Reanalysis of the Gaia Data Release 2 photometric sensitivity curves using HST/STIS spectrophotometry

• Published in: Astronomy and astrophysics (Berlin) Vol. 619; p. A180
• Main Authors: Maíz Apellániz, J., Weiler, M.
• Format: Journal Article
• Language: English
• Published: Heidelberg EDP Sciences 01.11.2018
• Subjects: Apertures; Calibration; Color; Hubble Space Telescope; Identification methods; Libraries; methods: data analysis; Photometry; Sensitivity; Sensitivity analysis; Space telescopes; Spectral energy distribution; Spectrophotometry; surveys; techniques: photometric
• ISSN: 0004-6361; 1432-0746
• DOI: 10.1051/0004-6361/201834051

Context. The second data release (DR2) from the European Space Agency mission Gaia took place on April 2018. DR2 included photometry for more than 1.3 × 109 sources in the three bands G, GBP, and GRP. Even though the Gaia DR2 photometry is very precise, there are currently three alternative definitions of the sensitivity curves that show significative differences. Aims. The aim of this paper is to improve the quality of the input calibration data to produce new compatible definitions of the G, GBP, and GRP bands and to identify the reasons for the discrepancies between previous definitions. Methods. We have searched the Hubble Space Telescope (HST) archive for Space Telescope Imaging Spectrograph (STIS) spectra with G430L+G750L data obtained with wide apertures and combined them with the CALSPEC library to produce a high quality spectral energy distribution (SED) library of 122 stars with a broad range of colors, including three very red stars. This library defines new sensitivity curves for G, GBP, and GRP using a functional analytical formalism. Results. The new sensitivity curves are significantly better than the two previous attempts we use as a reference, REV (Evans et al. 2018, A&A, 616, A4) and WEI (Weiler 2018, A&A, 616, A17). For G we confirm the existence of a systematic bias in magnitude and correct a color term present in REV. For GBP we confirm the need to define two magnitude ranges with different sensitivity curves and measure the cut between them at Gphot = 10.87 mag with a significant increase in precision. The new curves also fit the data better than either REV or WEI. For GRP, our new sensitivity curve fits the STIS spectra better and the differences with previous attempts reside in a systematic effect between ground-based and HST spectral libraries. Additional evidence from color–color diagrams indicate that the new sensitivity curve is more accurate. Nevertheless, there is still room for improvement in the accuracy of the sensitivity curves because of the current dearth of good-quality red calibrators: adding more to the sample should be a priority before Gaia data release 3 takes place.