MAIN
# This section is quite free form: parameters may appear in any order,
# lines begining with #, % or blank space are for comments, otherwise
# from column 1 to 10 an identifier of the parameter (case sensitive)
# from 11 to 20 its value (always real with explicit decimal point)
# from 21 on comments.
#2345678901234567890123456789
#
#flutmc    0.0
#emiflag   1.0
#istarfo   0.0       sets the kind of SF law:
#istarfo=0  SFR from che_evo code
#istarfo=1  analytical SFR (parameters in section ANALY).
#istarfo=2  SFR from a chemical evolution code. When required the 
# residual gas fraction can be imposed through gastmp and igastmp in
# section MAIN
#istarfo=3  burst superimposed to the SFR provided by a chemical 
# evolution code. Parameters in section BURST
#istarfo=4  SFR from semianalytical hierarchical clustering models
#rsfmin, dtcurmax, dtcurmin are specific of istarfo 2 or 3.
#their value should not be changed
#ssp_mass4 5.015     IMF mass integral from Mlow to 120Mo;used for istarfo=1,4
tgal      13.0      age of the model
# NOTE: when tgal < 0 it is ignored and read instead in age.par.
# this is a trick to be used in programs running GRASIL for the same
# model at different ages. See for instance program AGETAB.
#extflag   1.0       if 1.0, the effective optical thickness 
# tau_eff = sqrt(tau_a*tau_e) is used in the diffuse component,
# if 0.0 tau_a is used
gastmp    6.0e-4    residual gas fraction is forced to gastmp when
# istarfo=2 and igastmp=1
igastmp   0.0       see gastmp
mmolfraz  0.80      fraction of molecular over total gas
# NOTE: if mmolfraz<0 no gas, useful for bare EPS
mcloud    1.0e6     Mass (Msun) of molecular clouds (MCs)
rcloud    15.0      radius (pc) of molecular clouds
#vout      -1.0      Gyr^-1 see below.  If <0 is set to 1/etastart.
etastart  0.003     Gyr see below
# fraction f of SSP energy inside MCs depends on its age t according to
# f=1 is t<etastart
# f=1-vout(t-etastart) if etastart<t<etastart+1/vout
# f=0 otherwise
#pahflag   0.0       if 0.0 no computation of PAHs features (speeds up)
# if 1.0 PAHs are computed
flutflag  0.0       if 0.0 no computation of T fluctuations of small
# grains (speeds up), if 1.0 fluctuations are computed
#hiiflag   0.0       if 1.0 computes lines and nebular continuum
#intrho    0.0       
# intrho 0 do nothing, 1 writes path normalized integrals 
# in a file, 2 reads from the same file instead of computing
dsug      1.0e-2    
idz       0.0            
# if idz=0.0 dsug is simply the dust/gas mass ratio, if idz=1.0
# (not meaningful for istarfo=1)
# then dsug becomes the proportionality factor between Z and dust/gas.
# in this case dsug=0.45 gives the standard DL dsug=1/110 for Zsun
tgra      400.0     maximum T of graphite grains in MCs
tsil      400.0     maximum T of silicate grains in MCs
#ndr       60.00     Number in radial bins (shells) in diffuse component
# 40 is usually a good choice for moderate optical thickness. Increase
# when energy is badly conserved; ndr has no effect for
# exponential profiles (igeo=2) for which ndr is optimized by the code
#nlf       200.0     Number of frequency bins
igeo      2.0       sets the geometry of stars and gas
#igeo=0 homogeneous
#igeo=1 King profiles: core radii given by rcstar and rcdiff
#igeo=2 Exponentials of distances from polar axis and from equator.
#scale lengths given by (rdstar,rddiff) and  (zdstar,zddiff) 
#igeo=3 elliptical galaxy defined by Witt et al. 1992, APJ,393,611 
#igeo=4 Cloudy galxy defined by Witt et al. 1992, APJ,393,611 
#igeo=5 like 1 but the exponent 3/2 replaced by gamdiff in diffuse gas
#for istarfo=4 only: 
#  igeo<=-2 for a pure bulge (igeo=1) or disk (igeo=2) geometry according 
#  the ratio Bulge/Total ratio in B magnitude of the SF model.#
# fburst is the ratio between the burst duration and the dynamical timescale,
# used only for istarfo=4fburst    1.0 
#  for istarfo=4 the radial scalelenghts are set as follows:
#  radial scale lengths for stars (rcstar, rdstar) are given by the SF model;
#  the other scalelenghts parameter given here are, for istarfo=4, ratios:
#  zdstar->(zdstar/rdstar); rddiff->(rddiff/r
rcstar    0.15      [kpc] igeo=1
rcdiff    0.20      [kpc] igeo=1
#gamdiff   0.5       [kpc] igeo=5
rdstar    5.0       [kpc] igeo=2
rddiff    5.0       [kpc] igeo=2
zdstar    0.4       [kpc] igeo=2
zddiff    0.4       [kpc] igeo=2
#
#
SPECTRA
Directions in degrees from the polar axis in which the SEDs are computed:
4  number of direction
0.0  degrees
30.0 degrees
45.0 degrees
90.0 degrees
#
#
SSP
Names of SSPs to be used. List ended by a comment line
First column put 1 if ssp is to be used, 0 otherwise. 
1    'gsrdk0bZ0004.sal'
1    'gsrdk0bZ004.sal'
1    'gsrdk0bZ008.sal'
1    'gsrdk0bZ02.sal'
1    'gsrdk0bZ05.sal'
#
MIXDIF
# Parameters setting the dust mixture in the diffuse component
# This section is quite free form: parameters may appear in any order,
# lines begining with #, % or blank space are for comments, otherwise
# from column 1 to 10 an identifier of the parameter (case sensitive)
# from 11 to 20 its value (always real with explicit decimal point)
# from 21 on comments.
#2345678901234567890123456789
#parameters for graphite follow  
amin_gr   0.0008e-4 minimum radius
amax_gr   0.25e-4   maximum radius
ab_gr     0.0050e-4 break radius between the two power laws
beta1_gr  -3.5      power law index from amax to ab
beta2_gr  -4.05     pawer law index from ab to amin
corgra    1.00      correction factor with respect to abundance in DL model
# can be used to vary the ratio between graphite and silicate
# parameters for silicate follow  
amin_si   0.0050e-4 minimum radius
amax_si   0.25e-4   maximum radius
ab_si     0.0003e-4 break radius between the two power laws
beta1_si  -3.5      power law index from amax to ab
beta2_si  -3.95     pawer law index from ab to amin
corsil    1.00      correction factor with respect to abundance in DL model
# can be used to vary the ratio between graphite and silicate
# parameters for PAHs follow
xx        3.03e-25  normalization power law PAHs
xh        0.2       hydro coverage PAHs
#
MIXMOL
# Parameters setting the dust mixture in the molecular clouds
# This section is quite free form: parameters may appear in any order,
# lines begining with #, % or blank space are for comments, otherwise
# from column 1 to 10 an identifier of the parameter (case sensitive)
# from 11 to 20 its value (always real with explicit decimal point)
# from 21 on comments.
#2345678901234567890123456789
#parameters for graphite follow  
amin_gr   0.0008e-4 minimum radius
amax_gr   0.25e-4   maximum radius
ab_gr     0.0050e-4 break radius between the two power laws
beta1_gr  -3.5      power law index from amax to ab
beta2_gr  -4.05     pawer law index from ab to amin
corgra    1.00      correction factor with respect to abundance in DL model
# can be used to vary the ratio between graphite and silicate
# parameters for silicate follow  
amin_si   0.0050e-4 minimum radius
amax_si   0.25e-4   maximum radius
ab_si     0.0003e-4 break radius between the two power laws
beta1_si  -3.5      power law index from amax to ab
beta2_si  -3.95     pawer law index from ab to amin
corsil    1.00      correction factor with respect to abundance in DL model
# can be used to vary the ratio between graphite and silicate
# parameters for PAHs follow
xx        3.03e-26  normalization power law PAHs
xh        0.2       hydro coverage PAHs
#
# is better to leave some comment line at the end