The miniJPAS survey: White dwarf science with 56 optical filters
Tremblay, P. -E.; Mendes de Oliveira, C.; Guerrero, M. A.; Akras, S.; Benítez, N.; Vázquez Ramió, H.; Varela, J.; Ederoclite, A.; Cenarro, A. J.; Chies-Santos, A. L.; Dupke, R. A.; Abramo, R.; Bonoli, S.; Carneiro, S.; Cristóbal-Hornillos, D.; López-Sanjuan, C.; Marín-Franch, A.; Moles, M.; Sodré, L.; Taylor, K.; Fernández-Ontiveros, J. A.; Lopes de Oliveira, R.; Jiménez-Esteban, F. M.; Alcaniz, J.
Spain, United Kingdom, Greece, Brazil, China, United States
Abstract
Aims: We analyze the white dwarf population in miniJPAS, the first square degree observed with 56 medium-band, 145 Å in width optical filters by the Javalambre Physics of the accelerating Universe Astrophysical Survey (J-PAS), to provide a data-based forecast for the white dwarf science with low-resolution (R ∼ 50) photo-spectra.
Methods: We define the sample of the bluest point-like sources in miniJPAS with r < 21.5 mag, a point-like probability larger than 0.5, (u − r)< 0.80 mag, and (g − i)< 0.25 mag. This sample comprises 33 sources with spectroscopic information: 11 white dwarfs and 22 quasi-stellar objects (QSOs). We estimate the effective temperature (Teff), the surface gravity, and the composition of the white dwarf population by a Bayesian fitting to the observed photo-spectra.
Results: The miniJPAS data are sensitive to the Balmer series and the presence of polluting metals. Our results, combined with those from the Javalambre Photometric Local Universe Survey (J-PLUS) which has a lower spectral resolution but has already observed thousands of white dwarfs, suggest that J-PAS photometry would permit - down to r ∼ 21.5 mag and at least for sources with 7000 < Teff < 22 000 K - both the classification of the observed white dwarfs into H-dominated and He-dominated with 99% confidence and the detection of calcium absorption for equivalent widths larger than 15 Å. The effective temperature is estimated with a 2% uncertainty, which is close to the 1% from spectroscopy. A precise estimation of the surface gravity depends on the available parallax information. In addition, the white dwarf population at Teff > 7000 K can be segregated from the bluest extragalactic QSOs, providing a clean sample based on optical photometry alone.
Conclusions: The J-PAS low-resolution photo-spectra would produce precise effective temperatures and atmospheric compositions for white dwarfs, complementing the data from Gaia. J-PAS will also detect and characterize new white dwarfs beyond the Gaia magnitude limit, providing faint candidates for spectroscopic follow-up.