Galaxy cluster bulk flows and collision velocities in qumond

Harley Katz, Stacy McGaugh, Peter Teuben, G. W. Angus

    Research output: Contribution to journalArticle

    7 Citations (Scopus)

    Abstract

    We examine the formation of clusters of galaxies in numerical simulations of a QUMOND cosmogony with massive sterile neutrinos. Clusters formed in these exploratory simulations develop higher velocities than those found in ΛCDM simulations. The bulk motions of clusters attain ∼1000 km s -1 by low redshift, comparable to observations whereas ΛCDM simulated clusters tend to fall short. Similarly, high pairwise velocities are common in cluster-cluster collisions like the Bullet Cluster. There is also a propensity for the most massive clusters to be larger in QUMOND and to appear earlier than in ΛCDM, potentially providing an explanation for "pink elephants" like El Gordo. However, it is not obvious that the cluster mass function can be recovered.

    Original languageEnglish
    Article number10
    JournalAstrophysical Journal
    Volume772
    Issue number1
    DOIs
    Publication statusPublished - Jul 20 2013

    Fingerprint

    collision
    galaxies
    collisions
    simulation
    elephant
    cosmology
    neutrinos

    All Science Journal Classification (ASJC) codes

    • Nuclear and High Energy Physics
    • Space and Planetary Science
    • Astronomy and Astrophysics

    Cite this

    Katz, Harley ; McGaugh, Stacy ; Teuben, Peter ; Angus, G. W. / Galaxy cluster bulk flows and collision velocities in qumond. In: Astrophysical Journal. 2013 ; Vol. 772, No. 1.
    @article{73ab26de828f4b218e3239fa57cc7666,
    title = "Galaxy cluster bulk flows and collision velocities in qumond",
    abstract = "We examine the formation of clusters of galaxies in numerical simulations of a QUMOND cosmogony with massive sterile neutrinos. Clusters formed in these exploratory simulations develop higher velocities than those found in ΛCDM simulations. The bulk motions of clusters attain ∼1000 km s -1 by low redshift, comparable to observations whereas ΛCDM simulated clusters tend to fall short. Similarly, high pairwise velocities are common in cluster-cluster collisions like the Bullet Cluster. There is also a propensity for the most massive clusters to be larger in QUMOND and to appear earlier than in ΛCDM, potentially providing an explanation for {"}pink elephants{"} like El Gordo. However, it is not obvious that the cluster mass function can be recovered.",
    author = "Harley Katz and Stacy McGaugh and Peter Teuben and Angus, {G. W.}",
    year = "2013",
    month = "7",
    day = "20",
    doi = "10.1088/0004-637X/772/1/10",
    language = "English",
    volume = "772",
    journal = "Astrophysical Journal",
    issn = "0004-637X",
    publisher = "IOP Publishing Ltd.",
    number = "1",

    }

    Galaxy cluster bulk flows and collision velocities in qumond. / Katz, Harley; McGaugh, Stacy; Teuben, Peter; Angus, G. W.

    In: Astrophysical Journal, Vol. 772, No. 1, 10, 20.07.2013.

    Research output: Contribution to journalArticle

    TY - JOUR

    T1 - Galaxy cluster bulk flows and collision velocities in qumond

    AU - Katz, Harley

    AU - McGaugh, Stacy

    AU - Teuben, Peter

    AU - Angus, G. W.

    PY - 2013/7/20

    Y1 - 2013/7/20

    N2 - We examine the formation of clusters of galaxies in numerical simulations of a QUMOND cosmogony with massive sterile neutrinos. Clusters formed in these exploratory simulations develop higher velocities than those found in ΛCDM simulations. The bulk motions of clusters attain ∼1000 km s -1 by low redshift, comparable to observations whereas ΛCDM simulated clusters tend to fall short. Similarly, high pairwise velocities are common in cluster-cluster collisions like the Bullet Cluster. There is also a propensity for the most massive clusters to be larger in QUMOND and to appear earlier than in ΛCDM, potentially providing an explanation for "pink elephants" like El Gordo. However, it is not obvious that the cluster mass function can be recovered.

    AB - We examine the formation of clusters of galaxies in numerical simulations of a QUMOND cosmogony with massive sterile neutrinos. Clusters formed in these exploratory simulations develop higher velocities than those found in ΛCDM simulations. The bulk motions of clusters attain ∼1000 km s -1 by low redshift, comparable to observations whereas ΛCDM simulated clusters tend to fall short. Similarly, high pairwise velocities are common in cluster-cluster collisions like the Bullet Cluster. There is also a propensity for the most massive clusters to be larger in QUMOND and to appear earlier than in ΛCDM, potentially providing an explanation for "pink elephants" like El Gordo. However, it is not obvious that the cluster mass function can be recovered.

    UR - http://www.scopus.com/inward/record.url?scp=84879906002&partnerID=8YFLogxK

    UR - http://www.scopus.com/inward/citedby.url?scp=84879906002&partnerID=8YFLogxK

    U2 - 10.1088/0004-637X/772/1/10

    DO - 10.1088/0004-637X/772/1/10

    M3 - Article

    VL - 772

    JO - Astrophysical Journal

    JF - Astrophysical Journal

    SN - 0004-637X

    IS - 1

    M1 - 10

    ER -