ULSA.emissivity_fitting.fit_emissivity_params.free_free

class:

class ULSA.emissivity_fitting.fit_emissivity_params.free_free(object):

method:

__init__(self, v, nside, index_type, dist, emi_form, I_E_form, R0_R1_equal, using_raw_diffuse, using_default_params, params_408=np.array([71.19, 4.23, 0.03, 0.47, 0.77]))

initial parameter function

Parameters

  • float (v) – The frequency of output sky map

  • nside (int) – The Nside value one choose in healpix mode, must be 2^N.

  • 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 as different type of spectral index one need to consider.

  • dist (int) – the maximux integrated distance of galaxy, normally setting to 50kpc.

  • emi_form – [‘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) – fixed True

  • using_raw_diffuse (bool) – if True, using the raw input data without smoothing.

  • using_default_params (bool) – if True, using the default spectral index value, if False calculate the spectral index value with the code, otherwise, one can simply input the spectral index to variable of using_default_params.

  • params_408 (array) – if the input of params_408 == [0.,0.,0.,0.,0.], the code will fit the parameters of emissivity in 408Mhz, or one can simply input the parameters of some other fitting result to params_408, if you input nothing, the code will take the default parameters.

params()

return the fitting params of emissivity in array form.

Returns

params in array form $array([A, R_0, alpha, Z_1, gamma])$.

Return type

np.array