Abstract:We present the results of a Spitzer/Herschel infrared photometric analysis of the largest (716) and highest-redshift (z = 1.8) sample of Brightest Cluster Galaxies (BCGs), those from the Spitzer Adaptation of the Red-Sequence Cluster Survey (SpARCS). Given the tension that exists between model predictions and recent observations of BCGs at z < 2, we aim to uncover the dominant physical mechanism(s) guiding the stellar mass buildup of this special class of galaxies, the most massive in the Universe and uniquely… Show more
“…Optical and near-infrared data show that the color evolution of BCGs is in good agreement with a passive population synthesis model (Stott et al 2008;Whiley et al 2008;Wen & Han 2011). However, several studies show signatures of ongoing star formation or active galactic nuclei (AGN) in some BCGs (Crawford et al 1999;McNamara et al 2006;Liu et al 2012;Fraser-McKelvie et al 2014;Green et al 2016;Donahue et al 2017;Bonaventura et al 2017). Previously, we found that richer clusters host more luminous BCGs at redshifts z < 0.42 (Wen et al 2012).…”
We identify a sample of 1959 massive clusters of galaxies in the redshift range of 0.7 < z < 1.0 from the survey data of Sloan Digital Sky Survey (SDSS) and Wide-field Infrared Survey Explorer (WISE). These clusters are recognized as the overdensity regions around the SDSS luminous red galaxies, having a richness greater than 15 or an equivalent mass M 500 ≥ 2.5 × 10 14 M ⊙ . Among them, 1505 clusters are identified for the first time, which significantly enlarge the number of high-redshift clusters of z > 0.75. By comparing them with clusters at lower redshifts, we confirm that richer clusters host more luminous brightest cluster galaxies (BCGs) also at high redshifts, and that the fraction of blue galaxies is larger in clusters at higher redshifts. A small fraction of BCGs show ongoing star formation or active nuclei. The number density profile of member galaxies in stacked samples of clusters shows no significant redshift evolution.
“…Optical and near-infrared data show that the color evolution of BCGs is in good agreement with a passive population synthesis model (Stott et al 2008;Whiley et al 2008;Wen & Han 2011). However, several studies show signatures of ongoing star formation or active galactic nuclei (AGN) in some BCGs (Crawford et al 1999;McNamara et al 2006;Liu et al 2012;Fraser-McKelvie et al 2014;Green et al 2016;Donahue et al 2017;Bonaventura et al 2017). Previously, we found that richer clusters host more luminous BCGs at redshifts z < 0.42 (Wen et al 2012).…”
We identify a sample of 1959 massive clusters of galaxies in the redshift range of 0.7 < z < 1.0 from the survey data of Sloan Digital Sky Survey (SDSS) and Wide-field Infrared Survey Explorer (WISE). These clusters are recognized as the overdensity regions around the SDSS luminous red galaxies, having a richness greater than 15 or an equivalent mass M 500 ≥ 2.5 × 10 14 M ⊙ . Among them, 1505 clusters are identified for the first time, which significantly enlarge the number of high-redshift clusters of z > 0.75. By comparing them with clusters at lower redshifts, we confirm that richer clusters host more luminous brightest cluster galaxies (BCGs) also at high redshifts, and that the fraction of blue galaxies is larger in clusters at higher redshifts. A small fraction of BCGs show ongoing star formation or active nuclei. The number density profile of member galaxies in stacked samples of clusters shows no significant redshift evolution.
“…For the purposes of our analysis here we do not focus on the ICM or BCG evolution during this merger, which is still ongoing at z = 0, but analysis of the impact of this event will be the focus of future work. The star formation history of the BCG is remarkably similar to the median sSFR values presented in Bonaventura et al (2017), which are derived from IR detections of clusters. The McDonald et al (2016) results use multiple methods to estimate star formation at various wavelengths, but find that cool core clusters have systematically higher SFRs compared to their overall sample, which could explain why RomulusC, which maintains a cool core until z ∼ 0.2, would also have comparatively more star formation.…”
Section: The Connection Between Agn Feedback and Bcg Quenchingsupporting
confidence: 75%
“…The peak of activity beginning around 8 Gyr and persisting through 10 Gyr is associated with the final quenching of the BCG. The sSFR history of the RomulusC BCG is remarkably close to the average evolution observed in clusters fromBonaventura et al (2017), but slightly high compared to results fromMcDonald et al (2016). The range in time shown is cut off just prior to the infall of the group seen inFigure 7.…”
“…However, the predicted growth seems to be somewhat larger than observed. This possible tension could be worsened by recent claims, based on FIR data, that BCGs exhibit a star formation activity at z 1 more significant than previously thought, and thus contributing in a non-negligible way to their late mass growth (Bonaventura et al 2017).…”
We analyze the stellar growth of Brightest Cluster Galaxies (BCGs) produced by cosmological zoom-in hydrodynamical simulations of the formation of massive galaxy clusters. The evolution of the stellar mass content is studied considering different apertures, and tracking backwards either the main progenitor of the z = 0 BCG or that of the cluster hosting the BCG at z = 0. Both methods lead to similar results up to z ≃ 1.5. The simulated BCGs masses at z = 0 are in agreement with recent observations. In the redshift interval from z = 1 to z = 0 we find growth factors 1.3, 1.6 and 3.6 for stellar masses within 30kpc, 50kpc and 10% of R 500 respectively. The first two factors, and in general the mass evolution in this redshift range, are in agreement with most recent observations. The last larger factor is similar to the growth factor obtained by a semi-analytical model (SAM). Half of the star particles that end up in the inner 50 kpc was typically formed by redshift ∼ 3.7, while the assembly of half of the BCGs stellar mass occurs on average at lower redshifts ∼ 1.5. This assembly redshift correlates with the mass attained by the cluster at high z 1.3, due to the broader range of the progenitor clusters at high-z. The assembly redshift of BCGs decreases with increasing apertures. Our results are compatible with the insideout scenario. Simulated BCGs could lack intense enough star formation (SF) at high redshift, while possibly exhibit an excess of residual SF at low redshift.
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