Do satellite galaxies trace matter in galaxy clusters?

Wang, Chunxiang; Li, Ran; Gao, Liang; Shan, Huanyuan; Kneib, Jean-Paul; Wang, Wenting; Chen, Gang; Makler, M.; Pereira, M. E. S.; Wang, Lin; Maia, M. A. G.; Erben, T.

doi:10.1093/mnras/sty073

Cited by 11 publications

(7 citation statements)

References 57 publications

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“…The nearly flat profiles indicate the radial distribution of satellites tend to trace the distribution of dark matter, in good agreement with previous studies (e.g. Wang et al 2018). In Figure 12, blue massive and red low-mass ICGs tend to have noisy measurements, which is due to the small number of galaxies with corresponding colors in these bins.…”

Section: Radial Dependence Of the Total Stellar Mass Fractionsupporting

confidence: 91%

“…Theoretically, it is expected that the spatial distribution of satellites largely follow dark matter in simulations (e.g., Gao et al 2004;Han et al 2016;Green et al 2021). At low and intermediate redshifts (z < 0.4), Wang et al (2018) reported that the projected density profiles of satellites and dark matter have similar shapes, both can be well fit by the NFW profile (Navarro et al 1996(Navarro et al , 1997. On small scales, a few authors found that satellite profiles are steeper than the NFW profile (e.g.…”

Section: Introductionmentioning

confidence: 97%

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The stellar mass in and around isolated central galaxies: connections to the total mass distribution through galaxy-galaxy lensing in the Hyper Suprime-Cam survey

Wang,

Li,

Shi

et al. 2021

Preprint

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Using photometric galaxies from the Hyper Suprime-Cam (HSC) imaging survey, we measure the stellar mass density profiles for satellite galaxies as a function of the projected distance, r p , to isolated central galaxies (ICGs) selected from SDSS/DR7 spectroscopic galaxies at z ∼ 0.1. By stacking HSC images and using Gaussian Process Regression to recover the stellar mass from the PSF-deconvolved color profiles, we also measure the projected stellar mass density profiles for ICGs and their stellar halos. The total mass distributions are further measured from HSC weak lensing signals. ICGs dominate within ∼0.15 times the halo virial radius (0.15R 200 ). The stellar mass versus total mass fractions drop with the increase in r p up to ∼ 0.15R 200 , beyond which the fractions are less than 1% while stay almost constant, indicating the radial distribution of satellites trace dark matter. The integrated stellar mass locked in satellites is proportional to the virial mass of the host halo, M 200 , for ICGs more massive than 10 10.5 M , i.e., M * ,sat ∝ M 200 , whereas the scaling relation between the stellar mass of ICGs + stellar halos and M 200 is close to M * ,ICG+diffuse ∝ M 1/2 200 . Below 10 10.5 M , the change in M 200 is much slower with the decrease in M * ,ICG+diffuse . At fixed stellar mass, red ICGs are hosted by more massive dark matter halos and have more satellites. Interestingly, at M 200 ∼ 10 12.7 M , both M * ,sat and the fraction of stellar mass in satellites versus total stellar mass, f sat , tend to be slightly higher around blue ICGs, perhaps implying the late formation of blue galaxies. f sat increases with the increase in both M * ,ICG+diffuse and M 200 , and scales more linearly with M 200 . We provide best-fitting relations to M 200 versus M * ,ICG+diffuse , M * ,sat or M * ,ICG+diffuse + M * ,sat , and to f sat versus M 200 or M * ,ICG+diffuse , for red and blue ICGs separately.

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Section: Radial Dependence Of the Total Stellar Mass Fractionsupporting

confidence: 91%

Section: Introductionmentioning

confidence: 97%

The stellar mass in and around isolated central galaxies: connections to the total mass distribution through galaxy-galaxy lensing in the Hyper Suprime-Cam survey

Wang,

Li,

Shi

et al. 2021

Preprint

Self Cite

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“…Instead, ensemble-averaged number density profiles are computed by stacking the host−satellite systems together (see, e.g., Sales et al 2007;Tal et al 2012;Guo et al 2013;Wang et al 2014;Ye et al 2017;Brainerd 2018). Even in the case of galaxy clusters, ensemble-averaged number density profiles are commonly used to assess the degree to which the spatial distribution of the cluster members traces that of the dark matter distribution (see, e.g., Gao et al 2004;Budzynski et al 2012;Ye et al 2017;Wang et al 2018). Below we adopt this standard technique and compute ensemble-averaged radial number density profiles for the host −satellite systems, stacked according to various criteria.…”

Section: Normalized Radial Density Profilesmentioning

confidence: 99%

“…Compared to predictions from ΛCDM, however, the concentration found by Budzynski et al (2012) was a factor of ∼2 lower than expected. In another study of observed galaxy clusters, Wang et al (2018) compared the locations of the satellites to the weak-lensing-derived cluster mass distribution. From this, Wang et al (2018) found that the satellite number density traced the mass density well, with both the satellite number density and the mass density being well fitted by an NFW profile.…”

Section: Introductionmentioning

confidence: 99%

The Distribution of Satellite Galaxies in the IllustrisTNG100 Simulation

McDonough

Brainerd

2022

ApJ

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We investigate the spatial distribution of the satellites of isolated host galaxies in the IllustrisTNG100 simulation. In agreement with a previous, similar analysis of the Illustris-1 simulation, the satellites are typically poor tracers of the mean host mass density. Unlike the Illustris-1 satellites, here the spatial distribution of the complete satellite sample is well fitted by an NFW profile; however, the concentration is a factor of ∼2 lower than that of the mean host mass density. The spatial distributions of the brightest 50% and faintest 50% of the satellites are also well fitted by NFW profiles, but the concentrations differ by a factor of ∼2. When the sample is subdivided by host color and luminosity, the number density profiles for blue satellites generally fall below the mean host mass density profiles, while the number density profiles for red satellites generally rise above the mean host mass density profiles. These opposite, systematic offsets combine to yield a moderately good agreement between the mean mass density profile of the brightest blue hosts and the corresponding number density profile of their satellites. Lastly, we subdivide the satellites according to the redshifts at which they joined their hosts. From this, we find that neither the oldest one-third of the satellites nor the youngest one-third of the satellites faithfully trace the mean host mass density.

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“…Budzynski et al (2012) found that the number density profile for satellites in groups and clusters was well-fitted by an NFW profile, but the concentration of the satellite distribution was a factor ∼ 2 lower than expected for the dark matter. In another cluster study, Wang et al (2018) compared the mass density profile obtained from weak lensing to the satellite distribution and concluded that both profiles were fitted well by NFW, with the satellites tracing the mass. Nierenberg et al (2012) concluded that satellites of massive galaxies (M * > 3 × 10 10 M ⊙ ) traced the mass distribution well.…”

Section: Introductionmentioning

confidence: 99%

Satellite Galaxies in the Illustris-1 Simulation: Poor Tracers of the Mass Distribution

Brainerd

2018

ApJL

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Number density profiles are computed for the satellites of relatively isolated host galaxies in the Illustris-1 simulation. The mean total mass density of the hosts is well-fitted by an NFW profile. The number density profile for the complete satellite sample is inconsistent with NFW and, on scales 0.5 r 200 , the satellites do not trace the hosts' mass. This differs substantially from previous results from semi-analytic galaxy formation models. The shape of the satellite number density profile depends on the luminosities of the hosts and the satellites, and on the host virial mass. The number density profile for the faintest satellites is well-fitted by an NFW profile, but the concentration is much less than the mean host mass density. The number density profile for the brightest satellites exhibits a steep increase in slope for host-satellite distances 0.1 r 200 , in qualitative agreement with recent observational studies that find a steep increase in the satellite number density at small host-satellite distances. On scales 0.1 r 200 the satellites of the faintest hosts trace the host mass reasonably well. On scales 0.4 r 200 , the satellites of the brightest hosts do not trace the host mass and the satellite number density increases steeply for host-satellite distances 0.1 r 200 . The discrepancy between the satellite number density profile and the host mass density is most pronounced for the most massive systems, with the satellite number density falling far below that of the mass density on scales 0.5 r 200 .

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Do satellite galaxies trace matter in galaxy clusters?

Cited by 11 publications

References 57 publications

The stellar mass in and around isolated central galaxies: connections to the total mass distribution through galaxy-galaxy lensing in the Hyper Suprime-Cam survey

The stellar mass in and around isolated central galaxies: connections to the total mass distribution through galaxy-galaxy lensing in the Hyper Suprime-Cam survey

The Distribution of Satellite Galaxies in the IllustrisTNG100 Simulation

Satellite Galaxies in the Illustris-1 Simulation: Poor Tracers of the Mass Distribution

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