pfile

#
# Basic hammurabi parameter file.
#

#################################################################################
#  Integrator parameters
#################################################################################

# The following control the resolution of the integration.  Use
# total_shell_numb to control the number of shells used, i.e. the
# number of times the resolution of pixels on the sky is increased.
# For total_shell_numb=1, the observation shell is the only shell.
# For total_shell_numb=3 and obs_shell_index_numb=2, then there are
# three shells.  The highest resolution shell is then averaged into
# the observed shell.  The parameter obs_NSIDE gives the resolution of
# the observation shell, and the resolutions of all the other shells
# are simply a factor of two more or less.

obs_shell_index_numb=1
total_shell_numb=1
obs_NSIDE=16

# The *total* number of radial bins to divide each sky pixel into to
# create vec_size_R 3D cells along the LOS.
vec_size_R=16

# The maximum radius from the observer that is integrated.  
max_radius=32

# Observed frequency for integration in GHz:
obs_freq_GHz=23.

# Flags to select which quantities to integrate:
#  synchrotron emission, RM, DM, optical depth, free-free
do_sync_emission=T
do_rm=T
do_dm=F
do_tau=F
do_ff=F

# Output maps:
obs_file_name=test_obs.fits
obs_RM_file_name=test_rm.fits
#obs_DM_file_name=
#obs_tau_file_name=
#obs_ff_file_name=

# If you do not wish a full sky map, you can give a list of HEALPix
# pixels at which you want the integration performed, and it will
# write the corresponding list of observables.  The pixlist.txt file contains
# one pixel number per line, the pixel number in the given Nside (see above) in 
# NESTED mode.  If the item_obs_freq_flag parameter is true, then the second
# column on each line is the frequency (GHz) at which to integrate for that pixel:
#
#list_in_file_name=pixlist.txt
#item_obs_freq_flag=F
#
#  The output is then an ASCII file with the following format:
#  ipix freq[GHz] I_s Q_s U_s I_d Q_d U_d int_dist[kpc] RM[rad/m^2] DM[pc/cm^3] 
#
#list_out_file_name=outlist.txt

#################################################################################
# Cosmic ray electron (CRE) parameters
#################################################################################

# CRE model:  exponential disk with power law spectrum
Cfield_type=1
# power law index
C1_p=3
# scale radius (kpc)
C1_hr=5
# scale height (kpc)
C1_hz=1
# Normalization:  flux density at Sun position in 1/(GeV m^2 s sr).  Default from
#  Strong, Moskalenko, & Ptuskin (2007, ARNPS, 57, p285).  
#  In Fig 4 from that paper, at 10GeV, we can read off
#  E^2*J(E)~250 GeV^2/(m^2 s sr) which corresponds to J(E=10GeV)=0.25(GeV m^2 s sr)^-1
#  or to roughly a number density normalization of  4x10^-5 cm^-3.  
#  See section 3.5 of Jaffe et al. (2010, MNRAS 401, 1013) for discussion. 
#  (Note that internally, hammurabi uses the number density in cm^-3 and 
#  that other implemented CRE functions from X. Sun et al. use that instead.)  
C1_JE=0.25

#################################################################################
# Thermal electrons (TE) parameters
#################################################################################
# By default, the NE2001 model is computed that requires no 
# parameters.  You can, however, specify a model given in a binary file
# (floating point type ) or a constant density.

# For a constant field of this density per cubic centimetre.  When
# zero, the NE2001 model is computed.
TE_constant_pccm=0

# Alternatively, specify a file name of binary data to read and its dimensions.
# A version can be found in the supplementary files on the Sourceforge repository,
# which is the NE2001 model updated following Gaensler et al. (ApJ 663, 258, 2008)
#
#TE_grid_filename=negrid_n400_gaensler.bin 
#TE_lx_kpc=400
#TE_ly_kpc=400
#TE_lz_kpc=80
#TE_nx=40
#TE_ny=40
#TE_nz=8

# Include coupling of thermal electrons and random field as in Sun et al. 2008
do_TE_Bran_coupling=F
TE_Bran_coupling=0.01

#################################################################################
#  B-field parameters
#################################################################################
#
# Select the field type.  Included fields are
#  1:  ASS model from WMAP, Page et al. (2007)
#  2:  Stanev BSS model (astro-ph/9607086)
#  3:  Sun et al. ASS+Ring model (A&A, 477, 2008)
#  4:  HRM model from Kachelriess et al. APh 2007 
#  5:  TT model from Kalchelriess et al. ApH 2007 
#  6:  External file, binary dump.  See code for format.
#  7:  Jansson & Farrar (2012, ApJ 757,14, and 2012, 761, L11)
#  8:  Fauvet et al. (2011, A&A, 526, 145)
#  10:  Jaffe et al. (2010, MNRAS, 401, 1013)
#
B_field_type=1

# Parameters for WMAP ASS model.  See code for parameters of other models.
B_field_b0=6
B_field_psi0_deg=35
B_field_psi1_deg=0.9
B_field_xsi0_deg=25

#  Include small-scale Gaussian random field (GRF) isotropic random component?
B_field_do_random=F

#  Mean amplitude of the GRF:  
B_field_RMS_uG=6 # microGauss

#  Index of 3-D power law turbulent spectrum (default -2.37 for large scales from 
#  Han et al. 2004, which gives -0.37 for 1D.)
#B_field_alpha=-2.37
# large-scale cut-off in kpc.  Default cutoff value of 0 means use no cutoff.
# This, or 5kpc, is physically unrealistic but meant for low-resolution testing.  
# Set to, e.g., 0.1 for more physically realistic, high resolution runs.  
B_field_cutoff=5.  # kpc

#  Specify the seed for the GRF in order to generate identical realizations.  
#  Default behavior (value 0) is to use the system clock to generate the seed.
B_field_seed=0

# For GRF as well as reading or writing coherent or total field models, 
# define a box with physical dimensions (kpc), default 40x40x8 kpc.  
#B_field_lx=40
#B_field_ly=40
#B_field_lz=8

# box resolution, default 256x256x51
#B_field_nx=256
#B_field_ny=256
#B_field_nz=51

# Output file to store GRF simulation as a binary dump of double-precision floats 
#  looping over bins first in x (outer loop), then y, and then z (innermost loop):   
#B_field_random_out=

# Output file to store total field, as above:
#B_field_total_out=

#  If you only wanted to write out the fields and do no integration, to tell it 
#  to stop, set this to true:  
#Only_write_B_field=F

# Input file for B_field_type=6, reads in the coherent field (or total
#  if you set B_field_do_random=F) in the same format as
#  B_field_random_out or B_field_total_out:
#B_field_coherent_inp=

# Input file to read in GRF simulation (e.g. produced by GARFIELDS)
#B_field_random_inp=
# Maximum galacto-centric radius to include random component
#B_field_rmax=
# Maximum sun-centric radius of validity of B-field model, beyond which 
# it is assumed zero:
#B_field_rmax_sun=

# To simulate a box that is not the whole galaxy but only a region centered
#  around the observer of the dimensions specified with the parameters above:
#B_field_ec=F

# To simulate a box that is not the whole galaxy but which has one end
#  at the observer and the x-axis pointing away from the observer at a
#  given lon,lat, use *both* of these (i.e. don't expect it to use
#  lat=0 if you only set lon):
#B_field_transform_lon=-999  # -999 means don't do any transform
#B_field_transform_lat=-999  #

#  To simulate a box that is not the whole galaxy but which is
#  centered at the specified lon,lat above and at a distance 
#  of R from the observer toward that lon,lat:
#B_field_transform_R=0  # kpc

# Misc parameters:
B_field_debug=F
B_field_quiet=0