Comparison between UBV- and RGU-photometrically determined density-functions for the (photometric) disc- and halo-populations in SA 82

Details Comparison between UBV- and RGU-photometrically determined density-functions for the (photometric) disc- and halo-populations in SA 82 Comparison between UBV- and RGU-photometrically determined density-functions for the (photometric) disc- and halo-populations in SA 82

Nov 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26as...58..357f&link_type=abstract

Astronomy and Astrophysics Supplement Series (ISSN 0365-0138), vol. 58, Nov. 1984, p. 357-364. Research supported by the Swiss N

Astronomy and Astrophysics

Astrophysics

5

Astronomical Photometry, Galactic Structure, Ubv Spectra, Visual Photometry, Space Density, Stellar Color

Scientific paper

A further field of the Basle Halo Program (BHP), SA 82, aiready treated in RGU by Becker and Steppe (1977), has been investigated applying analogously the BHP methods in UBV in order to compare the performance of both systems in this respect. 734 stars have been treated independently in UBV and in RGU; their two-colour diagrams for consecutive intervals in apparent V- and G-magnitude are given in figures 1 and 2, respectively. They are the basis for the calculation of logarithmic space-density-functions for both (photometric) populations (disc and halo), for consecutive 1m-intervals in absolute magnitudes (Figs. 3 and 4), as well as for the whole range covered by them (Fig. 3), as they result from their determination in each system. The overall density-functions (Fig. 5) of both systems are compared. They agree almost completely for both populations. The mean misidentification-rate per system of 4.5% is less than half the one for SA 54 of 9.2% (Fenkart and Esin-YiImaz, 1983), still further strengthening the conjecture of comparable performance of both systems in the frame of method and purpose of the BHP.

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