The LFSM implementation of the NE2001 electron model using in 3D emissivity of galaxy.
The output can be stored either in memory by means of a numpy array, or in a HDF5 format file.
as root user:
python setup.py install or python setup.py develop
for user only:
python setup.py install --user
To use this code, one can simply do::
>>> from LFSM.absorp_sky_map.global_spectrum_new import absorption_JRZ
>>> f = absorption_JRZ(v = v, nside = nside, clumping_factor = 1., index_type = 'constant_index_minus_I_E', distance = dist, test = False, emi_form = 'exp',I_E_form = 'seiffert',R0_R1_equal=True,using_raw_diffuse = False,only_fit_Anu = False)
>>> f.mpi()
v int: frequency in MHz of the input skymap \\
nside int: the NSIDE of the skymap in healpix mode \\
clumping_factor float: the clumping factor influnce the absorption, the value set to one in our model. \\
index_type str: ['constant_index_minus_I_E','freq_dependence_index_minus_I_E','pixel_dependence_index_minus_I_E'], one of them can be choose with different type of spectral index. \\
distance kpc: the integration max distance for galaxy absorption. \\
test: normally False, if True will do some test programm. \\
emi_form str: ['exp','sech'] the distribution form of emissivity, normally choosen 'exponantial'. \\
I_E_form str: ['seiffert'], the form of extragalactic component except for CMB. \\
R0_R1_equal bool: in this paper we fixed R0 equals to R1 in emissivity. \\
using_raw_diffue bool: the input data for fitting parameter of emissivity, if True the data will be smoothed by hp.smooth() method. \\
only_fit_Anu: fixed False. \\
There are an example in ./test_ground, one can simpyly go to the dir and run test.py
Documentation can be found at https://lfsm-01.readthedocs.io/en/latest/.