Confirmation of the Galactic thick disk component by the Basle RGU- and UBV-photometric space densities. IV - Synopsis of 25 years Basle Halo Program: SA 107, SA 51

Details Confirmation of the Galactic thick disk component by the Basle RGU- and UBV-photometric space densities. IV - Synopsis of 25 years Basle Halo Program: SA 107, SA 51 Confirmation of the Galactic thick disk component by the Basle RGU- and UBV-photometric space densities. IV - Synopsis of 25 years Basle Halo Program: SA 107, SA 51

Dec 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26as...81..187f&link_type=abstract

Astronomy and Astrophysics Supplement Series (ISSN 0365-0138), vol. 81, no. 2, Dec. 1989, p. 187-195. Research supported by SNSF

Astronomy and Astrophysics

Astrophysics

24

Astronomical Models, Astronomical Photometry, Galactic Structure, Space Density, Ubv Spectra, Halos, Least Squares Method

Scientific paper

This is the last contribution to the four part Basle synopsis which compares RGU-photometrically determined space densities in both photometric populations, I and II, with density gradients of a discriminative set of multicomponent models. It submits two fields, SA 107 and SA 51, to the involved comparison procedure in this separate paper (N), since their density histograms had been derived, for one or more luminosity-groups, over distance intervals which, partly, are not the same for both populations; so they had to be approximated by least-square solution curves to be added to total (I+II) densities which, in this form, can be compared to the total model densities. The comparison procedure itself, as well as the model definitions, are fully described in the appendix, and the model parameters are given in its table A The slight, technically caused modification of the comparison method evidently does not afflict the homogeneity of the procedure, nor the consistency of the obtained results with the ones of the whole synopsis. The observations in both fields, again, prefer the Thick Disk model GW IV as best fitting. SA 51, almost in anticentre-direction, does so quite unconditionally, like the overwhelming majority of all fields treated within the comparison phase of the Basle Halo Program. For SA 107, this is true to a lesser degree, conform to its position in the centre-hemisphere (cf. the similar behaviour of the fields in paper II (Fenkart, 1989b)).

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