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 no more used # istarfo=2 no more used # istarfo=3 no more used # istarfo=4 SFR from semianalytical hierarchical clustering models # istarfo=5 as 4 but writes only files with SFR including bursts # For istarfo=0 the residual gas fraction can be imposed, when # required, through gastmp and igastmp in section MAIN. # #ssp_mass4 5.015 # ssp_mass4 = IMF mass integral from Mlow to 120Mo;used for istarfo=4. # For istarfo=0 it is read in the SFR file. It is used to normalize the # SSP spectra (set in section SSP). Note that the SSP are computed for a # given IMF (slopes and mass limits), thus the only meaningful IMF variations. # change ssp_mass4 if change IMF # if ssp_mass4<0, use the one written in SSP files, i.e. assumes same Mlow as SSP # for Mlow=0.15, ssp_mass4= 5.015, 2.950, 5.920 for Salpeter, Kennicutt, k1p # for Mlow=0.1, ssp_mass4= 5.862, 3.065, 6.036 for Salpeter, Kennicutt, k1p # tgal 13.0 age of the model # NOTE: when tgal < 0 it is ignored and # 1) for istarfo=0 is read 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. # 2) for istarfo=4 tgal is reset to tb+abs(tgal)*te, where tb and te are # the time and e-folding time of the last burst listed in bursts_bulge file. #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 #lam_tru 40.0 #exp_tru 1.5 # lam_tru is the wavelength in micron above which the slope of the dust absorption #efficiency is set equal to exp_tru. These parameters are optional. gastmp 6.0e-4 if igastmp=1 then gas mass is forced to # gastmp*(final total mass in .sf file), if igastmp=0 then gastmp is not # used and the actual gas mass at tgal, as listed in .sf file is adopted # istarfo=0 and igastmp=1 igastmp 0.0 see gastmp mmolfraz 0.70 fraction of molecular over total gas # NOTE: if mmolfraz<0 no gas, useful for bare EPS # if mmolfraz>1, then it is reset to min(1,SFR(tgal)/mmolfraz), # where SFR is in Msun/yr. This is used to have mmolfraz proportional to SFR. mcloud 1.1e6 Mass (Msun) of molecular clouds (MCs) # NOTE: if mcloud<0, then -mcloud is interpreted as the required 1 micron # optical depth of clouds, and mcloud is reset accordingly. rcloud 14.0 radius (pc) of molecular clouds #vout -1.0 Gyr^-1 see below. If <0 is set to 1/etastart. etastart 0.009 Gyr see below # fraction f of SSP energy inside MCs depends on its age t according to # f=1 if t<=etastart # f=1-vout*(t-etastart) if etastart.ssp.. # In this way the stellar features can be studied. # If wavsspout is 0.0 or not present, these files are not produced 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 # igeo=-1 for a bulge+disk composite geometry. For istarfo=4 separate # SF history for the 2 components are available. For istarfo=0,2,3 # the same SF history is assigned to the 2 components according to # bulge/total mass ratio read in file mon_name.bst # For istarfo=4 only: # igeo<=-2 for a pure bulge (igeo=1) or disk (igeo=2) geometry according # the ratio Bulge/Total ratio in K magnitude of the SF model. # 2 more parameters have to be given in input: # fburst = the ratio between the burst duration and the bulge dynamical timescale. # beta = half-mass radius of exponential disk where ongoing bursts occur is # beta*rbulge # littleh= Ho/100 # tbemin = min e-folding time scale for bursts Gyr # dtbe = sets the duration of bursts= dtbe * burst e-folding time #fburst 2.0 #beta 0.1 #littleh 0.7 #tbemin 5.0e-3 0.0 Gyr #dtbe 5.0 # 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 scalelenght parameters are ratios: # rcdiff is (rcdiff/rcstar); # zdstar is (zdstar/rdstar); rddiff is (rddiff/rdstar); zddiff is (zddiff/rddiff). 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 # #MC_LINE #Optional section to define a distribution of values of optical depths of MCs #and of escape time scales of young stars from them #2 n_tau_mc: number of tau and t0 for MCs #16. 65.32 r_mc_arr: MC radii in pc #0.625 0.375 f_mc_arr: numerical fractions of MCs with given radius (i.e. tau) #0.008 0.008 t0_arr : Gyr, see etastart in sec MAIN # SPECTRA Directions in degrees from the polar axis in which the SEDs are computed: 4 number of direction 0.0 degrees 20.0 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' # NB must set ssp_mass4 consistent with choice of IMF & Mlow,Mup # #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 'grdb0sZ0004.sal' #1 'grdb0sZ004.sal' #1 'grdb0sZ008.sal' #1 'grdb0sZ02.sal' #1 'grdb0sZ05.sal' # NB must set ssp_mass4 consistent with choice of IMF & Mlow,Mup # 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