lte-codes sterne spectrum ffit sfit grids idlines
commands ffit

FFIT


Solves for T, theta, E(B-V) for one or two stars by fitting theoretical flux distributions to observed fluxes and/or photometry.

Example 1. Fit Teff, theta and E(B-V) to IUE spectrum and uvby photometry using a grid of helium-rich model flux distributions.

models{
2
t01980001 Helium-rich constant g
11 1 1
0 0 0
/simon/models/01980001/19325he90L.s
/simon/models/01980001/20325he90L.s
/simon/models/01980001/21325he90L.s
/simon/models/01980001/22325he90L.s
/simon/models/01980001/23325he90L.s
/simon/models/01980001/24325he90L.s
/simon/models/01980001/25325he90L.s
/simon/models/01980001/26325he90L.s
/simon/models/01980001/27325he90L.s
/simon/models/01980001/28325he90L.s
}

!---! define model spectrum grid
! file format specifier
! grid title
! grid dimensions
! grid wavelength (use defaults)
! grid filenames

 

wavelengths{
iue
phot 4 uvby
}

!---! define photmetric system
! use standard IUE wavelength range
! use Stromgren magnitudes

parameters{
3
20.0 1.0 'Teff kK'
0.03 0.01 'Ebv'
3.0E-11 0.5E-11 'theta'
}

 
data{
folder .
iue 059x.sp2
phot 10.487 10.516 10.501 10.559
errors 0.03 0.03 0.03 0.001
}


!---! read spectrum to fit
! data in current folder
! IUE data file in "spectrum format 2"
! uvby magnitudes
! uvby errors (in mag.)

solve

end

! compute a solution

This page is maintained by:
Simon Jeffery (csj@star.arm.ac.uk)
Last modified: 06/06/01