Hyperzmass needs as input files hyperzmass.param as well as a file
with the list of SEDs to be used (see e.g. spectra_bc03.param in the
tar file), a file with the filters' transmission functions, a file
with the list of filters to be used and the photometric catalogue.
To compute stellar masses the programme needs both the files *.ised of
the Bruzual&Charlot library (only this format is implemented in
hyperzmass) and the corresponding *.4color files (in the same
directory than *.ised files), containing the value of the stellar mass
to be normalized with the best fit.
An estimate of the error on stellar mass is computed by means of
delta(chi2) and a parameter called "PRIOR" imposes constraints on the
best fit models similar to the ones in Fontana et al. 2004, i.e.
1. skip models with tau < 0.6Gyr and ages for which zform<1
2. skip models with AV > 0.6 and no star formation, i.e. age/tau>4
The parameters that adjust the constraints are
avlim=0.6D0
ttaulim=4.D0
zform=1.0D0
You can modify them in hyper_zmass.f and then you have to recompile
the program to activate the new values.
The lines where the prior is acting are enclosed between the lines
ccccccccccccccc begin PRIOR cccccccccccccccccccccccc
ccccccccccccccc end PRIOR cccccccccccccccccccccccc
The output format is the following (nfilter is the number of the filters
in the input catalogue):
1. ID
2. z
3. reduced chi2
4. probability(reduced chi2)
5. type (integer)
6. record of age (integer)
7. age[Gyr]
8. A_V
9. normalization
10. Mgal
11. M*
12 -- 12+nfilter-1. apparent magnitudes form template best fit
13+nfilter-1. absolute magnitude
14+nfilter-1. M*inf (99%)
15+nfilter-1. M*sup (99%)
16+nfilter-1. M*inf (90%)
17+nfilter-1. M*sup (90%)
18+nfilter-1. M*inf (68%)
19+nfilter-1. M*sup (68%)
20+nfilter-1. SFR[M_sun/yr]
21+nfilter-1. tau model best fit (0 if SSP, -1 if constant star formation)
22+nfilter-1. number of filters used in the fitting procedure
23+nfilter-1. Luminosity distance at z