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The Stellar Mass of M31 as inferred by the Andromeda Optical & Infrared Disk Survey

Published online by Cambridge University Press:  10 April 2015

Jonathan Sick ,
Stephane Courteau ,
Jean-Charles Cuillandre ,
Julianne Dalcanton ,
Roelof de Jong ,
Michael McDonald ,
Dana Simard  and
R. Brent Tully
Jonathan Sick
Affiliation:
Department of Physics, Engineering Physics & Astronomy, Queen's University, Kingston, ON, CanadaK7L 3N6. email: jsick@astro.queensu.ca, courteau@astro.queensu.ca
Stephane Courteau
Affiliation:
Department of Physics, Engineering Physics & Astronomy, Queen's University, Kingston, ON, CanadaK7L 3N6. email: jsick@astro.queensu.ca, courteau@astro.queensu.ca
Jean-Charles Cuillandre
Affiliation:
IRFU, Centre d'études de Saclay, Francejcc@cfht.hawaii.edu
Julianne Dalcanton
Affiliation:
Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA. jd@astro.washingston.edu
Roelof de Jong
Affiliation:
Leibniz Institut fr Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany. rdejong@aip.de
Michael McDonald
Affiliation:
Kavli Institute for Astrophysics and Space Research, MIT, Cambridge, MA, USA. mcdonald@space.mit.edu
Dana Simard
Affiliation:
Department of Physics, Engineering Physics & Astronomy, Queen's University, Kingston, ON, CanadaK7L 3N6. email: jsick@astro.queensu.ca, courteau@astro.queensu.ca
R. Brent Tully
Affiliation:
Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI, USA. tully@ifa.hawaii.edu
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Abstract

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Our proximity and external vantage point make M31 an ideal testbed for understanding the structure of spiral galaxies. The Andromeda Optical and Infrared Disk Survey (ANDROIDS) has mapped M31's bulge and disk out to R=40 kpc in ugriJKs bands with CFHT using a careful sky calibration. We use Bayesian modelling of the optical-infrared spectral energy distribution (SED) to estimate profiles of M31's stellar populations and mass along the major axis. This analysis provides evidence for inside-out disk formation and a declining metallicity gradient. M31's i-band mass-to-light ratio (M/Li*) decreases from 0.5 dex in the bulge to ~ 0.2 dex at 40 kpc. The best-constrained stellar population models use the full ugriJKs SED but are also consistent with optical-only fits. Therefore, while NIR data can be successfully modelled with modern stellar population synthesis, NIR data do not provide additional constraints in this application. Fits to the gi-SED alone yield M/Li* that are systematically lower than the full SED fit by 0.1 dex. This is still smaller than the 0.3 dex scatter amongst different relations for M/Li via g – i colour found in the literature. We advocate a stellar mass of M*(30 kpc) = 10.3+2.3-1.7 × 1010 M⊙ for the M31 bulge and disk.

Keywords

galaxies: spiral - galaxies: stellar content - galaxies: photometry
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Issue S311: Galaxy Masses as Constraints of Formation Models , July 2014 , pp. 82 - 85
Copyright
Copyright © International Astronomical Union 2015 

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