The DOI matches its Crossref record; 167 of the 169 references it cites were found in a registry or an index, and 2 are not checked yet.
Individual stellar haloes of massive galaxies measured to 100 kpc at 0.3 < z < 0.5 using Hyper Suprime-Cam
Open accessAbstract
Massive galaxies display extended light profiles that can reach several hundreds of kilo parsecs. These stellar halos provide a fossil record of galaxy assembly histories. Using data that is both wide (~100 square degree) and deep (i>28.5 mag/arcsec^2 in i-band), we present a systematic study of the stellar halos of a sample of more than 3000 galaxies at 0.3 < z < 0.5 with $\log M_{\star}/M_{\odot} > 11.4$. Our study is based on high-quality (0.6 arcsec seeing) imaging data from the Hyper Suprime-Cam (HSC) Subaru Strategic Program (SSP), which enables us to individually estimate surface mass density profiles to 100 kpc without stacking. As in previous work, we find that more massive galaxies exhibit more extended outer profiles. When this extended light is not properly accounted for as a result of shallow imaging or inadequate profile modeling, the derived stellar mass function can be significantly underestimated at the highest masses. Across our sample, the ellipticity of outer light profiles increases substantially as we probe larger radii. We show for the first time that these ellipticity gradients steepen dramatically as a function of galaxy mass, but we detect no mass-dependence in outer color gradients. Our results support the two-phase formation scenario for massive galaxies in which outer envelopes are built up at late times from a series of merging events. We provide surface mass surface mass density profiles in a convenient tabulated format to facilitate comparisons with predictions from numerical simulations of galaxy formation.
Overview
The claims and statistics of this paper haven’t been checked yet.
Run the check — free, no account needed. It reads the open-access text and checks the sources it cites.
Integrity signals
Registry
Cites
Statistics
Verification
Claims the paper makes
The claims and statistics of this paper haven’t been checked yet.
Run the check — free, no account needed. It reads the open-access text and checks the sources it cites.
Claims other papers make about this one
Each is checked against this paper’s own text: does it say what the citing paper says it does?
The source backs part of the claim, not all of it — or backs it for a different population, condition or comparison.
In the citing paper
“HSC-PDR2 has been widely tested for low surface brightness studies (e.g. Huang et al. 2018, 2020; Li et al. 2022; Martínez-Lombilla et al. 2023) and fulfils the requirements for our study.”
From Detecting galaxy tidal features using self-supervised representation learning (2024) · cites this paper as Huang et al. 2018
Experimental — accuracy not yet measured
Self-check
Percentages, sums and reported differences re-computed from the paper’s own numbers.
The self-check needs the paper’s full text.
Citations
Cites
Matplotlib: a 2D graphics environment
Hunter, J. D. (2007) · Computing in Science & Engineering · doi:10.1109/mcse.2007.55 · Cited by 39,249
Astropy: A community Python package for astronomy
The Astropy Collaboration, Robitaille, T. P., Tollerud, E. J., Greenfield, P., Droettboom, M., Bray, E., Aldcroft, T., Davis, M., Ginsburg, A., Price-Whelan, A. M., et al. (2013) · Astronomy & Astrophysics · doi:10.1051/0004-6361/201322068 · Cited by 14,620
The NumPy Array: A Structure for Efficient Numerical Computation
van der Walt, S., Colbert, S. C., & Varoquaux, G. (2011) · Computing in Science & Engineering · doi:10.1109/mcse.2011.37 · Cited by 9,381
Galactic Stellar and Substellar Initial Mass Function
Chabrier, G. (2003) · Publications of the Astronomical Society of the Pacific · doi:10.1086/376392 · Cited by 9,071
The Luminosity function and stellar evolution
Salpeter, E. (1955) · The Astrophysical Journal · doi:10.1086/145971 · Cited by 6,816
The Dust Content and Opacity of Actively Star‐forming Galaxies
Calzetti, D., Armus, L., Bohlin, R. C., Kinney, A. L., Koornneef, J., & Storchi‐Bergmann, T. (2000) · The Astrophysical Journal · doi:10.1086/308692 · Cited by 5,707
IPython: A System for Interactive Scientific Computing
Pérez, F., & Granger, B. (2007) · Computing in Science & Engineering · doi:10.1109/mcse.2007.53 · Cited by 4,129
Galactic Stellar and Substellar Initial Mass FunctionPreprint
Chabrier, G. (2003) · Cited by 4,012
MEASURING REDDENING WITH SLOAN DIGITAL SKY SURVEY STELLAR SPECTRA AND RECALIBRATING SFD
Schlafly, E., & Finkbeiner, D. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/737/2/103 · Cited by 3,969
The EAGLE project: simulating the evolution and assembly of galaxies and their environments
Schaye, J., Crain, R. A., Bower, R. G., Furlong, M., Schaller, M., Theuns, T., Dalla Vecchia, C., Frenk, C. S., McCarthy, I. G., Helly, J. C., et al. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu2058 · Cited by 3,601
Flagged first, then by citations
Research works printed but not linked: 11
- Barbary, 2015, sep: v0.3.0
- Bernardi, 2017, MNRAS, 467, 2217
- Diemer, 2015, Astrophysics Source Code Library
- Genel, 2018, MNRAS, 3976
- Huang, 2017, PASJ
- Jones, 2001, SciPy: Open source scientific tools for Python
- Miyazaki, 2012, Proc. SPIE, 84460Z
- Niederste-Ostholt, 2010, MNRAS, 405, 2023
- Pedregosa, 2011, J. Mach. Lear. Res., 12, 2825
- Pillepich, 2018, MNRAS, 4077
- VanderPlas, 2012, Proceedings of Conference on Intelligent Data Understanding (CIDU), 47
Cited by
Sorted by citations
Items 101–111 of 111
HSC-XXL: Baryon budget of the 136 XXL groups and clusters
Akino, D., Eckert, D., Okabe, N., Sereno, M., Umetsu, K., Oguri, M., Gastaldello, F., Chiu, I.-N. T., Ettori, S., EVRARD, A. E., et al. (2021) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psab115 · Cited by 1
Self-citationTwo-phase formation of galaxies: the coevolution between galaxies and dark matter haloes
Ma, Q., Chen, Y., & Mo, H. J. (2026) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stag562 · Cited by 1
Hα emission in the outskirts of galaxies atz= 0.4
Shimakawa, R., Tanaka, M., Kikuta, S., & Hayashi, M. (2021) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psab127 · Cited by 1
Self-citationThe merger-driven evolution of massive early-type galaxies
Cannarozzo, C., Nipoti, C., Sonnenfeld, A., Leauthaud, A., Huang, S., Diemer, B., & Oyarzún, G. A. (2019) · Proceedings of the International Astronomical Union · doi:10.1017/s1743921320002434 · Cited by 1
Self-citationFu, H., Shankar, F., Ayromlou, M., Dickson, M., Koutsouridou, I., Rosas-Guevara, Y., Marsden, C., Brocklebank, K., Bernardi, M., Shiamtanis, N., et al. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac2205
Liu, R., Sonnenfeld, A., Nipoti, C., & Li, R. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202553788
SITCOMTN-165: Surface brightness profiles around massive galaxies in LSSTComCam data
Zhou, C., Jeltema, T., von der Linden, A., Kelvin, L. S., Dell’Antonio, I., Taranu, D. S., Englert, A., & Leauthaud, A. (2025) · DOE SLAC National Accelerator Laboratory Repository · doi:10.71929/rubin/3000576
Self-citationVicentin, M. C., Strauss, M. A., Junior, L. S., Yates, R. M., Araya-Araya, P., & Stoppacher, D. (2026) · The Astrophysical Journal · doi:10.3847/1538-4357/ae45fc
Probing galactic growth with low surface brightness (LSB) data from deep imaging surveys
Sola, E. (2023) · theses.fr (ABES) · doi:10.70675/c03459f6z8feez4c3dzaba6ze65ac73c08ad
The Role of Cluster Environments in Quiescent Galaxy Stellar Halo Assembly
Williams, D. J., Damjanov, I., Sawicki, M., Souchereau, H. J., Chen, L., Desprez, G., George, A., Gwyn, S., & Arnouts, S. (2026) · The Astrophysical Journal · doi:10.3847/1538-4357/ae95fc
Metadata
- Authors
- Huang, S., Leauthaud, A., Greene, J. E., Bundy, K., Lin, Y.-T., Tanaka, M., Miyazaki, S., & Komiyama, Y.
- Affiliations
- Kavli Institute for the Physics and Mathematics of the Universe (JP)
- University of California, Santa Cruz (US)
- Institute of Astronomy and Astrophysics, Academia Sinica (TW)
- National Astronomical Observatory of Japan (JP)
- The Graduate University for Advanced Studies, SOKENDAI (JP)
- Corresponding author
- Huang, Song
- ORCID
- Venue
- Monthly Notices of the Royal Astronomical Society
- Publisher
- Oxford University Press (OUP)
- Published
- 2017-12-15
- Volume
- 475
- Issue
- 3
- Pages
- 3348-3368
- ISSN
- 0035-8711 (ISSN-L)
- 1365-2966
- OpenAlex
- W2730169491
- Cited by
- 113
- References
- 168
- Citations by year
- 2026: 3 · 2025: 11 · 2024: 9 · 2023: 10 · 2022: 23 · 2021: 21 · 2020: 11 · 2019: 13 · 2018: 9 · 2017: 3
- FWCI
- 5.39
- Type
- journal article
- Language
- en
- Open access
- green
- arxiv.org
- Locations
- Monthly Notices of the Royal Astronomical Society (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- arXiv (Cornell University)
- Funders
- National Science Foundation (1714610, AST-1238877, PHY11-25915)
- National Aeronautics and Space Administration (NNX08AR22G)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysical Phenomena and Observations
- Keywords
- stellar haloes, massive galaxies, color gradients, stellar mass function, galaxy assembly history, galaxy mergers, Hyper Suprime-Cam Subaru Strategic Program, intermediate-redshift galaxies
About these checks
Registry, retraction, Cites and statistics results are computed, not judged, with one exception: a printed reference that no index lists is read once by a model before it counts as a citation error. Claims are extracted by a model and kept only when their quote appears verbatim in the text; each cited source is then checked, with a model’s help, for whether it says what the claim relies on. Those verdicts can be wrong — read the claim’s quote and the cited source before relying on one.
Statistics and arithmetic are recomputed, not judged.
Confidence bands are shown only for fields calibrated on our annotated test set. None is calibrated yet, so no band is shown.
What counts as a claim ›How we measure confidence ›How we check this ›
Are you an author, or do you see a problem with this page? Request a review