Volume 658, February 2022
|Number of page(s)||17|
|Section||Stellar structure and evolution|
|Published online||03 February 2022|
J-PLUS: Spectral evolution of white dwarfs by PDF analysis⋆
Centro de Estudios de Física del Cosmos de Aragón (CEFCA), Unidad Asociada al CSIC, Plaza San Juan 1, 44001 Teruel, Spain
2 Department of Physics, University of Warwick, Coventry CV4 7AL, UK
3 Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo, 05508-090 São Paulo, Brazil
4 Institut de Ciències del Cosmos, Universitat de Barcelona (IEEC-UB), Martí i Franquès 1, 08028 Barcelona, Spain
5 Observatório Nacional – MCTI (ON), Rua Gal. José Cristino 77, São Cristóvão, 20921-400 Rio de Janeiro, Brazil
6 European Southern Observatory, Karl Schwarzschild Straße 2, Garching 85748, Germany
7 Centro de Astrobiología (CSIC-INTA), ESAC Campus, Camino Bajo del Castillo s/n, 28692 Villanueva de la Cañada, Spain
8 Spanish Virtual Observatory, 28692 Villanueva de la Cañada, Spain
9 Donostia International Physics Centre (DIPC), Paseo Manuel de Lardizabal 4, 20018 Donostia-San Sebastián, Spain
10 IKERBASQUE, Basque Foundation for Science, 48013 Bilbao, Spain
11 University of Michigan, Department of Astronomy, 1085 South University Ave., Ann Arbor, MI 48109, USA
12 University of Alabama, Department of Physics and Astronomy, Gallalee Hall, Tuscaloosa, AL 35401, USA
13 Instituto de Astrofísica de Canarias, La Laguna, 38205 Tenerife, Spain
14 Departamento de Astrofísica, Universidad de La Laguna, 38206 Tenerife, Spain
Accepted: 26 October 2021
Aims. We estimated the spectral evolution of white dwarfs with effective temperature using the Javalambre Photometric Local Universe Survey (J-PLUS) second data release (DR2), which provides 12 photometric optical passbands over 2176 deg2.
Methods. We analyzed 5926 white dwarfs with r ≤ 19.5 mag in common between a white dwarf catalog defined from Gaia EDR3 and J-PLUS DR2. We performed a Bayesian analysis by comparing the observed J-PLUS photometry with theoretical models of hydrogen- and helium-dominated atmospheres. We estimated the probability distribution functions for effective temperature (Teff), surface gravity, parallax, and composition; and the probability of having a H-dominated atmosphere (pH) for each source. We applied a prior in parallax, using Gaia EDR3 measurements as a reference, and derived a self-consistent prior for the atmospheric composition as a function of Teff.
Results. We described the fraction of white dwarfs with a He-dominated atmosphere (fHe) with a linear function of the effective temperature at 5000 < Teff < 30 000 K. We find fHe = 0.24 ± 0.01 at Teff = 10 000 K, a change rate along the cooling sequence of 0.14 ± 0.02 per 10 kK, and a minimum He-dominated fraction of 0.08 ± 0.02 at the high-temperature end. We tested the obtained pH by comparison with spectroscopic classifications, finding that it is reliable. We estimated the mass distribution for the 351 sources with distance d < 100 pc, mass M > 0.45 M⊙, and Teff > 6000 K. The result for H-dominated white dwarfs agrees with previous studies, with a dominant M = 0.59 M⊙ peak and the presence of an excess at M ∼ 0.8 M⊙. This high-mass excess is absent in the He-dominated distribution, which presents a single peak.
Conclusions. The J-PLUS optical data provide a reliable statistical classification of white dwarfs into H- and He-dominated atmospheres. We find a 21 ± 3% increase in the fraction of He-dominated white dwarfs from Teff = 20 000 K to Teff = 5000 K.
Key words: white dwarfs / methods: statistical
The catalog with the atmospheric parameters and composition of the analyzed white dwarfs is available in electronic form both on the jplus.WhiteDwarf table at the J-PLUS database and at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (188.8.131.52) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/658/A79
© ESO 2022
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