Progress on the calibration of surface brightness-color relations for early- and late-type stars. (arXiv:2106.01073v2 [astro-ph.SR] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Salsi_A/0/1/0/all/0/1">Anthony Salsi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nardetto_N/0/1/0/all/0/1">Nicolas Nardetto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mourard_D/0/1/0/all/0/1">Denis Mourard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Graczyk_D/0/1/0/all/0/1">Dariusz Graczyk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Taormina_M/0/1/0/all/0/1">Monica Taormina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Creevey_O/0/1/0/all/0/1">Orlagh Creevey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hocde_V/0/1/0/all/0/1">Vincent Hocdé</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morand_F/0/1/0/all/0/1">Frédéric Morand</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perraut_K/0/1/0/all/0/1">Karine Perraut</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pietrzynski_G/0/1/0/all/0/1">Grzegorz Pietrzynski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schaefer_G/0/1/0/all/0/1">Gail H. Schaefer</a>
Surface brightness-color relations (SBCRs) are used for estimating angular
diameters and deriving stellar properties. They are critical to derive
extragalactic distances of early-type and late-type eclipsing binaries or,
potentially, for extracting planetary parameters of late-type stars hosting
planets. Various SBCRs have been implemented so far, but strong discrepancies
in terms of precision and accuracy still exist in the literature. We aim to
develop a precise SBCR for early-type B and A stars using selection criteria,
based on stellar characteristics, and combined with homogeneous interferometric
angular diameter measurements. We also improve SBCRs for late-type stars, in
particular in the Gaia photometric band. We observed 18 early-type stars with
the VEGA interferometric instrument, installed on the CHARA array. We then
applied additional criteria on the photometric measurements, together with
stellar characteristics diagnostics in order to build the SBCRs. We calibrated
a SBCR for subgiant and dwarf early-type stars. The RMS of the relation is
$sigma_{F_{V_{0}}} = 0.0051,$mag, leading to an average precision of 2.3% on
the estimation of angular diameters, with 3.1% for $V-K < -0.2,$mag and 1.8%
for $V-K > -0.2,$mag. We found that the conversion between Johnson-$K$ and
2MASS-$K_s$ photometries is a key issue for early-type stars. Following this
result, we have revisited our previous SBCRs for late-type stars by calibrating
them with either converted Johnson-$K$ or 2MASS-$K_s$ photometries. We also
improve the calibration of these SBCRs based on the Gaia photometry. The
expected precision on the angular diameter using our SBCRs for late-type stars
ranges from 1.0% to 2.7%. By reaching a precision of 2.3% on the estimation of
angular diameters for early-type stars, significant progress has been made to
determine extragalactic distances using early-type eclipsing binaries.
Surface brightness-color relations (SBCRs) are used for estimating angular
diameters and deriving stellar properties. They are critical to derive
extragalactic distances of early-type and late-type eclipsing binaries or,
potentially, for extracting planetary parameters of late-type stars hosting
planets. Various SBCRs have been implemented so far, but strong discrepancies
in terms of precision and accuracy still exist in the literature. We aim to
develop a precise SBCR for early-type B and A stars using selection criteria,
based on stellar characteristics, and combined with homogeneous interferometric
angular diameter measurements. We also improve SBCRs for late-type stars, in
particular in the Gaia photometric band. We observed 18 early-type stars with
the VEGA interferometric instrument, installed on the CHARA array. We then
applied additional criteria on the photometric measurements, together with
stellar characteristics diagnostics in order to build the SBCRs. We calibrated
a SBCR for subgiant and dwarf early-type stars. The RMS of the relation is
$sigma_{F_{V_{0}}} = 0.0051,$mag, leading to an average precision of 2.3% on
the estimation of angular diameters, with 3.1% for $V-K < -0.2,$mag and 1.8%
for $V-K > -0.2,$mag. We found that the conversion between Johnson-$K$ and
2MASS-$K_s$ photometries is a key issue for early-type stars. Following this
result, we have revisited our previous SBCRs for late-type stars by calibrating
them with either converted Johnson-$K$ or 2MASS-$K_s$ photometries. We also
improve the calibration of these SBCRs based on the Gaia photometry. The
expected precision on the angular diameter using our SBCRs for late-type stars
ranges from 1.0% to 2.7%. By reaching a precision of 2.3% on the estimation of
angular diameters for early-type stars, significant progress has been made to
determine extragalactic distances using early-type eclipsing binaries.
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