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Weak lensing reveals a tight connection between dark matter halo mass and the distribution of stellar mass in massive galaxies

Journal Article · · Monthly Notices of the Royal Astronomical Society
 [1];  [2];  [3];  [4];  [2];  [2];  [5];  [6];  [2];  [7];  [8];  [7]
  1. Univ. of California, Santa Cruz, CA (United States); Univ. of Tokyo (Japan); Princeton Univ., NJ (United States)
  2. Univ. of California, Santa Cruz, CA (United States)
  3. Argonne National Lab. (ANL), Argonne, IL (United States)
  4. Univ. of Arizona, Tucson, AZ (United States)
  5. Harvard Univ., Cambridge, MA (United States)
  6. Carnegie Mellon Univ., Pittsburgh, PA (United States)
  7. Princeton Univ., NJ (United States)
  8. Pontificia Univ. Católica de Valparaíso (Chile)
Using deep images from the Hyper Suprime-Cam (HSC) survey and taking advantage of its unprecedented weak lensing capabilities, we reveal here 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 ($$M_{\star }^{\mathrm{max}}$$) 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 $$M_{\star }^{10}$$. Our two-parameter $$M_{\star }^{\mathrm{max}}$$–$$M_{\star }^{10}$$ 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 https://github.com/dr-guangtou/asap
Research Organization:
Argonne National Laboratory (ANL), Argonne, IL (United States)
Sponsoring Organization:
Alfred P. Sloan Foundation; David and Lucile Packard Foundation; Kavli Institute for Theoretical Physics; National Aeronautics and Space Administration (NASA); National Science Foundation (NSF)
Grant/Contract Number:
AC02-06CH11357
OSTI ID:
1633084
Journal Information:
Monthly Notices of the Royal Astronomical Society, Journal Name: Monthly Notices of the Royal Astronomical Society Journal Issue: 3 Vol. 492; ISSN 0035-8711
Publisher:
Royal Astronomical SocietyCopyright Statement
Country of Publication:
United States
Language:
English

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A universal model for halo concentrations text January 2014
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LoCuSS: Weak-lensing mass calibration of galaxy clusters text January 2015
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Forward Modeling of Large-Scale Structure: An open-source approach with Halotools text January 2016
The Correlation Between Halo Mass and Stellar Mass for the Most Massive Galaxies in the Universe text January 2016
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Beyond Assembly Bias: Exploring Secondary Halo Biases for Cluster-size Haloes text January 2017
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The Dependence of Halo Mass on Galaxy Size at Fixed Stellar Mass Using Weak Lensing text January 2017
Galaxy And Mass Assembly (GAMA): the G02 field, Herschel-ATLAS target selection and Data Release 3 text January 2017
Galaxy-Galaxy Lensing in HSC: Validation Tests and the Impact of Heterogeneous Spectroscopic Training Sets text January 2019
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