Keywords

freeform

indicates whether or not the linelist will be read in under format control (7e10.3) or will be free-form. If freeform = 0, the default value, then the old-style formatted input will be used; If freeform = 1, unformatted read will be used, BUT the user must then give values for all quantities (that is, explicit zeros will need to be put instead of blank spaces.

RUN

signals that there are either multiple syntheses being done or multiple comparisons with observed spectra.

standard_out

controls the name of the verbose standard output.

summary_out

controls the name of either the EW summary or the raw synthesis output.

hardpost_out

controls the name of a postscript plot output.

speccomp_out

controls the name of a text file containing the comparisons (wavelength shifts, sigmas, etc.) between observed and synthetic spectra

bin_raw_out

controls the name of a file containing the raw synthesis of a spectroscopic binary, with an appropriate velocity difference and luminosity ratio dialed in

bin_smo_out

controls the name of a file containing the smoothed synthesis of a spectroscopic binary

summary_in

controls the name of the raw synthesis file, created previously, that will be read in for plotting purposes

smoothed_out

controls the name of the smoothed synthesis output

keeplines_out

controls the name of the list of kept lines for future synthetic spectrum runs

tosslines_out

controls the name of the list of discarded lines that are too weak to keep in future synthetic spectrum runs

iraf_out

controls the name of the optional IRAF output

model_in

controls the name of input model atmosphere file

lines_in

controls the name of the input line list

stronglines_in

controls the name of the input strong line list

observed_in

controls the name of the input observed spectrum

table_in

controls the name of the extra input instruction file

table_out

controls the name of the extra input instruction file

popsyn_out

controls the name of the extra input instruction file

rawbin_out

controls the name of the input observed spectrum

smoobin_out

controls the name of the input observed spectrum

atmosphere

controls the output of atmosphere quantities:

0 = do not print out the atmosphere
1 = print out the standard things about an atmsophere
2 = print standard things and additional stuff like continuous opacities, etc.

molecules

controls the molecular equilibrium calculations:

0 = do not do molecular equilibrium
1 = do molecular equilibrium but do not print results
2 = do molecular equilibrium and print results

molset

controls the choice of which set of molecules will be used in molecular equilibrium calculations.

1 = the small set involving H, C, N, O, Mg, Ti (DEFAULT)
2 = the large set more useful for very cool stars

deviations

controls whether, for synthetic spectrum computations, an ‘obs-comp plot will be made in addition to the normal spectrum plot

0 = do not plot the obs-comp plot
1 = plot the obs-comp plot

lines

controls the output of line data

0 = print out nothing about the input lines
1 = print out standard information about the input line list
2 = gory line data print (usually for diagnostic purposes)

gfstyle

controls the output of line data

0 = base-10 logarithms of the gf values (DEFAULT)
1 = straight gf values

contnorm

allows multiplicative adjustment of the continuum; useful probably only for batch syntheses the numbers employed should be around 1.0; default is 1.000000.

plotpars

allows you to set all of the plotting parameters if you know them in advance:

0 = none set (default); user can change in plotting routine
1 = given in following lines as follows
- xlow xhi ylo yhi
- vshift lamshift obsadd obsmult
- smooth-type FWHM-Gauss vsini L.D.C. FWHM-Macro FWHM-Loren

trudamp

should moog use the detailed line damping for those transitions that have information stored in subroutine trudamp? (Default is no)

veladjust

shoud moog try to do a cross-correlation between observed and synthetic spectra and use that to align the spectra better in wavelength (Default is no)

units

controls the units in which moog outputs the final spectrum:

0 = angs
1 = microns
2 = 1/cm

iraf

allows the user to output a raw spectrum in a form suitable for IRAF’s rtext input command

0 = don’t do this, make output the normal way.
1 = make an IRAF-compatible output

scat

allows the user to employ a source function which has both scattering and absorption components

0 = NO scattering
1 = scattering

flux/int

choses integrated flux or central intensity

0 = integrated flux calculations
1 = central intensity calculations

damping

here are the calculations to set up the damping; dampingopt is the damping parameter, and dampnum is the damping value read from the line list. For atomic lines there are several options:

dampingopt = 0 and dampnum < 0 —> gammav = 10^{dampnum(i)}(T/10000K)^0.3n_HI
dampingopt = 0 and dampnum = 0 —> c6 = Unsold formula
dampingopt = 0 and dampnum > 10^(-10) —> c6 = (Unsold formula)*dampnum(i)
dampingopt = 0 and dampnum(i) < 10^(-10) —> c6 = dampnum(i)
dampingopt = 1 —> gammav = gamma_Barklem if possible, otherwise use dampingopt=0 options
dampingopt = 2 —> c6 = c6_Blackwell-group
dampingopt = 3 and dampnum <= 10^(-10) —> c6 = c6_NEXTGEN for H I, He I, H2
dampingopt = 3 and dampnum > 10^(-10) —> c6 = (c6_NEXTGEN for H I, He I, H2)*dampnum For molecular lines (lacking a better idea) —> c6 done as in dampingopt = 0

obspectrum

controls the file type of the observed spectrum

0 = no observed spectrum is to be input
1 = read a true FITS file with internal read statements
-1 = as if obspectrum = 1, but on a byte-swapping machine
2 = (not implemented yet)
3 = read a true Fits file with the FITSIO package
4 = (not implemented yet)
5 = read a special MONGO style (wavelength, flux pair) file

histogram

makes histogram plots of observed spectra if histoyes = 1

terminal

gives the sm plotting window type smterm = a character string of the sm window type (see the appropriate sm manual for a list)

plot

decides whether or not to make a plot of results c 0 = do not make a plot c For syntheses: 1 = plot only synthetic spectra c 2 = plot synthetic and observed spectra c 3 = smooth the syntheses but don’t plot c For line analyses: # = the minimum number of lines of a c species necessary to trigger a plot c For curves-of-growth: 1 = make plots c For flux curves: 1 = make plots

abundances

gives the changes to be applied to the abundances c # = the number of different syntheses to run c (the next line gives the different abundance factors c to use) c minimum error check: numatomsyn must equal numisosyn or code will stop

isotopes

gives the isotopes used in the line list and their abundance relative to the parent spiecies. minimum error check: numatomsyn must equal numisosyn or code will stop

lumratio

gives the ratio of the luminosity of two stars at a specific wavelength in a binary star system (used only with driver “binary”)

deltaradvel

gives the velocity difference between the stars binary star system (used only with driver “binary”)

synlimits

gives the wavelength parameters for syntheses; start and sstop are beginning and ending wavelengths, step is the step size in the syntheses, and delta is the wavelength range to either side of a synthesis point to consider for line opacity calculations

fluxlimits

gives the wavelength parameters for flux curves; start and sstop are beginning and ending wavelengths, and step is the step size in the flux curve

blenlimits

gives the parameters for blended line abundance matches. delwave is the wavelength offset to the blue of first and to the red of the last line in the blend to extend the syntheses; step is the wavelength step size in the computations; cogatom is the name of the element whose abundance should be varied to achieve an EW match with observations.

coglimits

gives the log(W/lambda) limits for curves-of-growth rwlow and rwhigh are the beginning and ending points of the log(red.width) values, rwstep is the step in log(red.width), cogatom is the declaration of which element will have its abundance varied (necessary only for spectrum synthesis curves-of-growth, and wavestep is a forced (if desired) step size in wavelength along the line (this applies to single line computations only

limits

old limits format…tell the user to change the keyword and quit.

strong

for lines which are to be considered for all of the synthesis

opacit

which takes the continuus opacity and scales it with the form of kaplam(i)= kaplam(i)((factor10000)/t(i)) in Opacit.f after it calulates the normal kaplam if value is <= 0 then it does not do it.