Local stellar formation history from the 40 pc white dwarf sample

Author:

Cukanovaite E1ORCID,Tremblay P-E1,Toonen S2,Temmink K D3,Manser Christopher J4ORCID,O’Brien M W1ORCID,McCleery J1

Affiliation:

1. Department of Physics, University of Warwick , Coventry CV4 7AL, UK

2. Anton Pannekoek Institute for Astronomy, University of Amsterdam , 1090 GE Amsterdam, The Netherlands

3. Department of Astrophysics/IMAPP, Radboud University Nijmegen , P.O. Box 9010, 6500 GL Nijmegen, The Netherlands

4. Astrophysics Group, Department of Physics, Imperial College London , Prince Consort Rd, London, SW7 2AZ, UK

Abstract

ABSTRACT We derive the local stellar formation history from the Gaia-defined 40 pc white dwarf sample. This is currently the largest volume-complete sample of white dwarfs for which spectroscopy is available, allowing for classification of the chemical abundances at the photosphere, and subsequently accurate determination of the atmospheric parameters. We create a population synthesis model and show that a uniform stellar formation history for the last ≈10.5 Gyr provides a satisfactory fit to the observed distribution of absolute Gaia G magnitudes. To test the robustness of our derivation, we vary various assumptions in the population synthesis model, including the initial mass function, initial-to-final mass relation, kinematic evolution, binary fraction, and white dwarf cooling time-scales. From these tests, we conclude that the assumptions in our model have an insignificant effect on the derived relative stellar formation rate as a function of look-back time. However, the onset of stellar formation (age of Galactic disc) is sensitive to a variety of input parameters including the white dwarf cooling models. Our derived stellar formation history gives a much better fit to the absolute Gaia G magnitudes than most previous studies.

Funder

Science and Technology Facilities Council

European Research Council

ESA

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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