Analysis of UBV photometry in selected area 133

Abstract

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 [F e/H] = +0.13 dex, due to apparently bright limiting magnitude, Vo = 16.5, whereas late-type giants extending up to z ∼ 4.5 kpc from the galactic plane have a multimodal distribution.

Galactic model parameters for field giants separated from field dwarfs by their 2MASS and V apparent magnitudes

“…(in RGU system M (G) ≥ 6 m and M (G) < 6 m , respectively). The works of Karaali (1992); Ak, Karaali & Buser (1998); Karatas ¸, Karaali & Buser (2001); Karaali et al (2004b); Bilir, Karaali & Buser (2004); and Karatas ¸et al (2004) can be given as examples for application of this procedure.…”

Separation of dwarf and giant stars with ROTSE–IIId

“…(in RGU system M (G) ≥ 6 m and M (G) < 6 m , respectively). The works of Karaali (1992); Ak, Karaali & Buser (1998); ; Karaali et al (2000); Karatas ¸, Karaali & Buser (2001); ; Bilir, Karaali & Correspondence to: sbilir@istanbul.edu.tr and Karatas ¸et al (2004) can be given as examples for application of this procedure.…”