Sign on

SAO/NASA ADS Astronomy Abstract Service


· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· arXiv e-print (arXiv:1107.4268)
· References in the article
· Citations to the Article (2) (Citation History)
· Refereed Citations to the Article
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Identification of field dwarfs and giants in the second Radial Velocity Experiment Data Release
Authors:
Bilir, S.; Karaali, S.; Ak, S.; Önal, Ö.; CoskunogLu, B.; Seabroke, G. M.
Affiliation:
AA(Istanbul University Science Faculty, Department of Astronomy and Space Sciences, 34119, University-Istanbul, Turkey), AB(Beykent University, Faculty of Science and Letters, Department of Mathematics and Computer, Beykent 34398, Istanbul, Turkey), AC(Istanbul University Science Faculty, Department of Astronomy and Space Sciences, 34119, University-Istanbul, Turkey), AD(Istanbul University Science Faculty, Department of Astronomy and Space Sciences, 34119, University-Istanbul, Turkey), AE(Istanbul University Science Faculty, Department of Astronomy and Space Sciences, 34119, University-Istanbul, Turkey), AF(Mullard Space Science Laboratory, University College London, Hombury St Mary, Dorking RH5 6NT)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 418, Issue 1, pp. 444-455. (MNRAS Homepage)
Publication Date:
11/2011
Origin:
WILEY
Astronomy Keywords:
techniques: photometric, catalogues, surveys
Abstract Copyright:
© 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS
DOI:
10.1111/j.1365-2966.2011.19495.x
Bibliographic Code:
2011MNRAS.418..444B

Abstract

The second Radial Velocity Experiment (RAVE) Data Release (DR2) derives log g values. However, we present a simpler and cleaner method of identifying dwarfs and giants by using only magnitudes, which does not require spectroscopic analysis. We confirm the method presented in an earlier paper, with which we estimate the number of dwarfs and giants using their positions in the J-V two-magnitude diagram, by applying it to RAVE DR2. It is effective in estimating the number of dwarfs and giants at J-H > 0.4 compared to RAVE's log g values. For J-H<= 0.4, where dwarfs and subgiants show a continuous transition in the J magnitude histogram, we used the Besançon Galaxy model predictions to statistically isolate giants. The percentages of giants for red stars and for the whole sample are 85 and 34 per cent, respectively. If we add the subgiants, the percentage of evolved stars for the whole sample increases to 59 per cent. For the first time in the literature, we have analysed the effect of CHISQ on RAVE's log g values (CHISQ is the penalized chi2 from RAVE's technique of finding an optimal match between the observed spectrum and synthetic spectra to derive stellar parameters). Neither the CHISQ values nor the signal-to-noise ratio bias the RAVE log g values. Therefore, the method of identifying dwarfs and giants using the two-magnitude diagram has been verified against an unbiased data set.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)

  New!

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints