VLT and ACS Observations of RDCS J1252.9−2927: Dynamical Structure and Galaxy Populations in a Massive Cluster at<i>z</i>= 1.237

Demarco, R.; Rosati, P.; Lidman, C.; Girardi, M.; Nonino, M.; Rettura, Alessandro; Strazzullo, V.; Wel, Arjen van der; Ford, H. C.; Mainieri, V.; Holden, B.; Stanford, S. A.; Blakeslee, John P.; Gobat, R.; Postman, Marc; Tozzi, P.; Overzier, Roderik; Zirm, A.; Benítez, N.; Homeier, N.; Illingworth, G. D.; Infante, L.; Jee, M. James; Mei, S.; Menanteau, F.; Motta, V.; Zheng, Wei; Clampin, M.; Hartig, G.

doi:10.1086/518117

Cited by 56 publications

(107 citation statements)

References 111 publications

(192 reference statements)

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“…Similar conclusions are reached for the early-type galaxies in J1252 from two studies of the colour-magnitude relation, which both suggest z f = 2.7 − 3.6 with subsequent passive evolution 14,58,59 . We conclude that since observations suggest Z ≥ 1.0 Z ⊙ and z f ≥ 3.0, our central result of negligible stellar mass evolution is not seriously compromised by the age and metallicity caveats and remains significant for the most plausible stellar evolution histories of these galaxies.…”

Section: Stability Of Bcg Mass Estimatessupporting

confidence: 77%

“…2. The k-correction is well understood over the wavelength range appropriate to our sample (0.9 − 2.2 µm) introducing an uncertainty of about 10% in the rest-frame The cluster X-ray luminosities are bolometric estimates taken from the literature and the cluster The photometry for J1252 and J0849 were sourced from the literature 14,21 and for these galaxies the total K s magnitudes and J − K s colours were measured in similar aperture sizes. All data have been analysed in an identical manner for direct comparison (see Supplementary Information).…”

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confidence: 99%

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Early assembly of the most massive galaxies

Collins

Stott

Hilton

et al. 2009

Nature

164

175

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The current consensus is that galaxies begin as small density fluctuations in the early Universe and grow by in situ star formation and hierarchical merging 1 . Stars begin to form relatively quickly in sub-galactic sized building blocks called haloes which are subsequently assembled into galaxies. However, exactly when this assembly takes place is a matter of some debate 2, 3 . Here we report that the stellar masses of brightest cluster galaxies, which are the most luminous objects emitting stellar light, some 9 billion years ago are not significantly different from their stellar masses today. Brightest cluster galaxies are almost fully assembled 4 − 5 Gyrs after the Big Bang, having 2 grown to more than 90% of their final stellar mass by this time. Our data conflict with the most recent galaxy formation models 4, 5 based on the largest simulations of dark matter halo development 1 . These models predict protracted formation of brightest cluster galaxies over a Hubble time, with only 22% of the stellar mass assembled at the epoch probed by our sample. Our findings suggest a new picture in which brightest cluster galaxies experience an early period of rapid growth rather than prolonged hierarchical assembly.Brightest cluster galaxies (BCGs) are located at the centres of galaxy clusters. They constitute a separate population from bright elliptical galaxies 6 and both their homogeneity and extreme luminosity have motivated their use as standard candles for cosmology 7-9 .Our investigation focuses on BCGs in the most distant X-ray emitting galaxy clusters at redshifts z = 1.2 −1.5, where (1 + z) is the expansion factor of the Universe relative to the present. It has been shown that X-ray cluster selection is currently the optimum strategy for an unbiased investigation of BCG evolution 10 . Properties of our BCGs and their host clusters are listed in Table 1. All five clusters were discovered serendipitously in X-rays and they are the most distant clusters discovered in their respective X-ray surveys 11-15 .The cluster J2215 was discovered as part of the XMM Cluster Survey (XCS 16,17 ) and has the highest redshift of any spectroscopically confirmed cluster 12,18 . 3The stellar mass of a BCG depends upon the hierarchical build up of its host dark matter halo and its stellar evolution history, along with the baryonic physics of the galaxy.We base our study of BCGs on photometry in the infrared wavebands J (1.26 µm) and K s (2.14 µm). Infrared imaging is essential at these large redshifts to compensate for the redshifting of the early-type galaxy spectra. Also, these wavebands are less sensitive than optical light to the presence of young stars and are a more accurate tracer of the underlying old stellar population and, hence, of the stellar mass of the systems. Fig. 1 shows an infrared image of the cluster J2235 from our sample (see also Supplementary Fig. 1).We start by examining the ages of the stars themselves in these galaxies using the run of J − K s colour evolution with redshift as shown in Fig. 2. For BCGs at ...

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Section: Stability Of Bcg Mass Estimatessupporting

confidence: 77%

mentioning

confidence: 99%

Early assembly of the most massive galaxies

Collins

Stott

Hilton

et al. 2009

Nature

164

175

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“…such red galaxies might indeed be found in clusters in reality, though the large spread in the observations makes this unclear. Demarco et al (2007) presented spectroscopy for the cluster of Strazzullo et al (2006) and measured [O II] emission lines in 38 cluster members. They estimated that the SFRs of those galaxies are in the range 0.5-2 M yr −1 , with the median SFR being ≈0.7 M yr −1 .…”

Section: Trends In Galaxy Propertiesmentioning

confidence: 99%

The abundance and colours of galaxies in high-redshift clusters in the cold dark matter cosmology

Merson¹,

Baugh²,

González-Pérez³

et al. 2015

Mon. Not. R. Astron. Soc.

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High redshift galaxy clusters allow us to examine galaxy formation in extreme environments.Here we compile data for 15 z > 1 galaxy clusters to test the predictions from a state-of-theart semi-analytical model of galaxy formation. The model gives a good match to the slope and zero-point of the cluster red sequence. The model is able to match the cluster galaxy luminosity function at faint and bright magnitudes, but under-estimates the number of galaxies around the break in the cluster luminosity function. We find that simply assuming a weaker dust attenuation improves the model predictions for the cluster galaxy luminosity function, but worsens the predictions for the red sequence at bright magnitudes. Examination of the properties of the bright cluster galaxies suggests that the default dust attenuation is large due to these galaxies having large reservoirs of cold gas as well as small radii. We find that matching the luminosity function and colours of high redshift cluster galaxies, whilst remaining consistent with local observations, poses a challenge for galaxy formation models.

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“…Results for eight z ∼ 1 clusters observed as part of the ACS intermediate redshift cluster survey (Blakeslee et al 2003a;Mei et al 2007;Holden et al 2005;Mei et al 2009, and references therein), and studies of individual distant clusters (RDCS 1252.9-2927 at z = 1.235: Lidman et al 2004;Demarco et al 2007; XMMU J2235.3-2557 at z = 1.393: Rosati et al 2009;Lidman et al 2008; XMMXCS J2215.9-1738 at z = 1.45, Stanford et al 2006) illustrate the prevalence of a tight RS up to z = 1.4, where the CMR slope and scatter are observed to have a negligible increase with redshift.…”

Section: Article Published By Edp Sciencesmentioning

confidence: 99%

Multiwavelength observations of a rich galaxy cluster at z $\thicksim$ 1

Santos

Rosati

Gobat

et al. 2009

A&A

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Context. XMMU J1229+0151 is a rich galaxy cluster with redshift z = 0.975 that was serendipitously detected in X-rays within the scope of the XMM-Newton Distant Cluster Project. Both HST/ACS observations in the i 775 and z 850 passbands and VLT/FORS2 spectroscopy were obtained, in addition to follow-up Near-Infrared (NIR) imaging in the J-and Ks-bands with NTT/SOFI. Aims. We investigate the photometric, structural, and spectral properties of the early-type galaxies in the high-redshift cluster XMMU J1229+0151. Methods. Source detection and aperture photometry are performed in the optical and NIR imaging. Galaxy morphology is inspected visually and by means of Sersic profile fitting to the 21 spectroscopically confirmed cluster members in the ACS field of view. The i 775 − z 850 colour−magnitude relation (CMR) is derived with a method based on galaxy magnitudes obtained by fitting the surface brightness of the galaxies with Sersic models. Stellar masses and formation ages of the cluster galaxies are derived by fitting the observed spectral energy distributions (SED) with models developed by Bruzual & Charlot. Star-formation histories of the early-type galaxies are constrained by analysing the stacked spectrophotometric data. Results. The structural Sersic index n obtained by model fitting agrees with the visual morphological classification of the confirmed members, indicating a clear predominance of elliptical galaxies (15/21). The i 775 − z 850 colour−magnitude relation of the spectroscopic members shows a very tight red-sequence with a zero point of 0.86 ± 0.04 mag, and intrinsic scatter equal to 0.039 mag. The CMR obtained with the galaxy models has similar parameters. By fitting both the spectra and SED of the early-type population, we obtain a star-formation-weighted age of 4.3 Gyr for a median galaxy stellar-mass of 7.4 × 10 10 M . Instead of identifying a brightest cluster galaxy (BCG) unambiguously, we find three bright galaxies with a similar z 850 magnitude, which are, in addition, the most massive cluster members, with ∼2 × 10 11 M . Our results strengthen the current evidence of a lack of significant evolution in both the scatter and slope of the red-sequence out to z ∼ 1.

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VLT and ACS Observations of RDCS J1252.9−2927: Dynamical Structure and Galaxy Populations in a Massive Cluster atz= 1.237

Cited by 56 publications

References 111 publications

Early assembly of the most massive galaxies

Early assembly of the most massive galaxies

The abundance and colours of galaxies in high-redshift clusters in the cold dark matter cosmology

Multiwavelength observations of a rich galaxy cluster at z $\thicksim$ 1

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