###################
# Global parameters
###################
# Virial velocity of the galaxy [km/s]
v200                    0.0
# Virial mass of the galaxy [1e10 Msol]
# Overrides the v200 parameter
m200                    112.127
# Halo spin parameter
lambda                  0.04
# Refinement level of the potential grid 
level_coarse            7
# Refinement level of the plane plane density grid 
level_grid_mid_dens     7
# Refinement level of the turbulence grid 
level_grid_turb         7
# Refinement level of the gaussian field grid
level_grid_dens_fluct   7
# Size of the potential grid [kpc]
boxsize1                320.0
boxsize2                160.0
boxsize3                80.0
boxsize4                40.0
boxsize5                20.0
boxsize6                10.0
boxsize7                5.0
# Dispersion for the Gaussian field fluctuations
dens_fluct_sigma        0.50
# Physical injection scale of the random field fluctuations [kpc]
dens_fluct_scale_inj    2.00
# Physical dissipation scale of the random field fluctuations [kpc]
dens_fluct_scale_diss   0.25
dens_fluct_seed         1212
# Seed for the random number generator
seed                    1246
# Switch to MCMC ntry algorithm to position particles for a value > 1
mcmc_ntry               1
# Number of iterations to reach hydrostatic equilibrium (zero to deactivate)
hydro_eq_niter          3


#######################
# Components parameters
#######################

#######################
# Component 1: Halo
#######################
# Fraction of the virial mass in the component 1
mass_frac1              0.9578424465115449
# Number of particles for the component 1
npart1                  1000000
# Target mass of individual particles [Msol]
#part_mass1              2e6
# Number of particles for the potential computation
npart_pot1              2000000
# Target mass of individual particles for potential computation [Msol]
#part_mass_pot1          1e6
# Component 1 density model
# Available models:
# 1  = Exponential disk + sech-z profile
# 2  = Myamoto-Nagai profile
# 3  = Exponential disk + exponential-z profile
# 4  = Hernquist profile
# 5  = Plummer profile
# 6  = Jaffe profile
# 7  = Isothermal profile
# 8  = NFW profile 
# 9  = Burkert
# 10 = Einasto profile
# 11 = Mestel profile
# 12 = Kalnajs profile
# 13 = Sersic profile
# 14 = Toomre-Kuzmin profile
# 15 = Uniform profile
# 16 = Pseudo-isothermal profile
model1                  8
# Scale length of the density profile [kpc]
scale_length1           1.0
# Core radius in the density profile [kpc]
rcore1                  0.
# Concentration parameter
# if positive, the scale length is recomputed to match the concentration
# the concentration parameter of an NFW halo with a mass M200*mass_frac
concentration1          10
# Gravitational softening for the poisson solver [kpc]
softening1              0.3
# Component 1 radial density cut [kpc] 
cut1                    0.0
# Component 1 thickness parameters
flatx1                  1.00
flaty1                  1.00
flatz1                  1.00
# Gaussian step for the MCMC Metropolis-Hasting particle postionning algorithm,
# expressed in units of the component scale length. Default value is 0.5.
mcmc_step1              0.50
# Maximum velocity for the component 1 particles in expressed in units of escape velocity
vmax_esc1               5.0
# Particles type (GADGET format -- 0=Gas,1=Halo,2=Disk,3=Bulge,4=Stars)
type1                   1
# Radius at which the density profile should have the exact same
# value as the NFW profile with the previously defined concentration
# and with a mass M200*mass_frac [kpc]
radius_nfw1             -1.0
# Cut the density function in the Jeans equation integration
jeans_mass_cut1         0
# Compute component velocity (debug option)
compute_vel1            1
# Number of integral of motion for the Jeans equations
# 0 = Do not use Jeans equation for sigma_r and sigma_z (model specidifed by sigmar_model and sigmaz_model)
# 1 = Spherically symmetric Jeans equation
# 2 = Jeans equations with 2 integrals of motion
# 3 = Jeans equations with 3 integrals of motion (solved on a 2D grid in the r-z plane)
jeans_dim1              1
# Method for streaming velocity computation
# 0 =               - User defined fixed fraction of the circular velocity profile (stream_fraction keyword)
# 1 = Bullock 2001  - Streaming velocity profile following the cumulative mass profile
# 2 = Springel 1999 - Streaming velocity profile following is a fixed fraction of the rotation curve 
# 3 =               - Solid Body rotation
stream_method1          1
# Streaming fraction of the component 1 (only for steam_method=4)
stream_fraction1        0.00
# Alpha coefficient for the generalized normal distribution [Gaussian=2.0]
# for the random generation of velocities
ggd_beta1               2.0
# Minimum acceptance for the MCMC chain
accept_min1             0.95
# Maximum acceptance for the MCMC chain
accept_max1             0.99

################################
# Component 2: Thin stellar disk
################################
mass_frac2              0.03066166043860979
npart2                  1000000
npart_pot2              2000000
model2                  3
# If the value is zero and the particle type is not 1 the size is determined using the spin conservation
# (Fitting formula from Mo, Mao & White 1998)
scale_length2           3.43218
cut2                    30.
flatz2                  0.1
mcmc_step2              0.3
type2                   1
stream_fraction2        1.00
# Epicycle approximation in the Jeans equations
epicycle2               1
# Minimal value for the Toomre parameter
Q_lim2                  1.5
# Fixed value for the Toomre parameter
Q_fixed2                0.0
# Additional term for the Toomre parameter
Q_boost2                0.0
# Past constant Star Formation Rate [Msol/yr]
# Negative value recomptes the SFR according to Bouché et al. 2010
SFR2                    -1.
# Minimum age of the stars [Myr]
min_age2                50.
# Metallicity of the stars [Zsolar]
metal2                  0.02041
# Gaussian fluctuations in the density field
dens_fluct2             0
# Use the density cut during the Jeans equation integration
jeans_mass_cut2         1
compute_vel2            1

###########################
# Component 3: Gaseous disk
###########################
mass_frac3              0.007663631417945721
npart3                  1000000
npart_pot3              2000000
model3                  3
scale_length3           3.43218
cut3                    30.
flatz3                  0.1
mcmc_step3              0.15
type3                   0
stream_fraction3        1.00
metal3                  0.02041
# Metallicity follows density gradient
metal_gradient3         0
# Temperature of the gas particles [K]
t_init3                 1e4
# Turbulent velocity dispersion [km/s]
turb_sigma3             20.0
# Turbulence injection scale [kpc]
turb_scale_inj3         0.34
# Turbulence dissipation scale [kpc]
turb_scale_diss3        0.005
# Seed for the turbulent gaussian field
turb_seed3              1234
# Compute hydrostatic equilibrium
hydro_eq3               0
# Gaussian step for the MCMC Metropolis-Hasting particle postionning algorithm
# within the hydro equilibrium algorithm
mcmc_step_hydro3        0.3
compute_vel3            1
# Polytropic index for the gas (1 = isothermal)
gamma_poly3             1.0

############################
# Component 4: Stellar bulge
############################
mass_frac4              0.0038322616318995422
npart4                  125000
npart_pot4              250000
model4                  4
scale_length4           0.343218
flatz4                  0.80
mcmc_step4              0.3
type4                   1
stream_fraction4        1.
min_age4                50.
metal4                  0.02041
Q_lim4                  1.5
epicycle4               1
compute_vel4            1