Galaxy halo masses and satellite fractions from galaxy-galaxy lensing in the Sloan Digital Sky Survey: stellar mass, luminosity, morphology and environment dependencies

Mandelbaum, R.; Seljak, U.; Kauffmann, G.; Hirata, C. M.; Brinkmann, J.

doi:10.1111/j.1365-2966.2006.10156.x

Cited by 728Galaxies: Formation, Evolution, PhenomenaCosmology and Gravitation TheoriesStellar, planetary, and galactic studies

Galaxy halo masses and satellite fractions from galaxy-galaxy lensing in the Sloan Digital Sky Survey: stellar mass, luminosity, morphology and environment dependencies

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Mandelbaum, R., Seljak, U., Kauffmann, G., Hirata, C. M., Brinkmann, J.·2006·Monthly Notices of the Royal Astronomical Society

DOI 10.1111/j.1365-2966.2006.10156.x

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Abstract

The relationship between galaxies and dark matter (DM) can be characterized by the halo mass of the central galaxy and the fraction of galaxies that are satellites. Here, we present observational constraints from the Sloan Digital Sky Survey on these quantities as a function of r-band luminosity and stellar mass using galaxy–galaxy weak lensing, with a total of 351 507 lenses. We use stellar masses derived from spectroscopy and virial halo masses derived from weak gravitational lensing to determine the efficiency with which baryons in the halo of the central galaxy have been converted into stars. We find that an L* galaxy with a stellar mass of 6 × 1010 M⊙ is hosted by a halo with mass of 1.4 × 1012h−1 M⊙, independent of morphology, yielding baryon conversion efficiencies of 17+10−5 per cent (early-types) and 16+15−6 per cent (late-types) at the 95 per cent confidence level (statistical, not including systematic uncertainty due to assumption of a universal initial mass function). We find that for a given stellar mass, the halo mass is independent of morphology below Mstellar= 1011 M⊙, in contrast to typically a factor of 2 difference in halo mass between ellipticals and spirals at a fixed luminosity. This suggests that stellar mass is a good proxy for halo mass in this range and should be used preferentially whenever a halo mass selected sample is needed. For higher stellar masses, the conversion efficiency is a declining function of stellar mass, and the differences in halo mass between early- and late-types become larger, reflecting the fact that most group and cluster haloes with masses above 1013 M⊙ host ellipticals at the centre, while even the brightest central spirals are hosted by haloes of mass below 1013 M⊙. We find that the fraction of spirals that are satellites is roughly 10–15 per cent independent of stellar mass or luminosity, while for ellipticals this fraction decreases with stellar mass from 50 per cent at 1010 M⊙ to 10 per cent at 3 × 1011 M⊙ or 20 per cent at the maximum luminosity considered. We split the elliptical sample by local density, and find that at a given luminosity there is no difference in the signal on scales below 100 h−1 kpc between high- and low-density regions, suggesting that tidal stripping inside large haloes does not remove most of the DM from the early-type satellites. This result is dominated by haloes in the mass range 1013–1014h−1 M⊙, and is an average over all separations from the group or cluster centre.

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Tens of thousands of galaxy-galaxy lenses will provide statistics to probe dark matter halo profiles and substructure.
“Tens of thousands of galaxy -galaxy lenses will provide the needed statistics to probe dark matter halo pro fi les and substructure ( e.g., Mandelbaum et al. 2006; Vegetti et al. 2012 ) .”
From LSST: From Science Drivers to Reference Design and Anticipated Data Products (2019) · cites this paper as Mandelbaum et al. 2006

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The DEEP2 Galaxy Redshift Survey: Spectral Classification of Galaxies at \documentclass{aastex} \usepackage{amsbsy} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{bm} \usepackage{mathrsfs} \usepackage{pifont} \usepackage{stmaryrd} \usepackage{textcomp} \usepackage{portland,xspace} \usepackage{amsmath,amsxtra} \usepackage[OT2,OT1]{fontenc} \newcommand\cyr{ \renewcommand\rmdefault{wncyr} \renewcommand\sfdefault{wncyss} \renewcommand\encodingdefault{OT2} \normalfont \selectfont} \DeclareTextFontCommand{\textcyr}{\cyr} \pagestyle{empty} \DeclareMathSizes{10}{9}{7}{6} \begin{document} \landscape $z\sim 1$ \end{document}
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Authors: Mandelbaum, R., Seljak, U., Kauffmann, G., Hirata, C. M., & Brinkmann, J.
Affiliations: Princeton University (US)
The Abdus Salam International Centre for Theoretical Physics (ICTP) (IT)
Max Planck Institute for Astrophysics (DE)
Institute for Advanced Study (US)
Corresponding author: Mandelbaum, R.
ORCID: Mandelbaum, R.
Seljak, U.
Kauffmann, G.
Hirata, C. M.
Venue: Monthly Notices of the Royal Astronomical Society
Publisher: Oxford University Press (OUP)
Published: 2006-05-11
Volume: 368
Issue: 2
Pages: 715-731
ISSN: 0035-8711 (ISSN-L)
1365-2966
DOI: 10.1111/j.1365-2966.2006.10156.x
OpenAlex: W2147981121
Cited by: 728
References: 125
Citations by year: 2026: 14 · 2025: 15 · 2024: 23 · 2023: 15 · 2022: 31 · 2021: 25 · 2020: 20 · 2019: 27 · 2018: 39 · 2017: 36 · 2016: 36 · 2015: 50 · 2014: 43 · 2013: 59 · 2012: 61
FWCI: 24.57
Type: journal article
Language: en
Open access: green
arxiv.org
Locations: Monthly Notices of the Royal Astronomical Society (publishedVersion)
arXiv (Cornell University) (acceptedVersion)
CERN Document Server (European Organization for Nuclear Research) (submittedVersion)
Max Planck Institute for Plasma Physics (submittedVersion)
Max Planck Digital Library (submittedVersion)
MPG.PuRe (Max Planck Society) (submittedVersion)
arXiv (Cornell University)
Topics: Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Cosmology and Gravitation Theories
Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
Keywords: galaxy-galaxy weak lensing, galaxy halo mass, satellite fraction, dark matter halos, stellar mass, baryon conversion efficiency, galaxy morphology, elliptical galaxies, spiral galaxies, local density, galaxy environment, galaxy clusters, galaxy groups, stellar mass-halo mass relation, galaxy luminosity, Sloan Digital Sky Survey galaxies

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Galaxy halo masses and satellite fractions from galaxy-galaxy lensing in the Sloan Digital Sky Survey: stellar mass, luminosity, morphology and environment dependencies

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