#X3 reunion no asteroids in list license

2004), complemented with IAU standards ( Udry et al. 2005), and “The Geneva-Copenhagen Survey of the Solar neighbourhood” ( Nordström et al. 2002), “Radial velocities for 6691 K and M giants” ( Famaey et al. 2007, 2010) that are all part of the HIPPARCOS catalogue and selected in three sources of RVs: “Radial velocities of 889 late-type stars” ( Nidever et al. A first list of 1420 RV-STD candidates was established ( Crifo et al. When we started to search for suitable RV-STDs in 2006, no catalogue existed that would have fulfilled the RVS requirements in terms of number of stars, magnitude range, sky coverage, and precision. The zero point (ZP) of the RVs needs to be fixed with RV standard stars (RV-STDs), however, that are known in advance and proved to be stable at a level of 300 m s −1 during the Gaia observations. (2018), the wavelength calibration is based on all bright, well-behaved, and stable FGK-type stars observed by the RVS. The latest news about Gaia can be found on the ESA website 1. The summary of the contents and survey properties of Gaia DR2 are presented in Gaia Collaboration (2018a). The RV precision is expected to be 1 km s −1 for GK type stars down to G = 12–13. The RVS will record 40 epochs on average per source during the 5 yr of the nominal mission. The RVS is an integral-field spectrograph with resolving power of ~11 500 covering the near-infra-red wavelength range at 845–872 nm. 2018), providing an unprecedented 6D map of the Milky Way ( Gaia Collaboration 2018b). The first RVS measurements are published in the Gaia Data Release 2 (DR2, Sartoretti et al. In addition to the position, parallax, and proper motion that is measured for more than one billion stars, the radial velocity (RV) is also determined for the ~150 million brightest stars ( G R V S ≲ 16.2) with the Radial Velocity Spectrometer (RVS, Katz et al. Gaia is currently scanning the sky continuously and observes all objects of magnitude 2 ≲ G ≤ 20.7. 1 IntroductionĪfter a successful launch on 19 December 2013 and after several months of commissioning activities, the Gaia satellite started its scientific observations in July 2014 ( Gaia Collaboration 2016b).

#X3 reunion no asteroids in list license

Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License ( ), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. The stars that were not used for calibration are used to validate the RVS data. A subset of the most stable stars fulfilling the RVS requirements was used to establish the radial velocity zero point provided in Gaia Data Release 2. The resulting catalogue has seven observations per star on average on a typical time baseline of 6 yr, with a median standard deviation of 15 m s −1. The zero point was established using asteroids. A catalogue of 4813 stars was built by combining these individual measurements. We compiled a dataset of ~71 000 radial velocity measurements from five high-resolution spectrographs. Therefore, the radial velocity zero point needs to be calibrated with stars that are proved to be stable at a level of 300 m s −1 during the Gaia observations. The Radial Velocity Spectrometer (RVS) on board the ESA satellite mission Gaia has no calibration device. Max Planck Institute for Extraterrestrial Physics, High Energy Group,Īims. Leibniz Institute for Astrophysics Potsdam (AIP),ĪTOS for CNES Centre Spatial de Toulouse,įaculty of Mathematics and Physics, University of Ljubljana, Institut d’Astrophysique et de Géophysique, Université de Liège,ĭepartment of Astronomy, University of Geneva, Mullard Space Science Laboratory, University College London,ĬRAAG – Centre de Recherche en Astronomie, Astrophysique et Géophysique, Observatoire de Genève, Université de Genève, Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, Bd de l’Observatoire, IMCCE, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Université, Univ. GEPI, Observatoire de Paris, Université PSL, CNRS, Bordeaux, CNRS,Į-mail: Univers et Particules de Montpellier, Université Montpellier, CNRS, Laboratoire d’astrophysique de Bordeaux, Univ. Astronomical objects: linking to databasesĬ.Including author names using non-Roman alphabets.Suggested resources for more tips on language editing in the sciences

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