Benson, B. A.; Bleem, L. E.; Brodwin, M.; Carlstrom, J. E.; Chiu, I.; Desai, S.; Gonzalez, Anthony H.; Hlavacek-Larrondo, J.; Holzapfel, W. L.; Marrone, Dan; Miller, Eric D.; Reichardt, Christian; Saliwanchik, B. R.; Saro, A.; Schrabback, T.; Stanford, S. A.; Stark, A. A.; Vieira, J. D.; Zenteno, A.

doi:10.3847/0004-637x/817/2/86

Cited by 86 publications

(113 citation statements)

References 117 publications

(247 reference statements)

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“…The raw number densities derived from the Maraston et al (2013) analysis of the M ⊙ and above, galaxies with significant star formation appear to be far more common. Assuming that most of these systems are Brightest Cluster Galaxies (BCGs), these results are consistent with BCG sample studied by McDonald et al (2016). They find that 34% of BCGs at 0.25 < z < 1.25 have SFR> 10 M ⊙ /yr.…”

Section: Comparisons To Other Resultssupporting

confidence: 87%

The Stripe 82 Massive Galaxy Project. III. A Lack of Growth among Massive Galaxies

Bundy

Leauthaud

Saito

et al. 2017

ApJ

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The average stellar mass (M * ) of high-mass galaxies (log M * /M ⊙ > 11.5) is expected to grow by ∼30% since z ∼ 1, largely through ongoing mergers that are also invoked to explain the observed increase in galaxy sizes. Direct evidence for the corresponding growth in stellar mass has been elusive, however, in part because the volumes sampled by previous redshift surveys have been too small to yield reliable statistics. In this work, we make use of the Stripe 82 Massive Galaxy Catalog (s82-mgc) to build a mass-limited sample of 41,770 galaxies (log M * /M ⊙ > 11.2) with optical to near-IR photometry and a large fraction (>55%) of spectroscopic redshifts. Our sample spans 139 deg 2 , significantly larger than previous efforts. After accounting for a number of potential systematic errors, including the effects of M * scatter, we measure galaxy stellar mass functions over 0.3 < z < 0.65 and detect no growth in the typical M * of massive galaxies with an uncertainty of 9%. This confidence level is dominated by uncertainties in the star formation history assumed for M * estimates, although our inability to characterize low surface-brightness outskirts may be the most important limitation of our study. Even among these high-mass galaxies, we find evidence for differential evolution when splitting the sample by recent star formation (SF) activity. While low-SF systems appear to become completely passive, we find a mostly sub-dominant population of galaxies with residual, but low rates of star formation (∼1 M ⊙ /yr) number density does not evolve. Interestingly, these galaxies become more prominent at higher M * , representing ∼10% of all galaxies at 10 12 M ⊙ and perhaps dominating at even larger masses.

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Section: Comparisons To Other Resultssupporting

confidence: 87%

The Stripe 82 Massive Galaxy Project. III. A Lack of Growth among Massive Galaxies

Bundy

Leauthaud

Saito

et al. 2017

ApJ

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“…In addition, McDonald (2011) andMcDonald et al (2016) pointed out that the fuel of star formation in BCGs was galaxy-galaxy interactions at early times, but the main source recently became inctracluster medium cooling. Therefore, the similar s v BCG -s v cl relation regardless of the BCG activity implies that the bulk of the main stellar body or potential formed at the early epoch and settled down.…”

Section: Stellar Mass To Cluster Massmentioning

confidence: 99%

The Dependence of Cluster Galaxy Properties on the Central Entropy of Their Host Cluster

Kim

Hwang

et al. 2017

ApJ

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Additional information: 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 present a study of the connection between brightest cluster galaxies (BCGs) and their host galaxy clusters. Using galaxy clusters at < < z 0.1 0.3 from the Hectospec Cluster Survey (HeCS) with X-ray information from the Archive of Chandra Cluster Entropy Profile Tables (ACCEPT), we confirm that BCGs in low central entropy clusters are well aligned with the X-ray center. Additionally, the magnitude difference between BCG and the second brightest galaxy also correlates with the central entropy of the intracluster medium. From the red-sequence (RS) galaxies, we cannot find significant dependence of RS color scatter and stellar population on the central entropy of the intracluster medium of their host cluster. However, BCGs in low-entropy clusters are systematically less massive than those in high-entropy clusters, although this is dependent on the method used to derive the stellar mass of BCGs. In contrast, the stellar velocity dispersion of BCGs shows no dependence on BCG activity and cluster central entropy. This implies that the potential of the BCG is established earlier and the activity leading to optical emission lines is dictated by the properties of the intracluster medium in the cluster core.

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“…Although most BCGs appear red and dead at present times (with typical star formation rates of a few M /yr at most; e.g. McDonald et al 2011), their star formation was dramatically higher over the last ∼9 Gyr (McDonald et al 2016), and in some cases, can still reach a few tens to hundreds M /yr at z 0 (O' Dea et al 2008). This past (and, sometimes, present) high star formation in BCGs could thus be responsible for the central excess of SNcc products seen in the ICM.…”

Section: Radial Contribution Of Snia and Sncc Productsmentioning

confidence: 99%

Radial metal abundance profiles in the intra-cluster medium of cool-core galaxy clusters, groups, and ellipticals

Mernier

Plaa

Kaastra

et al. 2017

A&A

110

159

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The hot intra-cluster medium (ICM) permeating galaxy clusters and groups is not pristine, as it has been continuously enriched by metals synthesised in Type Ia (SNIa) and core-collapse (SNcc) supernovae since the major epoch of star formation (z 2-3). The cluster/group enrichment history and mechanisms responsible for releasing and mixing the metals can be probed via the radial distribution of SNIa and SNcc products within the ICM. In this paper, we use deep XMM-Newton/EPIC observations from a sample of 44 nearby cool-core galaxy clusters, groups, and ellipticals (CHEERS) to constrain the average radial O, Mg, Si, S, Ar, Ca, Fe, and Ni abundance profiles. The radial distributions of all these elements, averaged over a large sample for the first time, represent the best constrained profiles available currently. Specific attention is devoted to a proper modelling of the EPIC spectral components, and to other systematic uncertainties that may affect our results. We find an overall decrease of the Fe abundance with radius out to ∼0.9r 500 and ∼0.6r 500 for clusters and groups, respectively, in good agreement with predictions from the most recent hydrodynamical simulations. The average radial profiles of all the other elements (X) are also centrally peaked and, when rescaled to their average central X/Fe ratios, follow well the Fe profile out to at least ∼0.5r 500 . As predicted by recent simulations, we find that the relative contribution of SNIa (SNcc) to the total ICM enrichment is consistent with being uniform at all radii, both for clusters and groups using two sets of SNIa and SNcc yield models that reproduce the X/Fe abundance pattern in the core well. In addition to implying that the central metal peak is balanced between SNIa and SNcc, our results suggest that the enriching SNIa and SNcc products must share the same origin and that the delay between the bulk of the SNIa and SNcc explosions must be shorter than the timescale necessary to diffuse out the metals. Finally, we report an apparent abundance drop in the very core of 14 systems (∼32% of the sample). Possible origins of these drops are discussed.

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STAR-FORMING BRIGHTEST CLUSTER GALAXIES AT 0.25 < z < 1.25: A TRANSITIONING FUEL SUPPLY

Cited by 86 publications

References 117 publications

The Stripe 82 Massive Galaxy Project. III. A Lack of Growth among Massive Galaxies

The Stripe 82 Massive Galaxy Project. III. A Lack of Growth among Massive Galaxies

The Dependence of Cluster Galaxy Properties on the Central Entropy of Their Host Cluster

Radial metal abundance profiles in the intra-cluster medium of cool-core galaxy clusters, groups, and ellipticals

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