The Observed Evolution of the Stellar Mass - Halo Mass Relation for Brightest Central Galaxies

Golden-Marx, Jesse B.; Miller, C. J.; Zhang, Y.; Ogando, R. L. C.; Palmese, A.; Abbott, T. M. C.; Aguena, M.; Allam, S.; Andrade-Oliveira, F.; Annis, J.; Bacon, D.; Bertin, E.; Brooks, D.; Buckley-Geer, E.; Rosell, A. Carnero; Kind, M. Carrasco; Castander, F. J.; Constanzi, M.; Crocce, M.; da Costa, L. N.; Pereira, M. E. S.; de Vicente, J.; Desai, S.; Diehl, H. T.; Doel, P.; Drlica-Wagner, A.; Everett, S.; Evrard, A. E.; Ferrero, I.; Flaugher, B.; Fosalba, P.; Frieman, J.; Garcia-Bellido, J.; Gaztanaga, E.; Gerdes, D. W.; Gruen, D.; Gruendl, R. A.; Gschwend, J.; Gutierrez, G.; Hartley, W. G.; Hinton, S. R.; Hollowood, D. L.; Honscheid, K.; Hoyle, B.; James, D. J.; Jeltema, T.; Kim, A. G.; Krause, E.; Kuehn, K.; Kuropatkin, N.; Lahav, O.; Lima, M.; Maia, M. A. G.; Marshall, J. L.; Melchior, P.; Menanteau, F.; Miquel, R.; Mohr, J. J.; Morgan, R.; Paz-Chinchon, F.; Petravick, D.; Pieres, A.; Malagon, A. A. Plazas; Prat, J.; Romer, A. K.; Sanchez, E.; Santiago, B.; Scarpine, V.; Schubnell, M.; Serrano, S.; Sevilla-Noarbe, I.; Smith, M.; Soares-Santos, M.; Suchyta, E.; Tarle, G.; Varga, T. N.

doi:10.48550/arxiv.2107.02197

Cited by 5 publications

(4 citation statements)

References 62 publications

(107 reference statements)

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“…Comparison between the BCG and cluster mass tests the co-evolution of a cluster and its BCG (e.g., Lin & Mohr 2004;Oliva-Altamirano et al 2014;Lin et al 2017;Kravtsov et al 2018;Wen & Han 2018;Erfanianfar et al jubee.sohn@cfa.harvard.edu 2019; Golden-Marx et al 2021). Many studies derive the ratio between the stellar mass of a central galaxy and its host halo mass.…”

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confidence: 99%

Co-evolution of the Brightest Cluster Galaxies and their Host Clusters in IllustrisTNG

Sohn,

Geller,

Vogelsberger

et al. 2022

Preprint

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We use the Illustris-TNG simulations to explore the dynamic scaling relation between massive clusters and their central galaxies (BCGs). The Illustris TNG300-1 simulation we use includes 280 massive clusters with M 200 > 10 14 M enabling a robust statistical analysis. We derive the line-of-sight velocity dispersion of the stellar particles of the BCGs (σ * ,BCG ), analogous to the observed BCG stellar velocity dispersion. We also compute the subhalo velocity dispersion to measure the cluster velocity dispersion (σ cl ). Both σ * ,BCG and σ cl are proportional to the cluster halo mass, but the slopes differ slightly. Thus like the observed relation, σ * ,BCG /σ cl declines as a function of σ cl , but the scatter is large. We explore the redshift evolution of σ * ,BCG − σ cl scaling relation for z 1 in a way that can be compared directly with observations. The scaling relation has a similar slope at high redshift, but the scatter increases because of the large scatter in σ * ,BCG . The simulations imply that high redshift BCGs are dynamically more complex than their low redshift counterparts.

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confidence: 99%

Co-evolution of the Brightest Cluster Galaxies and their Host Clusters in IllustrisTNG

Sohn,

Geller,

Vogelsberger

et al. 2022

Preprint

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“…In order for dry mergers to drive a correlated scatter between BCG stellar mass and satellite richness, the merger-induced stellar growth should be significant, e.g., comparable with the intrinsic scatter in the cluster SHMR of ∼0.05−0.1 dex (Golden-Marx et al 2021). Observationally, the stellar growth from dry mergers since 𝑧∼1 varies between 30% (Collins et al 2009;Bundy et al 2017;Lin et al 2017) and almost a factor of two (Whiley et al 2008;Burke & Collins 2013;Lidman et al 2013).…”

Section: Could Dry Mergers Drive the Strong Bcg-satellitementioning

confidence: 98%

Strong Conformity and Assembly Bias: Towards a Physical Understanding of the Galaxy-Halo Connection in SDSS Clusters

Zu,

Song,

Shao

et al. 2021

Preprint

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Understanding the physical connection between cluster galaxies and massive haloes is key to mitigating systematic uncertainties in next-generation cluster cosmology. We develop a novel method to infer the level of conformity between the stellar mass of the brightest central galaxies (BCGs) 𝑀 BCG * and the satellite richness 𝜆, defined as their correlation coefficient 𝜌 cc at fixed halo mass, using the abundance and weak lensing of SDSS clusters as functions of 𝑀 BCG * and 𝜆. We detect a halo mass-dependent conformity as 𝜌 cc =0.60+0.08 ln(𝑀 ℎ /3×10 14 ℎ −1 𝑀 ). The strong conformity successfully resolves the "halo mass equality" conundrum discovered in Zu et al. ( 2021) -when split by 𝑀 BCG * at fixed 𝜆, the low and high-𝑀 BCG * clusters have the same average halo mass despite having a 0.34 dex discrepancy in average 𝑀 BCG * . On top of the best-fitting conformity model, we develop a cluster assembly bias (AB) prescription calibrated against the CosmicGrowth simulation, and build a conformity+AB model for the cluster weak lensing measurements. Our model predicts that with a ∼20% lower halo concentration 𝑐, the low-𝑀 BCG * clusters are ∼10% more biased than the high-𝑀 BCG * systems, in excellent agreement with the observations. We also show that the observed conformity and assembly bias are unlikely due to projection effects. Finally, we build a toy model to argue that while the earlytime BCG-halo co-evolution drives the 𝑀 BCG * -𝑐 correlation, the late-time dry merger-induced BCG growth naturally produces the 𝑀 BCG * -𝜆 conformity despite the well-known anti-correlation between 𝜆 and 𝑐. Our method paves the path towards simultaneously constraining cosmology and cluster formation with future cluster surveys.

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“…Naively, we would expect different shape measurement methods to be more consistent with one another for the most relaxed clusters, which have a minimum of massive substructures (Lauer et al 2014;Golden-Marx et al 2021). As a proxy for this in projected stellar density space, we checked whether a stricter cut on the centroid offset would further improve the correlation illustrated in the blue lines in Figure 5.…”

Section: An Optical Relaxation Selection: Minδ𝑥 8096mentioning

confidence: 99%

Brightest cluster galaxies trace weak lensing mass bias and halo triaxiality in the three hundred project

Herbonnet

Crawford

Avestruz

et al. 2022

Monthly Notices of the Royal Astronomical Society

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Galaxy clusters have a triaxial matter distribution. The weak-lensing signal, an important part in cosmological studies, measures the projected mass of all matter along the line-of-sight, and therefore changes with the orientation of the cluster. Studies suggest that the shape of the brightest cluster galaxy (BCG) in the centre of the cluster traces the underlying halo shape, enabling a method to account for projection effects. We use 324 simulated clusters at four redshifts between 0.1 and 0.6 from ‘The Three Hundred Project’ to quantify correlations between the orientation and shape of the BCG and the halo. We find that haloes and their embedded BCGs are aligned, with an average ∼20 degree angle between their major axes. The bias in weak lensing cluster mass estimates correlates with the orientation of both the halo and the BCG. Mimicking observations, we compute the projected shape of the BCG, as a measure of the BCG orientation, and find that it is most strongly correlated to the weak-lensing mass for relaxed clusters. We also test a 2-dimensional cluster relaxation proxy measured from BCG mass isocontours. The concentration of stellar mass in the projected BCG core compared to the total stellar mass provides an alternative proxy for the BCG orientation. We find that the concentration does not correlate to the weak-lensing mass bias, but does correlate with the true halo mass. These results indicate that the BCG shape and orientation for large samples of relaxed clusters can provide information to improve weak-lensing mass estimates.

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The Observed Evolution of the Stellar Mass - Halo Mass Relation for Brightest Central Galaxies

Cited by 5 publications

References 62 publications

Co-evolution of the Brightest Cluster Galaxies and their Host Clusters in IllustrisTNG

Co-evolution of the Brightest Cluster Galaxies and their Host Clusters in IllustrisTNG

Strong Conformity and Assembly Bias: Towards a Physical Understanding of the Galaxy-Halo Connection in SDSS Clusters

Brightest cluster galaxies trace weak lensing mass bias and halo triaxiality in the three hundred project

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