2018
DOI: 10.1051/0004-6361/201832756
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Gaia Data Release 2

Abstract: Aims. We describe the photometric content of the second data release of the Gaia project (Gaia DR2) and its validation along with the quality of the data. Methods. The validation was mainly carried out using an internal analysis of the photometry. External comparisons were also made, but were limited by the precision and systematics that may be present in the external catalogues used. Results. In addition to the photometric quality assessment, we present the best estimates of the three photometric passbands. V… Show more

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Cited by 669 publications
(312 citation statements)
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References 27 publications
(56 reference statements)
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“…We found excellent agreement with Bessell & Murphy (2012) and Cohen et al (2003). The Gaia G B and G R filter function (see Evans et al 2018) were obtained from the Gaia website. To be consistent with our calculations for the other passbands we then determined zero points for these filters again by using HST Vega stis005 spectrum.…”
Section: Interstellar Reddening and Distancesupporting
confidence: 69%
“…We found excellent agreement with Bessell & Murphy (2012) and Cohen et al (2003). The Gaia G B and G R filter function (see Evans et al 2018) were obtained from the Gaia website. To be consistent with our calculations for the other passbands we then determined zero points for these filters again by using HST Vega stis005 spectrum.…”
Section: Interstellar Reddening and Distancesupporting
confidence: 69%
“…The similarities between the Gaia G-band ( 20% transmission 4000-9000Å; Evans et al 2018) and Kepler Kp-band helped us to identify our K2 target in the Gaia data in the case of multiple cross-matches, which could be a binary companion or background source. There are 212,376 K2 targets with a single Gaia crossmatch within 4 ′′ , 21,075 K2 targets with more than one cross-match, and 41,702 without any Gaia matches.…”
Section: Gaiamentioning
confidence: 99%
“…We follow Bergeron et al (1997) to perform our SED analysis (also see Gentile Fusillo et al 2019). We first construct the SED of the white dwarf using photometry from Gaia DR2, PS1, and the UKIDSS Hemisphere Survey (Table 1), and convert magnitudes into fluxes using zero-point fluxes from Evans et al (2018), Tonry et al (2012), and Lawrence et al (2007), respectively. We do not include 2MASS photometry, whose uncertainties are too large to constrain models.…”
Section: The White Dwarf Primarymentioning
confidence: 99%