Resurrecting the red from the dead: optical properties of BCGs in X-ray luminous clusters★

Bildfell, C.; Hoekstra, Henk; Babul, Arif; Mahdavi, Andisheh

doi:10.1111/j.1365-2966.2008.13699.x

Cited by 163 publications

(312 citation statements)

References 61 publications

(85 reference statements)

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“…A common prediction is that gas cooling from the intra-cluster medium may be forming stars which will result in young ages (e.g. Edwards et al 2007;O'Dea et al 2008;Bildfell et al 2008;Loubser 2014). For most of the clusters considered here, X-ray imaging is not available, so that we cannot assess whether they host a cool core or not.…”

Section: Stellar Agesmentioning

confidence: 99%

The accretion histories of brightest cluster galaxies from their stellar population gradients

Oliva-Altamirano

Brough

Jimmy

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We analyse the spatially-resolved stellar populations of 9 local (z < 0.1) Brightest Cluster Galaxies (BCGs) observed with VIMOS in IFU mode. Our sample is composed of 7 slowrotating and 2 fast-rotating BCGs. We do not find a connection between stellar kinematics and stellar populations in this small sample. The BCGs have shallow metallicity gradients (medianand a wide range of central ages (from 5 to 15 Gyr). We propose that the reason for this is diverse evolutionary paths in BCGs. 67 per cent of the sample (6/9) show ∼ 7 Gyr old central ages, which reflects an active accretion history, and 33 per cent of the sample (3/9) have central ages older than 11 Gyr, which suggest no star formation since z = 2. The BCGs show similar central stellar populations and stellar population gradients to early-type galaxies of similar mass (M dyn > 10 11.3 M ) from the ATLAS 3D survey (median [Z/H] = 0.04 ± 0.07, ∆[Z/H] = −0.19 ± 0.1). However, massive early-type galaxies from ATLAS 3D have consistently old ages (median Age = 12.0 ± 3.8 Gyr). We also analyse the close massive companion galaxies of two of the BCGs. These galaxies have similar stellar populations to their respective BCGs.

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Section: Stellar Agesmentioning

confidence: 99%

The accretion histories of brightest cluster galaxies from their stellar population gradients

Oliva-Altamirano

Brough

Jimmy

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…A residual star formation at low redhshift seems quite common in Brightest Cluster Galaxies (BGCs) hosted in cool-core clusters (Hicks & Mushotzky 2005;O'Dea et al 2008;Bildfell et al 2008). Using the Bildfell et al (2008) sample, Pipino et al (2008b) demonstrate, for the first time, a one-to-one correspondence between blue cores in elliptical galaxies and a UVenhancement observed using GALEX.…”

Section: Introductionmentioning

confidence: 98%

“…Using the Bildfell et al (2008) sample, Pipino et al (2008b) demonstrate, for the first time, a one-to-one correspondence between blue cores in elliptical galaxies and a UVenhancement observed using GALEX. However, only a small fraction of elliptical galaxies shows current star formation.…”

Section: Introductionmentioning

confidence: 99%

Cosmological formation and chemical evolution of an elliptical galaxy

Colavitti

Pipino

Matteuccí

2009

A&A

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Aims. We aim to study the effect of a cosmologically motivated gas infall law for the formation of a massive elliptical galaxy in order to understand its impact on the formation of spheroids. Methods. We replace the empirical infall law of the model by Pipino & Matteucci with a cosmologically derived infall law for the formation of an elliptical galaxy. We compare our predictions with observations. We also compare the obtained results with those of Pipino & Matteucci.Results. We computed models with and without galactic winds; we found that models without wind predict a too large current SNIa rate. In particular, the cosmological model produces a current SNIa value which is about ten times higher than the observed values. Moreover models without wind predict a high current SNII rate, too large even if compared with the recent GALEX data. The predicted SNII rate for the model with wind, on the other hand, is too low if compared with the star formation histories given by GALEX. The mean value for the [Mg/Fe] ratio in the dominant stellar population of the simulated galaxy, as predicted by the cosmological model, is too low if compared to observations. This is a very important result indicating that the cosmological infall law is in contradiction to the chemical evolution. Conclusions. A cosmologically derived infall law for an elliptical galaxy cannot reproduce all the chemical constraints given by observations. The problem resides in the fact that the cosmologically derived infall law implies a slow gas accretion with a consequent star formation rate active for a long period. In this situation low [Mg/Fe] ratios are produced for the dominant stellar population in a typical elliptical, at variance with observations.

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“…Although the trend is visible in each morphological sub-sample, the most extreme deviations occur in the intermediate and disturbed systems, which all have the largest offsets between X-ray and BCG positions. This is a well-known characteristic of the observed cluster population (e.g., Bildfell et al 2008;Sanderson et al 2009;Haarsma et al 2010). We tested the effect of using a different centre on the X-ray mass for two systems.…”

Section: Centre Offsetsmentioning

confidence: 99%

Planckintermediate results

Ade¹,

Aghanim²,

Arnaud³

et al. 2013

A&A

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We examine the relation between the galaxy cluster mass M and Sunyaev-Zeldovich (SZ) effect signal D 2 A Y 500 for a sample of 19 objects for which weak lensing (WL) mass measurements obtained from Subaru Telescope data are available in the literature. Hydrostatic X-ray masses are derived from XMM-Newton archive data, and the SZ effect signal is measured from Planck all-sky survey data. We find an M WL −D 2 A Y 500 relation that is consistent in slope and normalisation with previous determinations using weak lensing masses; however, there is a normalisation offset with respect to previous measures based on hydrostatic X-ray mass-proxy relations. We verify that our SZ effect measurements are in excellent agreement with previous determinations from Planck data. For the present sample, the hydrostatic X-ray masses at R 500 are on average ∼20 percent larger than the corresponding weak lensing masses, which is contrary to expectations. We show that the mass discrepancy is driven by a difference in mass concentration as measured by the two methods and, for the present sample, that the mass discrepancy and difference in mass concentration are especially large for disturbed systems. The mass discrepancy is also linked to the offset in centres used by the X-ray and weak lensing analyses, which again is most important in disturbed systems. We outline several approaches that are needed to help achieve convergence in cluster mass measurement with X-ray and weak lensing observations.

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Resurrecting the red from the dead: optical properties of BCGs in X-ray luminous clusters★

Cited by 163 publications

References 61 publications

The accretion histories of brightest cluster galaxies from their stellar population gradients

The accretion histories of brightest cluster galaxies from their stellar population gradients

Cosmological formation and chemical evolution of an elliptical galaxy

Planckintermediate results

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