Статья

<i>Gaia</i>Early Data Release 3

M. RielloInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UKF. De AngeliInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UKD. W. EvansInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UKP. MontegriffoINAF – Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, via Gobetti 93/3, 40129 Bologna, ItalyJ. M. CarrascoInstitut de Ciències del Cosmos (ICC), Universitat de Barcelona (IEEC-UB), c/ Martí i Franquès, 1, 08028 Barcelona, SpainG. BussoInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UKL. PalaversaRuđer Bošković Institute, Bijenička cesta 54, Zagreb, CroatiaP. W. BurgessInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UKC. DienerInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UKM. DavidsonInstitute for Astronomy, School of Physics and Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh, EH9 3HJ, UKN. RowellInstitute for Astronomy, School of Physics and Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh, EH9 3HJ, UKC. FabriciusInstitut de Ciències del Cosmos (ICC), Universitat de Barcelona (IEEC-UB), c/ Martí i Franquès, 1, 08028 Barcelona, SpainC. JordiInstitut de Ciències del Cosmos (ICC), Universitat de Barcelona (IEEC-UB), c/ Martí i Franquès, 1, 08028 Barcelona, SpainM. BellazziniINAF – Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, via Gobetti 93/3, 40129 Bologna, ItalyE. PancinoINAF – Osservatorio Astrofisico di Arcetri, Largo E. Fermi, 5, 50125 Firenze, ItalyD. L. HarrisonInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UKC. CacciariINAF – Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, via Gobetti 93/3, 40129 Bologna, ItalyF. van LeeuwenInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UKN. C. HamblyInstitute for Astronomy, School of Physics and Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh, EH9 3HJ, UKS. T. HodgkinInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UKP. OsborneInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UKG. AltavillaINAF – Osservatorio Astronomico di Roma, via Frascati 33, 00078 Monte Porzio Catone (Roma), ItalyM. A. BarstowSchool of Physics & Astronomy, University of Leicester, Leicester LE9 1UP, UKA. G. A. BrownLeiden Observatory, Leiden University, Niels Bohrweg 2, 2333 CA Leiden, The NetherlandsM. CastellaniINAF – Osservatorio Astronomico di Roma, via Frascati 33, 00078 Monte Porzio Catone (Roma), ItalyS. CowellInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UKF. De LuiseINAF - Osservatorio Astronomico d’Abruzzo, Via Mentore Maggini, 64100 Teramo, ItalyG. GilmoreInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UKG. GiuffridaINAF – Osservatorio Astronomico di Roma, via Frascati 33, 00078 Monte Porzio Catone (Roma), ItalyS. L. HidalgoIAC - Instituto de Astrofisica de Canarias, Via Láctea s/n, 38200 La Laguna S.C., Tenerife, SpainG. HollandInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UKS. MarinoniINAF – Osservatorio Astronomico di Roma, via Frascati 33, 00078 Monte Porzio Catone (Roma), ItalyC. PaganiSchool of Physics & Astronomy, University of Leicester, Leicester LE9 1UP, UKA. M. PiersimoniINAF - Osservatorio Astronomico d’Abruzzo, Via Mentore Maggini, 64100 Teramo, ItalyL. PuloneINAF – Osservatorio Astronomico di Roma, via Frascati 33, 00078 Monte Porzio Catone (Roma), ItalyS. RagainiINAF – Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, via Gobetti 93/3, 40129 Bologna, ItalyM. RainerINAF – Osservatorio Astrofisico di Arcetri, Largo E. Fermi, 5, 50125 Firenze, ItalyP. J. RichardsSTFC, Rutherford Appleton Laboratory, Harwell, Didcot, OX11 0QX, UKN. SannaINAF – Osservatorio Astrofisico di Arcetri, Largo E. Fermi, 5, 50125 Firenze, ItalyN. A. WaltonInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UKM. WeilerInstitut de Ciències del Cosmos (ICC), Universitat de Barcelona (IEEC-UB), c/ Martí i Franquès, 1, 08028 Barcelona, SpainA. YoldasInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK

2020en

ABI

Аннотация

Context. Gaia Early Data Release 3 ( Gaia EDR3) contains astrometry and photometry results for about 1.8 billion sources based on observations collected by the European Space Agency Gaia satellite during the first 34 months of its operational phase. Aims. In this paper, we focus on the photometric content, describing the input data, the algorithms, the processing, and the validation of the results. Particular attention is given to the quality of the data and to a number of features that users may need to take into account to make the best use of the Gaia EDR3 catalogue. Methods. The processing broadly followed the same procedure as for Gaia DR2, but with significant improvements in several aspects of the blue and red photometer (BP and RP) preprocessing and in the photometric calibration process. In particular, the treatment of the BP and RP background has been updated to include a better estimation of the local background, and the detection of crowding effects has been used to exclude affected data from the calibrations. The photometric calibration models have also been updated to account for flux loss over the whole magnitude range. Significant improvements in the modelling and calibration of the Gaia point and line spread functions have also helped to reduce a number of instrumental effects that were still present in DR2. Results. Gaia EDR3 contains 1.806 billion sources with G -band photometry and 1.540 billion sources with G BP and G RP photometry. The median uncertainty in the G -band photometry, as measured from the standard deviation of the internally calibrated mean photometry for a given source, is 0.2 mmag at magnitude G = 10–14, 0.8 mmag at G ≈ 17, and 2.6 mmag at G ≈ 19. The significant magnitude term found in the Gaia DR2 photometry is no longer visible, and overall there are no trends larger than 1 mmag mag −1 . Using one passband over the whole colour and magnitude range leaves no systematics above the 1% level in magnitude in any of the bands, and a larger systematic is present for a very small sample of bright and blue sources. A detailed description of the residual systematic effects is provided. Overall the quality of the calibrated mean photometry in Gaia EDR3 is superior with respect to DR2 for all bands.

Перевод пока недоступен

Идентификаторы

DOI: 10.1051/0004-6361/202039587

Цитирования и источники

Цитирований: 2Использованных источников: 0

Показатели — AkademScholar