GAIA: Composition, formation and evolution of the Galaxy

By M. Perryman, K. S. Boer, G. Gilmore, E. Høg, M. Lattanzi, L. Lindegren, X. Luri, F. Mignard, O. Pace, P. de Zeeuw. 2001

957 citations recorded by the source corpus.

The GAIA astrometric mission has recently been approved as one of thenext two ``cornerstones'' of ESA's science programme, with a launch datetarget of not later than mid-2012. GAIA will provide positional andradial velocity measurements with the accuracies needed to produce astereoscopic and kinematic census of about one billion stars throughoutour Galaxy (and into the Local Group), amounting to about 1 percent ofthe Galactic stellar population. GAIA's main scientific goal is toclarify the origin and history of our Galaxy, from a quantitative censusof the stellar populations. It will advance questions such as when thestars in our Galaxy formed, when and how it was assembled, and itsdistribution of dark matter. The survey aims for completeness to V=20mag, with accuracies of about 10 mu as at 15 mag. Combined withastrophysical information for each star, provided by on-boardmulti-colour photometry and (limited) spectroscopy, these data will havethe precision necessary to quantify the early formation, and subsequentdynamical, chemical and star formation evolution of our Galaxy.Additional products include detection and orbital classification of tensof thousands of extra-Solar planetary systems, and a comprehensivesurvey of some 105-106 minor bodies in our SolarSystem, through galaxies in the nearby Universe, to some 500 000 distantquasars. It will provide a number of stringent new tests of generalrelativity and cosmology. The complete satellite system was evaluated aspart of a detailed technology study, including a detailed payloaddesign, corresponding accuracy assesments, and results from a prototypedata reduction development. (Less)

Subfields: Astronomy and Astrophysics, Computational Mechanics, Instrumentation

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Citations in the corpus

The RAVE Survey: Constraining the Local Galactic Escape Speed (2006, background): “…diminishing due to the large kinemat- ically unbiased surveys that are now underway or planned, such as RAdial Velocity Experiment (RAVE; Steinmetz et al. 2006; see also Section 4.1), Sloan Extension for Galactic Understanding and Exploration (Beers et al. 2004) and Gaia (Perryman et al. 2001).”
THE DISCOVERY AND ANALYSIS OF VERY METAL-POOR STARS IN THE GALAXY (2005, neutral): “GAIA Gaia7 is an astrometric satellite that, according to current plans, will be launched by ESA in mid-2011 (Perryman et al. 2001).”
A VLBA survey of the core shift effect in AGN jets - I. Evidence of dominating synchrotron opacity (2011, methodology): “…into account for accurate radio–optical reference frame alignme t in the era of modern space-based astrometric missions (Lindegren 2007) such as GAIA (Perryman et al. 2001) and for accurate spacecraft navigation with VLBI (e.g., Hildebrand et al. 1994, Sekido et al. 2004, Pogrebenko et al. 2009).”
Gaia FGK benchmark stars: Effective temperatures and surface gravities (2015, methodology): “We are about to revolutionise our knowledge about the Milky Way Galaxy thanks to the recently launched Gaia mission (e.g. Perryman et al. 2001; Turon et al. 2005; Lindegren et al. 2008).”
A Gaia DR2 view of the open cluster population in the Milky Way (2018, background): “The ongoing ESA mission Gaia (Perryman et al. 2001; Gaia Collaboration 2016b) is carrying out an unprecedented astrometric, photometric, and spectroscopic all-sky survey, reducing the need for cross-matching catalogues or compiling complementary data.”
The Tycho-Gaia astrometric solution. How to get 2.5 million parallaxes with less than one year of Gaia data (2014, background): “The ESA astrometry satellite Gaia was launched in December 2013 with the aim of mapping more than a billion stars (V <∼ 20) in our Galaxy (Perryman et al. 2001; de Bruijne 2012).”
Gaia broad band photometry (2010, background): “Perryman et al. (2001) and ESA (2000) presented the mission as it was approved in 2000.”
Gaia FGK benchmark stars: Metallicity (2013, background): “A major contribution in the study of the Milky Way is expected from the Gaia mission (Perryman et al. 2001).”
A non-LTE study of neutral and singly-ionized calcium in late-type stars (2006, background): “The Ca ii triplet lies at the focus of cool star research with the advent of large spectroscopic surveys of the Galaxy like the Radial Velocity Experiment (RAVE, Steinmetz et al. 2006) and the upcoming ESA Gaia satellite mission (Perryman et al. 2001).”
HABITABLE ZONES AROUND MAIN-SEQUENCE STARS: NEW ESTIMATES (2013, background): “Estimates of luminosities will be derived using photometric and spectroscopic distances for now (in cases where parallax measurements are absent), but eventually GAIA (Perryman et al. 2001) will yield very precise parallaxes (and by extension precise luminosities) for all these target stars.”
The Gaia-ESO Survey: the analysis of high-resolution UVES spectra of FGK-type stars (2014, background): “The value of the Gaia-ESO science products will be further enhanced when the results of the Gaia mission (Perryman et al. 2001) become available.”
CONSTRAINING THE MILKY WAY POTENTIAL WITH A SIX-DIMENSIONAL PHASE-SPACE MAP OF THE GD-1 STELLAR STREAM (2009, methodology): “But before the launch of Gaia, we suggest that further observations of radial velocities of stars in the stream (with deeper spectroscopy) and improvements in proper motion precision (with e.g. Pan-STARRS Kaiser et al. 2002) should be able to reduce the error bars on Galaxy parameters significantly.”
AGaiaData Release 2 catalogue of white dwarfs and a comparison with SDSS (2018, background): “Gaia determined positions, parallaxes, and proper motions for ≈ 1 per cent of the stars in the Galaxy and it aims to be complete across the full sky down to Gaia G = 20 − 21 magnitudes (Perryman et al. 2001; Gaia Collaboration et al. 2016).”
Large Synoptic Survey Telescope: From Science Drivers to Reference Design (2008, background): “The same accuracy follows from the requirement to obtain the same proper motion accuracy as Gaia (Perryman et al. 2001) at its faint limit (r ∼ 20).”