The scatter about the 'Universal' dwarf spheroidal mass profile

A kinematic study of the M31 satellites And V and And VI

M. L.M. Collins, S. C. Chapman, R. M. Rich, M. J. Irwin, J. Peñarrubia, R. A. Ibata, N. Arimoto, Alyson Brooks, A. M.N. Ferguson, G. F. Lewis, A. W. McConnachie, K. Venn

Research output: Contribution to journalArticle

19 Citations (Scopus)

Abstract

While the satellites of the Milky Way (MW) have been shown to be largely consistent in terms of their mass contained within one half-light radius (Mhalf) with a 'universal' mass profile, a number of M31 satellites are found to be inconsistent with these relations, and seem kinematically colder in their central regions than their MW cousins. In this work, we present new kinematic and updated structural properties for two M31 dwarf spheroidals (dSph), And V and And VI, using data from the Keck Low Resolution Imaging Spectrograph (LRIS) and the DEep Imaging Multi-Object Spectrograph (DEIMOS) instruments and the Subaru Suprime-Cam imager. We measure systemic velocities of vr=-393.1 ± 4.2 and -344.8 ± 2.5kms-1, and dispersions of σv= 11.5+5.3 -4.4 and 9.4+3.2 - 2.4kms-1 for And V and And VI, respectively, meaning these two objects are consistent with the trends in σv and rhalf set by their MW counterparts. We also investigate the nature of this scatter about the MW dSph mass profiles for the 'classical' (i.e. MV < -8) MW and M31 dSph. When comparing both the 'classical' MW and M31 dSph to the best-fitting mass profiles in the size-velocity dispersion plane, we find general scatter in both the positive (i.e. hotter) and negative (i.e. colder) directions from these profiles. However, barring one exception (CVnI) only the M31 dSph are found to scatter towards a colder regime, and, excepting the And I dSph, only MW objects scatter to hotter dispersions. The scatter for the combined population is greater than expected from measurement errors alone. We assess this divide in the context of the differing disc-to-halo mass (i.e. stars and baryons to total virial mass) ratios of the two hosts and argue that the underlying mass profiles for dSph differ from galaxy to galaxy, and are modified by the baryonic component of the host.

Original languageEnglish (US)
Pages (from-to)1170-1182
Number of pages13
JournalMonthly Notices of the Royal Astronomical Society
Volume417
Issue number2
DOIs
StatePublished - Oct 1 2011

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kinematics
profiles
spectrographs
galaxies
cams
mass ratios
baryons
halos
trends
stars
radii
cold

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Keywords

  • Dark matter
  • Galaxies: dwarf
  • Galaxies: kinematics and dynamics
  • Galaxies: photometry
  • Local Group

Cite this

Collins, M. L.M. ; Chapman, S. C. ; Rich, R. M. ; Irwin, M. J. ; Peñarrubia, J. ; Ibata, R. A. ; Arimoto, N. ; Brooks, Alyson ; Ferguson, A. M.N. ; Lewis, G. F. ; McConnachie, A. W. ; Venn, K. / The scatter about the 'Universal' dwarf spheroidal mass profile : A kinematic study of the M31 satellites And V and And VI. In: Monthly Notices of the Royal Astronomical Society. 2011 ; Vol. 417, No. 2. pp. 1170-1182.
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Collins, MLM, Chapman, SC, Rich, RM, Irwin, MJ, Peñarrubia, J, Ibata, RA, Arimoto, N, Brooks, A, Ferguson, AMN, Lewis, GF, McConnachie, AW & Venn, K 2011, 'The scatter about the 'Universal' dwarf spheroidal mass profile: A kinematic study of the M31 satellites And V and And VI', Monthly Notices of the Royal Astronomical Society, vol. 417, no. 2, pp. 1170-1182. https://doi.org/10.1111/j.1365-2966.2011.19342.x

The scatter about the 'Universal' dwarf spheroidal mass profile : A kinematic study of the M31 satellites And V and And VI. / Collins, M. L.M.; Chapman, S. C.; Rich, R. M.; Irwin, M. J.; Peñarrubia, J.; Ibata, R. A.; Arimoto, N.; Brooks, Alyson; Ferguson, A. M.N.; Lewis, G. F.; McConnachie, A. W.; Venn, K.

In: Monthly Notices of the Royal Astronomical Society, Vol. 417, No. 2, 01.10.2011, p. 1170-1182.

Research output: Contribution to journalArticle

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T1 - The scatter about the 'Universal' dwarf spheroidal mass profile

T2 - A kinematic study of the M31 satellites And V and And VI

AU - Collins, M. L.M.

AU - Chapman, S. C.

AU - Rich, R. M.

AU - Irwin, M. J.

AU - Peñarrubia, J.

AU - Ibata, R. A.

AU - Arimoto, N.

AU - Brooks, Alyson

AU - Ferguson, A. M.N.

AU - Lewis, G. F.

AU - McConnachie, A. W.

AU - Venn, K.

PY - 2011/10/1

Y1 - 2011/10/1

N2 - While the satellites of the Milky Way (MW) have been shown to be largely consistent in terms of their mass contained within one half-light radius (Mhalf) with a 'universal' mass profile, a number of M31 satellites are found to be inconsistent with these relations, and seem kinematically colder in their central regions than their MW cousins. In this work, we present new kinematic and updated structural properties for two M31 dwarf spheroidals (dSph), And V and And VI, using data from the Keck Low Resolution Imaging Spectrograph (LRIS) and the DEep Imaging Multi-Object Spectrograph (DEIMOS) instruments and the Subaru Suprime-Cam imager. We measure systemic velocities of vr=-393.1 ± 4.2 and -344.8 ± 2.5kms-1, and dispersions of σv= 11.5+5.3 -4.4 and 9.4+3.2 - 2.4kms-1 for And V and And VI, respectively, meaning these two objects are consistent with the trends in σv and rhalf set by their MW counterparts. We also investigate the nature of this scatter about the MW dSph mass profiles for the 'classical' (i.e. MV < -8) MW and M31 dSph. When comparing both the 'classical' MW and M31 dSph to the best-fitting mass profiles in the size-velocity dispersion plane, we find general scatter in both the positive (i.e. hotter) and negative (i.e. colder) directions from these profiles. However, barring one exception (CVnI) only the M31 dSph are found to scatter towards a colder regime, and, excepting the And I dSph, only MW objects scatter to hotter dispersions. The scatter for the combined population is greater than expected from measurement errors alone. We assess this divide in the context of the differing disc-to-halo mass (i.e. stars and baryons to total virial mass) ratios of the two hosts and argue that the underlying mass profiles for dSph differ from galaxy to galaxy, and are modified by the baryonic component of the host.

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KW - Dark matter

KW - Galaxies: dwarf

KW - Galaxies: kinematics and dynamics

KW - Galaxies: photometry

KW - Local Group

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