2004/05/25 by Yüksel Karataş, Y. Karatas, S. Bilir +3
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Galactic halo #Galactic plane #Galaxies: Formation, Evolution, Phenomena #Galaxy #Halo #Metallicity #Photometry (optics) #Physics #Stars #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1002/asna.200310254
7 pages, 7 figures and 3 tables, accepted for publication in AN
arxiv created 2004/05/25 · openalex publication_date 2004/11/18 · arxiv updated 2015/06/24 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Abstract We interpret the de‐reddened UBV data for the field SA 133 to deduce the stellar density and metallicity distribution functions. The logarithmic local space density for giants, D *(0) = 6.40, and the agreement of the luminosity function for dwarfs and sub‐giants with the one of Hipparcos confirms the empirical method used for their separation. The metallicity distribution for dwarfs gives a narrow peak at [ Fe/H ] = +0.13 dex, due to apparently bright limiting magnitude, V o = 16.5, whereas late‐type giants extending up to z ∼ 4.5 kpc from the galactic plane have a multimodal distribution. The metallicity distribution for giants gives a steep gradient d[Fe/H]/d z = –0.75 dex kpc –1 for thin disk and thick disk whereas a smaller value for the halo, i.e. d[Fe/H]/d z = –0.45 dex kpc –1 . (© 2004 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)