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Binary White Dwarfs in the Galactic Halo

Published online by Cambridge University Press:  06 January 2014

Pim van Oirschot ,
Gijs Nelemans ,
Amina Helmi ,
Else Starkenburg ,
Onno Pols  and
Anthony G.A. Brown
Pim van Oirschot*
Affiliation:
Department of Astrophysics / IMAPP, Radboud University Nijmegen, P.O. Box 9010, 6500 GL Nijmegen, The Netherlands
Gijs Nelemans
Affiliation:
Department of Astrophysics / IMAPP, Radboud University Nijmegen, P.O. Box 9010, 6500 GL Nijmegen, The Netherlands Institute for Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
Amina Helmi
Affiliation:
Kapteyn Astronomical Institute, University of Groningen, P.O. Box 800, 9700 AV, Groningen, The Netherlands
Else Starkenburg
Affiliation:
Department of Physics and Astronomy, University of Victoria, P.O. Box 3055, STN CSC, Victoria BC V8W 3P6, Canada
Onno Pols
Affiliation:
Department of Astrophysics / IMAPP, Radboud University Nijmegen, P.O. Box 9010, 6500 GL Nijmegen, The Netherlands
Anthony G.A. Brown
Affiliation:
Leiden Observatory, Leiden University, P.O. Box 9513, 2300 RA Leiden, The Netherlands
*
*email: [email protected]
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We use the stellar population synthesis code SeBa (Portegies Zwart & Verbunt (1996), Toonen, Nelemans & Portegies Zwart (2012)) to study the halo white dwarf population. Here we assume a Kroupa initial mass function and compare 4 models, varying two parameters: the star formation (SF) history of the halo (either continuous SF during 2.5 Gyr, which started 13.2 Gyr ago, or a SF burst during 360 Myr, which started 12.9 Gyr ago – see the left panel of the figure) and the binary fraction of the halo (either 100% single stars, or 100% binaries). White dwarf cooling models (Althaus et al. (2009) and Renedo et al. (2010)) allow us to plot the halo white dwarf luminosity function for these 4 models, as is done in the right panel of the figure. Combined with an assumption about the density distribution of halo stars, we will study which of these white dwarfs Gaia can see, and what that can tell us about the initial parameter distributions in the halo. In the near future, we plan to use the Munich-Groningen semi-analytical galaxy formation model (Starkenburg et al. (2013)), to obtain key ingredients for the population synthesis modeling, such as a realistic star formation history (see the left panel of the figure).

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S298: Setting the scene for Gaia and LAMOST , May 2013 , pp. 431
Copyright
Copyright © International Astronomical Union 2014 

References

Portegies Zwart, S. & Verbunt, F. 1996, A&A, 309, 179Google Scholar
Toonen, S., Nelemans, G., & Portegies Zwart, S. 2012, A&A, 546, A70Google Scholar
Althaus, L. G., et al. 2009, A&A, 502, 207Google Scholar
Renedo, I., et al. 2010, ApJ, 717, 183CrossRefGoogle Scholar
Starkenburg, E., et al. 2013, MNRAS, 429, 725CrossRefGoogle Scholar