We have exploited the very precise parallaxes, proper motions, and photometry of Gaia Data Release 2 to study white dwarf members of the Hyades star cluster. Gaia photometry and parallaxes for the eight DA white dwarfs confirmed members have been then used to compute absolute magnitudes and colours. These were compared to three independent sets of white dwarf evolutionary tracks, to derive cooling times and white dwarf (final) masses. All sets of models provide the same mass values, with only small differences in the cooling ages. The precision in the derived masses and cooling ages is typically 1-3 per cent. Our derived masses are generally consistent with spectroscopic estimates from the literature, whilst cooling ages are generally large...
We present a spectro-photometric analysis of 2880 cool white dwarfs within 100 pc of the Sun and coo...
Context. The initial-final mass relationship of white dwarfs, which is poorly constrained, is of par...
We present the initial–final mass relation derived from 10 white dwarfs in wide binaries that consis...
We have exploited Gaia Data Release 2 to study white dwarf members of the Praesepe star cluster. We ...
Context: Open clusters (OCs) provide homogeneous samples of white dwarfs (WDs) with known distances,...
We use data from Gaia’s second data release (DR2) to constrain the initial-final mass relation (IFMR...
textOur group has developed a Bayesian modeling technique to determine the ages of stellar populatio...
We have extended our Bayesian modeling of stellar clusters—which uses main-sequence stellar evolutio...
Using Gaia DR2 data, we present an up-to-date sample of white dwarfs within 20 pc of the Sun. In tot...
White dwarfs (WDs) offer unrealized potential in solving two problems in astrophysics: stellar age a...
We have extended our Bayesian modeling of stellar clusters-which uses main-sequence stellar evolutio...
The Gaia Data Release 1 (DR1) sample of white dwarf parallaxes is presented, including six directly ...
We present a catalogue of 73¿221 white dwarf candidates extracted from the astrometric and photometr...
Context. The initial-final mass relationship of white dwarfs, which is poorly constrained, is of par...
We report on a comparison of spectroscopic analyses for hydrogen (DA) and helium atmosphere (DB) whi...
We present a spectro-photometric analysis of 2880 cool white dwarfs within 100 pc of the Sun and coo...
Context. The initial-final mass relationship of white dwarfs, which is poorly constrained, is of par...
We present the initial–final mass relation derived from 10 white dwarfs in wide binaries that consis...
We have exploited Gaia Data Release 2 to study white dwarf members of the Praesepe star cluster. We ...
Context: Open clusters (OCs) provide homogeneous samples of white dwarfs (WDs) with known distances,...
We use data from Gaia’s second data release (DR2) to constrain the initial-final mass relation (IFMR...
textOur group has developed a Bayesian modeling technique to determine the ages of stellar populatio...
We have extended our Bayesian modeling of stellar clusters—which uses main-sequence stellar evolutio...
Using Gaia DR2 data, we present an up-to-date sample of white dwarfs within 20 pc of the Sun. In tot...
White dwarfs (WDs) offer unrealized potential in solving two problems in astrophysics: stellar age a...
We have extended our Bayesian modeling of stellar clusters-which uses main-sequence stellar evolutio...
The Gaia Data Release 1 (DR1) sample of white dwarf parallaxes is presented, including six directly ...
We present a catalogue of 73¿221 white dwarf candidates extracted from the astrometric and photometr...
Context. The initial-final mass relationship of white dwarfs, which is poorly constrained, is of par...
We report on a comparison of spectroscopic analyses for hydrogen (DA) and helium atmosphere (DB) whi...
We present a spectro-photometric analysis of 2880 cool white dwarfs within 100 pc of the Sun and coo...
Context. The initial-final mass relationship of white dwarfs, which is poorly constrained, is of par...
We present the initial–final mass relation derived from 10 white dwarfs in wide binaries that consis...