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