Weak lensing reveals a tight connection between dark matter halo mass and the distribution of stellar mass in massive galaxies
AffiliationUniv Arizona, Dept Astron
Univ Arizona, Steward Observ
Keywordsgalaxies: elliptical and lenticular, cD
MetadataShow full item record
PublisherOXFORD UNIV PRESS
CitationSong Huang, Alexie Leauthaud, Andrew Hearin, Peter Behroozi, Christopher Bradshaw, Felipe Ardila, Joshua Speagle, Ananth Tenneti, Kevin Bundy, Jenny Greene, Cristóbal Sifón, Neta Bahcall, Weak lensing reveals a tight connection between dark matter halo mass and the distribution of stellar mass in massive galaxies, Monthly Notices of the Royal Astronomical Society, Volume 492, Issue 3, March 2020, Pages 3685–3707, https://doi.org/10.1093/mnras/stz3314
RightsCopyright © 2019 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at email@example.com.
AbstractUsing deep images from the Hyper Suprime-Cam (HSC) survey and taking advantage of its unprecedented weak lensing capabilities, we reveal a remarkably tight connection between the stellar mass distribution of massive central galaxies and their host dark matter halo mass. Massive galaxies with more extended stellar mass distributions tend to live in more massive dark matter haloes. We explain this connection with a phenomenological model that assumes, (1) a tight relation between the halo mass and the total stellar content in the halo, (2) that the fraction of in situ and ex situ mass at r <10 kpc depends on halo mass. This model provides an excellent description of the stellar mass functions (SMFs) of total stellar mass (M-star(max)) and stellar mass within inner 10 kpc (M-star(10)) and also reproduces the HSC weak lensing signals of massive galaxies with different stellar mass distributions. The best-fitting model shows that halo mass varies significantly at fixed total stellar mass (as much as 0.4 dex) with a clear dependence on M-star(10). Otu' two-parameter M-star(max) -M-star(10) description provides a more accurate picture of the galaxy halo connection at the high-mass end than the simple stellar halo mass relation (SHMR) and opens a new window to connect the assembly history of haloes with those of central galaxies. The model also predicts that the ex situ component dominates the mass profiles of galaxies at r < 10 kpc for log M-star >= 11,7. The code used for this paper is available online haps://github.com/dr-guangfou/asap
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