Models described in: P. Anders & U. Fritze-v. Alvensleben, A&A 401, 1063 (2003)

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ChangeLog:
29. 7. 2005: corrected a bug in the emission line routine
13. 6. 2007: corrected a bug for the Scalo models
             implemented larger set of input spectra
	     minor changes in spectra selection
	     change in lower mass limit
	     minor technical changes
28. 10. 2007: added Geneva models, with consistent lower IMF mass limit = 0.1 Msun
              Attention: Geneva models have variable time steps!
              Padova models are unchanged, only directories are renamed
              Added 2 tarballs of all models, of which one tarball also contains 
	      	magnitudes with extinction applied
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The files have the following naming conventions and formats:

Each directory is labelled SSP_zx_y_z. Here:
x (=0..4) indicates the metallicity:
	Padova: z0 <-> Z=0.0004, z1 <-> Z=0.004, z2 <-> Z=0.008, 
		z3 <-> Z=0.02, z4 <-> Z=0.05
	Geneva: z0 <-> Z=0.001 , z1 <-> Z=0.004, z2 <-> Z=0.008, 
		z3 <-> Z=0.02, z4 <-> Z=0.04
y is the used set of isochrones:
	Padova: Isochrones from the Padova group, as described in Bertelli et al., 
		1994, A&AS, 106, 275 (and references therein; 
		with an update on TP-AGB phase 1999)
	Geneva: Isochrones for non-rotating stars from the Geneva group, as described in 
		Lejeune & Schaerer, 2001, A&A, 366, 538 (and references therein)
z is the assumed IMF Phi(m) = m^{alpha} 
	'Salpeter' <-> alpha=-2.35 for all masses
	'Scalo' <-> alpha=-1.25 for m <= 1 Msun, alpha=-2.35 
		for 1 Msun < m <= 2 Msun and alpha=-3.00 for 2 Msun < m
	'Kroupa01' <-> alpha=-1.3 for m <= 0.5 Msun, alpha=-2.3 
		for 0.5 Msun < m
	Lower mass limit is always 0.1 Msun.
	Upper mass limit: 
		Padova: determined by isochrones (approx. 50 Msun 
			for super-solar metallicity, and around 70 Msun for the rest).
		Geneva: always 120 Msun
		
Each directory contains a file named 'mass.galev' containing the cluster mass 
as a function of age, a file named 'spec.galev' containing the integrated 
cluster spectra as a function of age, and a file named 'All_HST_Standard_Cardelli_1.dat' 
containing the integrated magnitudes of the clusters as a function of age 
in various passbands. These files have the following structures:

Attention: ALL (INCLUDING HST) MAGNITUDES ARE GIVEN IN THE VEGAMAG SYSTEM!!!!!! 
A simple filter-dependent offset is needed to convert them into 
STMAG magnitudes.

'mass.galev':
1st column: gives the cluster age in years
2nd column: gives the stellar mass of the cluster in solar masses


'spec.galev':
1st row: gives the number of spectra and the number of 
	wavelength points (should be 1221)
2nd row: gives the ages of the spectra
3rd row: blank
after 3rd row:
1st column: gives a wavelength counter
2nd column: gives the wavelength in Angstroem
From 3rd column onwards: gives the flux for the respective age and wavelength 
	in erg cm^(-2) s^(-1) Angstroem^(-1)


'All_HST_Standard_Cardelli_1.dat': ALL (including HST) magnitudes are in the VEGAMAG 
	system!!!
1st row: specifies the content of the data columns, number after filter name 
	indicates data column in which to find the respective magnitude
2nd row: indicates column number (for easier handling)
3rd row: indicates magnitude system (should be VEGA MAG)
4th row: 0.000
From 5th row onwards: 
1st column: gives an age counter
2nd row: gives the cluster age in years
From 3rd column onwards: Absolute magnitudes in the passbands specified in the 
	1st row

In addition, the tarball file 'Release_with_extinction.tgz' contains magnitude files 
	after applying extinctions laws to it. These files use the spectra from 'spec.galev', 
	multiply it with a given extinction law (Cardelli or Calzetti) with a range of values 
	for E(B-V) and then determine the magnitudes for these reddened spectra.
The structure is as for 'All_HST_Standard_Cardelli_1.dat', except:
	- 4th row: value of E(B-V) in extinction law
	- File name contains the extinction law used (Cardelli or Calzetti) 
		and a counter ranging from 1 (E(B-V)=0) to 21 (E(B-V)=1).
	- Cardelli law as in Cardelli et al., 1989, ApJ, 345, 245, with the 
		average value for the Galaxy R_V=3.1
	- Calzetti starburst attenuation law as in Calzetti 2001, PASP, 113, 1449