On the use of <i>Gaia</i> magnitudes and new tables of bolometric corrections

Casagrande, Luca; VandenBerg, Don A.

doi:10.1093/mnrasl/sly104

Cited by 228 publications

(157 citation statements)

References 19 publications

(21 reference statements)

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“…This correction places magnitudes about 30 mmag higher than when using the Casagrande & VandenBerg (2018b) correction in the applicable magnitude range. We expect the scale of this systematic offset to have a negligible impact on our results, and therefore adopt the Casagrande & VandenBerg (2018b) correction in this work for consistency with our chosen G band extinction coefficients and bolometric corrections. Our model also uses an extinction for each star in each band.…”

Section: Datamentioning

confidence: 96%

“…We converted reddening to the band-specific extinctionÂ λ using extinction coefficients unique to the Green et al (2018) map for the K band 4 . For the Gaia G-band we calculated our band-specific extinction using the mean extinction coefficient presented in Casagrande & VandenBerg (2018b), after converting our reddening value to a measure of E(B − V) following the conventions presented in Green et al (2018). (Paxton et al 2011(Paxton et al , 2013(Paxton et al , 2015(for details about the physical inputs of the models see Khan et al 2018).…”

Section: Datamentioning

confidence: 99%

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Testing asteroseismology with Gaia DR2: hierarchical models of the Red Clump

Hall

Davies

Elsworth

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Asteroseismology provides fundamental stellar parameters independent of distance, but subject to systematics under calibration. Gaia DR2 has provided parallaxes for a billion stars, which are offset by a parallax zero-point ( zp ). Red Clump (RC) stars have a narrow spread in luminosity, thus functioning as standard candles to calibrate these systematics. This work measures how the magnitude and spread of the RC in the Kepler field are affected by changes to temperature and scaling relations for seismology, and changes to the parallax zero-point for Gaia. We use a sample of 5576 RC stars classified through asteroseismology. We apply hierarchical Bayesian latent variable models, finding the population level properties of the RC with seismology, and use those as priors on Gaia parallaxes to find zp . We then find the position of the RC using published values for zp . We find a seismic temperature insensitive spread of the RC of ∼ 0.03 mag in the 2MASS K band and a larger and slightly temperature-dependent spread of ∼ 0.13 mag in the Gaia G band. This intrinsic dispersion in the K band provides a distance precision of ∼ 1% for RC stars. Using Gaia data alone, we find a mean zero-point of −41 ± 10 µas. This offset yields RC absolute magnitudes of −1.634 ± 0.018 in K and 0.546 ± 0.016 in G. Obtaining these same values through seismology would require a global temperature shift of ∼ −70 K, which is compatible with known systematics in spectroscopy.

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Section: Datamentioning

confidence: 96%

Section: Datamentioning

confidence: 99%

Testing asteroseismology with Gaia DR2: hierarchical models of the Red Clump

Hall

Davies

Elsworth

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…G brighter and fainter than 11 mag and a correction for the G magnitude drift Weiler 2018;Casagrande & VandenBerg 2018) of 3.5 mmag per magnitude. Stars brighter than G < 6 mag have been removed to avoid saturation issues and fainter than G BP < 18 to avoid background subtraction issues (Evans et al 2018;Arenou et al 2018).…”

Section: Deriving the Extinctionmentioning

confidence: 99%

Gaia-2MASS 3D maps of Galactic interstellar dust within 3 kpc

Lallement

Babusiaux

Vergely

et al. 2019

A&A

346

365

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Gaia stellar measurements are currently revolutionizing our knowledge of the evolutionary history of the Milky Way. 3D maps of the interstellar dust provide complementary information and are a tool for a wide range of uses. We aimed at building 3D maps of the dust in the Local arm and surrounding regions. To do so, Gaia DR2 photometric data were combined with 2MASS measurements to derive extinction towards stars that possess accurate photometry and relative uncertainties on DR2 parallaxes smaller than 20%. We applied to the individual extinctions a new hierarchical inversion algorithm adapted to large datasets and to a inhomogeneous target distribution. Each step associates regularized Bayesian inversions along all radial directions and a subsequent inversion in 3D of all their results. Each inverted distribution serves as a prior for the subsequent step and the spatial resolution is progressively increased. We present the resulting 3D distribution of the dust in a 6 x 6 x 0.8 kpc 3 volume around the Sun. Its main features are found to be elongated along different directions that vary from below to above the mid-plane: the outer part of Carina-Sagittarius, mainly located above the mid-plane, the Local arm/Cygnus Rift around and above the mid-plane and the fragmented Perseus arm are oriented close to the direction of circular motion. The more than 2 kpc long spur (nicknamed the split) that extends between the Local Arm and Carina-Sagittarius, the compact near side of Carina-Sagittarius and the Cygnus Rift below the Plane are oriented along l∼40 to 55 • . Dust density images in vertical planes reveal in some regions a wavy pattern and show that the solar neighborhood within ∼500 pc remains atypical by its extent above and below the Plane. We show several comparisons with the locations of molecular clouds, HII regions, O stars and masers. The link between the dust concentration and these tracers is markedly different from one region to the other.

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“…For Ret III, which has no available measurement of [Fe/H], we assumed the mean value for all the UFDs, which is −2.4 dex. For the reddening correction we used A G = 2.740 E(B − V ) (Casagrande & VandenBerg 2018). The excess color E(B − V ) (Schlegel et al 1998) was obtained using the python task dustmaps (Green 2018).…”

Section: Distancesmentioning

confidence: 99%

Gaia RR Lyrae Stars in Nearby Ultra-faint Dwarf Satellite Galaxies

Vivas

Martı́nez-Vázquez

Walker

2020

ApJS

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We search for RR Lyrae stars in 27 nearby (< 100 kpc) ultra-faint dwarf satellite galaxies using the Gaia DR2 catalog of RR Lyrae stars. Based on proper motions, magnitudes and location on the sky, we associate 47 Gaia RR Lyrae stars to 14 different satellites. Distances based on RR Lyrae stars are provided for those galaxies. We have identified RR Lyrae stars for the first time in the Tucana II dwarf galaxy, and find additional members in Ursa Major II, Coma Berenices, Hydrus I, Bootes I and Bootes III. In addition we have identified candidate extra-tidal RR Lyrae stars in six galaxies which suggest they may be undergoing tidal disruption. We found 10 galaxies have no RR Lyrae stars neither in Gaia nor in the literature. However, given the known completeness of Gaia DR2 we cannot conclude these galaxies indeed lack variable stars of this type.

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On the use of Gaia magnitudes and new tables of bolometric corrections

Cited by 228 publications

References 19 publications

Testing asteroseismology with Gaia DR2: hierarchical models of the Red Clump

Testing asteroseismology with Gaia DR2: hierarchical models of the Red Clump

Gaia-2MASS 3D maps of Galactic interstellar dust within 3 kpc

Gaia RR Lyrae Stars in Nearby Ultra-faint Dwarf Satellite Galaxies

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