PySM Documentation

This code generates full-sky simulations of Galactic foregrounds in intensity and polarization relevant for CMB experiments. The components simulated are: thermal dust, synchrotron, AME, free-free, and CMB at a given Nside, with an option to integrate over a top hat bandpass, to add white instrument noise, and to smooth with a given beam.

There is scope for a few options for the model for each component, attempting to be consistent with current data.

Currently much of the available data is limited in resolution at degree-scale. We therefore make efforts to provide reasonable small-scale simulations to extend the data to higher multipoles. The details of the procedures developed can be found in the accompanying paper.

This code is based on the large-scale Galactic part of Planck Sky Model (Delabrouille 2012) code and uses some of its inputs.


Each model is identified with a letter and a number, the letter indicates the kind of emission and the number the type of model, generally in order of complexity starting at 1. For example for dust we start with d1 based on Planck commander results, d4 has 2 dust populations and d6 implements a model of dust frequency decorrelation.

For example free-free:

f1: We model the free-free emission using the analytic model assumed in the Commander fit to the Planck 2015 data (Draine 2011 Physics of the Interstellar and Intergalactic Medium) to produce a degree-scale map of free-free emission at 30 GHz. We add small scales to this using a procedure outlined in the accompanying paper. This map is then scaled in frequency by applying a spatially constant power law index of -2.14.


PySM is written in Python and requires:

In order to run in parallel with MPI, it also needs:

  • mpi4py

To support distributed smoothing, it also requires:


Clone the GitHub repository and run:

pip install .

for a development installation, instead run:

pip install -e .


pysm Package



Apply smoothing and coordinate rotation to an input map

bandpass_unit_conversion(freqs, weights, …)

Unit conversion from uK_RJ to output unit given a bandpass


Function to check that the input to Model.get_emission is a np.ndarray.

mpi_smoothing(input_map, fwhm, map_dist)

normalize_weights(freqs, weights)

read_map(path, nside[, unit, field, …])

Wrapper of healpy.read_map for PySM data.


Run the tests for the package.


CMBLensed(nside, cmb_spectra[, cmb_seed, …])

Lensed CMB

CMBMap(nside[, map_IQU, map_I, map_Q, …])


DecorrelatedModifiedBlackBody([map_I, …])

See parent class for other documentation.

InterpolatingComponent(path, input_units, nside)

PySM component interpolating between precomputed maps

MapDistribution([pixel_indices, mpi_comm, …])

Define how a map is distributed

Model(nside[, map_dist, dataurl])

This is the template object for PySM objects.

ModifiedBlackBody(map_I, map_Q, map_U, …)

This is a model for modified black body emission.

PowerLaw(map_I, freq_ref_I, map_pl_index, nside)

This is a model for a simple power law synchrotron model.

Sky([nside, component_objects, …])

This class is a convenience object that wraps together a group of component models.

SpDust(map_I, freq_ref_I, emissivity, …[, …])

Implementation of the SpDust2 code of (Ali-Haimoud et al 2012) evaluated for a Cold Neutral Medium.

SpDustPol(map_I, freq_ref_I, emissivity, …)

SpDust2 model with Polarized emission


Class Inheritance Diagram

Inheritance diagram of pysm.models.cmb.CMBLensed, pysm.models.cmb.CMBMap, pysm.models.dust.DecorrelatedModifiedBlackBody, pysm.models.interpolating.InterpolatingComponent, pysm.distribution.MapDistribution, pysm.models.template.Model, pysm.models.dust.ModifiedBlackBody, pysm.models.power_law.PowerLaw,, pysm.models.spdust.SpDust, pysm.models.spdust.SpDustPol, pysm.UnsupportedPythonError