TY - JOUR
T1 - A detection of the environmental dependence of the sizes and stellar haloes of massive central galaxies
AU - Huang, Song
AU - Leauthaud, Alexie
AU - Greene, Jenny
AU - Bundy, Kevin
AU - Lin, Yen Ting
AU - Tanaka, Masayuki
AU - Mandelbaum, Rachel
AU - Miyazaki, Satoshi
AU - Komiyama, Yutaka
N1 - Funding Information:
The authors thank Frank van den Bosch for insightful discussions and Shun Saito for helping us estimate the fraction of satellite galaxies in our sample. We also thank Felipe Ardilla and Christopher Bradshaw for useful comments. SH thanks Feng-Shan Liu for sharing the μ profile of the z~ 1 BCG from his work. This material is based upon work supported by the National Science Foundation under grant no. 1714610. The HSC collaboration includes the astronomical communities of Japan and Taiwan, and Princeton University. The HSC instrumentation and software were developed by National Astronomical Observatory of Japan (NAOJ), Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), University of Tokyo, High Energy Accelerator Research Organization (KEK), Academia Sinica Institute for Astronomy and Astrophysics in Taiwan (ASIAA), and Princeton University. Funding was contributed by the FIRST program from Japanese Cabinet Office, Ministry of Education, Culture, Sports, Science and Technology (MEXT), Japan Society for the Promotion of Science (JSPS), Japan Science and Technology Agency (JST), Toray Science Foundation, NAOJ, Kavli IPMU, KEK, ASIAA, and Princeton University. Funding for SDSS-III has been provided by Alfred P. Sloan Foundation, the Participating Institutions, National Science Foundation, and U.S. Department of Energy. The SDSS-III website is http://www.sdss3.org. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSSIII Collaboration, including University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, University of Florida, the French Participation Group, the German Participation Group, Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. The Pan-STARRS1 surveys (PS1) have been made possible through contributions of Institute for Astronomy; University of Hawaii; the Pan-STARRS Project Office; the Max-Planck Society and its participating institutes: the Max Planck Institute for Astronomy, Heidelberg, and the Max Planck Institute for Extraterrestrial Physics, Garching; Johns Hopkins University; Durham University; University of Edinburgh; Queen's University Belfast; Harvard-Smithsonian Center for Astrophysics; Las Cumbres Observatory Global Telescope Network Incorporated; National Central University of Taiwan; Space Telescope Science Institute; National Aeronautics and Space Administration under grant no. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate; National Science Foundation under grant no. AST-1238877; University of Maryland, and Eotvos Lorand University. This paper makes use of software developed for the LSST. We thank the LSST project for making their code available as free software at http://dm.lsstcorp.org. This research was supported in part by National Science Foundation under grant no. NSF PHY11-25915 and grant no. NSF PHY17-48958 This research made use of STSCI PYTHON, a general astronomical data analysis infrastructure in Python. STSCI PYTHON is a product of the Space Telescope Science Institute, which is operated by Association of Universities for Research in Astronomy (AURA) for NASA; SciPy, an open source scientific tool for Python (Jones et al. 2001); NumPy, a fundamental package for scientific computing with Python (Walt, Colbert & Varoquaux 2011); Matplotlib, a 2D plotting library for Python (Hunter 2007); Astropy, a community-developed core Python package for astronomy (Astropy Collaboration 2013); scikit-learn, a machine-learning library in Python (Pedregosa et al. 2011); astroML, a machine-learning library for astrophysics (Vanderplas et al. 2012); IPython, an interactive computing system for Python (Pérez & Granger 2007); sep Source Extraction and Photometry in Python (Barbary 2016); palettable, colour palettes for Python; emcee, Seriously Kick-Ass MCMC in Python; Colossus, COsmology, haLO and large-Scale StrUcture toolS (Diemer 2015).
Publisher Copyright:
© 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.
PY - 2018/10/11
Y1 - 2018/10/11
N2 - We use ~100 deg2 of deep (> 28.5 mag arcsec-2 in i band), high-quality (median 0.6 arcsec seeing) imaging data from the Hyper Suprime-Cam (HSC) survey to reveal the halo mass dependence of the surface mass density profiles and outer stellar envelopes of massive galaxies. The i-band images from the HSC survey reach ~4 mag deeper than Sloan Digital Sky Survey and enable us to directly trace stellar mass distributions to 100 kpc without requiring stacking. We conclusively show that, at fixed stellar mass, the stellar profiles of massive galaxies depend on the masses of their dark matter haloes. On average, massive central galaxies with log10(M*, 100 kpc/M⊙) > 11.6 in more massive haloes at 0.3 < z < 0.5 have shallower inner stellar mass density profiles (within ~10-20 kpc) and more prominent outer envelopes. These differences translate into a halo mass dependence of the mass-size relation. Central galaxies in haloes with log10(M200b/M⊙) > 14.0 are ~20 per cent larger in R50 at fixed M*, 100 kpc. Such dependence is also reflected in the relationship between the stellarmass within 10 and 100 kpc. Comparing to the mass-size relation, the M*, 100 kpc-M*, 10 kpc relation avoids the ambiguity in the definition of size, and can be straightforwardly compared with simulations. Our results demonstrate that, with deep images from HSC, we can quantify the connection between halo mass and the outer stellar halo, which may provide new constraints on the formation and assembly of massive central galaxies.
AB - We use ~100 deg2 of deep (> 28.5 mag arcsec-2 in i band), high-quality (median 0.6 arcsec seeing) imaging data from the Hyper Suprime-Cam (HSC) survey to reveal the halo mass dependence of the surface mass density profiles and outer stellar envelopes of massive galaxies. The i-band images from the HSC survey reach ~4 mag deeper than Sloan Digital Sky Survey and enable us to directly trace stellar mass distributions to 100 kpc without requiring stacking. We conclusively show that, at fixed stellar mass, the stellar profiles of massive galaxies depend on the masses of their dark matter haloes. On average, massive central galaxies with log10(M*, 100 kpc/M⊙) > 11.6 in more massive haloes at 0.3 < z < 0.5 have shallower inner stellar mass density profiles (within ~10-20 kpc) and more prominent outer envelopes. These differences translate into a halo mass dependence of the mass-size relation. Central galaxies in haloes with log10(M200b/M⊙) > 14.0 are ~20 per cent larger in R50 at fixed M*, 100 kpc. Such dependence is also reflected in the relationship between the stellarmass within 10 and 100 kpc. Comparing to the mass-size relation, the M*, 100 kpc-M*, 10 kpc relation avoids the ambiguity in the definition of size, and can be straightforwardly compared with simulations. Our results demonstrate that, with deep images from HSC, we can quantify the connection between halo mass and the outer stellar halo, which may provide new constraints on the formation and assembly of massive central galaxies.
KW - CD- galaxies: formation
KW - Galaxies: elliptical and lenticular
KW - Galaxies: haloes
KW - Galaxies: photometry
KW - Galaxies: structure
UR - http://www.scopus.com/inward/record.url?scp=85052573542&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85052573542&partnerID=8YFLogxK
U2 - 10.1093/mnras/sty1136
DO - 10.1093/mnras/sty1136
M3 - Article
AN - SCOPUS:85052573542
SN - 0035-8711
VL - 480
SP - 521
EP - 537
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 1
ER -