Volume 653, September 2021
|Number of page(s)||11|
|Published online||13 September 2021|
Exploiting the Gaia EDR3 photometry to derive stellar temperatures
Dipartimento di Fisica e Astronomia Augusto Righi, Università degli Studi di Bologna,
Via Gobetti 93/2,
2 INAF – Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Via Gobetti 93/3, 40129 Bologna, Italy
3 University of Groningen, Kapteyn Astronomical Institute, 9747 AD Groningen, The Netherlands
Accepted: 3 June 2021
We present new colour–effective temperature (Teff) transformations based on the photometry of the early third data release (EDR3) of the ESA/Gaia mission. These relations are calibrated on a sample of about 600 dwarf and giant stars for which Teff has previously been determined with the infrared flux method from dereddened colours. The 1σ dispersion of the transformations is of 60–80 K for the pure Gaia colours (BP−RP)0, (BP−G)0, and (G−RP)0, improving to 40–60 K for colours including the 2MASS Ks-band, namely (BP−Ks)0, (RP−Ks)0, and (G−Ks)0. We validate these relations in the most challenging case of dense stellar fields, where the Gaia EDR3 photometry could be less reliable, providing guidance for the safe use of Gaia colours in crowded environments. We compare the Teff from the Gaia EDR3 colours with those obtained from standard (V−Ks)0 colours for stars in three Galactic globular clusters of different metallicity, namely NGC 104, NGC 6752, and NGC 7099. The agreement between the two estimates of Teff is excellent, with mean differences of between –50 and +50 K, depending on the colour, and with 1σ dispersions around the mean Teff differences of 25–50 K for most of the colours and below 10 K for (BP−Ks)0 and (G−Ks)0. This demonstrates that these colours are analogous to (V−Ks)0 as Teff indicators.
Key words: stars: fundamental parameters / stars: atmospheres / techniques: photometric
© ESO 2021
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