Dissecting the spin distribution of dark matter haloes

V. Antonuccio-Delogu, A. Dobrotka, U. Becciani, S. Cielo, C. Giocoli, Andrea Maccio, A. Romeo-Veloná

    Research output: Contribution to journalArticle

    Abstract

    The spin probability distribution of dark matter haloes has often been modelled as being very near to a lognormal. Most of the theoretical attempts to explain its origin and evolution invoke some hypotheses concerning the influence of tidal interactions or merging on haloes. Here we apply a very general statistical theorem introduced by Cramér (1936) to study the origin of the deviations from the reference lognormal shape: we find that these deviations originate from correlations between two quantities entering the definition of spin, namely the ratio J/M5/2 (which depends only on mass) and the modulus E of the total (gravitational + kinetic) energy.To reach this conclusion, we have made usage of the results deduced from two high spatial- and mass-resolution simulations. Our simulations cover a relatively small volume and produce a sample of more than 16 000 gravitationally bound haloes, each traced by at least 300 particles. We verify that our results are stable to different systematics, by comparing our results with those derived by the gif2 and by a more recent simulation performed by Macciò et al.We find that the spin probability distribution function shows systematic deviations from a lognormal, at all redshifts z ≲ 1. These deviations depend on mass and redshift: at small masses they change little with redshift, and also the best lognormal fits are more stable. The J -M relationship is well described by a power law of exponent α very near to the linear theory prediction (α = 5/3), but systematically lower than this at z ≲ 0.3. We argue that the fact that deviations from a lognormal PDF are present only for high-spin haloes could point to a role of large-scale tidal fields in the evolution of the spin PDF.

    Original languageEnglish (US)
    Pages (from-to)1338-1346
    Number of pages9
    JournalMonthly Notices of the Royal Astronomical Society
    Volume407
    Issue number2
    DOIs
    StatePublished - Sep 1 2010

    Fingerprint

    halos
    dark matter
    deviation
    simulation
    probability distribution functions
    kinetic energy
    power law
    theorems
    distribution
    exponents
    prediction
    predictions
    interactions

    Keywords

    • Cosmology: dark matter
    • Galaxies: haloes
    • Methods: numerical

    ASJC Scopus subject areas

    • Astronomy and Astrophysics
    • Space and Planetary Science

    Cite this

    Antonuccio-Delogu, V., Dobrotka, A., Becciani, U., Cielo, S., Giocoli, C., Maccio, A., & Romeo-Veloná, A. (2010). Dissecting the spin distribution of dark matter haloes. Monthly Notices of the Royal Astronomical Society, 407(2), 1338-1346. https://doi.org/10.1111/j.1365-2966.2010.16989.x

    Dissecting the spin distribution of dark matter haloes. / Antonuccio-Delogu, V.; Dobrotka, A.; Becciani, U.; Cielo, S.; Giocoli, C.; Maccio, Andrea; Romeo-Veloná, A.

    In: Monthly Notices of the Royal Astronomical Society, Vol. 407, No. 2, 01.09.2010, p. 1338-1346.

    Research output: Contribution to journalArticle

    Antonuccio-Delogu, V, Dobrotka, A, Becciani, U, Cielo, S, Giocoli, C, Maccio, A & Romeo-Veloná, A 2010, 'Dissecting the spin distribution of dark matter haloes', Monthly Notices of the Royal Astronomical Society, vol. 407, no. 2, pp. 1338-1346. https://doi.org/10.1111/j.1365-2966.2010.16989.x
    Antonuccio-Delogu V, Dobrotka A, Becciani U, Cielo S, Giocoli C, Maccio A et al. Dissecting the spin distribution of dark matter haloes. Monthly Notices of the Royal Astronomical Society. 2010 Sep 1;407(2):1338-1346. https://doi.org/10.1111/j.1365-2966.2010.16989.x
    Antonuccio-Delogu, V. ; Dobrotka, A. ; Becciani, U. ; Cielo, S. ; Giocoli, C. ; Maccio, Andrea ; Romeo-Veloná, A. / Dissecting the spin distribution of dark matter haloes. In: Monthly Notices of the Royal Astronomical Society. 2010 ; Vol. 407, No. 2. pp. 1338-1346.
    @article{aa7a1bc7cc1a4d58b0785374d3658990,
    title = "Dissecting the spin distribution of dark matter haloes",
    abstract = "The spin probability distribution of dark matter haloes has often been modelled as being very near to a lognormal. Most of the theoretical attempts to explain its origin and evolution invoke some hypotheses concerning the influence of tidal interactions or merging on haloes. Here we apply a very general statistical theorem introduced by Cram{\'e}r (1936) to study the origin of the deviations from the reference lognormal shape: we find that these deviations originate from correlations between two quantities entering the definition of spin, namely the ratio J/M5/2 (which depends only on mass) and the modulus E of the total (gravitational + kinetic) energy.To reach this conclusion, we have made usage of the results deduced from two high spatial- and mass-resolution simulations. Our simulations cover a relatively small volume and produce a sample of more than 16 000 gravitationally bound haloes, each traced by at least 300 particles. We verify that our results are stable to different systematics, by comparing our results with those derived by the gif2 and by a more recent simulation performed by Macci{\`o} et al.We find that the spin probability distribution function shows systematic deviations from a lognormal, at all redshifts z ≲ 1. These deviations depend on mass and redshift: at small masses they change little with redshift, and also the best lognormal fits are more stable. The J -M relationship is well described by a power law of exponent α very near to the linear theory prediction (α = 5/3), but systematically lower than this at z ≲ 0.3. We argue that the fact that deviations from a lognormal PDF are present only for high-spin haloes could point to a role of large-scale tidal fields in the evolution of the spin PDF.",
    keywords = "Cosmology: dark matter, Galaxies: haloes, Methods: numerical",
    author = "V. Antonuccio-Delogu and A. Dobrotka and U. Becciani and S. Cielo and C. Giocoli and Andrea Maccio and A. Romeo-Velon{\'a}",
    year = "2010",
    month = "9",
    day = "1",
    doi = "10.1111/j.1365-2966.2010.16989.x",
    language = "English (US)",
    volume = "407",
    pages = "1338--1346",
    journal = "Monthly Notices of the Royal Astronomical Society",
    issn = "0035-8711",
    publisher = "Oxford University Press",
    number = "2",

    }

    TY - JOUR

    T1 - Dissecting the spin distribution of dark matter haloes

    AU - Antonuccio-Delogu, V.

    AU - Dobrotka, A.

    AU - Becciani, U.

    AU - Cielo, S.

    AU - Giocoli, C.

    AU - Maccio, Andrea

    AU - Romeo-Veloná, A.

    PY - 2010/9/1

    Y1 - 2010/9/1

    N2 - The spin probability distribution of dark matter haloes has often been modelled as being very near to a lognormal. Most of the theoretical attempts to explain its origin and evolution invoke some hypotheses concerning the influence of tidal interactions or merging on haloes. Here we apply a very general statistical theorem introduced by Cramér (1936) to study the origin of the deviations from the reference lognormal shape: we find that these deviations originate from correlations between two quantities entering the definition of spin, namely the ratio J/M5/2 (which depends only on mass) and the modulus E of the total (gravitational + kinetic) energy.To reach this conclusion, we have made usage of the results deduced from two high spatial- and mass-resolution simulations. Our simulations cover a relatively small volume and produce a sample of more than 16 000 gravitationally bound haloes, each traced by at least 300 particles. We verify that our results are stable to different systematics, by comparing our results with those derived by the gif2 and by a more recent simulation performed by Macciò et al.We find that the spin probability distribution function shows systematic deviations from a lognormal, at all redshifts z ≲ 1. These deviations depend on mass and redshift: at small masses they change little with redshift, and also the best lognormal fits are more stable. The J -M relationship is well described by a power law of exponent α very near to the linear theory prediction (α = 5/3), but systematically lower than this at z ≲ 0.3. We argue that the fact that deviations from a lognormal PDF are present only for high-spin haloes could point to a role of large-scale tidal fields in the evolution of the spin PDF.

    AB - The spin probability distribution of dark matter haloes has often been modelled as being very near to a lognormal. Most of the theoretical attempts to explain its origin and evolution invoke some hypotheses concerning the influence of tidal interactions or merging on haloes. Here we apply a very general statistical theorem introduced by Cramér (1936) to study the origin of the deviations from the reference lognormal shape: we find that these deviations originate from correlations between two quantities entering the definition of spin, namely the ratio J/M5/2 (which depends only on mass) and the modulus E of the total (gravitational + kinetic) energy.To reach this conclusion, we have made usage of the results deduced from two high spatial- and mass-resolution simulations. Our simulations cover a relatively small volume and produce a sample of more than 16 000 gravitationally bound haloes, each traced by at least 300 particles. We verify that our results are stable to different systematics, by comparing our results with those derived by the gif2 and by a more recent simulation performed by Macciò et al.We find that the spin probability distribution function shows systematic deviations from a lognormal, at all redshifts z ≲ 1. These deviations depend on mass and redshift: at small masses they change little with redshift, and also the best lognormal fits are more stable. The J -M relationship is well described by a power law of exponent α very near to the linear theory prediction (α = 5/3), but systematically lower than this at z ≲ 0.3. We argue that the fact that deviations from a lognormal PDF are present only for high-spin haloes could point to a role of large-scale tidal fields in the evolution of the spin PDF.

    KW - Cosmology: dark matter

    KW - Galaxies: haloes

    KW - Methods: numerical

    UR - http://www.scopus.com/inward/record.url?scp=77956402035&partnerID=8YFLogxK

    UR - http://www.scopus.com/inward/citedby.url?scp=77956402035&partnerID=8YFLogxK

    U2 - 10.1111/j.1365-2966.2010.16989.x

    DO - 10.1111/j.1365-2966.2010.16989.x

    M3 - Article

    VL - 407

    SP - 1338

    EP - 1346

    JO - Monthly Notices of the Royal Astronomical Society

    JF - Monthly Notices of the Royal Astronomical Society

    SN - 0035-8711

    IS - 2

    ER -