Mass models of disc galaxies from the DiskMass Survey in modified Newtonian dynamics

G. W. Angus, G. Gentile, R. Swaters, B. Famaey, A. Diaferio, S. S. McGaugh, K. J. Van Der Heyden

    Research output: Contribution to journalArticle

    8 Citations (Scopus)

    Abstract

    This article explores the agreement between the predictions of modified Newtonian dynamics (MOND) and the rotation curves and stellar velocity dispersion profiles measured by the DiskMass Survey (DMS). A bulge-disk decomposition was made for each of the thirty published galaxies, and a MOND Poisson solver was used to simultaneously compute, from the baryonicmass distributions, model rotation curves and vertical velocity dispersion profiles, which were compared to the measured values. The two main free parameters, the stellar disk's mass-to-light ratio (M/L) and its exponential scaleheight (hz), were estimated by Markov Chain Monte Carlo modelling. The average best-fitting K-band stellar mass-to-light ratio was M/L ≃ 0.55 ± 0.15. However, to match the DMS data, the vertical scaleheights would have to be in the range hz = 200-400 pc which is a factor of 2 lower than those derived from observations of edge-on galaxies with a similar scalelength. The reason is that modified gravity versions of MOND characteristically require a larger M/L to fit the rotation curve in the absence of dark matter and therefore predict a stronger vertical gravitational field than Newtonian models. It was found that changing the MOND acceleration parameter, the shape of the velocity dispersion ellipsoid, the adopted vertical distribution of stars, as well as the galaxy inclination, within any realistic range, all had little impact on these results.

    Original languageEnglish
    Pages (from-to)3551-3580
    Number of pages30
    JournalMonthly Notices of the Royal Astronomical Society
    Volume451
    Issue number4
    DOIs
    Publication statusPublished - Apr 24 2015

    Fingerprint

    disk galaxies
    mass to light ratios
    galaxies
    curves
    Markov chain
    vertical distribution
    Markov chains
    profiles
    extremely high frequencies
    ellipsoids
    stellar mass
    decomposition
    gravitational fields
    gravity
    inclination
    dark matter
    gravitation
    prediction
    stars
    modeling

    All Science Journal Classification (ASJC) codes

    • Astronomy and Astrophysics
    • Space and Planetary Science

    Cite this

    Angus, G. W., Gentile, G., Swaters, R., Famaey, B., Diaferio, A., McGaugh, S. S., & Van Der Heyden, K. J. (2015). Mass models of disc galaxies from the DiskMass Survey in modified Newtonian dynamics. Monthly Notices of the Royal Astronomical Society, 451(4), 3551-3580. https://doi.org/10.1093/mnras/stv1132
    Angus, G. W. ; Gentile, G. ; Swaters, R. ; Famaey, B. ; Diaferio, A. ; McGaugh, S. S. ; Van Der Heyden, K. J. / Mass models of disc galaxies from the DiskMass Survey in modified Newtonian dynamics. In: Monthly Notices of the Royal Astronomical Society. 2015 ; Vol. 451, No. 4. pp. 3551-3580.
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    Angus, GW, Gentile, G, Swaters, R, Famaey, B, Diaferio, A, McGaugh, SS & Van Der Heyden, KJ 2015, 'Mass models of disc galaxies from the DiskMass Survey in modified Newtonian dynamics', Monthly Notices of the Royal Astronomical Society, vol. 451, no. 4, pp. 3551-3580. https://doi.org/10.1093/mnras/stv1132

    Mass models of disc galaxies from the DiskMass Survey in modified Newtonian dynamics. / Angus, G. W.; Gentile, G.; Swaters, R.; Famaey, B.; Diaferio, A.; McGaugh, S. S.; Van Der Heyden, K. J.

    In: Monthly Notices of the Royal Astronomical Society, Vol. 451, No. 4, 24.04.2015, p. 3551-3580.

    Research output: Contribution to journalArticle

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    AU - Angus, G. W.

    AU - Gentile, G.

    AU - Swaters, R.

    AU - Famaey, B.

    AU - Diaferio, A.

    AU - McGaugh, S. S.

    AU - Van Der Heyden, K. J.

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    N2 - This article explores the agreement between the predictions of modified Newtonian dynamics (MOND) and the rotation curves and stellar velocity dispersion profiles measured by the DiskMass Survey (DMS). A bulge-disk decomposition was made for each of the thirty published galaxies, and a MOND Poisson solver was used to simultaneously compute, from the baryonicmass distributions, model rotation curves and vertical velocity dispersion profiles, which were compared to the measured values. The two main free parameters, the stellar disk's mass-to-light ratio (M/L) and its exponential scaleheight (hz), were estimated by Markov Chain Monte Carlo modelling. The average best-fitting K-band stellar mass-to-light ratio was M/L ≃ 0.55 ± 0.15. However, to match the DMS data, the vertical scaleheights would have to be in the range hz = 200-400 pc which is a factor of 2 lower than those derived from observations of edge-on galaxies with a similar scalelength. The reason is that modified gravity versions of MOND characteristically require a larger M/L to fit the rotation curve in the absence of dark matter and therefore predict a stronger vertical gravitational field than Newtonian models. It was found that changing the MOND acceleration parameter, the shape of the velocity dispersion ellipsoid, the adopted vertical distribution of stars, as well as the galaxy inclination, within any realistic range, all had little impact on these results.

    AB - This article explores the agreement between the predictions of modified Newtonian dynamics (MOND) and the rotation curves and stellar velocity dispersion profiles measured by the DiskMass Survey (DMS). A bulge-disk decomposition was made for each of the thirty published galaxies, and a MOND Poisson solver was used to simultaneously compute, from the baryonicmass distributions, model rotation curves and vertical velocity dispersion profiles, which were compared to the measured values. The two main free parameters, the stellar disk's mass-to-light ratio (M/L) and its exponential scaleheight (hz), were estimated by Markov Chain Monte Carlo modelling. The average best-fitting K-band stellar mass-to-light ratio was M/L ≃ 0.55 ± 0.15. However, to match the DMS data, the vertical scaleheights would have to be in the range hz = 200-400 pc which is a factor of 2 lower than those derived from observations of edge-on galaxies with a similar scalelength. The reason is that modified gravity versions of MOND characteristically require a larger M/L to fit the rotation curve in the absence of dark matter and therefore predict a stronger vertical gravitational field than Newtonian models. It was found that changing the MOND acceleration parameter, the shape of the velocity dispersion ellipsoid, the adopted vertical distribution of stars, as well as the galaxy inclination, within any realistic range, all had little impact on these results.

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