Instrument models
This module contains models to perform NSC on GLINT Mark II (2019-2021) and LBTI nuller.
- How to build a model:
1st argument = null depth,
2nd = wavelength scale
3rd = int representing the iteration over wavelength scale
next: “constants” values (not random values for MC)
end: quantities generated by MC
- instrument_models.glint_model(na, opd, wavelength, wl_idx, spec_chan_width, spectra, zeta_minus_A, zeta_minus_B, zeta_plus_A, zeta_plus_B, injA, injB, dark_null, dark_antinull)
Model of the GLINT instrument (version of the instrument 2019 - 2021).
Parameters
- nalist-like
List containing the deterministic value astrophysical null depth
- opdlist-like
Sequence of OPD. If single value, must be in an array of shape (1,1).
- wavelength1d-array
Wavelength in the same unit as the OPD.
- wl_idxint
wavelength cursor.
- spec_chan_widthfloat
Width of a spectral channel, in the same unit as
wavelength.- spectra2d-array
Spectrum of the source seen by both aperture.
- zeta_minus_A1d-array
Splitting ratio between the null output and the photometric output of beam A.
- zeta_minus_B1d-array
Splitting ratio between the null output and the photometric output of beam B.
- zeta_plus_A1d-array
Splitting ratio between the anti-null output and the photometric output of beam A.
- zeta_plus_B1d-array
Splitting ratio between the anti-null output and the photometric output of beam B.
- injA1d-array
Sequence of injection of beam A.
- injB1d-array
Sequence of injection of beam B.
- dark_null1d-array
Detector noise in the null output.
- dark_antinull1d-array
Detector noise in the anti-null output.
Returns
- null1d-array
Sequence of simulated null depth.
- Iminus1d-array
Sequence of simulated null output.
- Iplus1d-array
Sequence of simulated anti-null output.
- instrument_models.lbti_model(na, opd, wavelength, wl_idx, spec_chan_width, phase_bias, IA, IB, thermal_bckg, sigma_eps)
Compute the null depth.
Compute the null depth from generated random values of photometries, detector noise and OPD. The estimator is the ratio of the null over the antinull fluxes.
Parameters
- nalist-like
List containing the deterministic value astrophysical null depth
- opdlist-like
Sequence of OPD. If single value, must be in an array of shape (1,1).
- wavelength1d-array
Wavelength in the same unit as the OPD.
- wl_idxint
wavelength cursor.
- spec_chan_widthfloat
Width of a spectral channel, in the same unit as
wavelength.- phase_biasfloat
Constant term of the phase, in radians.
- IA1d-array
Sequence of intensity of beam 1 contributing to the interferences. If single value, must be in an array of shape (1,).
- IB1d-array
Sequence of intensity of beam 2 contributing to the interferences. If single value, must be in an array of shape (1,).
- thermal_bckg1d-array
Sequence of therma background. If single value, must be in an array of shape (1,).
- sigma_eps1d-array
Sequence of intra-frame phase fluctuations. If single value, must be in an array of shape (1,).
Returns
- null1d-array
Sequence of simulated null depth. If cupy is installed, this is a cupy (GPU hosted) array
- Iminus1d-array
Sequence of simulated destructive interference. If cupy is installed, this is a cupy (GPU hosted) array
- Iplus1d-array
Sequence of simulated constructive interference. If cupy is installed, this is a cupy (GPU hosted) array
- instrument_models.test_multiargs(deterministic_params_to_fit, rv_fit, wavelength, wl_idx, spec_chan_width, phase_bias, IA, IB, thermal_bckg)
Compute the null depth.
Compute the null depth from generated random values of photometries, detector noise and OPD. The estimator is the ratio of the null over the antinull fluxes.
This version needs 6 parameters to fit: Null depth, mu and sigma OPD, factor correction of the thermal background ir, mu and sigma of the fringe blurring sigma_eps.
This model is used to test the ability of GRIP to handle models with more than 3 parameters and parameters of different natures (of the instrument model or governing the noise in the model).
Parameters
- deterministic_params_to_fitlist-like
List of the parameters to fit that are not parameters of statistical distributions.
- rv_fitlist-like
List of random values generated from distributions which parameters are to fit.
- wavelength1d-array
Wavelength in the same unit as the OPD.
- wl_idxint
wavelength cursor.
- spec_chan_widthfloat
Width of a spectral channel, in the same unit as
wavelength.- phase_biasfloat
Constant term of the phase, in radians.
- opd1d-array
Sequence of OPD. If single value, must be in an array of shape (1,).
- IA1d-array
Sequence of intensity of beam 1 contributing to the interferences. If single value, must be in an array of shape (1,).
- IB1d-array
Sequence of intensity of beam 2 contributing to the interferences. If single value, must be in an array of shape (1,).
- thermal_bckg1d-array
Sequence of therma background. If single value, must be in an array of shape (1,).
- sigma_eps1d-array
Sequence of intra-frame phase fluctuations. If single value, must be in an array of shape (1,).
Returns
- null1d-array
Sequence of simulated null depth. If cupy is installed, this is a cupy (GPU hosted) array
- Iminus1d-array
Sequence of simulated destructive interference. If cupy is installed, this is a cupy (GPU hosted) array
- Iplus1d-array
Sequence of simulated constructive interference. If cupy is installed, this is a cupy (GPU hosted) array