Bahcall and Soniera help page
C
C Bahcall-Soneira Galaxy model for star counts October 1978
C Visual Band counts with B-V colors
C
C Provision for transformation to February 1983
C other bands and colors
C R.M. Soneira
c
c Includes reddening as well as obscuration. R. M. Soneira/
c J. N. Bahcall
c (about 6/85)
c
c Modified to output UV magnitudes. N. Brosch
c (from 4/1989)
c Modified for 1500A calculations N.B. end July 1989
c
c Modified to include white dwarfs component and
c output magnitudes in one of 3 UV bands (1500A, 2000A and 2500A)
c which is selected interactively. E. Almoznino,
c (Feb.90)
c
c Includes cutoff in disk giants at Mabs = -1.5 (B-V = 1.7) Bahcall
c (5/86)
c Uses IMSL subroutines for spline fitting of color-magnitude
c diagrams.
c
c Ported to SUN SPARC by NB NB (Feb 1991)
c
C------------------------------------------------------------------------------
c
C The model is based on the following papers:
C 1. Ap. J. Suppl. 44, 73 (1980) - Original model paper
C 2. Ap. J. Letters 238, L17 (1980) - Principal results from above
C 3. Ap. J. 246, 122 (1981) - Bright stars and disk giants
C 4. Ap. J. Suppl. 47, 401 (1981) - Tabulated counts; halo counts
C 5. Ap. J. 255, 181 (1982) - Luminosity function in R,I,J,K bands
C 6. Ap. J. 265, 730 (1983) - Galactic spheroid in detail
C 7. Ap. J. 272, 627 (1983) - Giants in the spheroid
C 8. Ap. J.,Suppl. 55, 67 (1984) - Comparisons with 5 Fields
C 9. IAU Colloquium 76, p. 259 (1983)-Discussion and comparison
c 10. Ap. J. 299, December 15(1984) -The Basel Catalog
c 11 Ann. Rev. Astr. Astrophys. 24 -Summary/Next Steps/Open Questions
c
C------------------------------------------------------------------------------
c
c
c ***********************************************************************
c
c For the purpose of this program only, IMSL has authorized the reprint
c of selected source code taken from the IMSL library. This source code
c is subject to copyright protection and is considered to be confidential
c and proprietary information of IMSL. Use, duplication, or distribution
c of the IMSL source code in any form is strictly prophibited.
c
c
c ************************************************************************
C
C The parameter values specified are for
C The Bahcall-Soneira Standard Galaxy Model for the Visual band.
C
C Those parameters which change with band are marked with the symbol ###
C See paper 5 for parameter values for the R, I, J, K bands.
C See papers 4 and 5 for transformation methods to other bands.
C
C It is possible to keep the absolute magnitude distribution in space
C in the Visual band and transform only the apparent magnitudes
C to any band which can be expressed in terms of V and B-V.
C Colors can also be transformed from B-V into any other system which
C can be expressed in terms of B-V and/or absolute Visual magnitude.
C The place to do this is in the subroutine BVC which
C knows both V and B-V.
C
C Note: If you are transforming only the apparent magnitudes,
C then use parameters for V absolute magnitudes throughout.
C
C * The modification for UV magnitudes relies on relationships between
C (UV-V) and (B-V) colors. The UV magnitudes are "monochromatic", i.e.
C they are a transformation of the measured UV flux density eye-averaged
C over a small (~50A) band centered on the nominal band center.
C
C * The UV measured flux densities, in erg/s/cm2/A, are from the
C ESA IUE spectral catalog and from the NASA IUE spectral catalog.
C
C El * The UV colors of white dwarfs are based on the assumption of
C black bodies. In order to change the output color for the white
C dwarfs component, the only change should be done on the conversion
C tables (COLO, UCOLO, UCOL20 and UCOL25) in function DWACOL.
C
C------------------------------------------------------------------------------
C The model has been compared to data down to 20 deg galactic latitude.
C This program has been tested to only 10 deg galactic latitude.
C Please exercise caution below these limits.
C------------------------------------------------------------------------------
Output:
Redden Out
Results of the calculation for each of the galaxy components. include header for
each component.
Magnitude
Counts per magnitude bin. the columns are: mag. bin, A(N), N(N). where A(N) is the
differential counts and N(N) is the integrated counts.
Color
Counts per color bin. the columns are:(B-V),(UV-V),Total,Disk contribution, Sphere
contribution, W.D. contribution.
Input Parameters
Graphic output
If yes two extra files without header will be produced, one for the total
number of stars per mag., and the second is the (B-V) distribution.
Galactic Latitude
Galactic Latitude, in f6.2 format
Galactic Longitude
Galactic Longitude in f6.2 format
Eccentricity
Spheroid axis ratio, E = Rez/Rex and Rey = Rex
Re(kpc)
de Vaucouleurs radius for spheroid (kpc). Rex * Rez = Re*Re = REK*REK
m1
default apparent magnitude interval for color distribution - lower limit
m2
default apparent magnitude interval for color distribution - upper limit
Mbright
luminosity function bright-end cutoff for disk
Mdimm
luminosity function dim-end cutoff
dM
apparent magnitude bin size
Benny Bilenko
Last modified: Sun Mar 5 01:40:07 PST 2000