Luminous red galaxies in clusters: central occupation, spatial distributions and miscentring

Hoshino, Hanako; Leauthaud, Alexie; Lackner, Claire; Hikage, Chiaki; Rozo, Eduardo; Rykoff, E. S.; Mandelbaum, Rachel; More, Surhud; More, Anupreeta; Saito, Shun; Vulcani, Benedetta

doi:10.1093/mnras/stv1271

Cited by 73 publications

(97 citation statements)

References 66 publications

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“…We found that the higher mass subcatalogue lacks a measurement of the pairwise kSZ signal, due to the high redshift range of the high-mass halos. Compared to the standard LRG criteria used in SDSS-I/II, the LowZ selection includes a bright magnitude cut, which excludes a significant number of low-redshift blue galaxies, but also excludes a fraction of bright galaxies in low-redshift massive clusters [46]. Figure 11 shows the redshift distribution of the lower halo mass, higher halo mass and total LowZ North CGC subcatalogues.…”

Section: E Mass Dependencementioning

confidence: 99%

Measurement of the pairwise kinematic Sunyaev-Zeldovich effect with Planck and BOSS data

Remazeilles

et al. 2018

Phys. Rev. D

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We present a new measurement of the kinetic Sunyaev-Zeldovich effect (kSZ) using Planck cosmic microwave background (CMB) and Baryon Oscillation Spectroscopic Survey (BOSS) data. Using the "LowZ North/South" galaxy catalogue from BOSS DR12, and the group catalogue from BOSS DR13, we evaluate the mean pairwise kSZ temperature associated with BOSS galaxies. We construct a "Central Galaxies Catalogue" (CGC) which consists of isolated galaxies from the original BOSS data set, and apply the aperture photometry (AP) filter to suppress the primary CMB contribution. By constructing a halo model to fit the pairwise kSZ function, we constrain the mean optical depth to beτ ¼ ð0.53 AE 0.32Þ × 10 −4 ð1.65σÞ for LowZ North CGC,τ ¼ ð0.30 AE 0.57Þ × 10 −4 ð0.53σÞ for LowZ South CGC, andτ ¼ ð0.43 AE 0.28Þ × 10 −4 ð1.53σÞ for DR13 Group. In addition, we vary the radius of the AP filter and find that the AP size of 7 arcmin gives the maximum detection forτ. We also investigate the dependence of the signal with halo mass and findτ ¼ ð0.32 AE 0.36Þ × 10 −4 ð0.8σÞ andτ ¼ ð0.67 AE 0.46Þ × 10 −4 ð1.4σÞ for DR13 Group with halo mass restricted to, respectively, less and greater than its median halo mass, 10 12 h −1 M ⊙ . For the LowZ North CGC sample restricted to M h ≳ 10 14 h −1 M ⊙ there is no detection of the kSZ signal because these high mass halos are associated with the high-redshift galaxies of the LowZ North catalogue, which have limited contribution to the pairwise kSZ signals.

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Section: E Mass Dependencementioning

confidence: 99%

Measurement of the pairwise kinematic Sunyaev-Zeldovich effect with Planck and BOSS data

Remazeilles

et al. 2018

Phys. Rev. D

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“…Using N-body simulations, Martel et al (2014) find that the fraction where the brightest galaxy is not the nearest to the centre increases from ∼25% to ∼50%, with a higher miscentring fraction towards higher mass. Hoshino et al (2015) study the distribution of LRGs in the redMaPPer clusters (Rykoff et al 2014) and find that 20-30% of the brightest LRGs are not the central galaxy. As the central galaxy might be somewhat offset from the peak of the dark matter, these results might be in agreement with our results.…”

Section: Miscentring Distributionmentioning

confidence: 99%

Weak-lensing-inferred scaling relations of galaxy clusters in the RCS2: mass-richness, mass-concentration, mass-bias, and more

Uitert

Gilbank

Hoekstra

et al. 2016

A&A

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We study a sample of ∼10 4 galaxy clusters in the redshift range 0.2 < z < 0.8 with masses M 200 > 5 × 10 13 h −1 70 M , discovered in the second Red-sequence Cluster Survey (RCS2). The depth and excellent image quality of the RCS2 enabled us to detect the cluster-mass cross-correlation up to z ∼ 0.7. To obtain cluster masses, concentrations, and halo biases, we fit a cluster halo model simultaneously to the lensing signal and to the projected density profile of red-sequence cluster members, because the latter provides tight constraints on the cluster miscentring distribution. We parametrised the mass-richness relation as 70 M and α = 0.73 ± 0.07 at low redshift (0.2 < z < 0.35). At intermediate redshift (0.35 < z < 0.55), we find a higher normalisation, which points towards a fractional increase in the richness towards lower redshift caused by the buildup of the red sequence. The miscentring distribution is well constrained. Only ∼30% of our BCGs coincide with the peak of the dark matter distribution. The distribution of the remaining BCGs are modelled with a 2D-Gaussian, whose width increases from 0.2 to 0.4 h −1 70 Mpc towards higher masses. The ratio of width and r 200 is constant with mass and has an average value of 0.44 ± 0.01. The mass-concentration and mass-bias relations agree fairly well with literature results at low redshift, but have a higher normalisation at higher redshifts, possibly because of selection and projection effects. The concentration of the satellite distribution decreases with mass and is correlated to the concentration of the halo.

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“…Contrary to what the name suggests, a BCG is in our adopted definition not necessarily the brightest galaxy in a cluster -it must also lie close to the cluster center as traced by the satellite galaxy distribution and/or the intracluster medium. Between 20% and 40% of central galaxies are not the brightest galaxy in their host clusters (Skibba et al 2011;Hoshino et al 2015). A famous example is M87 in the Virgo cluster.…”

Section: Introductionmentioning

confidence: 99%

Structure of Brightest Cluster Galaxies and Intracluster Light

Kluge

Neureiter

Riffeser

et al. 2020

ApJS

120

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Observations of 170 local (z 0.08) galaxy clusters in the northern hemisphere have been obtained with the Wendelstein Telescope Wide Field Imager (WWFI). We correct for systematic effects such as PSF broadening, foreground stars contamination, relative bias offsets and charge persistence. Scattered light induced background inhomogeneities are reduced down to ∆SB > 31 g' mag arcsec −2 by large dithering and subtraction of night-sky flats. Residual background inhomogeneities brighter than SB σ < 27.6 g' mag arcsec −2 caused by galactic cirrus are detected in front of 23% of the clusters. However, the large field of view allows to discriminate between accretion signatures and galactic cirrus. We detect accretion signatures in form of tidal streams in 22%, shells in 9.4%, multiple nuclei in 47% and two Brightest Cluster Galaxies (BCGs) in 7% of the clusters / BCGs.We measure semi-major axis surface brightness profiles of the BCGs and their surrounding Intracluster Light (ICL) down to a limiting surface brightness of SB = 30 g' mag arcsec −2 . The spatial resolution in the inner regions is increased by combining the WWFI light profiles with those that we measured from archival Hubble Space Telescope images or deconvolved WWFI images. We find that 71% of the BCG+ICL systems have SB profiles that are well described by a single Sérsic (SS) function whereas 29% require a double Sérsic (DS) function to obtain a good fit. SS BCGs, having more symmetric isophotal shapes and fewer detected accretion signatures than DS BCGs, appear to have slightly more relaxed morphology than their DS counterparts. Members of the latter type encompass S2 = 52 ± 21% of their total light in the outer Sérsic component. There is a wide scatter in transition radii r × between the two Sérsic components and surface brightnesses at the transition radii SB(r × ). The integrated brightnesses of the BCG+ICL systems correlate only weakly with S2, r × and SB(r × ). That indicates that the outer Sérsic component is unlikely to trace the dynamically hot ICL since BCG+ICL systems grow at present epoch predominantly in their outskirts.We find that BCGs have scaling relations that differ markedly from those of normal ellipticals, likely due to their indistinguishable embedding in the ICL. The most extended BCG+ICL systems have luminosities and radii comparable to whole clusters. We use different plausible estimates for the ICL component (based on an integrated brightness threshold, SB thresholds and profile decompositions) and find that they do not affect our conclusions about the properties of the ICL. On average, the ICL seems to be better aligned than the BCG with the host cluster in terms of position angle and centering. That makes it a potential Dark Matter tracer. We find positive correlations between BCG+ICL brightness and cluster mass, cluster radius, cluster richness and integrated satellite brightness, confirming that BCG/ICL growth is indeed coupled with cluster growth.

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Luminous red galaxies in clusters: central occupation, spatial distributions and miscentring

Cited by 73 publications

References 66 publications

Measurement of the pairwise kinematic Sunyaev-Zeldovich effect with Planck and BOSS data

Measurement of the pairwise kinematic Sunyaev-Zeldovich effect with Planck and BOSS data

Weak-lensing-inferred scaling relations of galaxy clusters in the RCS2: mass-richness, mass-concentration, mass-bias, and more

Structure of Brightest Cluster Galaxies and Intracluster Light

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