ECLIPSE -- like 'COMDAT' computes data equivalent to a particular image,
but also accounts for eclipses and therefore requires you to
specify parameters that allow it to convert from velocity to
position (it assumes a "keplerian" flow).
Parameters:
IMAGE -- The image file to load
TEMPLATE -- TRUE if template data file is to be used otherwise the user
must define pixels sizes etc.
If TEMPLATE
DATA -- Data file containing example format data
Else
NPIX -- Number of pixels/spectrum
NSPEC -- Number of spectra
VDATA -- Velocity km/s/pixel
WCEN -- Central wavelength (Angstroms)
WIDTH -- Phase width of exposures
OUTPUT -- Calculated data file name
KW -- White dwarf's semi-amplitude
KR -- Red star's semi-amplitude
IANGLE -- Inclination angle
OVER -- Over sampling factor. This makes the program
over-sample the velocity grid to produce
smoother time dependence. You should be very careful
with this parameter as the computation time scales as
OVER**2.
RMAX -- maximum distance in terms of RL1 to attempt computation
of eclipse. Any emission that translates to a place
beyond this radius is assumed not eclipsed. You could
allow this to extend beyond 1, but I don't know how
it will cope with points that end up inside the mass
donor.
If NADD
CONT -- Effective continuum for noise computation
NOISE -- Signal-to-noise in effective continuum
SEED -- Seed integer to start noise generator if NADD
This command belongs to the class: extra