!+ ! ! bd10_synth.sfit ! An SFIT input file ! ! Purpose: != compute abundances for BD+10 2179 ! using lines in the wavalength range: 3700 4830 ! a high resolution echelle spectrum ! and assuming an old LTE model helium star atmosphere (1725L.q) ! ! Mode: ! SYN / LEVENBURG / HIRES ! ! Method: ! Read in a model atmosphere and assume a set of starting abundances ! Read in a hires optical spectrum and mask out lines to be ignored ! Synthesize hires spectrum ! Use levenburg-marquardt method to optimize selected abundances ! ! Version: ! 2004-Oct-14 (CSJ) ! 2004-Aug-17 (GJP: original) ! ! Notes: ! input for SFIT version 2.5 or later ! !- echo on sterne /electra/models/h00he99c003/t180g300he90L.q method_levenburg method_range 4052 4548 method_tolerance 0.002 ! restrict the wavelength range to save computing time method_range 4100 4400 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 ! Variable: syn_vsini 25. 10.0 ! set the rotational broadening, syn_vrad1 136.4 10.0 ! set the radial velocity !Fixed: syn_vturb 3.65 ! Fixed: Pandey's value. ! Mask braod HeI lines from fit... ! since the HeI line wings don't fit in this model, ! other lines will be affected mask{ 3 4130 4160 100 4370 4410 100 4450 4490 100 } ! Test mode: ! a) just calculate a spectrum with fixed abundances ! b) Solve for carbon abundance ! c) Solve for all light elements abundances { 1 8.53 0.0 2 11.54 0.0 5 0.10 0.0 6 8.00 1.0 7 7.81 1.0 8 7.10 1.0 12 7.01 1.0 13 5.73 1.0 14 6.94 1.0 15 5.50 1.0 16 6.75 1.0 18 6.10 1.0 20 5.10 1.0 21 1.70 0.0 22 3.84 0.0 23 2.82 0.0 24 4.06 0.0 25 3.71 0.0 26 6.18 0.0 27 4.26 0.0 28 5.05 0.0 29 3.20 0.0 30 4.34 0.0 39 1.42 0.0 40 2.40 0.0 -1 0 0 } synth save end