% halo properties
CC             			6.0			% halo concentration
V200	       			152	  		% circular velocity v_200 (in km/sec)
LAMBDA         			0.05		% spin parameter          
%AnisotropyRadius    	0.0     	% anisotropy radius, in terms of
                            		% hernquist profile radius RH


% mass fractions
MD             			0.04637469      	% disk mass fraction      
MB             			0.00304548    	% bulge mass fraction     
MBH            			0.00001    	% black hole mass fraction. If zero, no black
                        			% hole is generated, otherwise one at the centre
                         	 		% is added.

% particle numbers
N_HALO         			1953609      % desired number of particles in dark halo
N_DISK         			2872269      	% desired number of collisionless particles in disk
N_GAS          			 700206      	% number of gas particles in disk
N_BULGE        			 816564       % number of bulge particles


Softening           0.1      	% soften force on small scales
%ErrTolTheta             0.15        % tree opening criteria

%UseQrng                 0           % 0=pseudorandom, 1=quasirandom numbers
%WriteDensity            0           % write density instead of mass


% disc structural properties

GasFraction    			0.28136657     	% relative content of gas in the disk, the rest is stars
JD             			0.019	#4600087	  	% disk spin fraction, typically chosen equal to MD (XXX how
									% is this divided among the stars and gas?)
%H			   			2.85		% disk radial scale length (kpc)
DiskHeight          	0.14     	% thickness of stellar disk in units of	radial scale length
RadialDispersionFactor  1.0         % radial dispersion in units of the vertical
MaxGasDiskHeight        5.0        	% prevent flaring of outer gas disk
%GasDistribution         1           % 0 = exponential disk (same scale radius for gas & stars)
                        			% 1 = exponential disk (with Rd_gas = Rd*alpha)
                        			% 2 = power law (PowerLawGamm < 2)
GasExpAlpha              3.0         % gas disk scale length multiplicative factor
%PowerLawGamma           1.0         % power law index, sigma = r^-gamma
                                    % gamma < 2, gamma = 1 is mestel
%PowerLawCutoff          1.0         % max radius of gas for power law distribution,
                                    % in units of H


% disc age and metallicity (set using Patrik's gal1-GO-set2 files; i.e., MA04
% gradient described in Rocha et al. (2008))

%DiskPopMode             exponential		% either "constant","instantaneous", or "exponential"
%DiskPopAge              14.0	       	% in Gyr
%DiskPopTau              10.0	      	% in Gyr (generally negative)
%Zmet0                   0.032       	% gas metallicity central value (fraction)
%ZmetGrad               	-0.06       	% gas metallicity gradient (dex/kpc)



% bulge properties

BulgeSize      			0.13        	% bulge scale length in units of disk scale length 
%BulgePopMode        	instantaneous   % either "constant", "instantaneous", or "exponential"
%BulgePopAge         	14.0	
%BulgePopTau         	0



HI_GasMassFraction     	0.1			% mass of extended, flat HI disk in terms of the total gas mass
HI_GasDiskScaleLength  	6.0			% scale length of extended gas disk in terms of scale length of the disk 



% Springel & Hernquist (2003) ISM model parameters

MaxSfrTimescale     	4.5         % Gas consumption timescale (multi-phase model)
FactorSN            	0.1         % beta, mass fraction of massive stars (multi-phase model)
FactorEVP           	3000        % A_0, evaporation parameter (multi-phase model)
TempSupernova       	3e+08       % T_SN, effective "supernova temperature",sets feedback energy (multi-phase model)
TempClouds          	1000        % temperature of cold clouds (multi-phase model)

FactorForSofterEQS  	1.0           % Can be used to make the equation of state
                                	% softer. For 1.0, the multiphase model is
									% used, while for 0.0 isothermal at 10^4 K is
									% assumed. Intermediate values interpolate
                                	% linearly between the two pressures.

% Redshift scaling

REDSHIFT            	0.0         % redshift to scale galaxy properties to
Omega_m0            	0.3         % Omega_m
Omega_L0            	0.7         % Omega_L