Evidence for significant growth in the stellar mass of brightest cluster galaxies over the past 10 billion years

Lidman, C.; Suherli, Janette; Muzzin, Adam; Wilson, G. W.; Demarco, R.; Brough, Sarah; Rettura, Alessandro; Cox, James; DeGroot, A.; Yee, H. K. C.; Gilbank, David; Hoekstra, Henk; Balogh, Michael L.; Ellingson, E.; Hicks, A. K.; Nantais, Julie; Noble, Allison; Lacy, Mark; Surace, J.; Webb, Tracy

doi:10.1111/j.1365-2966.2012.21984.x

Cited by 189 publications

(300 citation statements)

References 78 publications

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“…By comparing the BCGs in our most massive progenitors at z = 1 with our results at z = 0, we find that the BCG grows by around a factor of 5, on average, in our AGN model (mainly by dry mergers). This is significantly higher than the observations, even when sample selection is accounted for (Lidman et al 2012), and requires further investigation. One explanation for these discrepancies is numerical resolution; we will discuss this possibility further in Section 6.…”

Section: Formation History and Distribution Of Starsmentioning

confidence: 62%

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Cosmological simulations of galaxy clusters with feedback from active galactic nuclei: profiles and scaling relations

Pike

Kay

Newton

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present results from a new set of 30 cosmological simulations of galaxy clusters, including the effects of radiative cooling, star formation, supernova feedback, black hole growth and AGN feedback. We first demonstrate that our AGN model is capable of reproducing the observed cluster pressure profile at redshift, z 0, once the AGN heating temperature of the targeted particles is made to scale with the final virial temperature of the halo. This allows the ejected gas to reach larger radii in highermass clusters than would be possible had a fixed heating temperature been used. Such a model also successfully reduces the star formation rate in brightest cluster galaxies and broadly reproduces a number of other observational properties at low redshift, including baryon, gas and star fractions; entropy profiles outside the core; and the Xray luminosity-mass relation. Our results are consistent with the notion that the excess entropy is generated via selective removal of the densest material through radiative cooling; supernova and AGN feedback largely serve as regulation mechanisms, moving heated gas out of galaxies and away from cluster cores. However, our simulations fail to address a number of serious issues; for example, they are incapable of reproducing the shape and diversity of the observed entropy profiles within the core region. We also show that the stellar and black hole masses are sensitive to numerical resolution, particularly the gravitational softening length; a smaller value leads to more efficient black hole growth at early times and a smaller central galaxy.

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Section: Formation History and Distribution Of Starsmentioning

confidence: 62%

“…Lidman et al (2012) find that the mass of BCGs increases by a factor of 1.8 ± 0.3 between z = 0.9 and 0.2. Specifically, the cumulative fraction of stellar mass formed by a given value of a is calculated for each cluster and the median curve is shown, re-scaled to the median final stellar mass.…”

Section: Formation History and Distribution Of Starsmentioning

confidence: 84%

Cosmological simulations of galaxy clusters with feedback from active galactic nuclei: profiles and scaling relations

Pike

Kay

Newton

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…11 we show where TXS 2353−003 and NVSS J210626−314003 fall relative to the K − z relationship of Seymour et al (2007) and De Breuck et al (2010), and that of Lidman et al (2012), who found a similar relationship for brightest cluster galaxies (BCGs). This figure shows the good agreement of our targets with both samples, as well as the self-consistency of both samples with each other (as expected if HzRGs are the progenitors of BCGs).…”

Section: K−z Relationshipmentioning

confidence: 91%

Defying jet-gas alignment in two radio galaxies atz~ 2 with extended light profiles: Similarities to brightest cluster galaxies

Collet

Nesvadba

Breuck

et al. 2015

A&A

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We report the detection of extended warm ionized gas in two powerful high-redshift radio galaxies, NVSS J210626-314003 at z = 2.10 and TXS 2353-003 at z = 1.49, that does not appear to be associated with the radio jets. This is contrary to what would be expected from the alignment effect, a characteristic feature of distant, powerful radio galaxies at z ≥ 0.6. The gas also has smaller velocity gradients and line widths than most other high-z radio galaxies with similar data. Both galaxies are part of a systematic study of 50 high-redshift radio galaxies with SINFONI, and are the only two that are characterized by the presence of high surface-brightness gas not associated with the jet axis and by the absence of such gas aligned with the jet. Both galaxies are spatially resolved with ISAAC broadband imaging covering the rest-frame R band, and have extended wings that cannot be attributed to line contamination. We argue that the gas and stellar properties of these galaxies are more akin to gas-rich brightest cluster galaxies in cool-core clusters than the general population of high-redshift radio galaxies at z > ∼ 2. In support of this interpretation, one of our sources, TXS 2353-003, for which we have Hα narrowband imaging, is associated with an overdensity of candidate Hα emitters by a factor of ∼8 relative to the field at z = 1.5. We discuss possible scenarios of the evolutionary state of these galaxies and the nature of their emission line gas within the context of cyclical AGN feedback.

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“…The full sample comprises 457 cluster members, obtained in 222 h of Gemini time over three years. Analysis of the brightest cluster galaxies in GCLASS is presented in Lidman et al (2012Lidman et al ( , 2013, while the dynamics of the cluster population are considered in papers by Noble et al (2013) and Muzzin et al (2014). The dynamical masses and redshifts of the clusters are shown as blue triangles in Fig.…”

Section: Gclassmentioning

confidence: 99%

Evidence for a change in the dominant satellite galaxy quenching mechanism atz = 1

Balogh

McGee

Mok

et al. 2016

Mon. Not. R. Astron. Soc.

133

230

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Evidence for significant growth in the stellar mass of brightest cluster galaxies over the past 10 billion years

Cited by 189 publications

References 78 publications

Cosmological simulations of galaxy clusters with feedback from active galactic nuclei: profiles and scaling relations

Cosmological simulations of galaxy clusters with feedback from active galactic nuclei: profiles and scaling relations

Defying jet-gas alignment in two radio galaxies atz~ 2 with extended light profiles: Similarities to brightest cluster galaxies

Evidence for a change in the dominant satellite galaxy quenching mechanism atz = 1

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