THE<i>XMM</i>CLUSTER SURVEY: THE BUILD-UP OF STELLAR MASS IN BRIGHTEST CLUSTER GALAXIES AT HIGH REDSHIFT

Stott, John P.; Collins, Chris; Sahlén, Martin; Hilton, Matthew; Lloyd-Davies, E. J.; Capozzi, D.; Hosmer, Mark; Liddle, Andrew R.; Mehrtens, Nicola; Miller, Christopher J.; Romer, A. K.; Stanford, S. A.; Viana, P. T. P.; Davidson, M.; Hoyle, B.; Kay, Scott T.; Nichol, R. C.

doi:10.1088/0004-637x/718/1/23

Cited by 116 publications

(214 citation statements)

References 94 publications

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“…Mortlock et al 2011). This lack of evolution in the massive galaxy population is consistent with studies of brightest cluster galaxies (BCGs) in which little change is observed in BCG stellar masses to redshifts of z ∼ 1−1.5 (Stott et al 2010). These observations corroborate the picture of galaxy evolution whereby a mass-dependent shut-down of star formation is experienced by galaxies (e.g.…”

Section: Redshiftsupporting

confidence: 87%

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The WIRCam Deep Survey

Bielby

Hudelot

McCracken

et al. 2012

A&A

171

208

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We present a new near-infrared imaging survey in the four CFHTLS deep fields: the WIRCam Deep Survey or "WIRDS". WIRDS comprises extremely deep, high quality (FWHM ∼ 0.6 ) J, H, and K s imaging covering a total effective area of 2.1 deg 2 and reaching AB 50% completeness limits of ≈24.5. We combine our images with the CFHTLS to create a unique eight-band ugrizJHK S photometric catalogues in the four CFHTLS deep fields; these four separate fields allow us to make a robust estimate of the effect of cosmic variance for all our measurements. We use these catalogues in combination with ≈9800 spectroscopic redshifts to estimate precise photometric redshifts (σ Δz/(1+z) 0.03 at i < 25), galaxy types, star-formation rates and stellar masses for a unique sample of ≈1.8 million galaxies. Our JHK s number counts are consistent with previous studies. We apply the "BzK" selection to our gzK filter set and find that the star forming BzK selection successfully selects 76% of star-forming galaxies in the redshift range 1.4 < z < 2.5 in our photometric catalogue, based on our photometric redshift measurement. Similarly the passive BzK selection returns 52% of the passive 1.4 < z < 2.5 population identified in the photometric catalogue. We present the mass functions of the total galaxy population as a function of redshift up to z = 2 and present fits using double Schechter functions. A mass-dependent evolution of the mass function is seen with the numbers of galaxies with masses of M 10 10.75 still evolving at z 1, but galaxies of higher mass reaching their present day numbers by z ∼ 0.8−1. This is consistent with the present picture of downsizing in galaxy evolution. We compare our results with the predictions of the GALFORM semi-analytical galaxy formation model and find that the simulations provide a relatively successful fit to the observed mass functions at intermediate masses (i.e. 10 log (M/M ) 11). However, as is common with semi-analytical predictions of the mass function, the GALFORM results under-predict the mass function at low masses (i.e. log (M/M ) 10), whilst the fit as a whole degrades beyond redshifts of z ∼ 1.2. All photometric catalogues and images are made publicly available from TERAPIX and CADC.

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Section: Redshiftsupporting

confidence: 87%

“…Mullis et al 2005;Stanford et al 2005Stanford et al , 2006Stott et al 2010;Fassbender et al 2011). Such observations have acted to stimulate significant progress in our understanding of galaxy formation processes, in particular highlighting the importance of feedback processes in shaping the pace and form of the growth of galaxies.…”

Section: Introductionmentioning

confidence: 99%

The WIRCam Deep Survey

Bielby

Hudelot

McCracken

et al. 2012

A&A

171

208

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“…The amount of stellar mass already in place for these galaxies at this redshift is immense considering the short period of time that they have had to form their stellar content. These stellar masses approach those of z ∼ 1 BCGs (e.g., Stott et al 2010;Lidman et al 2012;Ascaso et al 2014), astounding considering these galaxies have ∼4 Gyr to evolve between the redshift of Cl J0227-0421 and that of z ∼ 1 cluster samples. The presence of these massive galaxies within Cl J0227-0421 appears, at least at the surface, to be consistent with the results of Diener et al (2013), in which an excess of massive galaxies was found within protocluster candidates in the COSMOS field at slightly lower redshifts (1.8 < z < 3.0) and in slightly less massive structures (σ v = 30−550 km s −1 ).…”

Section: The Density Of Massive Galaxies In CL J0227-0421mentioning

confidence: 66%

VIMOS Ultra-Deep Survey (VUDS): Witnessing the assembly of a massive cluster atz~ 3.3

Lemaux

Cucciati

Tasca

et al. 2014

A&A

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Using new spectroscopic observations obtained as part of the VIMOS Ultra-Deep Survey (VUDS), we performed a systematic search for overdense environments in the early universe (z > 2) and report here on the discovery of Cl J0227-0421, a massive protocluster at z = 3.29. This protocluster is characterized by both the large overdensity of spectroscopically confirmed members, δ gal = 10.5 ± 2.8, and a significant overdensity in photometric redshift members. The halo mass of this protocluster is estimated by a variety of methods to be ∼3 × 10 14 M at z ∼ 3.3, which, evolved to z = 0 results in a halo mass rivaling or exceeding that of the Coma cluster. The properties of 19 spectroscopically confirmed member galaxies are compared with a large sample of VUDS/VVDS galaxies in lower density field environments at similar redshifts. We find tentative evidence for an excess of redder, brighter, and more massive galaxies within the confines of the protocluster relative to the field population, which suggests that we may be observing the beginning of environmentally induced quenching. The properties of these galaxies are investigated, including a discussion of the brightest protocluster galaxy, which appears to be undergoing vigorous coeval nuclear and starburst activity. The remaining member galaxies appear to have characteristics that are largely similar to the field population. Though we find weaker evidence of the suppression of the median star formation rates among and differences in the stacked spectra of member galaxies with respect to the field, we defer any conclusions about these trends to future work with the ensemble of protostructures that are found in the full VUDS sample.

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“…Observed K-band magnitude of brightest-cluster galaxies (shown as "+") and radio galaxies (shown as "x") as a function of redshift (plot reproduced from Lidman et al 2012). Some of the data points were taken from Stott et al (2008Stott et al ( , 2010. The large red stars illustrate that TXS 2353−003 and NVSS J210626−314003 fall well within the expected range of K-band magnitude, and also have typical K-band magnitudes for HzRGs at their redshifts (black crosses; Seymour et al 2007; see also De Breuck et al 2002;Willott et al 2003;Bryant et al 2009).…”

Section: K−z Relationshipmentioning

confidence: 99%

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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THEXMMCLUSTER SURVEY: THE BUILD-UP OF STELLAR MASS IN BRIGHTEST CLUSTER GALAXIES AT HIGH REDSHIFT

Cited by 116 publications

References 94 publications

The WIRCam Deep Survey

The WIRCam Deep Survey

VIMOS Ultra-Deep Survey (VUDS): Witnessing the assembly of a massive cluster atz~ 3.3

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

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