A New Class of X-Ray Tails of Early-type Galaxies and Subclusters in Galaxy Clusters: Slingshot Tails versus Ram Pressure Stripped Tails

Alex Sheardown, Thomas M. Fish, Elke Roediger, Matthew Hunt, John ZuHone, Yuanyuan Su, Ralph P. Kraft, Paul Nulsen, Eugene Churazov, William Forman, Christine Jones, Natalya Lyskova, Dominique Eckert, Sabrina De Grandi

    Research output: Contribution to journalArticle

    Abstract

    We show that there is a new class of gas tails-slingshot tails-that form as a subhalo (i.e., a subcluster or early-type cluster galaxy) moves away from the cluster center toward the apocenter of its orbit. These tails can point perpendicular or even opposite to the subhalo direction of motion, not tracing the recent orbital path. Thus, the observed tail direction can be misleading, and we caution against naive conclusions regarding the subhalo's direction of motion based on the tail direction. A head-tail morphology of a galaxy's or subcluster's gaseous atmosphere is usually attributed to ram pressure stripping, and the widely applied conclusion is that gas stripped tail traces the most recent orbit. However, during the slingshot tail stage, the subhalo is not being ram pressure stripped (RPS) and the tail is shaped by tidal forces more than just the ram pressure. Thus, applying a classic RPS scenario to a slingshot tail leads not only to an incorrect conclusion regarding the direction of motion but also to incorrect conclusions regarding the subhalo velocity, expected locations of shear flows, instabilities, and mixing. We describe the genesis and morphology of slingshot tails using data from binary cluster merger simulations and discuss their observable features and how to distinguish them from classic RPS tails. We identify three examples from the literature that are not RPS tails but slingshot tails and discuss other potential candidates.

    Original languageEnglish
    Article number112
    Number of pages15
    JournalAstrophysical Journal
    Volume874
    Issue number2
    DOIs
    Publication statusPublished - 1 Apr 2019

    Cite this

    Sheardown, Alex ; Fish, Thomas M. ; Roediger, Elke ; Hunt, Matthew ; ZuHone, John ; Su, Yuanyuan ; Kraft, Ralph P. ; Nulsen, Paul ; Churazov, Eugene ; Forman, William ; Jones, Christine ; Lyskova, Natalya ; Eckert, Dominique ; De Grandi, Sabrina. / A New Class of X-Ray Tails of Early-type Galaxies and Subclusters in Galaxy Clusters : Slingshot Tails versus Ram Pressure Stripped Tails. In: Astrophysical Journal. 2019 ; Vol. 874, No. 2.
    @article{1bda4d6eb5c64a36a4166996babab8c0,
    title = "A New Class of X-Ray Tails of Early-type Galaxies and Subclusters in Galaxy Clusters: Slingshot Tails versus Ram Pressure Stripped Tails",
    abstract = "We show that there is a new class of gas tails-slingshot tails-that form as a subhalo (i.e., a subcluster or early-type cluster galaxy) moves away from the cluster center toward the apocenter of its orbit. These tails can point perpendicular or even opposite to the subhalo direction of motion, not tracing the recent orbital path. Thus, the observed tail direction can be misleading, and we caution against naive conclusions regarding the subhalo's direction of motion based on the tail direction. A head-tail morphology of a galaxy's or subcluster's gaseous atmosphere is usually attributed to ram pressure stripping, and the widely applied conclusion is that gas stripped tail traces the most recent orbit. However, during the slingshot tail stage, the subhalo is not being ram pressure stripped (RPS) and the tail is shaped by tidal forces more than just the ram pressure. Thus, applying a classic RPS scenario to a slingshot tail leads not only to an incorrect conclusion regarding the direction of motion but also to incorrect conclusions regarding the subhalo velocity, expected locations of shear flows, instabilities, and mixing. We describe the genesis and morphology of slingshot tails using data from binary cluster merger simulations and discuss their observable features and how to distinguish them from classic RPS tails. We identify three examples from the literature that are not RPS tails but slingshot tails and discuss other potential candidates.",
    keywords = "galaxies: clusters: general, galaxies: clusters: intracluster medium, methods: numerical, X-rays: galaxies, X-rays: galaxies: clusters, COLD FRONTS, CHANDRA OBSERVATION, GAS, SHOCKS, SIMULATIONS, EVOLUTION, EMISSION, ORIGIN, HALOES, INFALL",
    author = "Alex Sheardown and Fish, {Thomas M.} and Elke Roediger and Matthew Hunt and John ZuHone and Yuanyuan Su and Kraft, {Ralph P.} and Paul Nulsen and Eugene Churazov and William Forman and Christine Jones and Natalya Lyskova and Dominique Eckert and {De Grandi}, Sabrina",
    year = "2019",
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    language = "English",
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    Sheardown, A, Fish, TM, Roediger, E, Hunt, M, ZuHone, J, Su, Y, Kraft, RP, Nulsen, P, Churazov, E, Forman, W, Jones, C, Lyskova, N, Eckert, D & De Grandi, S 2019, 'A New Class of X-Ray Tails of Early-type Galaxies and Subclusters in Galaxy Clusters: Slingshot Tails versus Ram Pressure Stripped Tails' Astrophysical Journal, vol. 874, no. 2, 112. https://doi.org/10.3847/1538-4357/ab0c06

    A New Class of X-Ray Tails of Early-type Galaxies and Subclusters in Galaxy Clusters : Slingshot Tails versus Ram Pressure Stripped Tails. / Sheardown, Alex; Fish, Thomas M.; Roediger, Elke; Hunt, Matthew; ZuHone, John; Su, Yuanyuan; Kraft, Ralph P.; Nulsen, Paul; Churazov, Eugene; Forman, William; Jones, Christine; Lyskova, Natalya; Eckert, Dominique; De Grandi, Sabrina.

    In: Astrophysical Journal, Vol. 874, No. 2, 112, 01.04.2019.

    Research output: Contribution to journalArticle

    TY - JOUR

    T1 - A New Class of X-Ray Tails of Early-type Galaxies and Subclusters in Galaxy Clusters

    T2 - Slingshot Tails versus Ram Pressure Stripped Tails

    AU - Sheardown, Alex

    AU - Fish, Thomas M.

    AU - Roediger, Elke

    AU - Hunt, Matthew

    AU - ZuHone, John

    AU - Su, Yuanyuan

    AU - Kraft, Ralph P.

    AU - Nulsen, Paul

    AU - Churazov, Eugene

    AU - Forman, William

    AU - Jones, Christine

    AU - Lyskova, Natalya

    AU - Eckert, Dominique

    AU - De Grandi, Sabrina

    PY - 2019/4/1

    Y1 - 2019/4/1

    N2 - We show that there is a new class of gas tails-slingshot tails-that form as a subhalo (i.e., a subcluster or early-type cluster galaxy) moves away from the cluster center toward the apocenter of its orbit. These tails can point perpendicular or even opposite to the subhalo direction of motion, not tracing the recent orbital path. Thus, the observed tail direction can be misleading, and we caution against naive conclusions regarding the subhalo's direction of motion based on the tail direction. A head-tail morphology of a galaxy's or subcluster's gaseous atmosphere is usually attributed to ram pressure stripping, and the widely applied conclusion is that gas stripped tail traces the most recent orbit. However, during the slingshot tail stage, the subhalo is not being ram pressure stripped (RPS) and the tail is shaped by tidal forces more than just the ram pressure. Thus, applying a classic RPS scenario to a slingshot tail leads not only to an incorrect conclusion regarding the direction of motion but also to incorrect conclusions regarding the subhalo velocity, expected locations of shear flows, instabilities, and mixing. We describe the genesis and morphology of slingshot tails using data from binary cluster merger simulations and discuss their observable features and how to distinguish them from classic RPS tails. We identify three examples from the literature that are not RPS tails but slingshot tails and discuss other potential candidates.

    AB - We show that there is a new class of gas tails-slingshot tails-that form as a subhalo (i.e., a subcluster or early-type cluster galaxy) moves away from the cluster center toward the apocenter of its orbit. These tails can point perpendicular or even opposite to the subhalo direction of motion, not tracing the recent orbital path. Thus, the observed tail direction can be misleading, and we caution against naive conclusions regarding the subhalo's direction of motion based on the tail direction. A head-tail morphology of a galaxy's or subcluster's gaseous atmosphere is usually attributed to ram pressure stripping, and the widely applied conclusion is that gas stripped tail traces the most recent orbit. However, during the slingshot tail stage, the subhalo is not being ram pressure stripped (RPS) and the tail is shaped by tidal forces more than just the ram pressure. Thus, applying a classic RPS scenario to a slingshot tail leads not only to an incorrect conclusion regarding the direction of motion but also to incorrect conclusions regarding the subhalo velocity, expected locations of shear flows, instabilities, and mixing. We describe the genesis and morphology of slingshot tails using data from binary cluster merger simulations and discuss their observable features and how to distinguish them from classic RPS tails. We identify three examples from the literature that are not RPS tails but slingshot tails and discuss other potential candidates.

    KW - galaxies: clusters: general

    KW - galaxies: clusters: intracluster medium

    KW - methods: numerical

    KW - X-rays: galaxies

    KW - X-rays: galaxies: clusters

    KW - COLD FRONTS

    KW - CHANDRA OBSERVATION

    KW - GAS

    KW - SHOCKS

    KW - SIMULATIONS

    KW - EVOLUTION

    KW - EMISSION

    KW - ORIGIN

    KW - HALOES

    KW - INFALL

    U2 - 10.3847/1538-4357/ab0c06

    DO - 10.3847/1538-4357/ab0c06

    M3 - Article

    VL - 874

    JO - The Astrophysical Journal

    JF - The Astrophysical Journal

    SN - 0004-637X

    IS - 2

    M1 - 112

    ER -