THE SPATIAL DISTRIBUTION of SATELLITE GALAXIES WITHIN HALOS: MEASURING the VERY SMALL SCALE ANGULAR CLUSTERING of SDSS GALAXIES

Jennifer A. Piscionere, Andreas A. Berlind, Cameron K. McBride, Romá Scoccimarro

    Research output: Contribution to journalArticle

    Abstract

    We measure the angular clustering of galaxies from the Sloan Digital Sky Survey (SDSS) Data Release 7 in order to probe the spatial distribution of satellite galaxies within their dark matter halos. Specifically, we measure the angular correlation function on very small scales (7″-320″) in a range of luminosity threshold samples (absolute r-band magnitudes from -18 up to -21) that are constructed from the subset of SDSS that has been spectroscopically observed more than once (the so-called plate overlap region). We choose to measure angular clustering in this reduced survey footprint in order to minimize the effects of fiber collision incompleteness, which are otherwise substantial on these small scales, and we discuss the possible impact that fiber collisions have on our measurements. We model our clustering measurements using a fully numerical halo model that populates dark matter halos in N-body simulations to create realistic mock galaxy catalogs. The model has free parameters that specify both the number and spatial distribution of galaxies within their host halos. We adopt a flexible density profile for the spatial distribution of satellite galaxies that is similar to the dark matter Navarro-Frenk-White (NFW) profile, except that the inner slope is allowed to vary. We find that the angular clustering of our most luminous samples ( < -20 and -21) suggests that luminous satellite galaxies have substantially steeper inner density profiles than NFW. Lower-luminosity samples are less constraining, however, and are consistent with satellite galaxies having shallow density profiles. Our results confirm the findings of Watson et al. while using different clustering measurements and modeling methodology.

    Original languageEnglish (US)
    Article number125
    JournalAstrophysical Journal
    Volume806
    Issue number1
    DOIs
    StatePublished - Jun 10 2015

    Fingerprint

    halos
    galaxies
    spatial distribution
    collision
    dark matter
    profiles
    footprint
    luminosity
    probe
    collisions
    fibers
    footprints
    methodology
    measuring
    angular correlation
    set theory
    catalogs
    modeling
    simulation
    slopes

    Keywords

    • dark matter
    • galaxies: halos
    • large-scale structure of universe
    • methods: numerical
    • surveys

    ASJC Scopus subject areas

    • Space and Planetary Science
    • Astronomy and Astrophysics

    Cite this

    THE SPATIAL DISTRIBUTION of SATELLITE GALAXIES WITHIN HALOS : MEASURING the VERY SMALL SCALE ANGULAR CLUSTERING of SDSS GALAXIES. / Piscionere, Jennifer A.; Berlind, Andreas A.; McBride, Cameron K.; Scoccimarro, Romá.

    In: Astrophysical Journal, Vol. 806, No. 1, 125, 10.06.2015.

    Research output: Contribution to journalArticle

    Piscionere, Jennifer A. ; Berlind, Andreas A. ; McBride, Cameron K. ; Scoccimarro, Romá. / THE SPATIAL DISTRIBUTION of SATELLITE GALAXIES WITHIN HALOS : MEASURING the VERY SMALL SCALE ANGULAR CLUSTERING of SDSS GALAXIES. In: Astrophysical Journal. 2015 ; Vol. 806, No. 1.
    @article{133d4b9aba4c46e18a74b50902b26750,
    title = "THE SPATIAL DISTRIBUTION of SATELLITE GALAXIES WITHIN HALOS: MEASURING the VERY SMALL SCALE ANGULAR CLUSTERING of SDSS GALAXIES",
    abstract = "We measure the angular clustering of galaxies from the Sloan Digital Sky Survey (SDSS) Data Release 7 in order to probe the spatial distribution of satellite galaxies within their dark matter halos. Specifically, we measure the angular correlation function on very small scales (7″-320″) in a range of luminosity threshold samples (absolute r-band magnitudes from -18 up to -21) that are constructed from the subset of SDSS that has been spectroscopically observed more than once (the so-called plate overlap region). We choose to measure angular clustering in this reduced survey footprint in order to minimize the effects of fiber collision incompleteness, which are otherwise substantial on these small scales, and we discuss the possible impact that fiber collisions have on our measurements. We model our clustering measurements using a fully numerical halo model that populates dark matter halos in N-body simulations to create realistic mock galaxy catalogs. The model has free parameters that specify both the number and spatial distribution of galaxies within their host halos. We adopt a flexible density profile for the spatial distribution of satellite galaxies that is similar to the dark matter Navarro-Frenk-White (NFW) profile, except that the inner slope is allowed to vary. We find that the angular clustering of our most luminous samples ( < -20 and -21) suggests that luminous satellite galaxies have substantially steeper inner density profiles than NFW. Lower-luminosity samples are less constraining, however, and are consistent with satellite galaxies having shallow density profiles. Our results confirm the findings of Watson et al. while using different clustering measurements and modeling methodology.",
    keywords = "dark matter, galaxies: halos, large-scale structure of universe, methods: numerical, surveys",
    author = "Piscionere, {Jennifer A.} and Berlind, {Andreas A.} and McBride, {Cameron K.} and Rom{\'a} Scoccimarro",
    year = "2015",
    month = "6",
    day = "10",
    doi = "10.1088/0004-637X/806/1/125",
    language = "English (US)",
    volume = "806",
    journal = "Astrophysical Journal",
    issn = "0004-637X",
    publisher = "IOP Publishing Ltd.",
    number = "1",

    }

    TY - JOUR

    T1 - THE SPATIAL DISTRIBUTION of SATELLITE GALAXIES WITHIN HALOS

    T2 - MEASURING the VERY SMALL SCALE ANGULAR CLUSTERING of SDSS GALAXIES

    AU - Piscionere, Jennifer A.

    AU - Berlind, Andreas A.

    AU - McBride, Cameron K.

    AU - Scoccimarro, Romá

    PY - 2015/6/10

    Y1 - 2015/6/10

    N2 - We measure the angular clustering of galaxies from the Sloan Digital Sky Survey (SDSS) Data Release 7 in order to probe the spatial distribution of satellite galaxies within their dark matter halos. Specifically, we measure the angular correlation function on very small scales (7″-320″) in a range of luminosity threshold samples (absolute r-band magnitudes from -18 up to -21) that are constructed from the subset of SDSS that has been spectroscopically observed more than once (the so-called plate overlap region). We choose to measure angular clustering in this reduced survey footprint in order to minimize the effects of fiber collision incompleteness, which are otherwise substantial on these small scales, and we discuss the possible impact that fiber collisions have on our measurements. We model our clustering measurements using a fully numerical halo model that populates dark matter halos in N-body simulations to create realistic mock galaxy catalogs. The model has free parameters that specify both the number and spatial distribution of galaxies within their host halos. We adopt a flexible density profile for the spatial distribution of satellite galaxies that is similar to the dark matter Navarro-Frenk-White (NFW) profile, except that the inner slope is allowed to vary. We find that the angular clustering of our most luminous samples ( < -20 and -21) suggests that luminous satellite galaxies have substantially steeper inner density profiles than NFW. Lower-luminosity samples are less constraining, however, and are consistent with satellite galaxies having shallow density profiles. Our results confirm the findings of Watson et al. while using different clustering measurements and modeling methodology.

    AB - We measure the angular clustering of galaxies from the Sloan Digital Sky Survey (SDSS) Data Release 7 in order to probe the spatial distribution of satellite galaxies within their dark matter halos. Specifically, we measure the angular correlation function on very small scales (7″-320″) in a range of luminosity threshold samples (absolute r-band magnitudes from -18 up to -21) that are constructed from the subset of SDSS that has been spectroscopically observed more than once (the so-called plate overlap region). We choose to measure angular clustering in this reduced survey footprint in order to minimize the effects of fiber collision incompleteness, which are otherwise substantial on these small scales, and we discuss the possible impact that fiber collisions have on our measurements. We model our clustering measurements using a fully numerical halo model that populates dark matter halos in N-body simulations to create realistic mock galaxy catalogs. The model has free parameters that specify both the number and spatial distribution of galaxies within their host halos. We adopt a flexible density profile for the spatial distribution of satellite galaxies that is similar to the dark matter Navarro-Frenk-White (NFW) profile, except that the inner slope is allowed to vary. We find that the angular clustering of our most luminous samples ( < -20 and -21) suggests that luminous satellite galaxies have substantially steeper inner density profiles than NFW. Lower-luminosity samples are less constraining, however, and are consistent with satellite galaxies having shallow density profiles. Our results confirm the findings of Watson et al. while using different clustering measurements and modeling methodology.

    KW - dark matter

    KW - galaxies: halos

    KW - large-scale structure of universe

    KW - methods: numerical

    KW - surveys

    UR - http://www.scopus.com/inward/record.url?scp=84934975377&partnerID=8YFLogxK

    UR - http://www.scopus.com/inward/citedby.url?scp=84934975377&partnerID=8YFLogxK

    U2 - 10.1088/0004-637X/806/1/125

    DO - 10.1088/0004-637X/806/1/125

    M3 - Article

    AN - SCOPUS:84934975377

    VL - 806

    JO - Astrophysical Journal

    JF - Astrophysical Journal

    SN - 0004-637X

    IS - 1

    M1 - 125

    ER -