# SpDust¶

class pysm.SpDust(map_I, freq_ref_I, emissivity, freq_peak, freq_ref_peak, nside, unit_I=None, map_dist=None)[source] [edit on github]

Bases: pysm.Model

Implementation of the SpDust2 code of (Ali-Haimoud et al 2012) evaluated for a Cold Neutral Medium. See: * https://arxiv.org/abs/1003.4732 * https://arxiv.org/abs/0812.2904

This function initializes the spinning dust model

Parameters: map_I : pathlib.Path object Paths to the map to be used as I templates. unit_I : string or Unit Unit string or Unit object for all input FITS maps, if None, the input file should have a unit defined in the FITS header. freq_ref_I : Quantity or string Reference frequencies at which the templates are defined. They should be a astropy Quantity object or a string (e.g. “1500 MHz”) compatible with GHz. freq_peak : pathlib.Path object or string Path to the map to be used as frequency of the peak of the emission or its scalar value as a Quantity or a string convertible to a Quantity freq_ref_peak : Quantity or string Reference frequency for the peak frequency map They should be a astropy Quantity object or a string (e.g. “1500 MHz”) compatible with GHz. nside: int Resolution parameter at which this model is to be calculated.

Methods Summary

 get_emission(self, freqs[, weights]) This function evaluates the component model at a either a single frequency, an array of frequencies, or over a bandpass.

Methods Documentation

get_emission(self, freqs: Unit("GHz"), weights=None)[source] [edit on github]

This function evaluates the component model at a either a single frequency, an array of frequencies, or over a bandpass.

Parameters: freqs: scalar or array astropy.units.Quantity Frequency at which the model should be evaluated, in a frequency which can be converted to GHz using astropy.units. If an array of frequencies is provided, integrate using trapz with a equal weighting, i.e. simulate a top-hat bandpass. weights: np.array, optional Array of weights describing the frequency response of the instrument, i.e. the bandpass. Weights are normalized and applied in Jy/sr. output : astropy.units.Quantity Simulated map at the given frequency or integrated over the given bandpass. The shape of the output is (3,npix) for polarized components, (1,npix) for temperature-only components. Output is in uK_RJ.