COLines¶
- class pysm3.COLines(nside, max_nside=None, has_polarization=True, lines=['10', '21', '32'], include_high_galactic_latitude_clouds=False, polarization_fraction=0.001, theta_high_galactic_latitude_deg=20.0, random_seed=1234567, verbose=False, run_mcmole3d=False, map_dist=None)[source] [edit on github]¶
Bases:
Model
Class defining attributes for CO line emission. CO templates are extracted from Type 1 CO Planck maps. See further details in: https://www.aanda.org/articles/aa/abs/2014/11/aa21553-13/aa21553-13.html
- Parameters:
- nsideint
HEALPix NSIDE of the output maps
- has_polarizationbool
whether or not to simulate also polarization maps
- lineslist of strings
CO rotational transitions to consider. Accepted values : 10, 21, 32
- polarization_fraction: float
polarisation fraction for polarised CO emission.
- include_high_galactic_latitude_clouds: bool
If True it includes a simulation from MCMole3D to include high Galactic Latitude clouds. (See more details at http://giuspugl.github.io/mcmole/index.html)
- run_mcmole3d: bool
If True it simulates HGL cluds by running MCMole3D, otherwise it coadds a map of HGL emission.
- random_seed: int
set random seed for mcmole3d simulations.
- theta_high_galactic_latitude_degfloat
Angle in degree to identify High Galactic Latitude clouds (i.e. clouds whose latitude b is
|b|> theta_high_galactic_latitude_deg
).- map_distmpi4py communicator
Read inputs across a MPI communicator, see pysm.read_map
Methods Summary
get_emission
(freqs[, weights])This function evaluates the component model at a either a single frequency, an array of frequencies, or over a bandpass.
Coadd High Galactic Latitude CO emission, simulated with MCMole3D.
simulate_polarized_emission
(I_map)Add polarized emission by means of: * an overall constant polarization fraction, * a depolarization map to mimick the line of sight depolarization effect at low Galactic latitudes * a polarization angle map coming from a dust template (we exploit the observed correlation between polarized dust and molecular emission in star forming regions).
Methods Documentation
- get_emission(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.
- Returns:
- outputastropy.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
.
- simulate_high_galactic_latitude_CO(line)[source] [edit on github]¶
Coadd High Galactic Latitude CO emission, simulated with MCMole3D.
- simulate_polarized_emission(I_map)[source] [edit on github]¶
Add polarized emission by means of: * an overall constant polarization fraction, * a depolarization map to mimick the line of sight depolarization effect at low Galactic latitudes * a polarization angle map coming from a dust template (we exploit the observed correlation between polarized dust and molecular emission in star forming regions).