spec_time_series

spec_time_series#

class spec_time_series[source]#

Bases: object

Attributes

Note: attributes inherited from parent classes are not shown here, if any

`directory`	Directory containing the RASSINE reduced data include the ending WORKSPACE/
`starname`	Name of the star
`dir_root`	Directory containing the data under processing, parent of the WORKSPACE/ folder
`simbad_folder`	Path to the SIMBAD database
`mask_ccf_folder`	Path to the MASK_CCF folder
`material_folder`	Path to the Material folder
`instrument`	Instrument used for the measurements
`planet`	If a planet has been injected
`fwhm`	Full width half maximum of the CCF
`info_reduction_ut`	If info_reduction has been loaded, modification time of the loaded file
`dico_tree`	Table of relations between outputs produced at different stages of the pipeline
`material`	Table with elements having a spectral wavelength dimension
`star_info`	Information about the star

Methods

`continuum_error`	Produce error on the continuum by interpolating the error flux value at anchor points
`dace_statistic`
`flux_error`	Produce flux errors on the pickles files defined as the ron plus square root of flux
`import_ccf`
`import_dace_sts`
`import_dico_chain`
`import_dico_tree`	rtype: `None`
`import_info_reduction`	rtype: `None`
`import_material`	rtype: `None`
`import_rassine_output`	Import all the RASSINE dictionnaries in a list
`import_spectrum`	Import a pickle file of a spectrum to get fast common information shared by all spectra
`import_star_info`	rtype: `None`
`import_sts_flux`	rtype: `Sequence`[`ndarray`]
`import_table`	rtype: `None`
`read_ccf_mask`	rtype: `ndarray`[`Any`, `dtype`[`float64`]]
`scale_cmap`
`snr_statistic`
`sorted_rassine_pickles`	rtype: `Sequence`[`str`]
`spectrum`	Produce a tableXY spectrum by specifying its index number
`suppress_low_snr_spectra`	Suppress spectra under fixed treshold in SNR
`suppress_time_RV`
`suppress_time_spectra`	Suppress spectra according to time
`uncorrect_hole`	rtype: `ndarray`
`update_info_reduction`	rtype: `None`
`yarara_activity_index`	Produce the activity proxy time-series.
`yarara_add_ccf_entry`
`yarara_add_map`
`yarara_add_step_dico`	Add the step kw for the dico chain, if chain is set to True numbered the full chain
`yarara_analyse_summary`	Produce a summary table with the RASSINE files of the specified directory
`yarara_berv_summary`	Produce a berv summary
`yarara_ccf`	Compute the CCF of a spectrum, reference to use always the same continuum (matching_anchors highest SNR).
`yarara_ccf_save`
`yarara_check_fwhm`
`yarara_check_rv_sys`
`yarara_color_template`	Define the color template used in the weighting of the lines for the CCF.
`yarara_comp_all`
`yarara_correct_activity`	Display the time-series spectra with proxies and its correlation
`yarara_correct_borders_pxl`	Produce a brute mask to flag lines crossing pixels according to min-max shift
`yarara_correct_brute`	Brutal suppression of flux value with variance to high (final solution)
`yarara_correct_cosmics`	Supress flux value outside k-sigma mad clipping
`yarara_correct_frog`	Correction of the stitching/ghost on the spectrum by PCA fitting
`yarara_correct_mad`	Suppress flux value outside k-sigma mad clipping
`yarara_correct_oxygen`	Display the time-series spectra with proxies and its correlation
`yarara_correct_pattern`	Suppress interferency pattern produced by a material of a certain width by making a Fourier filtering.
`yarara_correct_secular_acc`	Compute the secular drift and correction the fluxes to cancel the drift
`yarara_correct_smooth`	rtype: `None`
`yarara_correct_telluric_gradient`	Display the time-series spectra with proxies and its correlation
`yarara_correct_telluric_proxy`	Display the time-series spectra with proxies and its correlation
`yarara_cut_spectrum`	Cut the spectrum time-series borders to reach the specified wavelength limits (included)
`yarara_exploding_pickle`	rtype: `None`
`yarara_flux_constant`	Compute the flux constant which allow to preserve the bolometric integrated flux
`yarara_get_berv_value`	Return the berv value for a given jdb date
`yarara_get_bin_length`
`yarara_get_first_wave`
`yarara_get_orders`	rtype: `ndarray`
`yarara_get_pixels`	rtype: `ndarray`
`yarara_map`	Display the time-series spectra with proxies and its correlation
`yarara_map_1d_to_2d`
`yarara_map_all`
`yarara_master_ccf`	rtype: `None`
`yarara_median_master`	Produce a median master by masking region of the spectrum
`yarara_non_zero_flux`	rtype: `Optional`[`ndarray`]
`yarara_obs_info`	Add some observationnal information in the RASSINE files and produce a summary table
`yarara_plot_all`	Plot all the RASSINE spectra in the same plot
`yarara_poissonian_noise`	rtype: `Tuple`[`ndarray`, `ndarray`]
`yarara_produce_mask_contam`	Creation of the stitching mask on the spectrum
`yarara_produce_mask_frog`	Correction of the stitching/ghost on the spectrum by PCA fitting
`yarara_retropropagation_correction`	rtype: `None`
`yarara_simbad_query`	Reads information about the star from the SIMBAD table and populates the Stellar_info_ pickle
`yarara_star_info`
`yarara_substract_map`
`yarara_suppress_doubtful_spectra`	Suppress outlier spectra
`yarara_telluric`	Plot all the RASSINE spectra in the same plot
`yarara_transit_def`	period in days, T0 transits center in jdb - 2'400'000, duration in hours

List of members of spec_time_series

yarara_correct_activity(sub_dico='matching_telluric', wave_min=3900.0, wave_max=4400.0, smooth_corr=5, reference='median', proxy_corr=['CaII'])#

Display the time-series spectra with proxies and its correlation

Parameters:

sub_dico (The sub_dictionnary used to select the continuum) –
continuum (The continuum to select (either linear or cubic)) –
wave_min (Minimum x axis limit) –
wave_max (Maximum x axis limit) –
zoom (int-type, to improve the resolution of the 2D plot) –
int-type (smooth_map =) –
convolution (smooth the 2D plot by gaussian 2D) –
curve (smooth_corr = smooth thecoefficient ofcorrelation) –
reference ('median', 'snr' or 'master' to select the reference normalised spectrum usedin the difference) –
proxy_corr (keyword of the first proxies from RASSINE dictionnary to use in the correlation) –
proxy_detrending (Degree of the polynomial fit to detrend the proxy) –
cmap (cmap of the 2D plot) –
dwin (window correction increase by dwin to slightly correct above around the peak of correlation) –

Return type:

None

continuum_error()#: Produce error on the continuum by interpolating the error flux value at anchor points

dace_statistic(substract_model=False, ymin=None, ymax=None, return_ylim=False)#

flux_error(ron=11)#

Produce flux errors on the pickles files defined as the ron plus square root of flux

Parameters:: ron – Read-out-Noise value of the reading detector errors
Return type:: None

import_dace_sts(substract_model=False)#

scale_cmap()#

snr_statistic(version=1)#

suppress_low_snr_spectra(suppress=False)#

Suppress spectra under fixed treshold in SNR

Parameters:: suppress (bool) – True/False to delete of simply hide the files

yarara_berv_summary(sub_dico='matching_diff', dbin_berv=0.3, nb_plot=3, telluric_fwhm=3.5)#

Produce a berv summary

Parameters:

sub_dico (The sub_dictionnary used to select the continuum) –
continuum (The continuum to select (either linear or cubic)) –
telluric_tresh (Treshold used to cover the position of the contaminated wavelength) –
wave_min (The minimum xlim axis) –
wave_max (The maximum xlim axis) –

yarara_check_fwhm(delta_window=5)#

yarara_check_rv_sys()#

yarara_color_template(sub_dico='matching_anchors', continuum='linear')#

Define the color template used in the weighting of the lines for the CCF. The color is defined as the matching_anchors continuum of the best SNR spectra. The product is saved in the Material file.

Parameters:

sub_dico (str) – The sub_dictionnary used to select the continuum
continuum (Literal[‘linear’]) – The continuum to select (can only be linear)

yarara_correct_secular_acc(update_rv=False)#

Compute the secular drift and correction the fluxes to cancel the drift

Parameters:: update_rv (True/False to update the flux value in order to cancel the secular drift) –

yarara_flux_constant()#: Compute the flux constant which allow to preserve the bolometric integrated flux

yarara_get_first_wave()#

yarara_map_1d_to_2d(instrument)#

yarara_simbad_query(starname=None)#

Reads information about the star from the SIMBAD table and populates the Stellar_info_ pickle

Return type:: None

yarara_suppress_doubtful_spectra(suppress=False)#

Suppress outlier spectra

Parameters:: suppress – Whether to hide or remove the file. Defaults to False.

yarara_transit_def(period=100000.0, T0=55000.0, duration=2.0, auto=False)#: period in days, T0 transits center in jdb - 2’400’000, duration in hours

yarara_ccf(mask, mask_name, sub_dico='matching_diff', ccf_name=None, ratio=False, reference=True, weighted=True, plot=False, save=True, save_ccf_profile=False, normalisation='left', del_outside_max=False, ccf_oversampling=1, rv_range=None, rv_borders=None, delta_window=5, rv_sys_='parameters_or_zero', rv_shift_='zeros', speed_up=True, force_brute=False, squared=True, p_noise=1 / np.inf, substract_map=[], add_map=[])#

Compute the CCF of a spectrum, reference to use always the same continuum (matching_anchors highest SNR). Display_ccf to plot all the individual CCF. Plot to plot the FWHM, contrast and RV.

mask: if was used previously as None, use sts.read_ccf_mask(sts.mask_harps) and set mask_name to sts.mask_harps

Parameters:

sub_dico (str) – The sub_dictionary used to select the continuum
mask (ndarray[Any, dtype[float64]]) – The line mask used to cross correlate with the spectrum (mask should be located in MASK_CCF otherwise KITCAT dico)
threshold_telluric – Maximum telluric contamination to keep a stellar line in the mask
reference (Union[bool, Literal[‘norm’], Literal[‘master_snr’]]) – True/False or ‘norm’, True use the matching anchors of reference, False use the continuum of each spectrum, norm use the continuum normalised spectrum (not )
plot (bool) – True/False to plot the RV time-series
display_ccf – display all the ccf subproduct
save (bool) – True/False to save the informations iun summary table
normalisation (Union[Literal[‘left’], Literal[‘slope’]]) – ‘left’ or ‘slope’. if left normalise the CCF by the most left value, otherwise fit a line between the two highest point
maximam (del_outside) – True/False to delete the CCF outside the two bump in personal mask
speed_up (bool) – remove region from the CCF not crossed by a line in the mask to speed up the code
force_brute (bool) – force to remove the region excluded by the brute mask
rv_sys – km/s
rv_shift – if nd_array, in m/s
mask_name (str) – Name used to save the mask in ANAL

Return type:

Dict[str, tableXY]

read_ccf_mask(mask_name)#

Return type:: ndarray[Any, dtype[float64]]

yarara_ccf_save(mask, sub_dico)#

yarara_master_ccf(sub_dico='matching_diff', name_ext='', rvs_=None)#

Return type:: None

yarara_get_berv_value(time_value, Draw=False, new=True, light_graphic=False, save_fig=True)#

Return the berv value for a given jdb date

Return type:: Union[ndarray[Any, dtype[float64]], float]

yarara_get_orders()#

Return type:: ndarray

yarara_get_pixels()#

Return type:: ndarray

yarara_correct_borders_pxl(pixels_to_reject=[2, 4095], min_shift=-30, max_shift=30)#

Produce a brute mask to flag lines crossing pixels according to min-max shift

Parameters:

pixels_to_reject (List of pixels) –
min_shift (min shist value in km/s) –
max_shift (max shist value in km/s) –

Return type:

None

yarara_correct_frog(sub_dico='matching_diff', correction='stitching', wave_min=3800.0, wave_max=3975.0, wave_min_train=3700.0, wave_max_train=6000.0, complete_analysis=False, reference='median', equal_weight=True, nb_pca_comp=10, pca_comp_kept_=None, rcorr_min=0.0, threshold_contam=0.5, algo_pca='empca')#

Correction of the stitching/ghost on the spectrum by PCA fitting

Parameters:

sub_dico (The sub_dictionnary used to select the continuum) –
continuum (The continuum to select (either linear or cubic)) –
reference ('median', 'snr' or 'master' to select the reference normalised spectrum used in the difference) –
extended (extension of the cluster size) –

Return type:

None

yarara_correct_pattern(sub_dico='matching_diff', wave_min=6000.0, wave_max=6100.0, reference='median', width_range=(0.1, 20.0), correct_blue=True, correct_red=True, jdb_range=None)#

Suppress interferency pattern produced by a material of a certain width by making a Fourier filtering. Width_min is the minimum width possible for the material in mm.

Parameters:

sub_dico (The sub_dictionnary used to select the continuum) –
wave_min (Minimum x axis limit for the plot) –
wave_max (Maximum x axis limit for the plot) –
reference ('median', 'snr' or 'master' to select the reference normalised spectrum usedin the difference) –
width_min (minimum width in mm above which to search for a peak in Fourier space) –
correct_blue (enable correction of the blue detector for HARPS) –
correct_red (enable correction of the red detector for HARPS) –

Return type:

None

yarara_produce_mask_contam(frog_file)#

Creation of the stitching mask on the spectrum

Parameters:: frog_file (files containing the wavelength of the stitching) –
Return type:: None

yarara_produce_mask_frog(frog_file)#

Correction of the stitching/ghost on the spectrum by PCA fitting

Params:: sub_dico: The sub_dictionnary used to select the continuum frog_file: files containing the wavelength of the stitching

Return type:: None

import_ccf()#

yarara_add_ccf_entry(kw, default_value=1)#

import_dico_chain(last_dico)#

import_dico_tree()#

Return type:: None

yarara_add_step_dico(sub_dico, step, sub_dico_used, chain=False)#

Add the step kw for the dico chain, if chain is set to True numbered the full chain

Return type:: None

import_sts_flux(load=['flux', 'flux_err', 'matching_diff'], num=None)#

Return type:: Sequence[ndarray]

import_material()#

Return type:: None

yarara_obs_info(df)#

Add some observationnal information in the RASSINE files and produce a summary table

Parameters:: kw (list-like with format [keyword,array]) –
Return type:: None

sorted_rassine_pickles()#

Return type:: Sequence[str]

yarara_exploding_pickle()#

Return type:: None

import_rassine_output(return_name=False, kw1=None, kw2=None)#

Import all the RASSINE dictionnaries in a list

Parameters:: return_name (True/False to also return the filenames) –
Return type:: Any
Returns:: Return the list containing all thedictionnary

import_info_reduction()#

Return type:: None

update_info_reduction()#

Return type:: None

import_spectrum(num=0)#

Import a pickle file of a spectrum to get fast common information shared by all spectra

Parameters:: num (int) – Index of the spectrum to extract (if None random selection)
Return type:: Dict[str, Any]
Returns:: The opened pickle file

spectrum(num=0, sub_dico='matching_diff', norm=False, planet=False, color_correction=False)#

Produce a tableXY spectrum by specifying its index number

Parameters:

num (int) – index of the spectrum to extract
sub_dico (str) – The sub_dictionnary used to select the continuum
continuum – The continuum to select (either linear or cubic)
norm (bool) – True/False button to normalize the spectrum

Return type:

tableXY

Returns:

The tableXY spectrum object

yarara_get_bin_length()#

import_star_info()#

Return type:: None

yarara_star_info(Rv_sys=None, simbad_name=None, magB=None, magV=None, magR=None, BV=None, VR=None, sp_type=None, Mstar=None, Rstar=None, Vsini=None, Vmicro=None, Teff=None, log_g=None, FeH=None, Prot=None, Fwhm=None, Contrast=None, CCF_delta=None, Pmag=None, stellar_template=None, Contam_BERV=None)#

yarara_analyse_summary(rm_old=False)#

Produce a summary table with the RASSINE files of the specified directory

Return type:: None

suppress_time_RV(liste)#

suppress_time_spectra(mask, suppress=False, name_ext='temp')#

Suppress spectra according to time

Parameters:

mask (ndarray[Any, dtype[bool_]]) – True for the ones to suppress
limit (jdb or num are both inclusive in lower and upper) –
snr_cutoff – treshold value of the cutoff below which spectra are removed
suppress (bool) – True/False to delete of simply hide the files

Return type:

None

import_table()#

Return type:: None

yarara_correct_brute(sub_dico='matching_mad', reference='median', win_roll=1000, min_length=5, percent_removed=10, k_sigma=2, extended=10, borders_pxl=False)#

Brutal suppression of flux value with variance to high (final solution)

Parameters:

sub_dico (The sub_dictionnary used to select the continuum) –
continuum (The continuum to select (either linear or cubic)) –
reference ('median', 'snr' or 'master' to select the reference normalised spectrum used in the difference) –
win_roll (window size of the rolling algorithm) –
min_length (minimum cluster length to be flagged) –
k_sigma (k_sigma of the rolling mad clipping) –
extended (extension of the cluster size) –
low (lowest cmap value) –
high (highest cmap value) –
cmap (cmap of the 2D plot) –

Return type:

None

yarara_correct_cosmics(sub_dico='matching_diff', k_sigma=3, bypass_warning=True)#

Supress flux value outside k-sigma mad clipping

Parameters:

sub_dico (The sub_dictionnary used to select the continuum) –
continuum (The continuum to select (either linear or cubic)) –

Return type:

None

yarara_correct_mad(sub_dico='matching_diff', k_sigma=2, k_mad=2, n_iter=1, ext='0')#

Suppress flux value outside k-sigma mad clipping

# SUPRESS VARIATION RELATIF TO MEDIAN-MAD SPECTRUM (OUTLIERS CORRECTION + ECCENTRIC PLANET)

Parameters:

sub_dico (str) – The sub_dictionnary used to select the continuum
ext (str) – Index used in saving the mad_statistics_iter_%d.png file

Return type:

ndarray

yarara_correct_smooth(sub_dico='matching_diff', reference='median', wave_min=4200.0, wave_max=4300.0, window_ang=5.0)#

Return type:: None

yarara_comp_all(sub_dico1='matching_cosmics', sub_dico2='matching_mad', analysis='h2o_1')#

yarara_plot_all(sub_dico='matching_diff', wave_min=4400.0, wave_max=4500.0, plot_median=False, berv_keys='none', cmap='brg', color='CaII', relatif=False, new=True, substract_map=[], p_noise=1 / np.inf)#

Plot all the RASSINE spectra in the same plot

Parameters:

sub_dico (The sub_dictionnary used to select the continuum) –
continuum (The continuum to select (either linear or cubic)) –
wave_min (The minimum xlim axis) –
wave_max (The maximum xlim axis) –
plot_median (True/False, Plot the median of the spectrum) –
berv_keys (The berv keyword from RASSINE dictionnary to remove the berv from the spectra (berv in kms)) –
planet (True/False to use the flux containing the injected planet or not) –

yarara_activity_index(sub_dico='matching_diff', plot=True, debug=False, calib_std=0, optimize=False, p_noise=1 / np.inf, save_kw=True)#

Produce the activity proxy time-series. Need to cancel the RV systemic of the star

Parameters:

sub_dico (The sub_dictionnary used to select the continuum) –
continuum (The continuum to select (either linear or cubic)) –
rv (The RV of the star system) –
plot (True/False, Plot the proxies time-series) –
debug (True/False, Plot the intermediate graphicwith the spectrum and area extraction for the proxies) –
ron (read-out-noise error injected by reading pixels) –
calib_std (std error due to flat-field photon noise (5.34e-4 or 10.00e-4 Cretignier+20)) –

Return type:

None

yarara_map(sub_dico='matching_diff', planet=False, unit=1.0, wave_min=4000.0, wave_max=4300.0, index='index', ratio=False, reference='median', new=True, plot=True, substract_map=[], add_map=[], correction_factor=True, p_noise=1 / np.inf)#

Display the time-series spectra with proxies and its correlation

Parameters:

sub_dico (The sub_dictionnary used to select the continuum) –
continuum (The continuum to select (either linear or cubic)) –
wave_min (Minimum x axis limit) –
wave_max (Maximum x axis limit) –
index ('index' or 'time' if 'time', display the time-series with blank color if no spectra at specific time (need roughly equidistant time-series spectra)) –
zoom (int-type, to improve the resolution of the 2D plot) –
int-type (smooth_map =) –
convolution (smooth the 2D plot by gaussian 2D) –
reference ('median', 'snr' or 'master' to select the reference normalised spectrum usedin the difference) –
rv_shift (keyword column to use to shift spectra, m/s speed) –
cmap (cmap of the 2D plot) –
low_cmap (vmin cmap colorbar) –
high_cmap (vmax cmap colorbar) –

Return type:

Tuple[ndarray, ndarray, ndarray]

yarara_retropropagation_correction(correction_map='matching_smooth', sub_dico='matching_cosmics')#

Return type:: None

uncorrect_hole(conti, conti_ref, values_forbidden=[0, np.inf])#

Return type:: ndarray

yarara_telluric(sub_dico='matching_anchors', suppress_broad=True, delta_window=5, telluric_tag='telluric', weighted=False, reference=True, ratio=False, normalisation='slope', ccf_oversampling=3)#

Plot all the RASSINE spectra in the same plot

Parameters:

mask_name –
The telluric tag used to find a mask to cross correlate with the spectrum

Mask should be located in MASK_CCF and have the filename mask_telluric_TELLURICTAG.txt
sub_dico (The sub_dictionnary used to select the continuum) –
continuum (The continuum to select (either linear or cubic)) –
reference (True/False or 'norm', True use the matching anchors of reference, False use the continuum of each spectrum, norm use the continuum normalised spectrum (not )) –
display_ccf (display all the ccf) –
normalisation ('left' or 'slope'. if left normalise the CCF by the most left value, otherwise fit a line between the two highest point) –
planet (True/False to use the flux containing the injected planet or not) –

Return type:

None

yarara_correct_telluric_proxy(sub_dico='matching_fourier', sub_dico_output='telluric', wave_min=5700.0, wave_max=5900.0, reference='master', smooth_corr=1, proxies_corr=['h2o_depth', 'h2o_fwhm'], proxies_detrending_=None, wave_min_correction_=4400.0, wave_max_correction_=None, min_r_corr_=0.40, sigma_ext=2)#

Display the time-series spectra with proxies and its correlation

Parameters:

sub_dico (The sub_dictionnary used to select the continuum) –
continuum (The continuum to select (either linear or cubic)) –
wave_min (Minimum x axis limit) –
wave_max (Maximum x axis limit) –
zoom (int-type, to improve the resolution of the 2D plot) –
int-type (smooth_map =) –
convolution (smooth the 2D plot by gaussian 2D) –
reference ('median', 'snr' or 'master' to select the reference normalised spectrum usedin the difference) –
proxy1_corr (keyword of the first proxies from RASSINE dictionnary to use in the correlation) –
proxy1_detrending (Degree of the polynomial fit to detrend the proxy) –
proxy2_corr (keyword of the second proxies from RASSINE dictionnary to use in the correlation) –
proxy2_detrending (Degree of the polynomial fit to detrend the proxy) –
cmap (cmap of the 2D plot) –
min_wave_correction (wavelength limit above which to correct) –
min_r_corr (minimum correlation coefficient of one of the two proxies to consider a line as telluric) –
dwin (window correction increase by dwin to slightly correct above around the peak of correlation) –
positive_coeff (The correction can only be absorption line profile moving and no positive) –

Return type:

None

yarara_correct_telluric_gradient(sub_dico_detection='matching_fourier', sub_dico_correction='matching_oxygen', wave_min_train=4200.0, wave_max_train=5000.0, wave_min_correction=4400, wave_max_correction=6600, smooth_map=1, reference='master', inst_resolution=110000, equal_weight=True, nb_pca_comp=20, nb_pca_comp_kept=None, nb_pca_max_kept=5, calib_std=1e-3)#

Display the time-series spectra with proxies and its correlation

Parameters:

sub_dico (The sub_dictionnary used to select the continuum) –
continuum (The continuum to select (either linear or cubic)) –
wave_min (Minimum x axis limit) –
wave_max (Maximum x axis limit) –
int-type (smooth_map =) –
convolution (smooth the 2D plot by gaussian 2D) –
cmap (cmap of the 2D plot) –
low_cmap (vmin cmap colorbar) –
high_cmap (vmax cmap colorbar) –

Return type:

None

yarara_correct_oxygen(sub_dico='matching_telluric', reference='master', wave_min=5760.0, wave_max=5850.0, oxygene_bands=[[5787.0, 5835.0], [6275.0, 6340.0], [6800.0, 6950.0]])#

Display the time-series spectra with proxies and its correlation

Parameters:

sub_dico (The sub_dictionnary used to select the continuum) –
wave_min (Minimum x axis limit) –
wave_max (Maximum x axis limit) –
int-type (smooth_map =) –
convolution (smooth the 2D plot by gaussian 2D) –

Return type:

None

yarara_cut_spectrum(wave_min=None, wave_max=None)#

Cut the spectrum time-series borders to reach the specified wavelength limits (included)

There is no way to cancel this step ! Use it wisely.

Return type:: None

yarara_add_map(flux_init, map_name, correction_factor=False)#

yarara_substract_map(flux_init, map_name, correction_factor=False)#

yarara_map_all(wave_min=None, wave_max=None, index='index', reference='median')#

yarara_median_master(*, sub_dico='matching_diff', method='mean', suppress_telluric=True, shift_spectrum=False, telluric_tresh=0.001, wave_min=5750.0, wave_max=5900.0, jdb_range=[-100000, 100000, 1])#

Produce a median master by masking region of the spectrum

Parameters:

sub_dico (The sub_dictionnary used to select the continuum) –
telluric_tresh (Treshold used to cover the position of the contaminated wavelength) –
wave_min (The minimum xlim axis) –
wave_max (The maximum xlim axis) –

Return type:

None

yarara_non_zero_flux(spectrum=None, min_value=None)#

Return type:: Optional[ndarray]

yarara_poissonian_noise(noise_wanted=1 / 100, wave_ref=None, flat_snr=True, seed=9)#

Return type:: Tuple[ndarray, ndarray]

__init__(directory, starname, instrument, simbad_folder, mask_ccf_folder, material_folder)[source]#

Creates a spec_time_series instance

Params:: directory: Directory containing the RASSINE reduced data include the ending WORKSPACE/ starname: Name of the star instrument: Name of the instrument (> 5 letters possible) simbad_folder: Path to the SIMBAD folder mask_ccf_folder: Path to the mask_ccf folder material_folder: Path to the material folder

directory: str#: Directory containing the RASSINE reduced data include the ending WORKSPACE/

starname: str#: Name of the star

dir_root: str#: Directory containing the data under processing, parent of the WORKSPACE/ folder

simbad_folder: Path#: Path to the SIMBAD database

mask_ccf_folder: Path#: Path to the MASK_CCF folder

material_folder: Path#: Path to the Material folder

instrument: str#: Instrument used for the measurements

planet: bool#: If a planet has been injected

dico_tree: DataFrame#: Table of relations between outputs produced at different stages of the pipeline

material: DataFrame#: Table with elements having a spectral wavelength dimension

star_info: StarInfo#: Information about the star

info_reduction_ut: float#: If info_reduction has been loaded, modification time of the loaded file

fwhm: float#: Full width half maximum of the CCF

yarara

spec_time_series

Contents

spec_time_series#