Journal
ASTRONOMY & ASTROPHYSICS
Volume 532, Issue -, Pages -Publisher
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201116715
Keywords
stars: distances; stars: fundamental parameters; Galaxy: abundances; Galaxy: disk; Galaxy: stellar content; Galaxy: structure
Categories
Funding
- AngloAustralian Observatory
- Astrophysical Institute Potsdam
- Australian National University
- Australian Research Council
- French National Research Agency
- German Research foundation
- Istituto Nazionale di Astrofisica at Padova
- Johns Hopkins University
- W.M. Keck foundation
- Macquarie University
- Netherlands Research School for Astronomy
- Natural Sciences and Engineering Research Council of Canada
- Slovenian Research Agency
- Swiss National Science Foundation
- Science & Technology Facilities Council of the UK
- US National Science Foundation [AST-0908326]
- Opticon
- Strasbourg Observatory
- University of Groningen
- PPARC/STFC
- Merton College
- Research Council under ERC-StG [GALACTICA-24027]
- University of Heidelberg
- University of Sydney
- STFC [ST/F002432/1, PP/D001242/1, ST/G002479/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/F002432/1, PP/D001242/1, ST/H00243X/1, ST/G002479/1] Funding Source: researchfish
- UK Space Agency [ST/I000852/1] Funding Source: researchfish
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [0908326] Funding Source: National Science Foundation
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We apply the method of Burnett & Binney (2010, MNRAS, 407, 339) for the determination of stellar distances and parameters to the internal catalogue of the RAdial Velocity Experiment (RAVE; Steinmetz et al. 2006, AJ, 132, 1645). Subsamples of stars that either have Hipparcos parallaxes or belong to well-studied clusters inspire confidence in the formal errors. Distances to dwarfs cooler than similar to 6000K appear to be unbiased, but those to hotter dwarfs tend to be too small by similar to 10% of the formal errors. Distances to giants tend to be too large by about the same amount. The median distance error in the whole sample of 216 000 stars is 28% and the error distribution is similar for both giants and dwarfs. Roughly half the stars in the RAVE survey are giants. The giant fraction is largest at low latitudes and in directions towards the Galactic Centre. Near the plane the metallicity distribution is remarkably narrow and centred on [M/H] = -0.04 dex; with increasing vertical bar z vertical bar it broadens out and its median moves to [M/H] similar or equal to -0.5. Mean age as a function of distance from the Galactic centre and distance vertical bar z vertical bar from the Galactic plane shows the anticipated increase in mean age with vertical bar z vertical bar.
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