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Searching for ZZ Ceti white dwarfs in the Gaia survey

Published online by Cambridge University Press:  09 October 2020

Olivier Vincent Open the ORCID record for Olivier Vincent [Opens in a new window] ,
Pierre Bergeron  and
David Lafrenière
Olivier Vincent
Affiliation:
Département de Physique, Université de Montréal, Montréal, Québec, H3T 1J4 emails: ovincent@astro.umontreal.ca, bergeron@astro.umontreal.ca, david@astro.umontreal.ca
Pierre Bergeron
Affiliation:
Département de Physique, Université de Montréal, Montréal, Québec, H3T 1J4 emails: ovincent@astro.umontreal.ca, bergeron@astro.umontreal.ca, david@astro.umontreal.ca
David Lafrenière
Affiliation:
Département de Physique, Université de Montréal, Montréal, Québec, H3T 1J4 emails: ovincent@astro.umontreal.ca, bergeron@astro.umontreal.ca, david@astro.umontreal.ca
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Abstract

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The Gaia satellite recently released parallax measurements for nearly 400,000 white dwarf stars, allowing for precise measurements of their physical parameters. By combining these parallaxes with Pan-STARRS and CFIS-u photometry, we measured the effective temperatures and surface gravities for all white dwarfs within 100 pc and identified a sample of ZZ Ceti white dwarf candidates within the instability strip. We report the results of a photometric follow-up, currently under way, aimed at identifying new ZZ Ceti stars among this sample using the PESTO camera attached to the 1.6-m telescope at the Mont Mégantic Observatory. Our goal is to verify that ZZ Ceti stars occupy a region in the logg-Teff plane where no nonvariable stars are found, supporting the idea that ZZ Ceti pulsators represent a phase through which all hydrogen-line (DA) white dwarfs must evolve.

Keywords

white dwarfsstars: variablesurveystechniques: photometric
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S357: White Dwarfs as Probes of Fundamental Physics: Tracers of Planetary, Stellar and Galactic Evolution , October 2019 , pp. 123 - 126
Copyright
© International Astronomical Union 2020

References

Bergeron, P., Dufour, P., Fontaine, G. et al. 2019, ApJ, 876, 67CrossRefGoogle Scholar
Cloutier, S. 2018, M.Sc. thesis, Université de MontréalGoogle Scholar
Green, E. M., Limoges, M.-M., Gianninas, A. et al. 2015, in Astronomical Society of the Pacific Conference Series, Vol. 493, 19th European Workshop on White Dwarfs, ed. P. Dufour, P. Bergeron & G. Fontaine, 237Google Scholar
Ibata, R. A., McConnachie, A., Cuillandre, J.-C. et al. 2017, ApJ, 848, 128CrossRefGoogle Scholar
Mukadam, A. S., Mullally, F., Nather, R. E. et al. 2017, ApJ, 607, 982CrossRefGoogle Scholar