lib.Instrument.Qacquisition module

class lib.Instrument.Qacquisition.JointAcquisitionComponentsMapMaking(d, comp, Nsub, nus_external, nsub_planck, nu_co=None, H=None, weight_planck=1.0)

Bases: object

Methods

get_invntt_operator
get_operator

get_invntt_operator(qubic_ndet, qubic_npho150, qubic_npho220, planck_ntot, seenpix=None)

get_operator(A, gain=None, fwhm=None, nu_co=None)

class lib.Instrument.Qacquisition.JointAcquisitionFrequencyMapMaking(d, Nrec, Nsub, H=None, nsub_planck=1, is_external_data=False, sampling=None)

Bases: object

Methods

get_invntt_operator
get_operator

get_invntt_operator(qubic_ndet, qubic_npho150, qubic_npho220, planck_ntot, seenpix, weight_planck=1, beam_correction=None)

get_operator(fwhm=None, seenpix=None)

class lib.Instrument.Qacquisition.PlanckAcquisition(nus, nside, comps=None, nsub_planck=1)

Bases: object

Methods

get_invntt_operator(planck_ntot[, ...])	Planck inverse noise covariance matrix.
get_noise(planck_ntot[, weight_planck, ...])	Planck Noise
get_operator([A, fwhm, comm, nu_co])	Planck Acquisition Operator.

get_invntt_operator(planck_ntot, weight_planck=1.0, seenpix=None, beam_correction=0)

Planck inverse noise covariance matrix.

Method to build Planck inverse noise covariance matrix, using sigma computed during the initialisation of the class.

Parameters:

• planck_ntot (float) – Multiplicative factor for the noise

• weight_planck (float, optional) – Weight of Planck information inside the QUBIC patch, by default 1.0

• seenpix (array, optional) – Array of pixels seen by QUBIC, by default None

• beam_correction (float, optional) – Correction factor for the beam, by default 0

Returns:

_description_

Return type:

_type_

get_noise(planck_ntot, weight_planck=1.0, seenpix=None, seed=None)

Planck Noise

Method to build Planck noise. It uses sigma values computed during initialisation of the classe.

Parameters:

• planck_ntot (float) – Multiplicative factor for the noise.

• weight_planck (float) – Weight of Planck information inside the QUBIC patch, by default 1.0

• seed (int, optional) – Seed for random noise generation, by default None

• seenpix (array, optional) – Array of pixels seen by QUBIC, by default None

Returns:

Array containing noise for Planck TOD

Return type:

array

get_operator(A=None, fwhm=None, comm=None, nu_co=None)

Planck Acquisition Operator.

Method to build the acquisition operator for Planck. This operator is composed at first by a convolution operator at Planck FWHM. Then, for the Component MapMaking, a Mixing Operator is added. Finally, we have the operator to turn maps into TOD.

Parameters:

• A (array, optional) – Mixing Matrix of Planck. If None, the Mixing Operator will be the Identity (FMM case), not None, the Mixing Operator will be computated and then added (CMM case), by default None

• fwhm (array, optional) – Array of lenght the number of Planck bands considered containing Planck FWHM. If None, the Convolution Operator will be Identity (case without convolution), if not None, the Convolution Operator will be computed and then added, by default None

• comm (MPI communicator, optional) – MPI communicator from pyoperators, by default None

• nu_co (bool, optional) – Bool to add Carbon Oxyde emission line, not supported yet, by default None

Returns:

Planck Acquisition Operator.

Return type:

BlockColumnOperator

class lib.Instrument.Qacquisition.QubicAcquisition(instrument, sampling, scene, d)

Bases: Acquisition

The QubicAcquisition class, which combines the instrument, sampling and scene models.

Methods

get_add_grids_operator()	Return operator to add signal from detector pairs.
get_aperture_integration_operator()	Integrate flux density in the telescope aperture.
get_convolution_peak_operator(**keywords)	Return an operator that convolves the Healpix sky by the gaussian kernel that, if used in conjonction with the peak sampling operator, best approximates the synthetic beam.
get_coverage()	Return the acquisition scene coverage as given by H.T(1), normalized so that its integral over the sky is the number of detectors times the duration of the acquisition.
get_detector_integration_operator()	Integrate flux density in detector solid angles.
get_detector_response_operator()	Return the operator for the bolometer responses.
get_distribution_operator()	Return the MPI distribution operator.
get_filter_operator()	Return the filter operator.
get_hitmap([nside])	Return a healpy map whose values are the number of times a pointing hits the pixel.
get_hwp_operator()	Return the operator for the bolometer responses.
get_invntt_operator(det_noise, photon_noise)	Return the inverse time-time noise correlation matrix as an Operator.
get_noise(det_noise, photon_noise[, seed, out])	Return the noise realization according the instrument's noise model.
get_observation(x[, noiseless, out, operation])	Return out=H(x)+n, the observation according to the acquisition model.
get_operator()	Return the operator of the acquisition.
get_operator_nbytes()	Return the number of bytes required to store the acquisition model as an operator.
get_polarizer_operator()	Return operator for the polarizer grid.
get_projection_operator([verbose])	Return the projection operator for the peak sampling.
get_subtract_grids_operator()	Return operator to subtract signal from detector pairs.
get_unit_conversion_operator()	Convert sky temperature into W / m^2 / Hz.
pack(x[, out, copy])	Convert a multi-dimensional array into a 1-dimensional array which only includes the selected components, potentially ordered according to a given ordering.
plot([map, header, new_figure, percentile])	map : ndarray of dim 2
unpack(x[, out, missing_value, copy])	Convert a 1-dimensional array into a multi-dimensional array which includes the non-selected components, mimicking the multi-dimensional layout.

get_diag_invntt_operator
get_preconditioner

get_add_grids_operator()

Return operator to add signal from detector pairs.

get_aperture_integration_operator()

Integrate flux density in the telescope aperture. Convert signal from W / m^2 / Hz into W / Hz.

get_convolution_peak_operator(**keywords)

Return an operator that convolves the Healpix sky by the gaussian kernel that, if used in conjonction with the peak sampling operator, best approximates the synthetic beam.

get_coverage()

Return the acquisition scene coverage as given by H.T(1), normalized so that its integral over the sky is the number of detectors times the duration of the acquisition.

get_detector_integration_operator()

Integrate flux density in detector solid angles. Convert W / sr into W.

get_detector_response_operator()

Return the operator for the bolometer responses.

get_diag_invntt_operator()

get_distribution_operator()

Return the MPI distribution operator.

get_filter_operator()

Return the filter operator. Convert units from W/Hz to W.

get_hitmap(nside=None)

Return a healpy map whose values are the number of times a pointing hits the pixel.

get_hwp_operator()

Return the operator for the bolometer responses.

get_invntt_operator(det_noise, photon_noise)

Return the inverse time-time noise correlation matrix as an Operator.

get_noise(det_noise, photon_noise, seed=None, out=None)

Return the noise realization according the instrument’s noise model.

Parameters:

out (ndarray, optional) – Placeholder for the output noise.

get_operator()

Return the operator of the acquisition. Note that the operator is only linear if the scene temperature is differential (absolute=False).

get_polarizer_operator()

Return operator for the polarizer grid.

get_preconditioner(cov)

get_projection_operator(verbose=True)

Return the projection operator for the peak sampling. Convert units from W to W/sr. :type verbose: :param verbose: If true, display information about the memory allocation. :type verbose: bool, optional

get_subtract_grids_operator()

Return operator to subtract signal from detector pairs.

get_unit_conversion_operator()

Convert sky temperature into W / m^2 / Hz. If the scene has been initialised with the ‘absolute’ keyword, the scene is assumed to include the CMB background and the fluctuations (in Kelvin) and the operator follows the non-linear Planck law. Otherwise, the scene only includes the fluctuations (in microKelvin) and the operator is linear (i.e. the output also corresponds to power fluctuations).

class lib.Instrument.Qacquisition.QubicInstrumentType(dictionary, nsub, nrec, comps=[], H=None, nu_co=None, sampling=None)

Bases: QubicMultiAcquisitions

Class providing methods necessary for all instrument types.

Methods

get_invntt_operator(wdet, wpho150, wpho220)	Method to compute the inverse noise covariance matrix in time-domain.
get_operator([A, gain, fwhm])	Method to generate the pointing matrix.
sum_over_band(h, algo[, gain])	Perform sum over sub-operators depending on the reconstruction algorithms (FMM or CMM)

get_invntt_operator(wdet, wpho150, wpho220)

Method to compute the inverse noise covariance matrix in time-domain.

get_operator(A=None, gain=None, fwhm=None)

Method to generate the pointing matrix.

mixing_matrixarray like containing mixing matrix elements. If the elements of the mixing matrix are constant across the sky,

mixing_matrix.shape = (nfreq, ncomp)

sum_over_band(h, algo, gain=None)

Perform sum over sub-operators depending on the reconstruction algorithms (FMM or CMM)

class lib.Instrument.Qacquisition.QubicMultiAcquisitions(dictionary, nsub, nrec, comps=[], H=None, nu_co=None, sampling=None)

Bases: object

Instance to define the multi-frequency instrument.

Input- dictionarycontains QUBIC informations

• Nsub : Number of sub-bands for integrating the physical bandwidth

• Nrec : Number of reconstructed maps (in the case of FMM)

• comps : List of astrophysical components (CMB, Dust, …)

• H : List of pointing matrix if not already computed

• nu_co : Frequency of a line emission