How to run a model with Starburst99

First you need to specify your input parameters. This is done from the input page. There are quite a few parameters to play with, all of which are explained below. If you are not sure about an input parameter, start out with the default value.

The output
Once the run is finished, you will be notified by e-mail. If everything went well, you should find the output files in the output directory. The e-mail gives you all the information you need to locate the files and the retrieve them. If you have set all output flags to "yes", you will find 16 files: 15 files with model results (note that (5) generates 2 files, therefore the 14 flags produce 15 files), and one output file which lists the model parameters which were used. The data files are:

  1. Computation of the number of ionizing photons. (7) must be set to "yes" since the spectrum below 912 A is needed. Output is the number of ionizing photons in the HI, HeI, and HeII continuum, their fractions relative to the total luminosity, and the total luminosity. Default filename: quanta
  2. Calculation of the supernova rate and the mechanical luminosities. It requires (4) to obtain the stellar wind luminosities. Otherwise it is independent of other subroutines. Default filename: snr
  3. HRD with a few evolutionary tracks. This is mostly useful for test purposes. This part is independent of all other subroutines and can be turned on/off without doing any harm. Default filename: hrd
  4. Mechanical luminosity and related quantities due to winds and supernovae. It does not depend on any other subroutine since no information on the energy distribution is needed. Default filename: power
  5. Two output files containing the stellar spectral types during each time step and the relative numbers of WR stars. The spectral types follow the scheme by Schmidt-Kaler, oversampled by a factor of 2. For instance, there are 18 entries for spectral type B. They are the number of stars for types B0, B0.5, B1,...B9.5 (total of 18). Schmidt-Kaler's table has B0, B1,....B9 (total of 9). The spectral types are printed out only every TDEL. Otherwise it is too bulky. Default filenames: sp1,sp2
  6. The mass in individual elements released via stellar winds and supernovae. No other subroutines are needed. Note that the elements are simply assumed to be ejected during a SN event. No nucleo-processing is included! Default filename: yield
  7. The spectrum of the stellar population for each time step. The columns are time, wavelength, stellar+nebular, stellar only, and nebular only fluxes. (1) is needed in order to calculate the nebular continuum. Default filename: spectrum
  8. The ultraviolet line spectrum at 0.75 A resolution from 1200 to 1600 A (LMC/SMC library) or to 1800 A (Milky Way library). The subroutine needs (7) to compute the stellar continuum and (1) for the nebular continuum. If (1) is turned off, the nebular contribution can not be added (it is often small, though). The columns have time, wavelength, absolute luminosity, and rectified (continuum=1) luminosity. Default filename: line
  9. Calculation of colors and magnitudes. The subroutine needs (7) to compute the stellar continuum and (1) for the nebular continuum. If (1) is turned off, the nebular contribution can not be added and the computed colors are for stars only (this may sometimes be desirable). The filter system is defined in the code. Default filename: color
  10. Calculation of the strengths of H_alpha, H_beta, Pa_beta, and Br_gamma. For each line we give the continuum luminosity, the line luminosity, and the equivalent width (everything logarithmic). The subroutine needs (7) to compute the stellar continuum and (1) for the nebular continuum. If (1) is turned off, the nebular contribution can not be added. Default filename: width
  11. Calculations of the strengths of various IR spectral features. First is the CO index as computed by Doyon et al. (1994, ApJ, 421, 101). (Please note that this calculation has no metallicity dependence. A later version of this routine will compute the CO index using the model atmospheres themselves and give metallicity-dependent results.) Next are two computations of the CaII IR triplet using the relations of Diaz et al. (1989, 239, 325). The relations from Diaz et al. have no temperature dependence; the first calculation has the feature present in stars of all temperatures; the second has the index set to zero strength for stars with T>7200K (spectral type A or earlier). Next come the 1.62 and 2.29 micron CO features, and the 1.59 micron Si feature, which were modeled for individual stars by Origlia et al. (1993, A&A, 280, 536.) The indices can be computed for solar [Si/Fe] and [C/Fe], or a model with enhanced [Si/Fe] and depleted [C/Fe] (as for young systems enriched primarily by Type II SNe), and for stellar atmospheric microturbulent velocities (MTVs) of 1-6 km/s. (Note that the changes to the abundance ratios and MTVs are are self-contained in this routine and have no effect upon the other outputs, e.g., colors, of the code.) Default filename: feature
  12. This subroutine is equivalent to (8), but it computes the spectral region around the O VI doublet. Default filename: ovi
  13. This subroutine is still under construction. Eventually it will compute the stellar absorption spectrum of the higher Balmer lines. Stay tuned! Default filename: balmer
  14. Calculation of the most important WR emission lines using the line luminosities of Schaerer & Vacca (1998, ApJ, 497, 658). These are only those lines originating in WR winds --- not the nebular lines in the HII region. Quantities given are the line fluxes and the equivalent widths. The subroutine needs (7) to compute the stellar continuum and (1) for the nebular continuum. If (1) is turned off, the nebular contribution can not be added. Default filename: wr

How to interpret the file time-used
The logfile "time-used" gives statistics on cpu and elapsed time, and it reports warnings and anomalies or errors that may have occurred during the run.

If you see "CANNOT COMPUTE....." you have specified to skip a particular output which was otherwise needed as input for another subroutine which you actually specified to compute. For instance, you may intentionally omit the nebular continuum (quanta) in order to compute a purely stellar continuum. But then you would not be able to compute equivalent widths (width) since the number of ionizing photons is needed for the emission line fluxes. When in doubt, compute all the output files. This will work.

"IEEE floating point exception flags" may also be ignored.