Gaia Data Release 2

By Gaia Collaboration, C. Babusiaux, F. V. Leeuwen, M. Barstow, C. Jordi, Antonella Vallenari, D. Bossini, A. Bressan, T. Cantat-Gaudin, M. Leeuwen and 443 more. Astronomy & Astrophysics, 2018

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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. Various colour-colour transformations are also derived to enable the users to convert between the Gaia and commonly used passbands. Conclusions. The internal analysis of the data shows that the photometric calibrations can reach a precision as low as 2 mmag on individual CCD measurements. Other tests show that systematic effects are present in the data at the 10 mmag level.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Instrumentation

View Paper: https://www.semanticscholar.org/paper/6bc7d19d883e9241e245de7ba2b98298f4eb157a

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Citations in the corpus

AGaiaData Release 2 catalogue of white dwarfs and a comparison with SDSS (2018, methodology): “By contrast, Gaia Data Release 2 (DR2; Gaia Collaboration et al. 2018a) is more complete by orders of magnitude, and it provides precise astrometry (Lindegren et al. 2018) as well as GBP (330–680 nm), GRP (640–1000 nm), and G (330–1000 nm) passband photometry (Evans et al. 2018).”
Painting a portrait of the Galactic disc with its stellar clusters (2020, methodology): “Since we binned the millimag-precision Gaia DR2 photometry (Evans et al. 2018) into a grid with a resolution of 0.2 mag in colour and 0.5 mag in G magnitude, our approach is obviously not able to take advantage of the finest features observed in some Gaia CMDs.”
Abundance Estimates for 16 Elements in 6 Million Stars from LAMOST DR5 Low-Resolution Spectra (2019, background): “The G, BP andRP photometries are from Gaia DR2 (Gaia Collaboration et al. 2018; Evans et al. 2018).”
Confirmation of the Gaia DR2 Parallax Zero-point Offset Using Asteroseismology and Spectroscopy in the Kepler Field (2018, neutral): “…eff d s d s= + +n ¢ , with i effsn as the astrometric_pseudo_colour_error field for star i from the DR2 catalog, and σiG the uncertainty on G, which we assign as 1%, which reflects the 10 mmag level systematics in Gaia photometry for G>3 based on comparison to external catalogs (Evans et al. 2018).”
A million binaries from Gaia eDR3: sample selection and validation of Gaia parallax uncertainties (2021, methodology): “ER18 and Tian et al. (2020) required both components of candidate binaries to have𝐺BP−𝐺RP colors and to pass photometric quality cuts related to the bp_rp_excess_factor reported in Gaia DR2 (Evans et al. 2018).”
Proper motions and dynamics of the Milky Way globular cluster system fromGaiaDR2 (2018, methodology): “…B1 – continued Isochrone tracks for the assumed age, metallicity and distance are plotted in the left panel by blue dots (PARSEC, Bressan et al. 2012) and green dots (MIST, Choi et al. 2016), with extinction and reddening computed using the coefficients from Table 1 in Babusiaux et al. (2018).”
The Optical to Mid-infrared Extinction Law Based on the APOGEE, Gaia DR2, Pan-STARRS1, SDSS, APASS, 2MASS, and WISE Surveys (2019, background): “Concerning the photometric content, the photometric calibrations can reach a precision as low as 2 mmag on individual measurements, and the systematic effects are present at the 10 mmag level (Evans et al. 2018).”
A Gaia DR2 view of the open cluster population in the Milky Way (2018, background): “As discussed in Evans et al. (2018) and illustrated in Arenou et al. (2018), the GBP and GRP fluxes of Gaia DR2 sources might be overestimated as a result of background contamination, and the effect is especially relevant in crowded fields such as the core of globular clusters.”
Gaia Data Release 2 (2018, background): “An indicator of possible issues with the BP and RP photometry is the flux excess factor E = (IBP + IRP)/IG (phot_bp_rp_excess_factor), where IX is the photometric flux in band X (Evans et al. 2018).”