antaress.ANTARESS_process.ANTARESS_plocc_spec module

def_in_plocc_profiles(inst, vis, gen_dic, data_dic, data_prop, coord_dic, system_param, theo_dic, glob_fit_dic, plot_dic)

Planet-occulted exposure profiles.

Calls requested function to define planet-occulted profiles associated with each observed exposure

• local profiles are used to correct differential profiles from stellar contamination

• intrinsic profiles are used to assess fit quality

Parameters:

TBD

Returns:

TBD

plocc_prof_meas(opt_dic, corr_mode, inst, vis, gen_dic, data_dic, data_prop, coord_dic)

Planet-occulted exposure profiles: measured

Sub-function to define planet-occulted profiles using measured profiles as best estimates of intrinsic profiles

When binned intrinsic profiles are used

• we first define the range and center of the binned profiles, along the bin dimension

• for each in-transit local profile, we find the nearest binned profile along the bin dimension (via their centers)

• we use intrinsic profiles that have already been aligned to a null rest frame, first shifting them to the rv of the target local profile, and then binning them

• we could use the original intrinsic profiles and shift them by their own rv minus that of the local profile, however in this way we can use directly the outputs of align_Intr(), and shifting the profiles in two steps is not an issue when they are not resampled until binned

• we finally bin the aligned profiles, and scale the binned profile to the level of the local one

Parameters:

TBD

Returns:

TBD

plocc_ar_prof_globmod(opt_dic, corr_mode, inst, vis, gen_dic, data_dic, data_prop, system_param, theo_dic, coord_dic, glob_fit_dic, ar_on)

Planet-occulted / active-region contaminated exposure profiles: global model

Sub-function to define planet-occulted and active region profiles using line profile models fitted to all

• intrinsic profiles together in fit_IntrProf_all(). This model can be based on analytical, measured, or theoretical profiles.

• to all differential profiles together with fit_DiffProf_all(). This model is based on analytical profiles.

Flux scaling is not applied to a global intrinsic profile using the chromatic light curve, but re-calculated for each planet-occulted intrinsic line profile for more flexibility (the cumulated scaling should be equivalent). rv used to shift the profiles are similarly re-calculated theoretically.

Parameters:

TBD

Returns:

TBD

plocc_prof_indivmod(opt_dic, corr_mode, inst, vis, gen_dic, data_dic)

Planet-occulted exposure profiles: individual model

Sub-function to define planet-occulted profiles using line profile model fitted to individual intrinsic lines. These models correspond directly to the measured profile and needs only be rescaled to the level of the local profile. This approach only works for exposures in which the stellar line could be fitted correctly after excluding the planet-contaminated range

Parameters:

TBD

Returns:

TBD

plocc_prof_rec(opt_dic, corr_mode, inst, vis, gen_dic, data_dic, coord_dic)

Planet-occulted exposure profiles: reconstructed

Sub-function to define planet-occulted profiles by reconstructing undefined pixels via a polynomial fit to defined pixels in complementary exposures, or via a 2D interpolation over complementary exposures and a narrow spectral band.

• providing the planetary track shifts sufficiently during the transit, we can reconstruct the local spectra at all wavelengths by interpolating the surrounding spectra at the wavelengths masked for planetary absorption. this approach allows accounting for changes in the shape of the local stellar spectra between exposures.

• we reconstruct undefined pixels in the map of intrinsic profiles aligned in the null rest frame and resampled on the common spectral table. for each exposure, we then shift the corresponding reconstructed profile to the stellar surface velocity associated with the exposure, and resample it on the exposure table. ideally the map should be first aligned at the stellar surface velocity of each exposure, and then resampled on its table, but that would take too much time and the error is likely lower than that introduced by the interpolation.

• no errors are propagated onto the new pixels.

• at defined pixels, the local profile and its best estimate for the intrinsic profile will have the same values, resulting in null values in the atmospheric profiles. there will be small differences due to the need to resample the estimate on a different table than the corresponding local profile.

Parameters:

TBD

Returns:

TBD

def_diff_profiles(inst, vis, gen_dic, data_dic, data_prop, coord_dic, system_param, theo_dic, glob_fit_dic, plot_dic)

Planet-occulted and active regions exposure profiles.

Calls requested function to define planet-occulted and active regions profiles associated with each observed exposure

Parameters:

TBD

Returns:

TBD

eval_diff_profiles(inst, vis, gen_dic, data_dic, data_prop, coord_dic, system_param, theo_dic, glob_fit_dic, plot_dic, calc_mode)

Differential profile correction

Uses previously computed estimates for planet-occulted and active region differential profiles to remove the impact of active regions. In doing so, the quiet star is put back as well.

Correcting exposure profile for the active region contamination - planet-active region overlap is accounted for Let us define F_exp as the profile of a given exposure. Then F_exp can be expressed as:

F_exp = F_DI - F_pl - F_ar

where F_DI is the unocculted star profile and F_pl, F_ar are planet and active region deviation profiles The planet-deviation profile can be re-written as:

F_pl = sum( pl, sum(region A, f) + sum(ar, sum(region B, s)))

where region A is the portion of the planet-occulted regions that covers the quiet star, region B is the portion of the planet-occulted regions that covers each active. We sum over ar’ which are the subset of active regions that are occulted by the planet. By construction in the code, we ensure that the active region - active region overlap is accounted for correctly (i.e. birght regions win the overlap). f is the profile that we use to tile the quiet stellar grid and s is the profile used to tile the active region grids.

While the active region-deviation profile is:

F_ar = sum( ar, sum(region B U C, f - s) )

where region B is the portion of active regions that is occulted by planet(s) and region C is the portion of active regions that is not occulted by planet(s).

To remove the impact of active regions in the exposure profile F_exp, we use the best-fit results from our fitting routine to find an estimate for F_sp and for the sums sum(ar’, sum(region B, s)). The latter will act to remove the active region contamination from the planet-occulted region while adding back the quiet star. We rename the model-derived portion as F_ar’ and s’. In this parametrization, we have:

F_exp ~= F_DI - F_ar’ - sum( pl, sum(region A, f) + sum( ar’, sum(region B, s’) ) ) <==> F_exp + F_ar’ + sum( pl, sum( ar’, sum(region B, s’) ) ) = F_DI - sum( pl, sum(region A, f))

At this point, we simply need to re-inject the quiet star in all the regions B to obtain an exposure profile uncontaminated by active regions:

F_exp + F_ar’ + sum( pl, sum( ar’, sum(region B, s’) ) ) - sum( pl, sum( ar’, sum(region B, f) ) ) = F_DI - sum( pl, sum(region A, f)) - sum( ar’, sum(region B, f) ) <==> F_exp + F_ar’ + sum( pl, sum( ar’, sum(region B, s’ - f) ) ) = F_DI - F_pl,clean

With F_pl,clean being the the planet deviation profile if active regions were not present in the planet-occulted region. In the code below, ar_prop_dic[chrom_mode][‘line_prof’][:,0] corresponds to F_ar’ while surf_prop_dic[chrom_mode][‘corr_supp’][:,0] corresponds to sum( pl, sum( ar’, sum(region B, s’ - f) ) ).

Parameters:

TBD

Returns:

TBD