Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26as...80...89f&link_type=abstract
Astronomy and Astrophysics Supplement Series (ISSN 0365-0138), vol. 80, no. 1, Oct. 1989, p. 89-101. Research supported by SNSF.
Astronomy and Astrophysics
Astrophysics
18
Astronomical Photometry, Galactic Structure, Space Density, Astronomical Models, Stellar Luminosity, Ultraviolet Photometry
Scientific paper
The stars in four fields of the Basle Halo Program (BHP), henceforth called "UBV-fields", had been (photographically) observed in RGU and in UBV, in order to treat their data in both photometric systems with the same stellar-statistical method for the determination of space density gradients, developed by Becker (1%5) for the RGU-fields of the BHP The purpose was to compare the corresponding results in both systems and to obtain an idea about their mutual performance with respect to this method. All four investigations (references in Tab. I) proved it to work about equally well in both systems, if the outcome is measured in terms of a relatively rough criterion, the so-called "mean misidentification-rate per system" (MMRS). In order to obtain a better founded view about the degree of equivalence of both systems with respect to their application for the three-colour photometrical purposes of the Basle programs, we decided to treat the UBV-fields in this third contribution to the present model-comparison synopsis, in RGU and in UBV, too, by comparing the total space densities observed in both systems with the five standard model gradients and according to the comparison method homogeneously used within the "comparison-phase" of the BHP which was initiated by del Rio and Fenkart (1987). In the appendix, as in paper I, the first contribution to this synopsis (Fenkart, 1989a), we give a full description of the comparison method, and the definition of the five standard models for the space density distribution in the Galaxy which are essentially three versions of the Bahcall-Soneira (1980) two-component model. BS II i(i = 1, 2, 3), as well as a three- and a four-component version of the Gilmore-Wyse (1985) model, without and with a Thick Disk component, GW III and GW IV respectively, together with their parameters in table In addition to that, paper I contains a full account of the almost 25 years old history of the BHP, of the motivation for this synopsis and of its general disposition; it is, therefore, recommended to be consulted, if a more detailed view of the whole project is desired. The present paper, after a short introduction (Sect. 1), is concerned with the extensive discussion of the comparison results for each of its four fields, in both photometric systems (Sect. 2), and summarizes, in section 3, the general findings which consist in the acknowledgement of a significantly better performance of the RGU-system with respect to the comparison procedure, and, overall, in the confirmation (SA 82, SA 57, SA 54), or at least not exclusion (SA 133) of the existence of a Thick Disk component in the involved directions.
No associations
LandOfFree
Confirmation of the Galactic thick disk component by the Basle RGU- and UBV-photometric space densities. Synopsis of 25 years Basle Halo Program. III - RGU + UBV: SA 82, SA 133, SA 57, SA 54 does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Confirmation of the Galactic thick disk component by the Basle RGU- and UBV-photometric space densities. Synopsis of 25 years Basle Halo Program. III - RGU + UBV: SA 82, SA 133, SA 57, SA 54, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Confirmation of the Galactic thick disk component by the Basle RGU- and UBV-photometric space densities. Synopsis of 25 years Basle Halo Program. III - RGU + UBV: SA 82, SA 133, SA 57, SA 54 will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1527282