!+
!
! bd10_solve.sfit
!   An SFIT input file
!
! Purpose:
!=  compute abundancesTeff, log g, etc,  for BD+10 2179
!   using lines in the wavalength range: 3800 5200
!   a high resolution echelle spectrum
!   and assuming the new (STERNE2) LTE model grid
!
!   :: NB the Opacity Sampling Grid will come soon. 
!
! Mode: 
!   SLV / LEVENBURG ?? / HIRES
!
! Method: 
!   Read in a model atmosphere grid (h00he99c003, he99c010, he97c030) 
!   Read in a hires optical spectrum [ and mask out lines to be ignored ]
!   Uses amoeba  to find optimum model.
! 
!   Solves first for (Teff, log g, vsini, vrad)
!   then solves for the helium abundance (nHe) which, with the given grid, 
!   is effectively a first approximation for the carbon abundance (nC). 
!   Finally, we check log g, Teff for this C abundance. 
!
!
! Version:
!   2004-Oct-14 (CSJ)
!
! Notes:
!   input for SFIT version 2.5 or later
!
!-




read_grid bd10_fine.grd

method_amoeba
method_range  4054 4545
method_tolerance 0.0001

data_spectrum bd10op.sp2       ! file name
data_sigma 0.007
data_instrument 0.10                 ! instrumental profile FWHM (Angstroms)
data_cosmic 1.2                      ! threshold for cosmic ray rejection

fix_ahe1   0.989 
slv_teff1  17.0  2.0 
slv_logg1  2.5   0.5
slv_vsini1 27.5  10.
slv_vrad1  137.4 10.

solve

fix_teff1 ; fix_logg1 ; fix_vsini1 ; fix_vrad1 ; slv_ahe1 

solve

slv_teff1 ; slv_logg1 ; fix_ahe1

solve

end