The PAndAS view of the andromeda satellite system. II. Detailed properties of 23 M31 dwarf spheroidal galaxies
- Observatoire astronomique de Strasbourg, Université de Strasbourg, CNRS, UMR 7550, 11 rue de l’Université, F-67000 Strasbourg (France)
- Sydney Institute for Astronomy, School of Physics A28, The University of Sydney, NSW 2006 (Australia)
- NRC Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria, BC V9E 2E7 (Canada)
- Department of Physics and Astronomy, University of Victoria, Victoria, BC V8P 1A1 (Canada)
- Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA (United Kingdom)
- Laboratoire Lagrange UMR 7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, CS 34229, F-06304, Nice Cedex 04 (France)
- Department of Physics and Atmospheric Science, Dalhousie University, Coburg Road, Halifax, NS B3H 1A6 (Canada)
- Department of Physics, University of Surrey, Guildford, Surrey GU2 7XH (United Kingdom)
- Physics Department, Texas Tech University, Lubbock, TX 79409 (United States)
- Department of Astronomy, University of Massachusetts, Amherst, MA 01003 (United States)
- Institute for Astronomy, University of Edinburgh, Blackford Hill, Edinburgh EH9 3HJ (United Kingdom)
- Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611 (Australia)
We present a comprehensive analysis of the structural properties and luminosities of the 23 dwarf spheroidal galaxies that fall within the footprint of the Pan-Andromeda Archaeological Survey (PAndAS). These dwarf galaxies represent the large majority of Andromeda’s known satellite dwarf galaxies and cover a wide range in luminosity (−11.6≲M{sub V}≲−5.8 or 10{sup 4.2}≲L≲10{sup 6.5} L{sub ⊙}) and surface brightness (25.1≲μ{sub 0}≲29.3 mag arcsec{sup −2}). We confirm most previous measurements, but we find And XIX to be significantly larger than before (r{sub h}=3065{sub −935}{sup +1065} pc, M{sub V}=−10.1{sub −0.4}{sup +0.8}) and cannot derive parameters for And XXVII as it is likely not a bound stellar system. We also significantly revise downward the luminosities of And XV and And XVI, which are now M{sub V}∼−7.5 or L∼10{sup 5} L{sub ⊙}. Finally, we provide the first detailed analysis of Cas II/And XXX, a fairly faint system (M{sub V}=−8.0{sub −0.3}{sup +0.4}) of typical size (r{sub h}=270±50 pc), located in close proximity to the two bright elliptical dwarf galaxies NGC 147 and NGC 185. Combined with the set of homogeneous distances published in an earlier contribution, our analysis dutifully tracks all relevant sources of uncertainty in the determination of the properties of the dwarf galaxies from the PAndAS photometric catalog. We further publish the posterior probability distribution functions of all the parameters we fit for in the form of MCMC chains available online; these inputs should be used in any analysis that aims to remain truthful to the data and properly account for covariance between parameters.
- OSTI ID:
- 22869668
- Journal Information:
- Astrophysical Journal, Vol. 833, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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