The Code (API)

S1_detector_processing

S1_detector_processing.ramp_fitting

class eureka.S1_detector_processing.ramp_fitting.Eureka_RampFitStep(name=None, parent=None, config_file=None, _validate_kwds=True, **kws)[source]

Bases: JwstStep

This step is an alternative to the pipeline rampfitstep to determine the count rate for each pixel.

Attributes

class_alias
correction_pars
input_dir
log_records: Retrieve logs from the most recent run of this step.
make_output_path: Return function that creates the output path
name_format

Methods

`__call__`(*args)	Run handles the generic setup and teardown that happens with the running of each step.
`build_config`(input, **kwargs)	Build the ConfigObj to initialize a Step
`call`(args, *kwargs)	Creates and runs a new instance of the class.
`closeout`([to_close, to_del])	Close out step processing
`default_output_file`([input_file])	Create a default filename based on the input name
`default_suffix`()	Return a default suffix based on the step
`export_config`(filename[, include_metadata])	Export this step's parameters to an ASDF config file.
`finalize_config`(config[, name, config_file, ...])	Load default config, merge with config_file if present, then validate.
`finalize_result`(result, reference_files_used)	Hook that allows subclasses to set mission-specific metadata on each step result before that result is saved.
`from_cmdline`(args)	Create a step from a configuration file.
`from_config_file`(config_file[, parent, name])	Create a step from a configuration file.
`from_config_section`(config[, parent, name, ...])	Create a step from a configuration file fragment.
`get_config_from_reference`(dataset[, ...])	Retrieve step parameters from reference database
`get_config_reftype`()	Get the CRDS reftype for this step's config reference.
`get_pars`([full_spec])	Retrieve the configuration parameters of a step
`get_ref_override`(reference_file_type)	Determine and return any override for reference_file_type.
`get_reference_file`(input_file, ...)	Get a reference file from CRDS.
`load_as_level2_asn`(obj)	Load object as an association
`load_as_level3_asn`(obj)	Load object as an association
`make_input_path`(file_path)	Create an input path for a given file path
`open_model`(init, **kwargs)	Open a datamodel
`prefetch`(*args)	Prefetch reference files, nominally called when self.prefetch_references is True.
`process`(input)	Process a Stage 0 _uncal.fits file to Stage 1 _rate.fits and *_rateints.fits files.
`record_step_status`(datamodel, cal_step[, ...])	Record whether or not a step completed in meta.cal_step
`reference_uri_to_cache_path`(reference_uri, ...)	Convert an abstract CRDS reference URI to an absolute file path in the CRDS cache.
`remove_suffix`(name)	Remove a known Step filename suffix from a filename (if present).
`resolve_file_name`(file_name)	Resolve a file name expressed relative to this Step's configuration file.
`run`(*args)	Run handles the generic setup and teardown that happens with the running of each step.
`save_model`(model[, suffix, idx, ...])	Saves the given model using the step/pipeline's naming scheme
`search_attr`(attribute[, default, parent_first])	Return first non-None attribute in step heirarchy
`set_primary_input`(obj[, exclusive])	Sets the name of the master input file and input directory.
`update_pars`(parameters)	Update step parameters

load_spec_file
merge_config
print_configspec

algorithm = 'differenced'

maximum_cores = 1

process(input)[source]

Process a Stage 0 *_uncal.fits file to Stage 1 *_rate.fits and *_rateints.fits files.

Steps taken to perform this processing can follow the default JWST pipeline, or alternative methods.

Parameters

inputstr, tuple, ~astropy.io.fits.HDUList, ndarray, dict, None

None: Create a default data model with no shape.
tuple: Shape of the data array. Initialize with empty data array with shape specified by the.
file path: Initialize from the given file (FITS or ASDF)
readable file object: Initialize from the given file object
~astropy.io.fits.HDUList: Initialize from the given ~astropy.io.fits.HDUList.
A numpy array: Used to initialize the data array

Returns

out_modeljwst.datamodels.ImageModel: The output ImageModel to be returned from the ramp fit step.
int_modeljwst.datamodels.CubeModel: The output CubeModel to be returned from the ramp fit step.

Notes

History:

October 2021 Aarynn Carter and Eva-Maria Ahrer
Initial version
February 2022 Aarynn Carter and Eva-Maria Ahrer
Updated for JWST version 1.3.3, code restructure

reference_file_types = ['readnoise', 'gain']

spec = "\n int_name = string(default='')\n save_opt = boolean(default=False) # Save optional output\n opt_name = string(default='')\n maximum_cores = option('none', 'quarter', 'half', 'all', default='none') # max number of processes to create\n "

weighting = 'optimal'

S1_detector_processing.s1_process

class eureka.S1_detector_processing.s1_process.EurekaS1Pipeline(*args, **kwargs)[source]

Bases: Detector1Pipeline

A wrapper class for the jwst.pipeline.calwebb_detector1.Detector1Pipeline

This wrapper class allows non-standard changes to Stage 1 for Eureka!.

Notes

History:

October 2021 Aarynn Carter / Eva-Maria Ahrer
Initial version
February 2022 Aarynn Carter / Eva-Maria Ahrer
Updated for JWST version 1.3.3, code restructure

Attributes

correction_pars
input_dir
log_records: Retrieve logs from the most recent run of this step.
make_output_path: Return function that creates the output path
name_format
reference_file_types: Collect the list of all reftypes for child Steps that are not skipped.

Methods

`__call__`(*args)	Run handles the generic setup and teardown that happens with the running of each step.
`build_config`(input, **kwargs)	Build the ConfigObj to initialize a Step
`call`(args, *kwargs)	Creates and runs a new instance of the class.
`closeout`([to_close, to_del])	Close out step processing
`default_output_file`([input_file])	Create a default filename based on the input name
`default_suffix`()	Return a default suffix based on the step
`export_config`(filename[, include_metadata])	Export this step's parameters to an ASDF config file.
`finalize_config`(config[, name, config_file, ...])	Load default config, merge with config_file if present, then validate.
`finalize_result`(result, reference_files_used)	Hook that allows subclasses to set mission-specific metadata on each step result before that result is saved.
`from_cmdline`(args)	Create a step from a configuration file.
`from_config_file`(config_file[, parent, name])	Create a step from a configuration file.
`from_config_section`(config[, parent, name, ...])	Create a step from a configuration file fragment.
`get_config_from_reference`(dataset[, ...])	Retrieve step parameters from reference database
`get_config_reftype`()	Get the CRDS reftype for this step's config reference.
`get_pars`([full_spec])	Retrieve the configuration parameters of a pipeline
`get_ref_override`(reference_file_type)	Return any override for reference_file_type for any of the steps in Pipeline self.
`get_reference_file`(input_file, ...)	Get a reference file from CRDS.
`load_as_level2_asn`(obj)	Load object as an association
`load_as_level3_asn`(obj)	Load object as an association
`make_input_path`(file_path)	Create an input path for a given file path
`merge_pipeline_config`(refcfg, ref_file)	Merge the config parameters from a pipeline config reference file into the config obtained from each step
`open_model`(init, **kwargs)	Open a datamodel
`prefetch`(*args)	Prefetch reference files, nominally called when self.prefetch_references is True.
`process`(input)	This is where real work happens.
`record_step_status`(datamodel, cal_step[, ...])	Record whether or not a step completed in meta.cal_step
`reference_uri_to_cache_path`(reference_uri, ...)	Convert an abstract CRDS reference URI to an absolute file path in the CRDS cache.
`remove_suffix`(name)	Remove a known Step filename suffix from a filename (if present).
`resolve_file_name`(file_name)	Resolve a file name expressed relative to this Step's configuration file.
`run`(*args)	Run handles the generic setup and teardown that happens with the running of each step.
`run_eurekaS1`(filename, meta, log)	Reduces uncal files from STScI into rateints files.
`save_model`(model[, suffix, idx, ...])	Saves the given model using the step/pipeline's naming scheme
`search_attr`(attribute[, default, parent_first])	Return first non-None attribute in step heirarchy
`set_primary_input`(obj[, exclusive])	Sets the name of the master input file and input directory.
`update_pars`(parameters)	Update step parameters

load_spec_file
merge_config
print_configspec
set_input_filename
setup_output

run_eurekaS1(filename, meta, log)[source]

Reduces uncal files from STScI into rateints files.

Parameters

filenamestr: A string pointing to the uncal file to be operated on.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The open log in which notes from this step can be added.

Notes

History:

October 2021 Aarynn Carter / Eva-Maria Ahrer
Initial version
February 2022 Aarynn Carter / Eva-Maria Ahrer
Updated for JWST version 1.3.3, code restructure

eureka.S1_detector_processing.s1_process.rampfitJWST(eventlabel, ecf_path=None)[source]

Process a Stage 0, _uncal.fits file to Stage 1 _rate.fits and _rateints.fits files.

Steps taken to perform this processing can follow the default JWST pipeline, or alternative methods.

Parameters

eventlabelstr: The unique identifier for these data.
ecf_pathstr; optional: The absolute or relative path to where ecfs are stored. Defaults to None which resolves to ‘./’.

Returns

metaeureka.lib.readECF.MetaClass: The metadata object.

Notes

History:

October 2021 Taylor Bell
Code fragments
October 2021 Aarynn Carter and Eva-Maria Ahrer
Initial version
February 2022 Aarynn Carter and Eva-Maria Ahrer
Updated for JWST version 1.3.3, code restructure

S2_calibrations

S2_calibrations.s2_calibrate

class eureka.S2_calibrations.s2_calibrate.EurekaImage2Pipeline(*args, **kwargs)[source]

Bases: Image2Pipeline

A wrapper class for the jwst.pipeline.calwebb_image2.Image2Pipeline.

This wrapper class allows non-standard changes to Stage 2 for Eureka!.

Notes

History:

October 2021 Taylor Bell
Initial version

Attributes

correction_pars
input_dir
log_records: Retrieve logs from the most recent run of this step.
make_output_path: Return function that creates the output path
name_format
reference_file_types: Collect the list of all reftypes for child Steps that are not skipped.

Methods

`__call__`(*args)	Run handles the generic setup and teardown that happens with the running of each step.
`build_config`(input, **kwargs)	Build the ConfigObj to initialize a Step
`call`(args, *kwargs)	Creates and runs a new instance of the class.
`closeout`([to_close, to_del])	Close out step processing
`default_output_file`([input_file])	Create a default filename based on the input name
`default_suffix`()	Return a default suffix based on the step
`export_config`(filename[, include_metadata])	Export this step's parameters to an ASDF config file.
`finalize_config`(config[, name, config_file, ...])	Load default config, merge with config_file if present, then validate.
`finalize_result`(result, reference_files_used)	Hook that allows subclasses to set mission-specific metadata on each step result before that result is saved.
`from_cmdline`(args)	Create a step from a configuration file.
`from_config_file`(config_file[, parent, name])	Create a step from a configuration file.
`from_config_section`(config[, parent, name, ...])	Create a step from a configuration file fragment.
`get_config_from_reference`(dataset[, ...])	Retrieve step parameters from reference database
`get_config_reftype`()	Get the CRDS reftype for this step's config reference.
`get_pars`([full_spec])	Retrieve the configuration parameters of a pipeline
`get_ref_override`(reference_file_type)	Return any override for reference_file_type for any of the steps in Pipeline self.
`get_reference_file`(input_file, ...)	Get a reference file from CRDS.
`load_as_level2_asn`(obj)	Load object as an association
`load_as_level3_asn`(obj)	Load object as an association
`make_input_path`(file_path)	Create an input path for a given file path
`merge_pipeline_config`(refcfg, ref_file)	Merge the config parameters from a pipeline config reference file into the config obtained from each step
`open_model`(init, **kwargs)	Open a datamodel
`prefetch`(*args)	Prefetch reference files, nominally called when self.prefetch_references is True.
`process`(input)	This is where real work happens.
`process_exposure_product`(exp_product[, ...])	Process an exposure found in the association product
`record_step_status`(datamodel, cal_step[, ...])	Record whether or not a step completed in meta.cal_step
`reference_uri_to_cache_path`(reference_uri, ...)	Convert an abstract CRDS reference URI to an absolute file path in the CRDS cache.
`remove_suffix`(name)	Remove a known Step filename suffix from a filename (if present).
`resolve_file_name`(file_name)	Resolve a file name expressed relative to this Step's configuration file.
`run`(*args)	Run handles the generic setup and teardown that happens with the running of each step.
`run_eurekaS2`(filename, meta, log)	Reduces rateints image files ouput from Stage 1 of the JWST pipeline into calints.
`save_model`(model[, suffix, idx, ...])	Saves the given model using the step/pipeline's naming scheme
`search_attr`(attribute[, default, parent_first])	Return first non-None attribute in step heirarchy
`set_primary_input`(obj[, exclusive])	Sets the name of the master input file and input directory.
`update_pars`(parameters)	Update step parameters

load_spec_file
merge_config
print_configspec
set_input_filename

run_eurekaS2(filename, meta, log)[source]

Reduces rateints image files ouput from Stage 1 of the JWST pipeline into calints.

Parameters

filenamestr: A string pointing to the rateint or rateints file to process.
metaMetaClass: The metadata object.
loglogedit.Logedit: The open log in which notes from this step can be added.

Notes

History:

03 Nov 2021 Taylor Bell
Initial version

class eureka.S2_calibrations.s2_calibrate.EurekaSpec2Pipeline(*args, **kwargs)[source]

Bases: Spec2Pipeline

A wrapper class for the jwst.pipeline.calwebb_spec2.Spec2Pipeline.

This wrapper class allows non-standard changes to Stage 2 for Eureka!.

Notes

History:

October 2021 Taylor Bell
Initial version

Attributes

correction_pars
input_dir
log_records: Retrieve logs from the most recent run of this step.
make_output_path: Return function that creates the output path
name_format
reference_file_types: Collect the list of all reftypes for child Steps that are not skipped.

Methods

`__call__`(*args)	Run handles the generic setup and teardown that happens with the running of each step.
`build_config`(input, **kwargs)	Build the ConfigObj to initialize a Step
`call`(args, *kwargs)	Creates and runs a new instance of the class.
`closeout`([to_close, to_del])	Close out step processing
`default_output_file`([input_file])	Create a default filename based on the input name
`default_suffix`()	Return a default suffix based on the step
`export_config`(filename[, include_metadata])	Export this step's parameters to an ASDF config file.
`finalize_config`(config[, name, config_file, ...])	Load default config, merge with config_file if present, then validate.
`finalize_result`(result, reference_files_used)	Hook that allows subclasses to set mission-specific metadata on each step result before that result is saved.
`from_cmdline`(args)	Create a step from a configuration file.
`from_config_file`(config_file[, parent, name])	Create a step from a configuration file.
`from_config_section`(config[, parent, name, ...])	Create a step from a configuration file fragment.
`get_config_from_reference`(dataset[, ...])	Retrieve step parameters from reference database
`get_config_reftype`()	Get the CRDS reftype for this step's config reference.
`get_pars`([full_spec])	Retrieve the configuration parameters of a pipeline
`get_ref_override`(reference_file_type)	Return any override for reference_file_type for any of the steps in Pipeline self.
`get_reference_file`(input_file, ...)	Get a reference file from CRDS.
`load_as_level2_asn`(obj)	Load object as an association
`load_as_level3_asn`(obj)	Load object as an association
`make_input_path`(file_path)	Create an input path for a given file path
`merge_pipeline_config`(refcfg, ref_file)	Merge the config parameters from a pipeline config reference file into the config obtained from each step
`open_model`(init, **kwargs)	Open a datamodel
`prefetch`(*args)	Prefetch reference files, nominally called when self.prefetch_references is True.
`process`(data)	Entrypoint for this pipeline
`process_exposure_product`(exp_product[, ...])	Process an exposure found in the association product
`record_step_status`(datamodel, cal_step[, ...])	Record whether or not a step completed in meta.cal_step
`reference_uri_to_cache_path`(reference_uri, ...)	Convert an abstract CRDS reference URI to an absolute file path in the CRDS cache.
`remove_suffix`(name)	Remove a known Step filename suffix from a filename (if present).
`resolve_file_name`(file_name)	Resolve a file name expressed relative to this Step's configuration file.
`run`(*args)	Run handles the generic setup and teardown that happens with the running of each step.
`run_eurekaS2`(filename, meta, log)	Reduces rateints spectrum files ouput from Stage 1 of the JWST pipeline into calints and x1dints.
`save_model`(model[, suffix, idx, ...])	Saves the given model using the step/pipeline's naming scheme
`search_attr`(attribute[, default, parent_first])	Return first non-None attribute in step heirarchy
`set_primary_input`(obj[, exclusive])	Sets the name of the master input file and input directory.
`update_pars`(parameters)	Update step parameters

load_spec_file
merge_config
print_configspec
set_input_filename

run_eurekaS2(filename, meta, log)[source]

Reduces rateints spectrum files ouput from Stage 1 of the JWST pipeline into calints and x1dints.

Parameters

filenamestr: A string pointing to the rateint or rateints file to process.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The open log in which notes from this step can be added.

Notes

History:

June 2021 Eva-Maria Ahrer and Aarynn Carter
Code fragments written
October 2021 Taylor Bell
Significantly overhauled code formatting
03 Nov 2021 Taylor Bell
Fragmented code to allow reuse of code between spectral and image analysis.

eureka.S2_calibrations.s2_calibrate.calibrateJWST(eventlabel, ecf_path=None, s1_meta=None)[source]

Reduces rateints spectrum or image files ouput from Stage 1 of the JWST pipeline into calints and x1dints.

This function does the preparation for running the STScI’s JWST pipeline and decides whether to run the Spec2Pipeline or Image2Pipeline.

Parameters

eventlabelstr: Unique label for this dataset.
ecf_pathstr; optional: The absolute or relative path to where ecfs are stored. Defaults to None which resolves to ‘./’.
s1_metaeureka.lib.readECF.MetaClass; optional: The metadata object from Eureka!’s S1 step (if running S1 and S2 sequentially). Defaults to None.

Returns

metaeureka.lib.readECF.MetaClass: The metadata object.

Notes

History:

03 Nov 2021 Taylor Bell
Initial version

S3_data_reduction

S3_data_reduction.background

eureka.S3_data_reduction.background.BGsubtraction(data, meta, log, m)[source]

Does background subtraction using inst.fit_bg & background.fitbg

Parameters

dataXarray Dataset: Dataset object containing data, uncertainty, and variance arrays in units of MJy/sr or electrons.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The open log in which notes from this step can be added.
mint: The current file/batch number.

Returns

dataXarray Dataset: Dataset object containing background subtracted data.

Notes

History:

Dec 10, 2021 Taylor Bell
Edited to pass the full DataClass object into inst.fit_bg
Apr 20, 2022 Kevin Stevenson
Convert to using Xarray Dataset

eureka.S3_data_reduction.background.fitbg(dataim, meta, mask, x1, x2, deg=1, threshold=5, isrotate=False, isplots=0)[source]

Fit sky background with out-of-spectra data.

Parameters

dataimndarray: The data array.
metaeureka.lib.readECF.MetaClass: The metadata object.
maskndarray: A mask array.
x1ndarray
x2ndarray
degint; optional: Polynomial order for column-by-column background subtraction Default is 1.
thresholdint; optional: Sigma threshold for outlier rejection during background subtraction. Defaullt is 5.
isrotatebool; optional: Default is False.
isplotsint; optional: The amount of plots saved; set in ecf. Default is 0.

Notes

History:

May 2013
Removed [::-1] for LDSS3
Feb 2014
Modified x1 and x2 to allow for arrays

eureka.S3_data_reduction.background.fitbg2(dataim, meta, mask, bgmask, deg=1, threshold=5, isrotate=False, isplots=0)[source]

Fit sky background with out-of-spectra data.

fitbg2 uses bgmask, a mask for the background region which enables fitting more complex background regions than simply above or below a given distance from the trace. This will help mask the 2nd and 3rd orders of NIRISS.

Parameters

dataimndarray: The data array.
metaeureka.lib.readECF.MetaClass: The metadata object.
maskndarray: A mask array.
bgmaskndarray: A background mask array.
degint; optional: Polynomial order for column-by-column background subtraction. Default is 1.
thresholdint; optional: Sigma threshold for outlier rejection during background subtraction. Default is 5.
isrotatebool; optional: Default is False.
isplotsint; optional: The amount of plots saved; set in ecf. Default is 0.

Notes

History:

September 2016 Kevin Stevenson
Initial version

eureka.S3_data_reduction.background.fitbg3(data, order_mask, readnoise=11, sigclip=[4, 2, 3], isplots=0)[source]

Fit sky background with out-of-spectra data. Optimized to remove the 1/f noise in the NIRISS spectra (works in the y-direction).

Parameters

isplotsbool; optional: Plots intermediate steps for the background fitting routine. Default is False.

Returns

dataobject: data object now contains new attribute bkg_removed.

S3_data_reduction.bright2flux

eureka.S3_data_reduction.bright2flux.bright2dn(data, meta, mjy=False)[source]

This function converts the data, uncertainty, and variance arrays from brightness units (MJy/sr) or (MJy) to raw units (DN).

Parameters

dataXarray Dataset: Dataset object containing data, uncertainty, and variance arrays in units of MJy/sr.
metaeureka.lib.readECF.MetaClass: The metadata object.

Returns

dataXarray Dataset: Dataset object containing data, uncertainty, and variance arrays in units of DN.

Notes

The photometry files can be downloaded from CRDS (https://jwst-crds.stsci.edu/browse_db/)

History:

2021-05-28 kbs
Initial version
2021-07-21 sz
Added functionality for MIRI
Apr 20, 2022 Kevin Stevenson
Convert to using Xarray Dataset

eureka.S3_data_reduction.bright2flux.bright2flux(data, pixel_area)[source]

This function converts the data and uncertainty arrays from brightness units (MJy/sr) to flux units (Jy/pix).

Parameters

dataXarray Dataset: Dataset object containing data, uncertainty, and variance arrays in units of MJy/sr.
pixel_areandarray: Pixel area (arcsec/pix)

Returns

dataXarray Dataset: Dataset object containing data, uncertainty, and variance arrays in units of Jy/pix.

Notes

The input arrays Data and Uncd are changed in place.

History:

2005-06-20 Statia Luszcz, Cornell (shl35@cornell.edu).
2005-10-13 jh
Renamed, modified doc, removed posmed, fixed nimpos default bug (was float rather than int).
2005-10-28 jh
Updated header to give units being converted from/to, made srperas value a calculation rather than a constant, added Allen reference.
2005-11-24 jh
Eliminated NIMPOS.
2008-06-28 jh
Allow npos=1 case.
2010-01-29 patricio (pcubillos@fulbrightmail.org)
Converted to python.
2010-11-01 patricio
Documented, and incorporated scipy.constants.
2021-05-28 kbs
Updated for JWST
2021-12-09 TJB
Updated to account for the new DataClass object
Apr 20, 2022 Kevin Stevenson
Convert to using Xarray Dataset

eureka.S3_data_reduction.bright2flux.convert_to_e(data, meta, log)[source]

This function converts the data object to electrons from MJy/sr or DN/s.

Parameters

dataXarray Dataset: Dataset object containing data, uncertainty, and variance arrays in units of MJy/sr or DN/s.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The open log in which notes from this step can be added.

Returns

dataXarray Dataset: Dataset object containing data, uncertainty, and variance arrays in units of electrons.
metaeureka.lib.readECF.MetaClass: The metadata object.

eureka.S3_data_reduction.bright2flux.dn2electrons(data, meta)[source]

This function converts the data, uncertainty, and variance arrays from raw units (DN) to electrons.

Parameters

dataXarray Dataset: Dataset object containing data, uncertainty, and variance arrays in units of DN.
metaeureka.lib.readECF.MetaClass: The metadata object.

Returns

dataXarray Dataset: Dataset object containing data, uncertainty, and variance arrays in units of electrons.

Notes

The gain files can be downloaded from CRDS (https://jwst-crds.stsci.edu/browse_db/)

History:

Jun 2021 Kevin Stevenson
Initial version
Jul 2021
Added gainfile rotation
Apr 20, 2022 Kevin Stevenson
Convert to using Xarray Dataset

eureka.S3_data_reduction.bright2flux.rate2count(data)[source]

This function converts the data, uncertainty, and variance arrays from rate units (#/s) to counts (#).

Parameters

dataXarray Dataset: Dataset object containing data, uncertainty, and variance arrays in rate units (#/s).

Returns

dataXarray Dataset: Dataset object containing data, uncertainty, and variance arrays in count units (#).

Notes

History:

Mar 7, 2022 Taylor J Bell
Initial version
Apr 20, 2022 Kevin Stevenson
Convert to using Xarray Dataset

eureka.S3_data_reduction.bright2flux.retrieve_ancil(fitsname)[source]

Use crds package to find/download the needed ancilliary files.

This code requires that the CRDS_PATH and CRDS_SERVER_URL environment variables be set in your .bashrc file (or equivalent, e.g. .bash_profile or .zshrc)

Parameters

fitsnamestr: The filename of the file currently being analyzed.

Returns

phot_filenamestr: The full path to the photom calibration file.
gain_filenamestr: The full path to the gain calibration file.

Notes

History:

2022-03-04 Taylor J Bell
Initial code version.
2022-03-28 Taylor J Bell
Removed jwst dependency, using crds package now instead.

S3_data_reduction.hst_scan

eureka.S3_data_reduction.hst_scan.calcDrift2D(im1, im2, n)[source]

Calculates 2D drift of im2 with respect to im1 for diagnostic use, to align the images, and/or for decorrelation.

Parameters

im1ndarray (2D): The reference image.
im2ndarray (2D): The current image.
nint: The current integration number.

Returns

drift2Dlist: The x and y offset of im2 with respect to im1.
nint: The current integration number.

Raises

ModuleNotFoundError: image_registration wasn’t installed with Eureka.

eureka.S3_data_reduction.hst_scan.calcTrace(x, centroid, grism)[source]

Calculates the WFC3 trace given the position of the direct image in physical pixels.

Parameters

xndarray: Physical pixel values along dispersion direction over which the trace is calculated
centroidlist: [y,x] pair describing the centroid of the direct image
grismstr: The grism being used.

Returns

yndarray: Computed trace.

Notes

History:

LK
Initial version
November 2021, Kevin Stevenson
Modified

eureka.S3_data_reduction.hst_scan.calibrateLambda(x, centroid, grism)[source]

Calculates the wavelength solution for WFC3 observations.

Parameters

xndarray: Physical pixel values along dispersion direction over which the trace is calculated
centroidlist: [y,x] pair describing the centroid of the direct image
grismstr: The grism being used.

Returns

yndarray: Computed wavelength values

Notes

History:

LK
Initial version
November 2021, Kevin Stevenson
Modified

eureka.S3_data_reduction.hst_scan.groupFrames(dates)[source]

Group frames by HST orbit and batch number.

Parameters

datesndarray (1D): Time in days

Returns

framenumndarray (1D): The frame numbers.
batchnumndarray (1D): The batch numbers.
orbitnumndarray (1D): The orbit numbers.

eureka.S3_data_reduction.hst_scan.imageCentroid(filenames, guess, trim, ny, CRPIX1, CRPIX2, POSTARG1, POSTARG2, meta, log)[source]

Calculate centroid for a list of direct images from HST.

Parameters

filenameslist: List of direct image filenames
guessarray_like: The initial guess of the position of the star. Has the form (x, y) of the guess center.
trimint: If trim!=0, trims the image in a box of 2*trim pixels around the guess center. Must be !=0 for ‘col’ method.
nyint: The value of NAXIS2
CRPIX1float: The value of CRPIX1 in the main FITS header
CRPIX2float: The value of CRPIX2 in the main FITS header
POSTARG1float: The value of POSTARG1 in the science FITS header
POSTARG2float: The value of POSTARG2 in the science FITS header
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The current log.

Returns

centerslist: Centroids

Notes

History:

November 2013, Kevin Stevenson
Initial version
March 2016, Kevin Stevenson
Added IRSUB256
December 8, 2021, Taylor J Bell
Updated for Eureka

eureka.S3_data_reduction.hst_scan.makeBasicFlats(flatfile, xwindow, ywindow, flatoffset, ny, nx, sigma=5, isplots=0)[source]

Makes master flatfield image (with no wavelength correction) and new mask for WFC3 data.

Parameters

flatfilelist: List of files containing flatfiles images
xwindowndarray: Array containing image limits in wavelength direction
ywindowndarray: Array containing image limits in spatial direction
n_specint: Number of spectra
sigmafloat: Sigma rejection level

Returns

flat_masterlist: Single master flatfield image
mask_masterlist: Single bad-pixel mask image

Notes

History:

November 2012, Kevin Stevenson
Initial version.
February 2018, Kevin Stevenson
Removed wavelength dependence.

eureka.S3_data_reduction.hst_scan.makeflats(flatfile, wave, xwindow, ywindow, flatoffset, n_spec, ny, nx, sigma=5, isplots=0)[source]

Makes master flatfield image and new mask for WFC3 data.

Parameters

flatfilelist: List of files containing flatfiles images.
wavendarray: Wavelengths.
xwindowlist: Array containing image limits in wavelength direction.
ywindowlist: Array containing image limits in spatial direction.
n_specint: Number of spectra.
sigmafloat: Sigma rejection level.

Returns

flat_masterlist: Single master flatfield image.
mask_masterlist: Single bad-pixel mask image.

Notes

History:

November 2012, Kevin Stevenson
Initial version.

S3_data_reduction.miri

eureka.S3_data_reduction.miri.cut_aperture(data, meta, log)[source]

Select the aperture region out of each trimmed image.

Uses the code written for NIRCam which works for MIRI as long as the MIRI data gets rotated.

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The current log.

Returns

apdatandarray: The flux values over the aperture region.
aperrndarray: The noise values over the aperture region.
apmaskndarray: The mask values over the aperture region.
apbgndarray: The background flux values over the aperture region.
apv0ndarray: The v0 values over the aperture region.

Notes

History:

2022-06-17, Taylor J Bell
Initial version based on the code in s3_reduce.py

eureka.S3_data_reduction.miri.fit_bg(dataim, datamask, n, meta, isplots=0)[source]

Fit for a non-uniform background.

Uses the code written for NIRCam which works for MIRI as long as the MIRI data gets rotated.

Parameters

dataimndarray (2D): The 2D image array.
datamaskndarray (2D): An array of which data should be masked.
nint: The current integration.
metaeureka.lib.readECF.MetaClass: The metadata object.
isplotsint; optional: The plotting verbosity, by default 0.

Returns

bgndarray (2D): The fitted background level.
maskndarray (2D): The updated mask after background subtraction.
nint: The current integration number.

eureka.S3_data_reduction.miri.flag_bg(data, meta, log)[source]

Outlier rejection of sky background along time axis.

Uses the code written for NIRCam which works for MIRI as long as the MIRI data gets rotated.

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The current log.

Returns

dataXarray Dataset: The updated Dataset object with outlier background pixels flagged.

eureka.S3_data_reduction.miri.read(filename, data, meta, log)[source]

Reads single FITS file from JWST’s MIRI instrument.

Parameters

filenamestr: Single filename to read.
dataXarray Dataset: The Dataset object in which the fits data will stored.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The current log.

Returns

dataXarray Dataset: The updated Dataset object with the fits data stored inside.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The current log.

Notes

History:

Nov 2012 Kevin Stevenson
Initial Version
May 2021 Kevin Stevenson
Updated for NIRCam
Jun 2021 Taylor Bell
Updated docs for MIRI
Jun 2021 Sebastian Zieba
Updated for MIRI
Apr 2022 Sebastian Zieba
Updated wavelength array
Apr 21, 2022 Kevin Stevenson
Convert to using Xarray Dataset

eureka.S3_data_reduction.miri.wave_MIRI_jwst(filename, meta, log)[source]

Compute wavelengths for simulated MIRI observations.

This code uses the jwst package to get the wavelength information out of the WCS.

Parameters

filenamestr: The filename of the file being read in.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The current log.

Returns

lam_x_fulllist: A list of the wavelengths

Notes

History:

August 2022 Taylor J Bell
Initial Version

S3_data_reduction.nircam

eureka.S3_data_reduction.nircam.cut_aperture(data, meta, log)[source]

Select the aperture region out of each trimmed image.

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The current log.

Returns

apdatandarray: The flux values over the aperture region.
aperrndarray: The noise values over the aperture region.
apmaskndarray: The mask values over the aperture region.
apbgndarray: The background flux values over the aperture region.
apv0ndarray: The v0 values over the aperture region.

Notes

History:

2022-06-17, Taylor J Bell
Initial version based on the code in s3_reduce.py

eureka.S3_data_reduction.nircam.do_oneoverf_corr(data, meta, i, star_pos_x, log)[source]

Correcting for 1/f noise in each amplifier region by doing a row-by-row subtraction while avoiding pixels close to the star.

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.
iint: The current integration.
star_pos_xint: The star position in columns (x dimension).
loglogedit.Logedit: The current log.

Returns

dataXarray Dataset: The updated Dataset object after the 1/f correction has been completed.

eureka.S3_data_reduction.nircam.fit_bg(dataim, datamask, n, meta, isplots=0)[source]

Fit for a non-uniform background.

Parameters

dataimndarray (2D): The 2D image array.
datamaskndarray (2D): An array of which data should be masked.
nint: The current integration.
metaeureka.lib.readECF.MetaClass: The metadata object.
isplotsint; optional: The plotting verbosity, by default 0.

Returns

bgndarray (2D): The fitted background level.
maskndarray (2D): The updated mask after background subtraction.
nint: The current integration number.

eureka.S3_data_reduction.nircam.flag_bg(data, meta, log)[source]

Outlier rejection of sky background along time axis.

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The current log.

Returns

dataXarray Dataset: The updated Dataset object with outlier background pixels flagged.

eureka.S3_data_reduction.nircam.flag_bg_phot(data, meta, log)[source]

Outlier rejection of segment along time axis adjusted for the photometry reduction routine.

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The current log.

Returns

dataXarray Dataset: The updated Dataset object with outlier background pixels flagged.

eureka.S3_data_reduction.nircam.read(filename, data, meta, log)[source]

Reads single FITS file from JWST’s NIRCam instrument.

Parameters

filenamestr: Single filename to read.
dataXarray Dataset: The Dataset object in which the fits data will stored.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The current log.

Returns

dataXarray Dataset: The updated Dataset object with the fits data stored inside.
metaeureka.lib.readECF.MetaClass: The updated metadata object.
loglogedit.Logedit: The current log.

Notes

History:

November 2012 Kevin Stevenson
Initial version
May 2021 KBS
Updated for NIRCam
July 2021
Moved bjdtdb into here
Apr 20, 2022 Kevin Stevenson
Convert to using Xarray Dataset

S3_data_reduction.niriss_profiles

A library of custom weighted profiles to fit to the NIRISS orders to complete the optimal extraction of the data.

eureka.S3_data_reduction.niriss_profiles.gaussian_1poly_piecewise(args, x)[source]

A piece-wise function consisting of 2 generalized normal distribution profiles connected with a 1D polynomial to mimic the bat-shaped profile of NIRISS.

Parameters

argsnp.ndarray: A list or array of parameters for the fits.
xnp.ndarray: X values to evaluate the shape over.

eureka.S3_data_reduction.niriss_profiles.gaussian_2poly_piecewise(args, x)[source]

A piece-wise function consisting of 2 generalized normal distribution profiles connected with a 2D polynomial to mimic the bat-shaped profile of NIRISS.

Parameters

argsnp.ndarray: A list or array of parameters for the fits.
xnp.ndarray: X values to evaluate the shape over.

eureka.S3_data_reduction.niriss_profiles.generalized_normal(x, mu, alpha, beta, scale)[source]

Generalized normal distribution.

Parameters

xnp.ndarray: X values to evaluate the distribution. over.
mufloat: Mean/center value of the distribution.
alphafloat: Sets the scale/standard deviation of the distribution.
betafloat: Sets the shape of the distribution. Beta > 2 becomes boxy. Beta < 2 becomes peaky. Beta = 2 is a normal Gaussian.
scalefloat: A value to scale the distribution by.

eureka.S3_data_reduction.niriss_profiles.moffat_1poly_piecewise(args, x)[source]

A piece-wise function consisting of 2 Moffat profiles connected with a 1D polynomial to mimic the bat-shaped profile of NIRISS.

Parameters

argsnp.ndarray: A list or array of parameters for the fits.
xnp.ndarray: X values to evaluate the shape over.

eureka.S3_data_reduction.niriss_profiles.moffat_2poly_piecewise(args, x)[source]

A piece-wise function consisting of 2 Moffat profiles connected with a 2D polynomial to mimic the bat-shaped profile of NIRISS.

Parameters

argsnp.ndarray: A list or array of parameters for the fits.
xnp.ndarray: X values to evaluate the shape over.

S3_data_reduction.niriss

eureka.S3_data_reduction.niriss.f277_mask(data, isplots=0)[source]

Marks the overlap region in the f277w filter image.

Parameters

dataobject
isplotsint; optional: Level of plots that should be created in the S3 stage. This is set in the .ecf control files. Default is 0. This stage will plot if isplots >= 5.

Returns

masknp.ndarray: 2D mask for the f277w filter.
midnp.ndarray: (x,y) anchors for where the overlap region is located.

eureka.S3_data_reduction.niriss.fit_bg(data, meta, n_iters=3, readnoise=11, sigclip=[4, 4, 4], isplots=0)[source]

Subtracts background from non-spectral regions.

Parameters

dataobject
metaobject
n_itersint; optional: The number of iterations to go over and remove cosmic rays. Default is 3.
readnoisefloat; optional: An estimation of the readnoise of the detector. Default is 5.
sigcliplist, array; optional: A list or array of len(n_iiters) corresponding to the sigma-level which should be clipped in the cosmic ray removal routine. Default is [4,2,3].
isplotsint; optional: The level of output plots to display. Default is 0 (no plots).

Returns

dataobject

eureka.S3_data_reduction.niriss.fit_orders(data, meta, which_table=2)[source]

Creates a 2D image optimized to fit the data. Currently runs with a Gaussian profile, but will look into other more realistic profiles at some point. This routine is a bit slow, but fortunately, you only need to run it once per observations.

Parameters

dataobject
metaobject
which_tableint; optional: Sets with table of initial y-positions for the orders to use. Default is 2.

Returns

metaobject: Adds two new attributes: order1_mask and order2_mask.

eureka.S3_data_reduction.niriss.fit_orders_fast(data, meta, which_table=2)[source]

A faster method to fit a 2D mask to the NIRISS data. Very similar to fit_orders, but works with scipy.optimize.leastsq.

Parameters

dataobject
metaobject
which_tableint; optional: Sets with table of initial y-positions for the orders to use. Default is 2.

Returns

metaobject

eureka.S3_data_reduction.niriss.image_filtering(img, radius=1, gf=4)[source]

Does some simple image processing to isolate where the spectra are located on the detector. This routine is optimized for NIRISS S2 processed data and the F277W filter.

Parameters

imgnp.ndarray: 2D image array.
radiusnp.float; optional: Default is 1.
gfnp.float; optional: The standard deviation by which to Gaussian smooth the image. Default is 4.

Returns

img_masknp.ndarray: A mask for the image that isolates where the spectral orders are.

eureka.S3_data_reduction.niriss.mask_method_one(data, meta, isplots=0, save=True)[source]

There are some hard-coded numbers in here right now. The idea is that once we know what the real data looks like, nobody will have to actually call this function and we’ll provide a CSV of a good initial guess for each order. This method uses some fun image processing to identify the boundaries of the orders and fits the edges of the first and second orders with a 4th degree polynomial.

Parameters

dataobject
metaobject
isplotsint; optional: Level of plots that should be created in the S3 stage. This is set in the .ecf control files. Default is 0. This stage will plot if isplots >= 5.
savebool; optional: An option to save the polynomial fits to a CSV. Default is True. Output table is saved under niriss_order_guesses.csv.

Returns

metaobject

eureka.S3_data_reduction.niriss.mask_method_two(data, meta, isplots=0, save=False)[source]

A second method to extract the masks for the first and second orders in NIRISS data. This method uses the vertical profile of a summed image to identify the borders of each order.

Parameters

dataobject
metaobject
isplotsint; optional: Level of plots that should be created in the S3 stage. This is set in the .ecf control files. Default is 0. This stage will plot if isplots >= 5.
savebool; optional: Has the option to save the initial guesses for the location of the NIRISS orders. This is set in the .ecf control files. Default is False.

Returns

metaobject

eureka.S3_data_reduction.niriss.read(filename, f277_filename, data, meta)[source]

Reads a single FITS file from JWST’s NIRISS instrument. This takes in the Stage 2 processed files.

Parameters

filenamestr: Single filename to read. Should be a .fits file.
dataobject: Data object in which the fits data will be stored.

Returns

dataobject: Data object now populated with all of the FITS file information.
metaastropy.table.Table: Metadata stored in the FITS file.

eureka.S3_data_reduction.niriss.simplify_niriss_img(data, meta, isplots=0)[source]

Creates an image to map out where the orders are in the NIRISS data.

Parameters

dataobject
metaobject
isplotsint; optional: Level of plots that should be created in the S3 stage. This is set in the .ecf control files. Default is 0.

Returns

gnp.ndarray: A 2D array that marks where the NIRISS first and second orders are.

eureka.S3_data_reduction.niriss.wave_NIRISS(wavefile, meta)[source]

Adds the 2D wavelength solutions to the meta object.

Parameters

wavefilestr: The name of the .FITS file with the wavelength solution.
metaobject

Returns

metaobject

S3_data_reduction.nirspec

eureka.S3_data_reduction.nirspec.cut_aperture(data, meta, log)[source]

Select the aperture region out of each trimmed image.

Uses the code written for NIRCam which works for NIRSpec.

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The current log.

Returns

apdatandarray: The flux values over the aperture region.
aperrndarray: The noise values over the aperture region.
apmaskndarray: The mask values over the aperture region.
apbgndarray: The background flux values over the aperture region.
apv0ndarray: The v0 values over the aperture region.

Notes

History:

2022-06-17, Taylor J Bell
Initial version based on the code in s3_reduce.py

eureka.S3_data_reduction.nirspec.fit_bg(dataim, datamask, n, meta, isplots=0)[source]

Fit for a non-uniform background.

Uses the code written for NIRCam which works for NIRSpec.

Parameters

dataimndarray (2D): The 2D image array.
datamaskndarray (2D): An array of which data should be masked.
nint: The current integration.
metaeureka.lib.readECF.MetaClass: The metadata object.
isplotsint; optional: The plotting verbosity, by default 0.

Returns

bgndarray (2D): The fitted background level.
maskndarray (2D): The updated mask after background subtraction.
nint: The current integration number.

eureka.S3_data_reduction.nirspec.flag_bg(data, meta, log)[source]

Outlier rejection of sky background along time axis.

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The current log.

Returns

dataXarray Dataset: The updated Dataset object with outlier background pixels flagged.

eureka.S3_data_reduction.nirspec.read(filename, data, meta, log)[source]

Reads single FITS file from JWST’s NIRCam instrument.

Parameters

filenamestr: Single filename to read.
dataXarray Dataset: The Dataset object in which the fits data will stored.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The current log.

Returns

dataXarray Dataset: The updated Dataset object with the fits data stored inside.
metaeureka.lib.readECF.MetaClass: The metadata object
loglogedit.Logedit: The current log.

Notes

History:

November 2012 Kevin Stevenson
Initial version
June 2021 Aarynn Carter/Eva-Maria Ahrer
Updated for NIRSpec
Apr 22, 2022 Kevin Stevenson
Convert to using Xarray Dataset

S3_data_reduction.optspex

eureka.S3_data_reduction.optspex.clean_median_flux(data, meta, log, m)[source]

Computes a median flux frame that is free of bad pixels.

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The current log.
mint: The file number.

Returns

dataXarray Dataset: The updated Dataset object.

Notes

History:

2022-08-03, KBS
Inital version

eureka.S3_data_reduction.optspex.optimize(meta, subdata, mask, bg, spectrum, Q, v0, p5thresh=10, p7thresh=10, fittype='smooth', window_len=21, deg=3, windowtype='hanning', n=0, m=0, meddata=None)[source]

Extract optimal spectrum with uncertainties for a single frame.

Parameters

metaeureka.lib.readECF.MetaClass: The metadata object.
subdatandarray: Background subtracted data.
maskndarray: Outlier mask.
bgndarray: Background array.
spectrumndarray: Standard spectrum.
Qfloat: The gain factor.
v0ndarray: Variance array for data.
p5threshfloat; optional: Sigma threshold for outlier rejection while constructing spatial profile. Defaults to 10.
p7threshfloat; optional: Sigma threshold for outlier rejection during optimal spectral extraction. Defaukts to 10.
fittypestr; optional: One of {‘smooth’, ‘meddata’, ‘wavelet2D’, ‘wavelet’, ‘gauss’, ‘poly’}. The type of profile fitting you want to do. Defaults to ‘smooth’.
window_lenint; optional: The dimension of the smoothing window. Defaults to 21.
degint; optional: Polynomial degree. Defaults to 3.
windowtypestr; optional: UNUSED. One of {‘flat’, ‘hanning’, ‘hamming’, ‘bartlett’, ‘blackman’}. The type of window. A flat window will produce a moving average smoothing. Defaults to ‘hanning’.
nint; optional: Integration number. Defaults to 0.
mint; optional: File number. Defaults to 0.
meddatandarray; optional: The median of all data frames. Defaults to None.

Returns

spectrumndarray: The optimally extracted spectrum.
specuncndarray: The standard deviation on the spectrum.
submaskndarray: The mask array.

eureka.S3_data_reduction.optspex.optimize_wrapper(data, meta, log, apdata, apmask, apbg, apv0, gain=1, windowtype='hanning', m=0)[source]

Extract optimal spectrum with uncertainties for many frames.

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The current log.
apdatandarray: Background subtracted data.
apmaskndarray: Outlier mask.
apbgndarray: Background array.
apv0ndarray: Variance array for data.
gainfloat: The gain factor. Defaults to 1 as the flux should already be in electrons.
windowtypestr; optional: UNUSED. One of {‘flat’, ‘hanning’, ‘hamming’, ‘bartlett’, ‘blackman’}. The type of window. A flat window will produce a moving average smoothing. Defaults to ‘hanning’.
mint; optional: File number. Defaults to 0.

Returns

dataXarray Dataset: The updated Dataset object.
metaeureka.lib.readECF.MetaClass: The updated metadata object.
loglogedit.Logedit: The updated log.

Notes

History:

2022-07-18, Taylor J Bell
Added optimize_wrapper to iterate over each frame.

eureka.S3_data_reduction.optspex.profile_gauss(subdata, mask, threshold=10, guess=None, isplots=0)[source]

Construct normalized spatial profile using a Gaussian smoothing function.

Parameters

subdatandarray: Background subtracted data.
maskndarray: Outlier mask.
thresholdfloat; optional: Sigma threshold for outlier rejection while constructing spatial profile. Defaults to 10.
guesslist; optional: UNUSED. The initial guess for the Gaussian parameters. Defaults to None.
isplotsint; optional: The plotting verbosity. Defaults to 0.

Returns

profilendarray: Fitted profile in the same shape as the input data array.

eureka.S3_data_reduction.optspex.profile_meddata(data, mask, meddata, threshold=10, isplots=0)[source]

Construct normalized spatial profile using median of all data frames.

Parameters

datandarray: Unused. Image data.
maskndarray: Unused. Outlier mask.
meddatandarray: The median of all data frames.
thresholdfloat; optional: Unused. Sigma threshold for outlier rejection while constructing spatial profile. Defaults to 10.
isplotsint; optional: Unused. The plotting verbosity. Defaults to 0.

Returns

profilendarray: Fitted profile in the same shape as the input data array.

eureka.S3_data_reduction.optspex.profile_poly(subdata, mask, deg=3, threshold=10, isplots=0)[source]

Construct normalized spatial profile using polynomial fits along the wavelength direction.

Parameters

subdatandarray: Background subtracted data.
maskndarray: Outlier mask.
degint; optional: Polynomial degree, defaults to 3.
thresholdfloat; optional: Sigma threshold for outlier rejection while constructing spatial profile, defaults to 10.
isplotsint; optional: The plotting verbosity. Defaults to 0.

Returns

profilendarray: Fitted profile in the same shape as the input data array.

eureka.S3_data_reduction.optspex.profile_smooth(subdata, mask, threshold=10, window_len=21, windowtype='hanning', isplots=0)[source]

Construct normalized spatial profile using a smoothing function.

Parameters

subdatandarray: Background subtracted data.
maskndarray: Outlier mask.
thresholdfloat; optional: Sigma threshold for outlier rejection while constructing spatial profile.
window_lenint; optional: The dimension of the smoothing window.
windowtypestr; optional: UNUSED. One of {‘flat’, ‘hanning’, ‘hamming’, ‘bartlett’, ‘blackman’}. The type of window. A flat window will produce a moving average smoothing. Defaults to ‘hanning’.
isplotsint; optional: The plotting verbosity. Defaults to 0.

Returns

profilendarray: Fitted profile in the same shape as the input data array.

eureka.S3_data_reduction.optspex.profile_wavelet(subdata, mask, wavelet, numlvls, isplots=0)[source]

This function performs 1D image denoising using BayesShrink soft thresholding.

Parameters

subdatandarray: Background subtracted data.
maskndarray: Outlier mask.
waveletWavelet object or name string: qWavelet to use
numlvlsint: Decomposition levels to consider (must be >= 0).
isplotsint; optional: The plotting verbosity. Defaults to 0.

Returns

profilendarray: Fitted profile in the same shape as the input data array.

References

Chang et al. “Adaptive Wavelet Thresholding for Image Denoising and Compression”, 2000

eureka.S3_data_reduction.optspex.profile_wavelet2D(subdata, mask, wavelet, numlvls, isplots=0)[source]

Construct normalized spatial profile using wavelets

This function performs 2D image denoising using BayesShrink soft thresholding.

Parameters

subdatandarray: Background subtracted data.
maskndarray: Outlier mask.
waveletWavelet object or name string: qWavelet to use
numlvlsint: Decomposition levels to consider (must be >= 0).
isplotsint; optional: The plotting verbosity. Defaults to 0.

Returns

profilendarray: Fitted profile in the same shape as the input data array.

References

Chang et al. “Adaptive Wavelet Thresholding for Image Denoising and Compression”, 2000

eureka.S3_data_reduction.optspex.standard_spectrum(data, apdata, aperr)[source]

Compute the standard box spectrum.

Parameters

dataXarray Dataset: The Dataset object.
apdatandarray: The pixel values in the aperture region.
aperrndarray: The noise values in the aperture region.

Returns

dataXarray Dataset: The updated Dataset object in which the spectrum data will stored.

S3_data_reduction.plots_s3

eureka.S3_data_reduction.plots_s3.add_colorbar(im, aspect=20, pad_fraction=0.5, **kwargs)[source]: Add a vertical color bar to an image plot. Taken from: https://stackoverflow.com/ questions/18195758/set-matplotlib-colorbar-size-to-match-graph

eureka.S3_data_reduction.plots_s3.curvature(meta, column_coms, smooth_coms, int_coms, m)[source]

Plot the measured, smoothed, and integer correction from the measured curvature. (Fig 3107)

Parameters

metaeureka.lib.readECF.MetaClass: The metadata object.
column_coms1D array: Measured center of mass (light) for each pixel column
smooth_coms1D array: Smoothed center of mass (light) for each pixel column
int_coms1D array: Integer-rounded center of mass (light) for each pixel column
mint: The file number.

Notes

History:

2022-07-31 KBS
Initial version

eureka.S3_data_reduction.plots_s3.drift_2D(data, meta)[source]

Plot the fitted 2D drift. (Fig 3106)

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.

eureka.S3_data_reduction.plots_s3.driftypos(data, meta)[source]

Plot the spatial jitter. (Fig 3104)

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.

Notes

History:

2022-07-11 Caroline Piaulet
First version of this function

eureka.S3_data_reduction.plots_s3.driftywidth(data, meta)[source]

Plot the spatial profile’s fitted Gaussian width. (Fig 3105)

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.

Notes

History:

2022-07-11 Caroline Piaulet
First version of this function

eureka.S3_data_reduction.plots_s3.image_and_background(data, meta, log, m)[source]

Make image+background plot. (Figs 3301)

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The current log.
mint: The file number.

eureka.S3_data_reduction.plots_s3.lc_nodriftcorr(meta, wave_1d, optspec, optmask=None)[source]

Plot a 2D light curve without drift correction. (Fig 3101+3102)

Fig 3101 uses a linear wavelength x-axis, while Fig 3102 uses a linear detector pixel x-axis.

Parameters

metaeureka.lib.readECF.MetaClass: The metadata object.
wave_1dXarray Dataset: Wavelength array with trimmed edges depending on xwindow and ywindow which have been set in the S3 ecf
optspecXarray Dataset: The optimally extracted spectrum.
optmaskXarray Dataset; optional: A mask array to use if optspec is not a masked array. Defaults to None in which case only the invalid values of optspec will be masked.

eureka.S3_data_reduction.plots_s3.median_frame(data, meta, m)[source]

Plot the cleaned time-median frame. (Fig 3308)

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.
mint: The file number.

Notes

History:

2022-08-06 KBS
Initial version

eureka.S3_data_reduction.plots_s3.optimal_spectrum(data, meta, n, m)[source]

Make optimal spectrum plot. (Figs 3302)

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.
nint: The integration number.
mint: The file number.

eureka.S3_data_reduction.plots_s3.phot_2d_frame(data, meta, m, i)[source]

Plots the 2D frame together with the centroid position, the target aperture and the background annulus. (Fig 3306) If meta.isplots_S3 >= 5, this function will additionally create another figure - Fig 3504 - but it only includes the target area. (Fig 3306 and 3504)

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.
iint: The integration number.
mint: The file number.

Notes

History:

2022-08-02 Sebastian Zieba
Initial version

eureka.S3_data_reduction.plots_s3.phot_2d_frame_diff(data, meta)[source]

Plots the difference between to consecutive 2D frames. This might be helpful in order to investigate flux changes due to mirror tilts which have been observed during commissioning. (Fig 3505)

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.

Notes

History:

2022-08-02 Sebastian Zieba
Initial version

eureka.S3_data_reduction.plots_s3.phot_2d_frame_oneoverf(data, meta, m, i, flux_w_oneoverf)[source]

Plots the 2D frame with a low vmax so that the background is well visible. The top panel is before the 1/f correction, the lower panel shows the 2D frame after the 1/f correction. The typical “stripy” structure for each row should have been mitigated after the 1/f correction in Stage 3. (Fig 3307)

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.
iint: The integration number.
mint: The file number.
flux_w_oneoverf2D numpy array: The 2D frame before the 1/f correction

Notes

History:

2022-08-02 Sebastian Zieba
Initial version

eureka.S3_data_reduction.plots_s3.phot_bg(data, meta)[source]

Plots the background flux as determined by the photometry routine as a function of time. (Fig 3305)

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.

Notes

History:

2022-08-02 Sebastian Zieba
Initial version

eureka.S3_data_reduction.plots_s3.phot_centroid(data, meta)[source]

Plots the (x, y) centroids and (sx, sy) the Gaussian 1-sigma half-widths as a function of time. (Fig 3109)

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.

Notes

History:

2022-08-02 Sebastian Zieba
Initial version

eureka.S3_data_reduction.plots_s3.phot_centroid_fgc(img, x, y, sx, sy, i, m, meta)[source]

Plot of the gaussian fit to the centroid cutout. (Fig 3503)

Parameters

img2D numpy array: Cutout of the center of the target which is used to determine the centroid position.
xfloat: Centroid position in x direction.
yfloat: Centroid position in y direction.
sxfloat: Gaussian Sigma of Centroid position in x direction.
syfloat: Gaussian Sigma of Centroid position in y direction.
iint: The integration number.
mint: The file number.
metaeureka.lib.readECF.MetaClass: The metadata object.

Notes

History:

2022-08-02 Sebastian Zieba
Initial version

eureka.S3_data_reduction.plots_s3.phot_lc(data, meta)[source]

Plots the flux as determined by the photometry routine as a function of time. (Fig 3108)

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.

Notes

History:

2022-08-02 Sebastian Zieba
Initial version

eureka.S3_data_reduction.plots_s3.phot_npix(data, meta)[source]

Plots the number of pixels within the target aperture and within the background annulus as a function of time. (Fig 3502)

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.

Notes

History:

2022-08-02 Sebastian Zieba
Initial version

eureka.S3_data_reduction.plots_s3.profile(meta, profile, submask, n, m)[source]

Plot weighting profile from optimal spectral extraction routine. (Figs 3303)

Parameters

metaeureka.lib.readECF.MetaClass: The metadata object.
profilendarray: Fitted profile in the same shape as the data array.
submaskndarray: Outlier mask.
nint: The current integration number.
mint: The file number.

eureka.S3_data_reduction.plots_s3.residualBackground(data, meta, m, vmin=-200, vmax=1000)[source]

Plot the median, BG-subtracted frame to study the residual BG region and aperture/BG sizes. (Fig 3304)

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.
mint: The file number.
vminint; optional: Minimum value of colormap. Default is -200.
vmaxint; optional: Maximum value of colormap. Default is 1000.

Notes

History:

2022-07-29 KBS
Initial version

eureka.S3_data_reduction.plots_s3.source_position(meta, x_dim, pos_max, m, n, isgauss=False, x=None, y=None, popt=None, isFWM=False, y_pixels=None, sum_row=None, y_pos=None)[source]

Plot source position for MIRI data. (Figs 3103)

Parameters

metaeureka.lib.readECF.MetaClass: The metadata object.
x_dimint: The number of pixels in the y-direction in the image.
pos_maxfloat: The brightest row.
mint: The file number.
nint: The integration number.
isgaussbool; optional: Used a guassian centring method.
xtype; optional: Unused.
ytype; optional: Unused.
poptlist; optional: The fitted Gaussian terms.
isFWMbool; optional: Used a flux-weighted mean centring method.
y_pixels1darray; optional: The indices of the y-pixels.
sum_row1darray; optional: The sum over each row.
y_posfloat; optional: The FWM central position of the star.

Notes

History:

2021-07-14: Sebastian Zieba
Initial version.
Oct 15, 2021: Taylor Bell
Tidied up the code a bit to reduce repeated code.

eureka.S3_data_reduction.plots_s3.subdata(meta, i, n, m, subdata, submask, expected, loc)[source]

Show 1D view of profile for each column. (Figs 3501)

Parameters

metaeureka.lib.readECF.MetaClass: The metadata object.
iint: The column number.
nint: The current integration number.
mint: The file number.
subdatandarray: Background subtracted data.
submaskndarray: Outlier mask.
expectedndarray: Expected profile
locndarray: Location of worst outliers.

S3_data_reduction.s3_reduce

eureka.S3_data_reduction.s3_reduce.reduce(eventlabel, ecf_path=None, s2_meta=None)[source]

Reduces data images and calculates optimal spectra.

Parameters

eventlabelstr: The unique identifier for these data.
ecf_pathstr; optional: The absolute or relative path to where ecfs are stored. Defaults to None which resolves to ‘./’.
s2_metaeureka.lib.readECF.MetaClass; optional: The metadata object from Eureka!’s S2 step (if running S2 and S3 sequentially). Defaults to None.

Returns

metaeureka.lib.readECF.MetaClass: The metadata object with attributes added by S3.

Notes

History:

May 2021 Kevin Stevenson
Initial version
October 2021 Taylor Bell
Updated to allow for inputs from S2
July 2022 Caroline Piaulet
Now computing the y pos and width for each integration + stored in Spec and add diagnostics plots
July 2022 Sebastian Zieba
Added photometry S3

S3_data_reduction.sigrej

eureka.S3_data_reduction.sigrej.sigrej(data, sigma, mask=None, estsig=None, ival=False, axis=0, fmean=False, fstddev=False, fmedian=False, fmedstddev=False)[source]

This function flags outlying points in a data set using sigma rejection.

Parameters

datandarray: Array of points to apply sigma rejection to.
sigmandarray (1D): 1D array of sigma values for each iteration of sigma rejection. Number of elements determines number of iterations.
maskbyte array; optional: Same shape as Data, where 1 indicates the corresponding element in Data is good and 0 indicates it is bad. Only rejection of good-flagged data will be further considered. This input mask is NOT modified in the caller.
estsigndarray; optional: [nsig] array of estimated standard deviations to use instead of calculated ones in each iteration. This is useful in the case of small datasets with outliers, in which case the calculated standard deviation can be large if there is an outlier and small if there is not, leading to rejection of good elements in a clean dataset and acceptance of all elements in a dataset with one bad element. Set any element of estsig to a negative value to use the calculated standard deviation for that iteration.
ivalndarray (2D); optional: (returned) 2D array giving the median and standard deviation (with respect to the median) at each iteration.
axisint; optional: The axis along which to compute the mean/median.
fmeanndarray; optional: (returned) the mean of the accepted data.
fstddevndarray; optional: (returned) the standard deviation of the accepted data with respect to the mean.
fmedianndarray; optional: (returned) the median of the accepted data.
fmedstddevndarray; optional: (returned) the standard deviation of the accepted data with respect to the median.

Returns

rettuple: This function returns a mask of accepted values in the data. The mask is a byte array of the same shape as Data. In the mask, 1 indicates good data, 0 indicates an outlier in the corresponding location of Data. fmean, fstddev, fmedian, and fmedstddev will also be updated and returned if they were passed in. All of these will be packaged together into a tuple.

Notes

SIGREJ flags as outliers points a distance of sigma* the standard deviation from the median. Unless given as a positive value in ESTSIG, standard deviation is calculated with respect to the median, using MEDSTDDEV. For each successive iteration and value of sigma SIGREJ recalculates the median and standard deviation from the set of ‘good’ (not masked) points, and uses these new values in calculating further outliers. The final mask contains a value of 1 for every ‘inlier’ and 0 for every outlying data point.

History:

2005-01-18 statia Statia Luszcz, Cornell. (shl35@cornell.edu)
Initial version
2005-01-19 statia
Changed function to return mask, rather than a list of outlying and inlying points, added final statistics keywords
2005-01-20 jh Joe Harrington, Cornell, (jh@oobleck.astro.cornell.edu)
Header update. Added example.
2005-05-26 jh
Fixed header typo.
2006-01-10 jh
Moved definition, added test to see if all elements rejected before last iteration (e.g., dataset is all NaN). Added input mask, estsig.
2010-11-01 patricio (pcubillos@fulbrightmail.org)
Converted to python.

Examples

Define the N-element vector of sample data.

>>> print(mean(x), stddev(x), median(x), medstddev(x))
1438.47      5311.67      67.0000      5498.10
>>> sr.sigrej(x, [9,3]), ival=ival, fmean=fmean, fmedian=fmedian)

>>> x = np.array([65., 667, 84, 968, 62, 70, 66,
>>>               78, 47, 71, 56, 65, 60])
>>> q,w,e,r,t,y = sr.sigrej(x, [2,1], ival=True, fmean=True,
>>>                         fstddev=True, fmedian=True,
>>>                         fmedstddev=True)

>>> print(q)
[True False True False True True True True True True True True
True]
>>> print(w)
[[66.          65.5       ]
[313.02675604  181.61572819]]
>>> print(e)
65.8181818182
>>> print(r)
10.1174916043
>>> print(t)
65.0
>>> print(y)
10.1538170163
>>> print(fmean, fmedian)
67.0000      67.0000

S3_data_reduction.source_pos

eureka.S3_data_reduction.source_pos.gauss(x, a, x0, sigma, off)[source]

A function to find the source location using a Gaussian fit.

Parameters

xndarray: The positions at which to evaluate the Gaussian.
afloat: The amplitude of the Gaussian.
x0float: The centre point of the Gaussian.
sigmafloat: The standard deviation of the Gaussian.
offfloat: A vertical offset in the Gaussian.

Returns

gaussianndarray: The 1D Gaussian evaluated at the points x, in the same shape as x.

Notes

History:

2021-07-14 Sebastian Zieba
Initial version
2021-10-15 Taylor Bell
Separated this into its own function to allow it to be used elsewhere.

eureka.S3_data_reduction.source_pos.source_pos(flux, meta, shdr, m, n, plot=True, guess=None)[source]

Determine the source position for one frames.

Parameters

fluxnp.ma.masked_array (2D): The 2D image from which to get the source position.
metaeureka.lib.readECF.MetaClass: The metadata object.
shdrastropy.io.fits.header.Header: The science header of the file being processed.
mint: The file number.
nint: The integration number.
plotbool; optional: If True, plot the source position determination. Defaults to True.
guessfloat; optional: The guess at the source position for WFC3 data.

Returns

src_yposint: The central position of the star.
src_ypos_exactfloat: The exact (not rounded) central position of the star.
src_ypos_widthfloat: If gaussian fit, the std of the Gaussian fitted to the image Otherwise, array of zeros.

Notes

History:

2022-07-11 Caroline Piaulet
Enable recording of the width if the source is fitted with a Gaussian + add an option to fit any integration (not hardcoded to be the first)
2022-07-18, Taylor J Bell
Tweaked to allow parallelized code if fitting multiple frames.

eureka.S3_data_reduction.source_pos.source_pos_FWM(flux, meta, m, n=0, plot=True)[source]

An alternative function to find the source location using a flux-weighted mean approach.

Parameters

fluxndarray: The 2D array of flux values.
metaeureka.lib.readECF.MetaClass: The metadata object.
mint: The file number.
nint; optional: The integration number. Default is 0 (first integration).
plotbool; optional: If True, plot the source position determination. Defaults to True.

Returns

y_posfloat: The central position of the star.

Notes

History:

2021-06-24 Taylor Bell
Initial version
2021-07-14 Sebastian Zieba
Modified
2022-07-11 Caroline Piaulet
Add option to fit any integration (not hardcoded to be the first)

eureka.S3_data_reduction.source_pos.source_pos_gauss(flux, meta, m, n=0, plot=True)[source]

A function to find the source location using a gaussian fit.

Parameters

fluxndarray: The 3D array of flux values.
metaeureka.lib.readECF.MetaClass: The metadata object.
mint: The file number.
nint; optional: The integration number. Default is 0 (first integration)
plotbool; optional: If True, plot the source position determination. Defaults to True.

Returns

y_posfloat: The central position of the star.
y_widthint: The std of the fitted Gaussian.

Notes

History:

2021-07-14 Sebastian Zieba
Initial version
2021-10-15 Taylor Bell
Tweaked to allow for cleaner plots_s3.py
2022-07-11 Caroline Piaulet
Enable recording of the width if the source is fitted with a Gaussian + add an option to fit any integration (not hardcoded to be the first)

eureka.S3_data_reduction.source_pos.source_pos_max(flux, meta, m, n=0, plot=True)[source]

A simple function to find the brightest row for source location

Parameters

fluxndarray: The 2D array of flux values.
metaeureka.lib.readECF.MetaClass: The metadata object.
mint: The file number.
nint; optional: The integration number. Default is 0 (first integration).
plotbool; optional: If True, plot the source position determination. Defaults to True.

Returns

y_posint: The central position of the star.

Notes

History:

6/24/21 Megan Mansfield
Initial version
2021-07-14 Sebastian Zieba
Modified
July 11, 2022 Caroline Piaulet
Add option to fit any integration (not hardcoded to be the first)

eureka.S3_data_reduction.source_pos.source_pos_wrapper(data, meta, log, m, integ=0)[source]

Determine the source position for many frames.

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The current log.
mint: The file number.
integint or None; optional: The integration number. Default is 0 (first integration). If set to None, the source position and width for each frame will be calculated and stored in data.centroid_y and data.centroid_sy.

Returns

dataXarray Dataset: The updated Dataset object.
metaeureka.lib.readECF.MetaClass: The updated metadata object.
loglogedit.Logedit: The updated log.

Notes

History:

2022-07-18, Taylor J Bell
Added source_pos_wrapper to allow multiple frames to get source positions in parallel.

S3_data_reduction.straighten

eureka.S3_data_reduction.straighten.find_column_median_shifts(data, meta, m)[source]

Takes the median frame (in time) and finds the center of mass (COM) in pixels for each column. It then returns the needed shift to apply to each column to bring the COM to the center

Parameters

datandarray (2D): The median of all data frames
metaeureka.lib.readECF.MetaClass: The metadata object.
mint: The file number.

Returns

shiftsndarray (2D): The shifts to apply to each column to straighten the trace.
new_centerint: The central row of the detector where the trace is moved to.

eureka.S3_data_reduction.straighten.roll_columns(data, shifts)[source]

For each column of each integration, rolls the columns by the values specified in shifts

Parameters

datandarray (3D): Image data.
shiftsndarray (2D): The shifts to apply to each column to straighten the trace.

Returns

rolled_datandarray (3D): Image data with the shifts applied.

eureka.S3_data_reduction.straighten.straighten_trace(data, meta, log, m)[source]

Takes a set of integrations with a curved trace and shifts the columns to bring the center of mass to the middle of the detector (and straighten the trace)

The correction is made by whole pixels (i.e. no fractional pixel shifts) The shifts to be applied are computed once from the median frame and then applied to each integration in the timeseries

Parameters

dataXarray Dataset: The Dataset object in which the fits data will stored.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The open log in which notes from this step can be added.
mint: The file number.

Returns

dataXarray Dataset: The updated Dataset object with the fits data stored inside.
metaeureka.lib.readECF.MetaClass: The updated metadata object.

S3_data_reduction.wfc3

eureka.S3_data_reduction.wfc3.conclusion_step(data, meta, log)[source]

Convert lists into arrays for saving and applies meta.sum_reads if requested.

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The current metadata object.
loglogedit.Logedit: The current log.

Returns

dataXarray Dataset: The updated Dataset object.
metaeureka.lib.readECF.MetaClass: The updated metadata object.
loglogedit.Logedit: The updated log.

eureka.S3_data_reduction.wfc3.correct_drift2D(data, meta, log, m)[source]

Correct for calculated 2D drift.

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The current log.
mint: The current file number.

Returns

dataXarray Dataset: The updated Dataset object after 2D drift correction.
metaeureka.lib.readECF.MetaClass: The updated metadata object.
loglogedit.Logedit: The current log.

eureka.S3_data_reduction.wfc3.cut_aperture(data, meta, log)[source]

Select the aperture region out of each trimmed image.

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The current log.

Returns

apdatandarray: The flux values over the aperture region.
aperrndarray: The noise values over the aperture region.
apmaskndarray: The mask values over the aperture region.
apbgndarray: The background flux values over the aperture region.
apv0ndarray: The v0 values over the aperture region.

Notes

History:

2022-06-17, Taylor J Bell
Initial version, edited to work for HST scanned observations.

eureka.S3_data_reduction.wfc3.difference_frames(data, meta, log)[source]

Compute differenced frames.

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The current log.

Returns

dataXarray Dataset: The updated Dataset object differenced frames.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The current log.

eureka.S3_data_reduction.wfc3.fit_bg(dataim, datamask, datav0, datavariance, guess, n, meta, isplots=0)[source]

Fit for a non-uniform background.

Uses the code written for NIRCam, but adds on some extra steps

Parameters

dataimndarray (2D): The 2D image array.
datamaskndarray (2D): An array of which data should be masked.
datav0ndarray (2D): readNoise**2.
datavariancendarray (2D): Initially an all zeros array.
nint: The current integration.
metaeureka.lib.readECF.MetaClass: The metadata object.
isplotsint; optional: The plotting verbosity, by default False.

Returns

bgndarray (2D): The fitted background level.
maskndarray (2D): The updated mask after background subtraction.
datav0ndarray (2D): readNoise**2+np.mean(bgerr**2)
datavariancendarray (2D): abs(dataim) / meta.gain + datav0
nint: The current integration number.

eureka.S3_data_reduction.wfc3.flag_bg(data, meta, log)[source]

Outlier rejection of sky background along time axis.

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The current log.

Returns

dataXarray Dataset: The updated Dataset object with outlier background pixels flagged.

eureka.S3_data_reduction.wfc3.flatfield(data, meta, log)[source]

Perform flatfielding.

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The current log.

Returns

dataXarray Dataset: The updated Dataset object with flatfielding applied.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The current log.

eureka.S3_data_reduction.wfc3.get_reference_frames(meta, log)[source]

Process the reference frames for each scan direction and save them in the meta object.

Parameters

metaeureka.lib.readECF.MetaClass: The current metadata object.

Returns

metaeureka.lib.readECF.MetaClass: The updated metadata object.

eureka.S3_data_reduction.wfc3.preparation_step(meta, log)[source]

Perform preperatory steps which require many frames.

Separate imaging and spectroscopy, separate observations into different scan directions, and calculate centroid for each frame.

Parameters

metaeureka.lib.readECF.MetaClass: The current metadata object.
loglogedit.Logedit: The current log.

Returns

metaeureka.lib.readECF.MetaClass: The updated metadata object.
loglogedit.Logedit: The updated log.

eureka.S3_data_reduction.wfc3.read(filename, data, meta, log)[source]

Reads single FITS file from HST’s WFC3 instrument.

Parameters

filenamestr: Single filename to read
dataXarray Dataset: The Dataset object in which the fits data will stored
metaeureka.lib.readECF.MetaClass: The metadata object
loglogedit.Logedit: The current log.

Returns

dataXarray Dataset: The updated Dataset object with the fits data stored inside
metaeureka.lib.readECF.MetaClass: The metadata object
loglogedit.Logedit: The current log.

Notes

History:

January 2017 Kevin Stevenson
Initial code as implemented in the WFC3 pipeline
18-19 Nov 2021 Taylor Bell
Edited and decomposed WFC3 code to integrate with Eureka!
May 9, 2022 Kevin Stevenson
Convert to using Xarray Dataset

eureka.S3_data_reduction.wfc3.separate_direct(meta, log)[source]

Separate out the direct observations from the science observations.

Parameters

metaeureka.lib.readECF.MetaClass: The current metadata object.
loglogedit.Logedit: The current log.

Returns

obstimesndarray: The times of each integration.
CRPIX1float: The CRPIX1 FITS header value.
CRPIX2float: The CRPIX2 FITS header value.
postarg1float: The POSTARG1 FITS header value.
postarg2float: The POSTARG2 FITS header value.
nyint: The NAXIS2 FITS header value.
metaeureka.lib.readECF.MetaClass: The updated metadata object.
loglogedit.Logedit: The updated log.

Raises

AssertionError: All observations cannot be in imaging mode.
AssertionError: All observations cannot be spectroscopic.
AssertionError: Unknown OBSTYPE(s) encountered.

eureka.S3_data_reduction.wfc3.separate_scan_direction(meta, log)[source]

Separate alternating scan directions.

Parameters

obstimesndarray: The times for each integration.
postarg2float: The POSTARG2 FITS header value.
metaeureka.lib.readECF.MetaClass: The current metadata object.
loglogedit.Logedit: The current log.

Returns

metaeureka.lib.readECF.MetaClass: The updated metadata object.
loglogedit.Logedit: The updated log.

S4_generate_lightcurves

S4_generate_lightcurves.drift

eureka.S4_generate_lightcurves.drift.highpassfilt(signal, highpassWidth)[source]

Run a signal through a highpass filter to remove high frequency signals.

This function can be used to compute the continuum of a signal to be subtracted.

Parameters

signalndarray (1D): 1D array of values.
highpassWidthint: The width of the boxcar filter to use.

Returns

smoothed_signalndarray (1D): An array containing the smoothed signal.

Notes

History:

14 Feb 2018 Lisa Dang
Written for early version of SPCA
23 Sep 2019 Taylor Bell
Generalized upon the code
02 Nov 2021 Taylor Bell
Added to Eureka!

eureka.S4_generate_lightcurves.drift.spec1D(spectra, meta, log, mask=None)[source]

Measures the 1D spectrum drift over all integrations.

Measure spectrum drift over all frames and all non-destructive reads.

Parameters

spectrandarray: 2D array of flux values (nint, nx).
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The open log in which notes from this step can be added.
maskndarray (1D); optional: A mask array to use if spectra is not a masked array. Defaults to None in which case only the invalid values of spectra will be masked.

Returns

drift1dndarray: 1D array of spectrum drift values.
driftwidthndarray: 1D array of the widths of the Gaussians fitted to the CCFs.
driftmaskndarray: 1D masked array, where True is masked.

Notes

History:

Dec 2013 KBS
Written for HST.
Jun 2021 KBS
Updated for JWST.
Oct 18, 2021 Taylor Bell
Minor tweak to cc_spec inputs.
Nov 02, 2021 Taylor Bell
Added option for subtraction of continuum using a highpass filter before cross-correlation.
Apr 23, 2022 Kevin Stevenson
Switched defition of mask to coincide with np.ma definition Removed drift1d and driftmask from meta
Jul 11, 2022 Caroline Piaulet
Added recording of driftwidth

S4_generate_lightcurves.generate_LD

eureka.S4_generate_lightcurves.generate_LD.exotic_ld(meta, spec, log, white=False)[source]

Generate limb-darkening coefficients using the exotic_ld package.

Parameters

metaeureka.lib.readECF.MetaClass: The metadata object.
specAstreaus object: Data object of wavelength-like arrrays.
loglogedit.Logedit: The open log in which notes from this step can be added.
whitebool; optional: If True, compute the limb-darkening parameters for the white-light light curve. Defaults to False.

Returns

ld_coeffstuple: Linear, Quadratic, Non-linear (3 and 4) limb-darkening coefficients

Notes

History:

July 2022, Eva-Maria Ahrer
Initial version based on exotic_ld documentation.

S4_generate_lightcurves.plots_s4

eureka.S4_generate_lightcurves.plots_s4.binned_lightcurve(meta, log, lc, i, white=False)[source]

Plot each spectroscopic light curve. (Figs 4102)

Parameters

metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The open log in which notes from this step can be added.
lcXarray Dataset: The Dataset object containing light curve and time data.
iint: The current bandpass number.
whitebool; optional: Is this figure for the additional white-light light curve

eureka.S4_generate_lightcurves.plots_s4.cc_spec(meta, ref_spec, fit_spec, n)[source]

Compare the spectrum used for cross-correlation with the current spectrum (Fig 4301).

Parameters

metaeureka.lib.readECF.MetaClass: The metadata object.
ref_specndarray (1D): The reference spectrum used for cross-correlation.
fit_specndarray (1D): The extracted spectrum for the current integration.
nint: The current integration number.

eureka.S4_generate_lightcurves.plots_s4.cc_vals(meta, vals, n)[source]

Make the cross-correlation strength plot (Fig 4302).

Parameters

metaeureka.lib.readECF.MetaClass: The metadata object.
valsndarray (1D): The cross-correlation strength.
nint: The current integration number.

eureka.S4_generate_lightcurves.plots_s4.driftxpos(meta, lc)[source]

Plot the 1D drift/jitter results. (Fig 4103)

Parameters

metaeureka.lib.readECF.MetaClass: The metadata object.
lcXarray Dataset: The light curve object containing drift arrays.

Notes

History:

Jul 11, 2022 Caroline Piaulet
Edited this function to use the new naming convention for drift

eureka.S4_generate_lightcurves.plots_s4.driftxwidth(meta, lc)[source]

Plot the 1D drift width results. (Fig 4104)

Parameters

metaeureka.lib.readECF.MetaClass: The metadata object.
lcXarray Dataset: The light curve object containing drift arrays.

Notes

History:

Jul 11, 2022 Caroline Piaulet
Created this function

eureka.S4_generate_lightcurves.plots_s4.lc_driftcorr(meta, wave_1d, optspec_in, optmask=None)[source]

Plot a 2D light curve with drift correction. (Fig 4101)

Parameters

metaeureka.lib.readECF.MetaClass: The metadata object.
wave_1dndarray: Wavelength array with trimmed edges depending on xwindow and ywindow which have been set in the S3 ecf.
optspec_inXarray DataArray: The optimally extracted spectrum.
optmaskXarray DataArray; optional: A mask array to use if optspec is not a masked array. Defaults to None in which case only the invalid values of optspec will be masked.

S4_generate_lightcurves.s4_genLC

eureka.S4_generate_lightcurves.s4_genLC.genlc(eventlabel, ecf_path=None, s3_meta=None)[source]

Compute photometric flux over specified range of wavelengths.

Parameters

eventlabelstr: The unique identifier for these data.
ecf_pathstr; optional: The absolute or relative path to where ecfs are stored. Defaults to None which resolves to ‘./’.
s3_metaeureka.lib.readECF.MetaClass: The metadata object from Eureka!’s S3 step (if running S3 and S4 sequentially). Defaults to None.

Returns

specAstreaus object: Data object of wavelength-like arrrays.
lcAstreaus object: Data object of time-like arrrays (light curve).
metaeureka.lib.readECF.MetaClass: The metadata object with attributes added by S4.

Notes

History:

June 2021 Kevin Stevenson
Initial version
October 2021 Taylor Bell
Updated to allow for inputs from new S3
April 2022 Kevin Stevenson
Enabled Astraeus
July 2022 Caroline Piaulet
Recording of x (computed in S4) and y (computed in S3) pos drifts and widths in Spec and LC objects
July 2022 Sebastian Zieba
Added photometry S4

eureka.S4_generate_lightcurves.s4_genLC.load_specific_s3_meta_info(meta)[source]

Load the specific S3 MetaClass object used to make this aperture pair.

Parameters

metaeureka.lib.readECF.MetaClass: The current metadata object.

Returns

eureka.lib.readECF.MetaClass: The current metadata object with values from the old MetaClass.

S4_generate_lightcurves.wfc3

eureka.S4_generate_lightcurves.wfc3.sum_reads(spec, lc, meta)[source]

Sum together the non-destructive reads from each file to reduce noise and data volume.

specXarray Dataset: The Dataset object containing the 2D spectra.
lcXarray Dataset: The Dataset object containing light curve and time data.
metaeureka.lib.readECF.MetaClass: The current metadata object.

Returns

specXarray Dataset: The updated spec Dataset object.
lcXarray Dataset: The updated lc Dataset object.
metaeureka.lib.readECF.MetaClass: The updated metadata object.

S5_lightcurve_fitting

S5_lightcurve_fitting.models.BatmanModels

class eureka.S5_lightcurve_fitting.models.BatmanModels.BatmanEclipseModel(**kwargs)[source]

Bases: Model

Eclipse Model

Attributes

flux: A getter for the flux.
parameters: A getter for the parameters.
units: A getter for the unit.s

Methods

`eval`(**kwargs)	Evaluate the function with the given values.
`interp`(new_time, **kwargs)	Evaluate the model over a different time array.
`plot`(time[, components, ax, draw, color, ...])	Plot the model.
`update`(newparams, **kwargs)	Update the model with new parameter values.

eval(**kwargs)[source]

Evaluate the function with the given values.

Parameters

**kwargsdict: Must pass in the time array here if not already set.

Returns

lcfinalndarray: The value of the model at the times self.time.

class eureka.S5_lightcurve_fitting.models.BatmanModels.BatmanTransitModel(**kwargs)[source]

Bases: Model

Transit Model

Attributes

flux: A getter for the flux.
parameters: A getter for the parameters.
units: A getter for the unit.s

Methods

`eval`(**kwargs)	Evaluate the function with the given values.
`interp`(new_time, **kwargs)	Evaluate the model over a different time array.
`plot`(time[, components, ax, draw, color, ...])	Plot the model.
`update`(newparams, **kwargs)	Update the model with new parameter values.

eval(**kwargs)[source]

Evaluate the function with the given values.

Parameters

**kwargsdict: Must pass in the time array here if not already set.

Returns

lcfinalndarray: The value of the model at the times self.time.

eureka.S5_lightcurve_fitting.models.BatmanModels.correct_light_travel_time(time, bm_params)[source]

Correct for the finite light travel speed.

This function uses the KeplerOrbit.py file from the Bell_EBM package as that code includes a newer, faster method of solving Kepler’s equation based on Tommasini+2018.

Parameters

timendarray: The times at which observations were collected
bm_paramsbatman.TransitParams: The batman TransitParams object that contains information on the orbit.

Returns

timendarray: Updated times that can be put into batman transit and eclipse functions that will give the expected results assuming a finite light travel speed.

Notes

History:

2022-03-31 Taylor J Bell
Initial version based on the Bell_EMB KeplerOrbit.py file by Taylor J Bell and the light travel time calculations of SPIDERMAN’s web.c file by Tom Louden

S5_lightcurve_fitting.models.ExpRampModel

class eureka.S5_lightcurve_fitting.models.ExpRampModel.ExpRampModel(**kwargs)[source]

Bases: Model

Model for single or double exponential ramps

Attributes

flux: A getter for the flux.
parameters: A getter for the parameters.
time: A getter for the time.
units: A getter for the unit.s

Methods

`eval`(**kwargs)	Evaluate the function with the given values.
`interp`(new_time, **kwargs)	Evaluate the model over a different time array.
`plot`(time[, components, ax, draw, color, ...])	Plot the model.
`update`(newparams, **kwargs)	Update the model with new parameter values.

eval(**kwargs)[source]

Evaluate the function with the given values.

Parameters

**kwargsdict: Must pass in the time array here if not already set.

Returns

lcfinalndarray: The value of the model at the times self.time.

property time: A getter for the time.

S5_lightcurve_fitting.models.GPModel

class eureka.S5_lightcurve_fitting.models.GPModel.GPModel(kernel_classes, kernel_inputs, lc, gp_code='george', **kwargs)[source]

Bases: Model

Model for Gaussian Process (GP)

Attributes

flux: A getter for the flux.
parameters: A getter for the parameters.
units: A getter for the unit.s

Methods

`eval`(fit[, gp])	Compute GP with the given parameters
`get_kernel`(kernel_name, i[, channel])	Get individual kernels.
`interp`(new_time, **kwargs)	Evaluate the model over a different time array.
`loglikelihood`(fit, unc_fit)	Compute log likelihood of GP
`plot`(time[, components, ax, draw, color, ...])	Plot the model.
`set_inputs`([normalise])	Setting up kernel inputs as array and standardizing them see e.g.
`setup_GP`(channel)	Set up GP kernels and GP object.
`update`(newparams, **kwargs)	Update the model with new parameter values.

eval(fit, gp=None, **kwargs)[source]

Compute GP with the given parameters

Parameters

fiteureka.S5_lightcurve_fitting.models.Model: Current model (i.e. transit model)
gpcelerite.GP, george.GP, or tinygp.GaussianProcess; optional: The current GP object.
**kwargsdict: Must pass in the time array here if not already set.

Returns

lcfinalndarray: Predicted systematics model

get_kernel(kernel_name, i, channel=0)[source]

Get individual kernels.

Parameters

kernel_namestr: The name of the kernel to get.
iint: The kernel number.
channelint; optional: The channel number, by default 0.

Returns

kernel: The requested george, celerite, or tinygp kernel.

Raises

AssertionError: Celerite currently only supports a Matern32 kernel.

loglikelihood(fit, unc_fit)[source]

Compute log likelihood of GP

Parameters

fitndarray: The fitted model.
unc_fitndarray: The fitted uncertainty.

Returns

float: log likelihood of the GP evaluated by george/tinygp/celerite

set_inputs(normalise=False)[source]

Setting up kernel inputs as array and standardizing them see e.g. Evans et al. 2017.

Parameters

normalisebool; optional: Standardize kernels following Evans+2017. Defaults to False.

setup_GP(channel)[source]

Set up GP kernels and GP object.

Parameters

channelint: The current channel number.

Returns

celerite.GP, george.GP, or tinygp.GaussianProcess: The GP object to use for this fit.

S5_lightcurve_fitting.models.KeplerOrbit

class eureka.S5_lightcurve_fitting.models.KeplerOrbit.KeplerOrbit(a=149597870700.0, Porb=None, inc=90.0, t0=0.0, e=0.0, Omega=270.0, argp=90.0, obliq=0.0, argobliq=0.0, Prot=None, m1=1.988409870698051e+30, m2=0.0)[source]

Bases: object

A Keplerian orbit.

Code taken from: https://github.com/taylorbell57/Bell_EBM/blob/master/Bell_EBM/KeplerOrbit.py

Attributes

afloat: The semi-major axis in m.
incfloat: The orbial inclination (in degrees above face-on)
t0float: The linear ephemeris in days.
efloat: The orbital eccentricity.
Protfloat: Body 2’s rotational period in days.
Omegafloat: The longitude of ascending node (in degrees CCW from line-of-sight).
argpfloat: The argument of periastron (in degrees CCW from Omega).
obliqfloat; optional: The obliquity (axial tilt) of body 2 (in degrees toward body 1).
argobliqfloat; optional: The reference orbital angle used for obliq (in degrees from inferior conjunction).
t_perifloat: Time of body 2’s closest approach to body 1.
t_eclfloat: Time of body 2’s eclipse by body 1.
mean_motionfloat: The mean motion in radians.

Methods

`FSSI`(Y, x, f, fP)	Fast Switch and Spline Inversion method from Tommasini+2018.
`FSSI_Eccentric_Inverse`(M[, xtol])	Convert mean anomaly to eccentric anomaly using FSSI (Tommasini+2018).
`Newton_Eccentric_Inverse`(M[, xtol])	Convert mean anomaly to eccentric anomaly using Newton.
`distance`([t, TA, xtol])	Find the separation between the two bodies.
`ea_to_ma`(ea)	Convert eccentric anomaly to mean anomaly.
`eccentric_anomaly`(t[, useFSSI, xtol])	Convert time to eccentric anomaly, numerically.
`get_phase`(t[, TA])	Get the orbital phase.
`get_sop`(t)	Calculate the sub-observer longitude and latitude.
`get_ssp`(t[, TA])	Calculate the sub-stellar longitude and latitude.
`mean_anomaly`(t)	Convert time to mean anomaly.
`plot_orbit`()	A convenience routine to visualize the orbit
`solve_period`()	Find the Keplerian orbital period.
`ta_to_ea`(ta)	Convert true anomaly to eccentric anomaly.
`ta_to_ma`(ta)	Convert true anomaly to mean anomaly.
`true_anomaly`(t[, xtol])	Convert time to true anomaly, numerically.
`xyz`(t[, xtol])	Find the coordinates of body 2 with respect to body 1.

FSSI(Y, x, f, fP)[source]

Fast Switch and Spline Inversion method from Tommasini+2018.

Parameters

Yndarray: The f(x) values to invert.
xndarray: x values spanning the domain (more values for higher precision).
fcallable: The function f.
fPcallable: The first derivative of the function f with respect to x.

Returns

ndarray: The numerical approximation of f^-(y).

FSSI_Eccentric_Inverse(M, xtol=1e-10)[source]

Convert mean anomaly to eccentric anomaly using FSSI (Tommasini+2018).

Parameters

Mndarray: The mean anomaly in radians.
xtolfloat; optional: tolarance on error in eccentric anomaly. Defaults to 1e-10.

Returns

ndarray: The eccentric anomaly in radians.

Newton_Eccentric_Inverse(M, xtol=1e-10)[source]

Convert mean anomaly to eccentric anomaly using Newton.

Parameters

Mndarray: The mean anomaly in radians.
xtolfloat; optional: tolarance on error in eccentric anomaly. Defaults to 1e-10.

Returns

ndarray: The eccentric anomaly in radians.

property Porb

Orbital period.

Changing this will update Prot if none was provided when the orbit was initialized.

Returns

float: Body 2’s orbital period in days.

distance(t=None, TA=None, xtol=1e-10)[source]

Find the separation between the two bodies.

Parameters

tndarray: The time in days.
TAndarray: The true anomaly in radians (if t and TA are given, only TA will be used).
xtolfloat; optional: tolarance on error in eccentric anomaly (calculated along the way). Defaults to 1e-10.

Returns

ndarray: The separation between the two bodies.

ea_to_ma(ea)[source]

Convert eccentric anomaly to mean anomaly.

Parameters

eandarray: The eccentric anomaly in radians.

Returns

ndarray: The mean anomaly in radians.

eccentric_anomaly(t, useFSSI=None, xtol=1e-10)[source]

Convert time to eccentric anomaly, numerically.

Parameters

tndarray: The time in days.
useFSSIbool; optional: Whether or not to use FSSI to invert Kepler’s equation. Defaults to None which uses FSSI if t.size > 8.
xtolfloat; optional: tolarance on error in eccentric anomaly. Defaults to 1e-10.

Returns

ndarray: The eccentric anomaly in radians.

get_phase(t, TA=None)[source]

Get the orbital phase.

Parameters

tndarray: The time in days.
TAndarray; optional: The true anomaly. Defaults to None which calculates the TA using self.true_anomaly(t).

Returns

ndarray: The orbital phase.

get_sop(t)[source]

Calculate the sub-observer longitude and latitude.

Parameters

tndarray: The time in days.

Returns

list: A list of 2 ndarrays containing the sub-observer longitude and latitude. Each ndarray is in the same shape as t.

get_ssp(t, TA=None)[source]

Calculate the sub-stellar longitude and latitude.

Parameters

tndarray: The time in days.
TAndarray; optional: The true anomaly. Defaults to None which calculates the TA using self.true_anomaly(t).

Returns

list: A list of 2 ndarrays containing the sub-stellar longitude and latitude. Each ndarray is in the same shape as t.

property m1

Body 1’s mass in kg.

If no period was provided when the orbit was initialized, changing this will update the period.

Returns

float: Body 1’s mass in kg.

property m2

Body 2’s mass in kg.

If no period was provided when the orbit was initialized, changing this will update the period.

Returns

float: Body 2’s mass in kg.

mean_anomaly(t)[source]

Convert time to mean anomaly.

Parameters

tndarray: The time in days.

Returns

ndarray: The mean anomaly in radians.

property phase_eclipse

Phase of eclipse.

Read-only.

Returns

float: The orbital phase of eclipse.

property phase_periastron

Phase of periastron.

Read-only.

Returns

float: The orbital phase of periastron.

property phase_transit

Phase of transit.

Read-only.

Returns

float: The orbital phase of transit.

plot_orbit()[source]

A convenience routine to visualize the orbit

Returns

figure: The figure containing the plot.

solve_period()[source]

Find the Keplerian orbital period.

Returns

float: The Keplerian orbital period.

property t_trans

Time of transit.

Read-only.

Returns

float: Time of body 1’s eclipse by body 2.

ta_to_ea(ta)[source]

Convert true anomaly to eccentric anomaly.

Parameters

tandarray: The true anomaly in radians.

Returns

ndarray: The eccentric anomaly in radians.

ta_to_ma(ta)[source]

Convert true anomaly to mean anomaly.

Parameters

tandarray: The true anomaly in radians.

Returns

ndarray: The mean anomaly in radians.

true_anomaly(t, xtol=1e-10)[source]

Convert time to true anomaly, numerically.

Parameters

tndarray: The time in days.
xtolfloat; optional: tolarance on error in eccentric anomaly (calculated along the way). Defaults to 1e-10.
Returns
——-
ndarray: The true anomaly in radians.

xyz(t, xtol=1e-10)[source]

Find the coordinates of body 2 with respect to body 1.

Parameters

tndarray: The time in days.
xtolfloat; optional: tolarance on error in eccentric anomaly (calculated along the way). Defaults to 1e-10.

Returns

list: A list of 3 ndarrays containing the x,y,z coordinate of body 2 with respect to body 1. - The x coordinate is along the line-of-sight. - The y coordinate is perpendicular to the line-of-sight and in the orbital plane. - The z coordinate is perpendicular to the line-of-sight and above the orbital plane

S5_lightcurve_fitting.models.Model

class eureka.S5_lightcurve_fitting.models.Model.CompositeModel(models, **kwargs)[source]

Bases: Model

A class to create composite models.

Attributes

flux: A getter for the flux.
parameters: A getter for the parameters.
units: A getter for the unit.s

Methods

`GPeval`(fit, **kwargs)	Evaluate the GP model components only.
`eval`([incl_GP])	Evaluate the model components.
`interp`(new_time, **kwargs)	Evaluate the model over a different time array.
`physeval`([interp])	Evaluate the physical model components only.
`plot`(time[, components, ax, draw, color, ...])	Plot the model.
`syseval`(**kwargs)	Evaluate the systematic model components only.
`update`(newparams, **kwargs)	Update parameters in the model components.

GPeval(fit, **kwargs)[source]

Evaluate the GP model components only.

Parameters

fitndarray: The model predictions (excluding the GP).
**kwargsdict: Must pass in the time array here if not already set.

Returns

fluxndarray: The evaluated GP model predictions at the times self.time.

eval(incl_GP=False, **kwargs)[source]

Evaluate the model components.

Parameters

incl_GPbool; optional: Whether or not to include the GP’s predictions in the evaluated model predictions.
**kwargsdict: Must pass in the time array here if not already set.

Returns

fluxndarray: The evaluated model predictions at the times self.time.

physeval(interp=False, **kwargs)[source]

Evaluate the physical model components only.

Parameters

interpbool; optional: Whether to uniformly sample in time or just use the self.time time points. Defaults to False.
**kwargsdict: Must pass in the time array here if not already set.

Returns

fluxndarray: The evaluated physical model predictions at the times self.time if interp==False, else at evenly spaced times between self.time[0] and self.time[-1] with spacing self.time[1]-self.time[0].

syseval(**kwargs)[source]

Evaluate the systematic model components only.

Parameters

**kwargsdict: Must pass in the time array here if not already set.

Returns

fluxndarray: The evaluated systematics model predictions at the times self.time.

update(newparams, **kwargs)[source]

Update parameters in the model components.

Parameters

newparamsndarray: New parameter values.
**kwargsdict: Additional parameters to pass to eureka.S5_lightcurve_fitting.models.Model.update().

class eureka.S5_lightcurve_fitting.models.Model.Model(**kwargs)[source]

Bases: object

Attributes

flux: A getter for the flux.
parameters: A getter for the parameters.
units: A getter for the unit.s

Methods

`interp`(new_time, **kwargs)	Evaluate the model over a different time array.
`plot`(time[, components, ax, draw, color, ...])	Plot the model.
`update`(newparams, **kwargs)	Update the model with new parameter values.

property flux: A getter for the flux.

interp(new_time, **kwargs)[source]

Evaluate the model over a different time array.

Parameters

new_timesequence: The time array.
**kwargsdict: Additional parameters to pass to self.eval().

property parameters: A getter for the parameters.

plot(time, components=False, ax=None, draw=False, color='blue', zorder=inf, share=False, chan=0, **kwargs)[source]

Plot the model.

Parameters

timearray-like: The time axis to use.
componentsbool; optional: Plot all model components.
axMatplotlib Axes; optional: The figure axes to plot on.
drawbool; optional: Whether or not to display the plot. Defaults to False.
colorstr; optional: The color to use for the plot. Defaults to ‘blue’.
zordernumeric; optional: The zorder for the plot. Defaults to np.inf.
sharebool; optional: Whether or not this model is a shared model. Defaults to False.
chanint; optional: The current channel number. Detaults to 0.
**kwargsdict: Additional parameters to pass to plot and self.eval().

Returns

figure: The figure.

property units: A getter for the unit.s

update(newparams, **kwargs)[source]

Update the model with new parameter values.

Parameters

newparamsndarray: New parameter values.
**kwargsdict: Unused by the base eureka.S5_lightcurve_fitting.models.Model class.

S5_lightcurve_fitting.models.PolynomialModel

class eureka.S5_lightcurve_fitting.models.PolynomialModel.PolynomialModel(**kwargs)[source]

Bases: Model

Polynomial Model

Attributes

flux: A getter for the flux.
parameters: A getter for the parameters.
time: A getter for the time.
units: A getter for the unit.s

Methods

`eval`(**kwargs)	Evaluate the function with the given values.
`interp`(new_time, **kwargs)	Evaluate the model over a different time array.
`plot`(time[, components, ax, draw, color, ...])	Plot the model.
`update`(newparams, **kwargs)	Update the model with new parameter values.

eval(**kwargs)[source]

Evaluate the function with the given values.

Parameters

**kwargsdict: Must pass in the time array here if not already set.

Returns

lcfinalndarray: The value of the model at the times self.time.

property time: A getter for the time.

S5_lightcurve_fitting.models.SinusoidPhaseCurve

class eureka.S5_lightcurve_fitting.models.SinusoidPhaseCurve.SinusoidPhaseCurveModel(transit_model=None, eclipse_model=None, **kwargs)[source]

Bases: Model

A sinusoidal phase curve model

Attributes

flux: A getter for the flux.
parameters: A getter for the parameters.
time: A getter for the time.
units: A getter for the unit.s

Methods

`eval`(**kwargs)	Evaluate the function with the given values.
`interp`(new_time, **kwargs)	Evaluate the model over a different time array.
`plot`(time[, components, ax, draw, color, ...])	Plot the model.
`update`(newparams, **kwargs)	Update the model with new parameter values.

eval(**kwargs)[source]

Evaluate the function with the given values.

Parameters

**kwargsdict: Must pass in the time array here if not already set.

Returns

lcfinalndarray: The value of the model at the times self.time.

property time: A getter for the time.

update(newparams, **kwargs)[source]

Update the model with new parameter values.

Parameters

newparamsndarray: New parameter values.
**kwargsdict: Additional parameters to pass to eureka.S5_lightcurve_fitting.models.Model.update().

S5_lightcurve_fitting.models.StepModel

class eureka.S5_lightcurve_fitting.models.StepModel.StepModel(**kwargs)[source]

Bases: Model

Model for step-functions in time

Attributes

flux: A getter for the flux.
parameters: A getter for the parameters.
units: A getter for the unit.s

Methods

`eval`(**kwargs)	Evaluate the function with the given values.
`interp`(new_time, **kwargs)	Evaluate the model over a different time array.
`plot`(time[, components, ax, draw, color, ...])	Plot the model.
`update`(newparams, **kwargs)	Update the model with new parameter values.

eval(**kwargs)[source]

Evaluate the function with the given values.

Parameters

**kwargsdict: Must pass in the time array here if not already set.

Returns

lcfinalndarray: The value of the model at the times self.time.

S5_lightcurve_fitting.fitters

eureka.S5_lightcurve_fitting.fitters.demcfitter(lc, model, meta, log, **kwargs)[source]

Perform sampling using Differential Evolution Markov Chain.

This is an empty placeholder function to be filled later.

Parameters

lceureka.S5_lightcurve_fitting.lightcurve.LightCurve: The lightcurve data object.
modeleureka.S5_lightcurve_fitting.models.CompositeModel: The composite model to fit.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The open log in which notes from this step can be added.
**kwargsdict: Arbitrary keyword arguments.

Returns

best_modeleureka.S5_lightcurve_fitting.models.CompositeModel: The composite model after fitting

Notes

History:

December 29, 2021 Taylor Bell
Updated documentation and arguments

eureka.S5_lightcurve_fitting.fitters.dynestyfitter(lc, model, meta, log, **kwargs)[source]

Perform sampling using dynesty.

Parameters

lceureka.S5_lightcurve_fitting.lightcurve.LightCurve: The lightcurve data object.
modeleureka.S5_lightcurve_fitting.models.CompositeModel: The composite model to fit.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The open log in which notes from this step can be added.
**kwargsdict: Arbitrary keyword arguments.

Returns

best_modeleureka.S5_lightcurve_fitting.models.CompositeModel: The composite model after fitting

Notes

History:

December 29, 2021 Taylor Bell
Updated documentation. Reduced repeated code.
January 7-22, 2022 Megan Mansfield
Adding ability to do a single shared fit across all channels
February 23-25, 2022 Megan Mansfield
Added log-uniform and Gaussian priors.
February 28-March 1, 2022 Caroline Piaulet
Adding scatter_ppm parameter.
Mar 13-Apr 18, 2022 Caroline Piaulet
Record an astropy table for mean, median, percentiles, +/- 1 sigma, all params

eureka.S5_lightcurve_fitting.fitters.emceefitter(lc, model, meta, log, **kwargs)[source]

Perform sampling using emcee.

Parameters

lceureka.S5_lightcurve_fitting.lightcurve.LightCurve: The lightcurve data object
modeleureka.S5_lightcurve_fitting.models.CompositeModel: The composite model to fit
metaeureka.lib.readECF.MetaClass: The metadata object
loglogedit.Logedit: The open log in which notes from this step can be added.
**kwargsdict: Arbitrary keyword arguments.

Returns

best_modeleureka.S5_lightcurve_fitting.models.CompositeModel: The composite model after fitting

Notes

History:

December 29, 2021 Taylor Bell
Updated documentation. Reduced repeated code.
January 7-22, 2022 Megan Mansfield
Adding ability to do a single shared fit across all channels
February 23-25, 2022 Megan Mansfield
Added log-uniform and Gaussian priors.
February 28-March 1, 2022 Caroline Piaulet
Adding scatter_ppm parameter. Added statements to avoid some initial state issues.
Mar 13-Apr 18, 2022 Caroline Piaulet
Record an astropy table for mean, median, percentiles, +/- 1 sigma, all params

eureka.S5_lightcurve_fitting.fitters.group_variables(model)[source]

Group variables into fitted and frozen.

Parameters

modeleureka.S5_lightcurve_fitting.models.CompositeModel: The composite model to fit

Returns

freenamesnp.array: The names of fitted variables.
freeparsnp.array: The fitted variables.
prior1np.array: The lower bound for constrained variables with uniform/log uniform priors, or mean for constrained variables with Gaussian priors.
prior2np.array: The upper bound for constrained variables with uniform/log uniform priors, or mean for constrained variables with Gaussian priors.
priortypenp.array: Keywords indicating the type of prior for each free parameter.
indep_varsdict: The frozen variables.

Notes

History:

December 29, 2021 Taylor Bell
Moved code to separate function to reduce repeated code.
January 11, 2022 Megan Mansfield
Added ability to have shared parameters
February 23-25, 2022 Megan Mansfield
Added log-uniform and Gaussian priors.

eureka.S5_lightcurve_fitting.fitters.group_variables_lmfit(model)[source]

Group variables into fitted and frozen for lmfit fitter.

Parameters

modeleureka.S5_lightcurve_fitting.models.CompositeModel: The composite model to fit

Returns

paramlistlist: The fitted variables.
freenamesnp.array: The names of fitted variables.
indep_varsdict: The frozen variables.

Notes

History:

December 29, 2021 Taylor Bell
Moved code to separate function to look similar to other fitters.

eureka.S5_lightcurve_fitting.fitters.initialize_emcee_walkers(meta, log, ndim, lsq_sol, freepars, prior1, prior2, priortype)[source]

Initialize emcee walker starting positions

Parameters

metaeureka.lib.readECF.MetaClass: The meta data object.
loglogedit.Logedit: The open log in which notes from this step can be added.
ndimint: The number of fitted parameters.
lsq_solThe results from the lsqfitter.: The results from the lsqfitter.
freeparslist: The names of the fitted parameters.
prior1list: The list of prior1 values.
prior2list: The list of prior2 values.
priortypelist: The types of each prior (to determine meaning of prior1 and prior2).

Returns

posndarray: The starting position of all walkers.
nwalkersint: The number of walkers (may differ from the requested number if unable to get all walkers within the priors).

Raises

AssertionError: Failed to initialize any walkers within the priors
AssertionError: Failed to initialize enough walkers within the priors

eureka.S5_lightcurve_fitting.fitters.lmfitter(lc, model, meta, log, **kwargs)[source]

Perform a fit using lmfit.

Parameters

lceureka.S5_lightcurve_fitting.lightcurve.LightCurve: The lightcurve data object.
modeleureka.S5_lightcurve_fitting.models.CompositeModel: The composite model to fit.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The open log in which notes from this step can be added.
**kwargsdict: Arbitrary keyword arguments.

Returns

best_modeleureka.S5_lightcurve_fitting.models.CompositeModel: The composite model after fitting

Notes

History:

December 29, 2021 Taylor Bell
Updated documentation. Reduced repeated code.
February 28-March 1, 2022 Caroline Piaulet
Adding scatter_ppm parameter.
Mar 13-Apr 18, 2022 Caroline Piaulet
Record an astropy table for parameter values

eureka.S5_lightcurve_fitting.fitters.load_old_fitparams(meta, log, channel, freenames)[source]

Load in the best-fit values from a previous fit.

Parameters

metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The open log in which notes from this step can be added.
channelint: Unused. The current channel.
freenameslist: The names of the fitted parameters.

Returns

fitted_valuesnp.array: The best-fit values from a previous fit

Raises

AssertionError: The old fit is incompatible with the current fit.

eureka.S5_lightcurve_fitting.fitters.lsqfitter(lc, model, meta, log, calling_function='lsq', **kwargs)[source]

Perform least-squares fit.

Parameters

lceureka.S5_lightcurve_fitting.lightcurve.LightCurve: The lightcurve data object.
modeleureka.S5_lightcurve_fitting.models.CompositeModel: The composite model to fit.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The open log in which notes from this step can be added.
calling_functionstr: The fitter that is being run (e.g. may be ‘emcee’ if running lsqfitter to initialize emcee walkers). Defailts to ‘lsq’.
**kwargsdict: Arbitrary keyword arguments.

Returns

best_modeleureka.S5_lightcurve_fitting.models.CompositeModel: The composite model after fitting

Notes

History:

December 29-30, 2021 Taylor Bell
Updated documentation and arguments. Reduced repeated code. Also saving covariance matrix for later estimation of sampler step size.
January 7-22, 2022 Megan Mansfield
Adding ability to do a single shared fit across all channels
February 28-March 1, 2022 Caroline Piaulet
Adding scatter_ppm parameter
Mar 13-Apr 18, 2022 Caroline Piaulet
Record an astropy table for param values

eureka.S5_lightcurve_fitting.fitters.save_fit(meta, lc, model, fitter, results_table, freenames, samples=[])[source]

Save a fit as a txt file as well as the entire chain if provided.

Parameters

metaeureka.lib.readECF.MetaClass: The metadata object.
lceureka.S5_lightcurve_fitting.lightcurve.LightCurve: The lightcurve data object.
modeleureka.S5_lightcurve_fitting.models.CompositeModel: The composite model to fit.
fitterstr: The current fitter being used.
fit_paramsnp.array: The best-fit values from the current fit.
freenameslist: The list of fitted parameter names.
samplesndarray; optional: The full chain from a sampling method, by default [].

Notes

History:

Mar 13-Apr 18, 2022 Caroline Piaulet
Record an astropy table for mean, median, percentiles, +/- 1 sigma, all params

eureka.S5_lightcurve_fitting.fitters.start_from_oldchain_emcee(meta, log, ndim, channel, freenames)[source]

Restart emcee using the ending point of an old chain.

Parameters

metaeureka.lib.readECF.MetaClass: The meta data object.
loglogedit.Logedit: The open log in which notes from this step can be added.
ndimint: The number of fitted parameters.
channelint: The channel number.
freenameslist: The names of the fitted parameters.

Returns

posndarray: The starting positions for all walkers.
nwalkersint: The number of walkers (may differ from the requested number if unable to get all walkers within the priors).

Raises

AssertionError: The old chain is not compatible with the current fit.
AssertionError: Unable to get enough walkers within the prior range.

S5_lightcurve_fitting.lightcurve

class eureka.S5_lightcurve_fitting.lightcurve.LightCurve(time, flux, channel, nchannel, log, longparamlist, parameters, unc=None, time_units='BJD', name='My Light Curve', share=False, white=False)[source]

Bases: Model

Attributes

flux: A getter for the flux.
parameters: A getter for the parameters.
units: A getter for the unit.s

Methods

`fit`(model, meta, log[, fitter])	Fit the model to the lightcurve
`interp`(new_time, **kwargs)	Evaluate the model over a different time array.
`plot`(meta[, fits])	Plot the light curve with all available fits.
`reset`()	Reset the results
`update`(newparams, **kwargs)	Update the model with new parameter values.

fit(model, meta, log, fitter='lsq', **kwargs)[source]

Fit the model to the lightcurve

Parameters

modeleureka.S5_lightcurve_fitting.models.CompositeModel: The model to fit to the data.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The open log in which notes from this step can be added.
fitterstr: The name of the fitter to use.
**kwargsdict: Arbitrary keyword arguments.

Notes

History:

Dec 29, 2021 Taylor Bell
Updated documentation and reduced repeated code

plot(meta, fits=True)[source]

Plot the light curve with all available fits. (Figs 5103)

Parameters

metaeureka.lib.readECF.MetaClass: The metadata object.
fitsbool; optional: Plot the fit models. Defaults to True.

reset()[source]: Reset the results

S5_lightcurve_fitting.likelihood

eureka.S5_lightcurve_fitting.likelihood.GP_loglikelihood(model, fit, unc_fit)[source]

Compute likelihood, when model fit includes GP

Parameters

modeleureka.S5_lightcurve_fitting.models.CompositeModel: The model including the GP model
fitndarray: The evaluated model without the GP
unc_fitndarray: The fitted (or initially provided) uncertainty on each data point.

Returns

loglikelihoodfloat: The likelihood of the model.

Notes

History:

March 11, 2022 Eva-Maria Ahrer
moved code from Model.py

eureka.S5_lightcurve_fitting.likelihood.computeRMS(data, maxnbins=None, binstep=1, isrmserr=False)[source]

Compute the root-mean-squared and standard error for various bin sizes.

Parameters

datandarray: The residuals after fitting.
maxnbinsint; optional: The maximum number of bins. Use None to default to 10 points per bin.
binstepint; optional: Bin step size. Defaults to 1.
isrmserrbool: True if return rmserr, else False. Defaults to False.

Returns

rmsndarray: The RMS for each bin size.
stderrndarray: The standard error for each bin size.
binszndarray: The different bin sizes.
rmserrndarray; optional: The uncertainty in the RMS. Only returned if isrmserr==True.

Notes

History:

December 29-30, 2021 Taylor Bell
Moved code to separate file, added documentation.

eureka.S5_lightcurve_fitting.likelihood.computeRedChiSq(lc, log, model, meta, freenames)[source]

Compute the reduced chi-squared value.

Parameters

lceureka.S5_lightcurve_fitting.lightcurve.LightCurve: The lightcurve data object
loglogedit.Logedit: The open log in which notes from this step can be added.
modeleureka.S5_lightcurve_fitting.models.CompositeModel: The composite model to fit
metaeureka.lib.readECF.MetaClass: The metadata object.
freenamesiterable: The names of the fitted parameters.

Returns

chi2redfloat: The reduced chi-squared value.

Notes

History:

December 29-30, 2021 Taylor Bell
Moved code to separate file, added documentation.
February, 2022 Eva-Maria Ahrer
Added GP functionality

eureka.S5_lightcurve_fitting.likelihood.ln_like(theta, lc, model, freenames)[source]

Compute the log-likelihood.

Parameters

thetandarray: The current estimate of the fitted parameters.
lceureka.S5_lightcurve_fitting.lightcurve.LightCurve: The lightcurve data object.
modeleureka.S5_lightcurve_fitting.models.CompositeModel: The composite model to fit.
freenamesiterable: The names of the fitted parameters.

Returns

ln_like_valndarray: The log-likelihood value at the position theta.

Notes

History:

December 29-30, 2021 Taylor Bell
Moved code to separate file, added documentation.
January 22, 2022 Megan Mansfield
Adding ability to do a single shared fit across all channels
February, 2022 Eva-Maria Ahrer
Adding GP likelihood

eureka.S5_lightcurve_fitting.likelihood.lnprior(theta, prior1, prior2, priortype)[source]

Compute the log-prior.

Parameters

thetandarray: The current estimate of the fitted parameters.
prior1ndarray: The lower-bound for uniform/log uniform priors, or mean for normal priors.
prior2ndarray: The upper-bound for uniform/log uniform priors, or std. dev. for normal priors.
priortypendarray: Keywords indicating the type of prior for each free parameter.

Returns

lnprior_probndarray: The log-prior probability value at the position theta.

Notes

History:

December 29-30, 2021 Taylor Bell
Moved code to separate file, added documentation.
February 23-25, 2022 Megan Mansfield
Added log-uniform and Gaussian priors.

eureka.S5_lightcurve_fitting.likelihood.lnprob(theta, lc, model, prior1, prior2, priortype, freenames)[source]

Compute the log-probability.

Parameters

thetandarray: The current estimate of the fitted parameters.
lceureka.S5_lightcurve_fitting.lightcurve.LightCurve: The lightcurve data object.
modeleureka.S5_lightcurve_fitting.models.CompositeModel: The composite model to fit.
prior1ndarray: The lower-bound for uniform/log uniform priors, or mean for normal priors.
prior2ndarray: The upper-bound for uniform/log uniform priors, or std. dev. for normal priors.
priortypendarray: Keywords indicating the type of prior for each free parameter.
freenamesiterable: The names of the fitted parameters.

Returns

ln_prob_valndarray: The log-probability value at the position theta.

Notes

History:

December 29-30, 2021 Taylor Bell
Moved code to separate file, added documentation.
February 23-25, 2022 Megan Mansfield
Added log-uniform and Gaussian priors.

eureka.S5_lightcurve_fitting.likelihood.ptform(theta, prior1, prior2, priortype)[source]

Compute the prior transform for nested sampling.

Parameters

thetandarray: The current estimate of the fitted parameters.
prior1ndarray: The lower-bound for uniform/log uniform priors, or mean for normal priors.
prior2ndarray: The upper-bound for uniform/log uniform priors, or std. dev. for normal priors.
priortypendarray: Keywords indicating the type of prior for each free parameter.

Returns

pndarray: The prior transform.

Notes

History:

February 23-25, 2022 Megan Mansfield
Added log-uniform and Gaussian priors.

eureka.S5_lightcurve_fitting.likelihood.transform_log_uniform(x, a, b)[source]

The log-uniform prior transform function needed for dynesty.

Parameters

xfloat: The position at which to calculate the prior.
afloat: The log lower limit.
bfloat: The log upper limit.

Returns

float: The log-uniform prior transform.

eureka.S5_lightcurve_fitting.likelihood.transform_normal(x, mu, sigma)[source]

The normal prior transform function needed for dynesty.

Parameters

xfloat: The position at which to calculate the prior.
mufloat: The prior mean.
sigmafloat: The prior standard deviation.

Returns

float: The normal prior transform.

eureka.S5_lightcurve_fitting.likelihood.transform_uniform(x, a, b)[source]

The uniform prior transform function needed for dynesty.

Parameters

xfloat: The position at which to calculate the prior.
afloat: The lower limit.
bfloat: The upper limit.

Returns

float: The uniform prior transform.

S5_lightcurve_fitting.limb_darkening_fit

A module to calculate limb darkening coefficients from a grid of model spectra

class eureka.S5_lightcurve_fitting.limb_darkening_fit.LDC(model_grid)[source]

Bases: object

A class to hold all the LDCs you want to run.

Examples

from exoctk.limb_darkening import limb_darkening_fit as lf from exoctk import modelgrid from svo_filters import Filter from pkg_resources import resource_filename fits_files = resource_filename(‘exoctk’, ‘data/core/modelgrid/’) model_grid = modelgrid.ModelGrid(fits_files, resolution=700) ld = lf.LDC(model_grid) bp = Filter(‘WFC3_IR.G141’, n_bins=5) ld.calculate(4000, 4.5, 0.0, ‘quadratic’, bandpass=bp) ld.calculate(4000, 4.5, 0.0, ‘4-parameter’, bandpass=bp) ld.plot(show=True)

Methods

`bootstrap_errors`(mu_vals, func, coeffs, errors)	Bootstrapping LDC errors.
`calculate`(Teff, logg, FeH, profile[, ...])	Calculates the limb darkening coefficients for a given synthetic spectrum.
`plot`([fig, show])	Plot the LDCs
`plot_tabs`([show])	Plot the LDCs in a tabbed figure

static bootstrap_errors(mu_vals, func, coeffs, errors, n_samples=1000)[source]

Bootstrapping LDC errors.

Parameters

mu_valssequence: The mu values.
funccallable: The LD profile function.
coeffssequence: The coefficients.
errorssequence: The errors on each coeff.
n_samplesint; optional: The number of samples. Defaults to 1000.

Returns

tuple: The lower and upper errors.

calculate(Teff, logg, FeH, profile, mu_min=0.05, ld_min=0.01, bandpass=None, name=None, color=None, **kwargs)[source]

Calculates the limb darkening coefficients for a given synthetic spectrum. If the model grid does not contain a spectrum of the given parameters, the grid is interpolated to those parameters.

Reference for limb-darkening laws: http://www.astro.ex.ac.uk/people/sing/David_Sing/Limb_Darkening.html

Parameters

Teffint: The effective temperature of the model.
loggfloat: The logarithm of the surface gravity.
FeHfloat: The logarithm of the metallicity.
profilestr: The name of the limb darkening profile function to use, including ‘uniform’, ‘linear’, ‘quadratic’, ‘squareroot’, ‘logarithmic’, ‘exponential’, and ‘4-parameter’.
mu_minfloat; optional: The minimum mu value to consider. Defaults to 0.05.
ld_minfloat; optional: The minimum limb darkening value to consider. Defaults to 0.01.
bandpasssvo_filters.svo.Filter(); optional: The photometric filter through which the limb darkening is to be calculated. Defaults to None.
namestr; optional: A name for the calculation. Defaults to None.
colorstr; optional: A color for the plotted result. Defaults to None.
**kwargsdict: Unused.

plot(fig=None, show=False, **kwargs)[source]

Plot the LDCs

Parameters

figmatplotlib.pyplot.figure, bokeh.plotting.figure; optional: An existing figure to plot on. Defaults to None.
showbool; optional: Show the figure. Defaults to False.
**kwargsdict: Additional parameters to be passed into plotting and utils.filter_table().

Returns

figmatplotlib.pyplot.figure, bokeh.plotting.figure; optional: The resulting figure. Only returned if show==False.

plot_tabs(show=False, **kwargs)[source]

Plot the LDCs in a tabbed figure

Parameters

showbool; optional: Show the figure. Defaults to False.
**kwargsdict: Unused.

Returns

finalbokeh.models.widgets.Tabs; optional: The final tabbed figure. Only returned if show==False.

eureka.S5_lightcurve_fitting.limb_darkening_fit.exponential(m, c1, c2)[source]

Exponential limb darkening.

Parameters

mndarray, float: The normalized radial coordinate.
c1float: The first limb darkening coefficient.
c2float: The second limb darkening coefficient.

Returns

ndarray, float: The relative intensity of the star at each position m.

eureka.S5_lightcurve_fitting.limb_darkening_fit.four_parameter(m, c1, c2, c3, c4)[source]

4-parameter limb darkening.

Parameters

mndarray, float: The normalized radial coordinate.
c1float: The first limb darkening coefficient.
c2float: The second limb darkening coefficient.
c3float: The third limb darkening coefficient.
c4float: The fourth limb darkening coefficient.

Returns

ndarray, float: The relative intensity of the star at each position m.

eureka.S5_lightcurve_fitting.limb_darkening_fit.kipping2013(m, c1, c2)[source]

Reparameterized Quadratic (Kipping 2013) limb darkening.

Parameters

mndarray, float: The normalized radial coordinate.
c1float: The first limb darkening coefficient.
c2float: The second limb darkening coefficient.

Returns

ndarray, float: The relative intensity of the star at each position m.

eureka.S5_lightcurve_fitting.limb_darkening_fit.ld_profile(name='quadratic', latex=False, use_gen_ld='batman')[source]

Define the function to fit the limb darkening profile.

Parameters

namestr; optional: The name of the limb darkening profile function to use, including ‘uniform’, ‘linear’, ‘quadratic’, ‘kipping2013’, ‘squareroot’, ‘logarithmic’, ‘exponential’, ‘3-parameter’, and ‘4-parameter’. Defaults to ‘quadratic’.
latexbool; optional: Return the function as a LaTeX formatted string. Defaults to False.
use_gen_ldstr; optional: Which tool will be doing the limb darkening modelling from [‘batman’, ‘exotic-ld’]. Defaults to ‘batman’.

Returns

function: The corresponding function for the given profile. Returned if latex==False.
OR str: A string representation of the corresponding function for the given profile. Returned if latex==True.

References

https://www.cfa.harvard.edu/~lkreidberg/batman/tutorial.html#limb-darkening-options https://exotic-ld.readthedocs.io/en/latest/views/quick_start.html

eureka.S5_lightcurve_fitting.limb_darkening_fit.linear(m, c1)[source]

Linear limb darkening.

Parameters

mndarray, float: The normalized radial coordinate.
c1float: The limb darkening coefficient.

Returns

ndarray, float: The relative intensity of the star at each position m.

eureka.S5_lightcurve_fitting.limb_darkening_fit.logarithmic(m, c1, c2)[source]

Logarithmic limb darkening.

Parameters

mndarray, float: The normalized radial coordinate.
c1float: The first limb darkening coefficient.
c2float: The second limb darkening coefficient.

Returns

ndarray, float: The relative intensity of the star at each position m.

eureka.S5_lightcurve_fitting.limb_darkening_fit.quadratic(m, c1, c2)[source]

Quadratic limb darkening.

Parameters

mndarray, float: The normalized radial coordinate.
c1float: The first limb darkening coefficient.
c2float: The second limb darkening coefficient.

Returns

ndarray, float: The relative intensity of the star at each position m.

eureka.S5_lightcurve_fitting.limb_darkening_fit.square_root(m, c1, c2)[source]

Squareroot limb darkening.

Parameters

mndarray, float: The normalized radial coordinate.
c1float: The first limb darkening coefficient.
c2float: The second limb darkening coefficient.

Returns

ndarray, float: The relative intensity of the star at each position m.

eureka.S5_lightcurve_fitting.limb_darkening_fit.three_parameter(m, c1, c2, c3)[source]

3-parameter limb darkening.

Parameters

mndarray, float: The normalized radial coordinate.
c1float: The first limb darkening coefficient.
c2float: The second limb darkening coefficient.
c3float: The third limb darkening coefficient.

Returns

ndarray, float: The relative intensity of the star at each position m.

eureka.S5_lightcurve_fitting.limb_darkening_fit.uniform(m)[source]

Uniform limb darkening.

Parameters

mndarray, float: The normalized radial coordinate.

Returns

ndarray, float: The relative intensity of the star at each position m.

S5_lightcurve_fitting.modelgrid

A module for creating and managing grids of model spectra

class eureka.S5_lightcurve_fitting.modelgrid.ModelGrid(model_directory, bibcode='2013A & A...553A...6H', names={'FeH': 'PHXM_H', 'Lbol': 'PHXLUM', 'Teff': 'PHXTEFF', 'logg': 'PHXLOGG', 'mass': 'PHXMASS'}, resolution=None, wave_units=Unit('um'), **kwargs)[source]

Bases: object

Creates a ModelGrid object which contains a multi-parameter grid of model spectra and its references

Parameters

pathstr: The path to the directory of FITS files used to create the ModelGrid
refslist, str: The references for the data contained in the ModelGrid
teff_rngtuple: The range of effective temperatures [K]
logg_rngtuple: The range of surface gravities [dex]
FeH_rngtuple: The range of metalicities [dex]
wave_rngarray-like: The wavelength range of the models [um]
n_binsint: The number of bins for the ModelGrid wavelength array
dataastropy.table.Table: The table of parameters for the ModelGrid
inv_filestr: An inventory file to more quickly load the database

Methods

`customize`([Teff_rng, logg_rng, FeH_rng, ...])	Trims the model grid by the given ranges in effective temperature, surface gravity, and metallicity.
`export`(filepath, **kwargs)	Export the model with the given parameters to a FITS file at the given filepath.
`get`(Teff, logg, FeH[, resolution, interp])	Retrieve the wavelength, flux, and effective radius for the spectrum of the given parameters
`grid_interp`(Teff, logg, FeH[, plot])	Interpolate the grid to the desired parameters
`info`()	Print a table of info about the current ModelGrid
`load_flux`([reset])	Retrieve the flux arrays for all models and load into the ModelGrid.array attribute with shape (Teff, logg, FeH, mu, wavelength)
`reset`()	Reset the current grid to the original state
`set_units`([wave_units])	Set the wavelength and flux units

customize(Teff_rng=(2300, 8000), logg_rng=(0, 6), FeH_rng=(-2, 1), wave_rng=(<Quantity 0. um>, <Quantity 40. um>), n_bins='')[source]

Trims the model grid by the given ranges in effective temperature, surface gravity, and metallicity. Also sets the wavelength range and number of bins for retrieved model spectra.

Parameters

Teff_rngarray-like; optional: The lower and upper inclusive bounds for the effective temperature (K). Defaults to (2300, 8000).
logg_rngarray-like; optional: The lower and upper inclusive bounds for the logarithm of the surface gravity (dex). Defaults to (0, 6).
FeH_rngarray-like; optional: The lower and upper inclusive bounds for the logarithm of the ratio of the metallicity and solar metallicity (dex). Defaults to (-2, 1).
wave_rngarray-like; optional: The lower and upper inclusive bounds for the wavelength (microns). Defaults to (0*q.um, 40*q.um).
n_binsint; optional: The number of bins for the wavelength axis. Defaults to ‘’.

export(filepath, **kwargs)[source]

Export the model with the given parameters to a FITS file at the given filepath.

Parameters

filepathstr: The path to the target FITS file.
**kwargsdict: Additional parameters to pass to self.get().

get(Teff, logg, FeH, resolution=None, interp=True)[source]

Retrieve the wavelength, flux, and effective radius for the spectrum of the given parameters

Parameters

Teffint: The effective temperature (K)
loggfloat: The logarithm of the surface gravity (dex)
FeHfloat: The logarithm of the ratio of the metallicity and solar metallicity (dex)
resolutionint; optional: The desired wavelength resolution (lambda/d_lambda). Defaults to None.
interpbool; optional: Interpolate the model if possible. Defaults to True.

Returns

spec_dictdict: A dictionary of arrays of the wavelength, flux, and mu values and the effective radius for the given model

grid_interp(Teff, logg, FeH, plot=False)[source]

Interpolate the grid to the desired parameters

Parameters

Teffint: The effective temperature (K)
loggfloat: The logarithm of the surface gravity (dex)
FeHfloat: The logarithm of the ratio of the metallicity and solar metallicity (dex)
plotbool; optional: Plot the interpolated spectrum along with the 8 neighboring grid spectra. Defaults to False.

Returns

grid_pointdict: A dictionary of arrays of the wavelength, flux, and mu values and the effective radius for the given model

info()[source]: Print a table of info about the current ModelGrid

load_flux(reset=False)[source]

Retrieve the flux arrays for all models and load into the ModelGrid.array attribute with shape (Teff, logg, FeH, mu, wavelength)

Parameters

resetbool; optional: Delete the old file and clear the flux attribute. Defaults to False.

reset()[source]: Reset the current grid to the original state

set_units(wave_units=Unit('um'))[source]

Set the wavelength and flux units

Parameters

wave_unitsstr, astropy.units.core.PrefixUnit/CompositeUnit; optional: The wavelength units. Defaults to astropy.units.um.

S5_lightcurve_fitting.plots_s5

eureka.S5_lightcurve_fitting.plots_s5.plot_GP_components(lc, model, meta, fitter, isTitle=True)[source]

Plot the lightcurve + GP model + residuals (Figs 5102)

Parameters

lceureka.S5_lightcurve_fitting.lightcurve.LightCurve: The lightcurve data object.
modeleureka.S5_lightcurve_fitting.models.CompositeModel: The fitted composite model.
metaeureka.lib.readECF.MetaClass: The metadata object.
fitterstr: The name of the fitter (for plot filename).
isTitlebool; optional: Should figure have a title. Defaults to True.

Notes

History:

February 28, 2022 Eva-Maria Ahrer
Written function
March 9, 2022 Eva-Maria Ahrer
Adapted with shared parameters

eureka.S5_lightcurve_fitting.plots_s5.plot_chain(samples, lc, meta, freenames, fitter='emcee', burnin=False, nburn=0, nrows=3, ncols=4, nthin=1)[source]

Plot the evolution of the chain to look for temporal trends. (Figs 5303)

Parameters

samplesndarray: The samples produced by the sampling algorithm.
lceureka.S5_lightcurve_fitting.lightcurve.LightCurve: The lightcurve data object.
metaeureka.lib.readECF.MetaClass: The metadata object.
freenamesiterable: The names of the fitted parameters.
fitterstr; optional: The name of the fitter (for plot filename). Defaults to ‘emcee’.
burninbool; optional: Whether or not the samples include the burnin phase. Defaults to False.
nburnint; optional: The number of burn-in steps that are discarded later. Defaults to 0.
nrowsint; optional: The number of rows to make per figure. Defaults to 3.
ncolsint; optional: The number of columns to make per figure. Defaults to 4.
nthinint; optional: If >1, the plot will use every nthin point to help speed up computation and reduce clutter on the plot. Defaults to 1.

Notes

History:

December 29, 2021 Taylor Bell
Moved plotting code to a separate function.

eureka.S5_lightcurve_fitting.plots_s5.plot_corner(samples, lc, meta, freenames, fitter)[source]

Plot a corner plot. (Figs 5501)

Parameters

samplesndarray: The samples produced by the sampling algorithm.
lceureka.S5_lightcurve_fitting.lightcurve.LightCurve: The lightcurve data object.
freenamesiterable: The names of the fitted parameters.
metaeureka.lib.readECF.MetaClass: The metadata object.
fitterstr: The name of the fitter (for plot filename).

Notes

History:

December 29, 2021 Taylor Bell
Moved plotting code to a separate function.

eureka.S5_lightcurve_fitting.plots_s5.plot_fit(lc, model, meta, fitter, isTitle=True)[source]

Plot the fitted model over the data. (Figs 5101)

Parameters

lceureka.S5_lightcurve_fitting.lightcurve.LightCurve: The lightcurve data object.
modeleureka.S5_lightcurve_fitting.models.CompositeModel: The fitted composite model.
metaeureka.lib.readECF.MetaClass: The metadata object.
fitterstr: The name of the fitter (for plot filename).
isTitlebool; optional: Should figure have a title. Defaults to True.

Notes

History:

December 29, 2021 Taylor Bell
Moved plotting code to a separate function.
January 7-22, 2022 Megan Mansfield
Adding ability to do a single shared fit across all channels
February 28-March 1, 2022 Caroline Piaulet
Adding scatter_ppm parameter

eureka.S5_lightcurve_fitting.plots_s5.plot_res_distr(lc, model, meta, fitter)[source]

Plot the normalized distribution of residuals + a Gaussian. (Fig 5302)

Parameters

lceureka.S5_lightcurve_fitting.lightcurve.LightCurve: The lightcurve data object.
modeleureka.S5_lightcurve_fitting.models.CompositeModel: The fitted composite model.
metaeureka.lib.readECF.MetaClass: The metadata object.
fitterstr: The name of the fitter (for plot filename).

Notes

History:

February 18, 2022 Caroline Piaulet
Created function

eureka.S5_lightcurve_fitting.plots_s5.plot_rms(lc, model, meta, fitter)[source]

Plot an Allan plot to look for red noise. (Figs 5301)

Parameters

lceureka.S5_lightcurve_fitting.lightcurve.LightCurve: The lightcurve data object.
modeleureka.S5_lightcurve_fitting.models.CompositeModel: The fitted composite model.
metaeureka.lib.readECF.MetaClass: The metadata object.
fitterstr: The name of the fitter (for plot filename).

Notes

History:

December 29, 2021 Taylor Bell
Moved plotting code to a separate function.
January 7-22, 2022 Megan Mansfield
Adding ability to do a single shared fit across all channels

S5_lightcurve_fitting.s5_fit

eureka.S5_lightcurve_fitting.s5_fit.fit_channel(meta, lc, time, flux, chan, flux_err, eventlabel, params, log, longparamlist, time_units, paramtitles, chanrng, ldcoeffs, white=False)[source]

Run a fit for one channel or perform a shared fit.

Parameters

metaeureka.lib.readECF.MetaClass: The metadata object.
lcXarray Dataset: The light curve object.
timendarray: The time array.
fluxndarray: The flux array.
chanint: The current channel number.
flux_errndarray: The uncertainty on each data point.
eventlabelstr: The unique identifier for this analysis.
paramseureka.lib.readEPF.Parameters: The Parameters object containing the fitted parameters and their priors.
loglogedit.Logedit: The current log in which to output messages from this current stage.
longparamlistlist: The long list of all parameters relevant to this fit.
time_unitsstr: The units of the time array.
paramtitleslist: The names of the fitted parameters.
chanrngint: The number of fitted channels.
ldcoeffslist: Limb-darkening coefficients if used from Stage 4, otherwise None.
whitebool; optional: Is this a white-light fit? Defaults to False.

Returns

metaeureka.lib.readECF.MetaClass: The updated metadata object.

eureka.S5_lightcurve_fitting.s5_fit.fitlc(eventlabel, ecf_path=None, s4_meta=None)[source]

Fits 1D spectra with various models and fitters.

Parameters

eventlabelstr: The unique identifier for these data.
ecf_pathstr; optional: The absolute or relative path to where ecfs are stored. Defaults to None which resolves to ‘./’.
s4_metaeureka.lib.readECF.MetaClass; optional: The metadata object from Eureka!’s S4 step (if running S4 and S5 sequentially). Defaults to None.

Returns

metaeureka.lib.readECF.MetaClass: The metadata object with attributes added by S5.

Notes

History:

November 12-December 15, 2021 Megan Mansfield
Original version
December 17-20, 2021 Megan Mansfield
Connecting S5 to S4 outputs
December 17-20, 2021 Taylor Bell
Increasing connectedness of S5 and S4
January 7-22, 2022 Megan Mansfield
Adding ability to do a single shared fit across all channels
January - February, 2022 Eva-Maria Ahrer
Adding GP functionality
April 2022 Kevin Stevenson
Enabled Astraeus

eureka.S5_lightcurve_fitting.s5_fit.load_specific_s4_meta_info(meta)[source]

Load the specific S4 MetaClass object used to make this aperture pair.

Parameters

metaeureka.lib.readECF.MetaClass: The current metadata object.

Returns

eureka.lib.readECF.MetaClass: The current metadata object with values from the old MetaClass.

eureka.S5_lightcurve_fitting.s5_fit.make_longparamlist(meta, params, chanrng)[source]

Make a long list of all relevant parameters.

Parameters

metaeureka.lib.readECF.MetaClass: The current metadata object.
paramseureka.lib.readEPF.Parameters: The Parameters object containing the fitted parameters and their priors.
chanrngint: The number of fitted channels.

Returns

longparamlistlist: The long list of all parameters relevant to this fit.
paramtitleslist: The names of the fitted parameters.

S5_lightcurve_fitting.simulations

eureka.S5_lightcurve_fitting.simulations.simulate_lightcurve(target, snr=1000.0, npts=1000, nbins=10, radius=None, ldcs=('quadratic', [0.1, 0.1]), plot=False)[source]

Simulate lightcurve data for the given target exoplanet

Parameters

targetstr: The name of the target to simulate.
snrfloat; optional: The signal to noise to use. Defaults to 1000.
nptsint; optional: The number of points in each lightcurve. Defaults to 1000.
nbinsint; optional: The number of lightcurves. Defaults to 10.
radiusarray-like, float; optional: The radius or radii value(s) to use. Defaults to None which will use the literature Rp/Rs value if found or 0.1 if not.
ldcssequence; optional: The limb darkening profile name and coefficients. Defaults to (‘quadratic’, [0.1, 0.1]).
plotbool; optional: If True, plot the figure. Defaults to False.

Returns

tuple: The time, flux, uncertainty, and transit parameters

S5_lightcurve_fitting.utils

A module for utility funtions

eureka.S5_lightcurve_fitting.utils.build_target_url(target_name)[source]

Build restful api url based on target name.

Parameters

target_namestr: The name of the target transit.

Returns

target_urlstr

eureka.S5_lightcurve_fitting.utils.calc_zoom(R_f, arr)[source]

Calculate the zoom factor required to make the given array into the given resolution.

Parameters

R_fint: The desired final resolution of the wavelength array.
arrarray-like: The array to zoom.

Returns

zfloat: The zoom factor

eureka.S5_lightcurve_fitting.utils.color_gen(colormap='viridis', key=None, n=10)[source]

Color generator for Bokeh plots.

Parameters

colormapstr, sequence: The name of the color map.
keystr; optional: The palette key. Defaults to None which uses the first palette key.
nint; optional: If palette is callable, the argument to that function. Defaults to 10.

Returns

generator: A generator for the color palette.

eureka.S5_lightcurve_fitting.utils.download_exoctk_data(download_location='/home/docs')[source]

Retrieves the exoctk_data materials from Box, downloads them to the user’s local machine, uncompresses the files, and arranges them into an exoctk_data directory.

Parameters

download_locationstr; optional: The path to where the ExoCTK data package will be downloaded. The default setting is the user’s $HOME directory.

eureka.S5_lightcurve_fitting.utils.filter_table(table, **kwargs)[source]

Retrieve the filtered rows.

Parameters

tableastropy.table.Table, pandas.DataFrame

The table to filter.

**kwargsdict

paramstr: The parameter to filter by, e.g. ‘Teff’.
valuestr, float, int, sequence: The criteria to filter by, which can be single valued like 1400 or a range with operators [<,<=,>,>=], e.g. (‘>1200’,’<=1400’).

Returns

astropy.table.Table, pandas.DataFrame: The filtered table.

eureka.S5_lightcurve_fitting.utils.find_closest(axes, points, n=1, values=False)[source]

Find the n-neighboring elements of a given value in an array.

Parameters

axeslist, np.array: The array(s) to search.
pointsarray-like, float: The point(s) to search for.
nint; optional: The number of values to the left and right of the points. Defaults to 1.
valuesbool; optional: Defaults to False.

Returns

np.ndarray: The n-values to the left and right of ‘points’ in ‘axes’.

eureka.S5_lightcurve_fitting.utils.get_canonical_name(target_name)[source]

Get ExoMAST prefered name for exoplanet.

Parameters

target_namestr: The name of the target transit.

Returns

canonical_namestr

eureka.S5_lightcurve_fitting.utils.get_env_variables()[source]

Returns a dictionary containing various environment variable information.

Returns

env_variablesdict: A dictionary containing various environment variable data

eureka.S5_lightcurve_fitting.utils.get_target_data(target_name)[source]

Send request to exomast restful api for target information.

Parameters

target_namestr: The name of the target transit

Returns

target_datajson: json object with target data.

eureka.S5_lightcurve_fitting.utils.interp_flux(mu, flux, params, values)[source]

Interpolate a cube of synthetic spectra for a given index of mu.

Parameters

muint: The index of the (Teff, logg, FeH, mu, wavelength) data cube to interpolate.
fluxnp.ndarray: The 5D data array.
paramslist: A list of each free parameter range.
valueslist: A list of each free parameter values.

Returns

tuple: The array of new flux values, and the generators.

eureka.S5_lightcurve_fitting.utils.rebin_spec(spec, wavnew, oversamp=100, plot=False)[source]

Rebin a spectrum to a new wavelength array while preserving the total flux.

Parameters

specarray-like: The wavelength and flux to be binned.
wavenewarray-like: The new wavelength array.
oversampint; optional: The oversampling factor. Defaults to 100.
plotbool; optional: Unused. Defaults to False.

Returns

np.ndarray: The rebinned flux

eureka.S5_lightcurve_fitting.utils.writeFITS(filename, extensions, headers=())[source]

Write some data to a new FITS file.

Parameters

filenamestr: The filename of the output FITS file.
extensionsdict: The extension name and associated data to include. in the file
headersarray-like; optional: The (keyword, value, comment) groups for the PRIMARY header extension. Defaults to ().

S6_planet_spectra

S6_planet_spectra.plots_s6

eureka.S6_planet_spectra.plots_s6.plot_spectrum(meta, model_x=None, model_y=None, y_scalar=1, ylabel='$R_{\\rm p}/R_{\\rm *}$', xlabel='Wavelength ($\\mu$m)', scaleHeight=None, planet_R0=None)[source]

Plot the planetary transmission or emission spectrum.

Parameters

metaeureka.lib.readECF.MetaClass: The meta data object.
model_xndarray; optional: The wavelength array for the model to plot, by default None
model_yndarray; optional: The transmission or emission spectrum from the model, by default None
y_scalarint; optional: The multiplier for the y-axis (100=%, 1e6=ppm), by default 1
ylabelstr; optional: The y-axis label, by default r’{rm p}/R_{rm *}$’
xlabelstr; optional: The x-axis label, by default r’Wavelength ($mu)’
scaleHeightfloat; optional: The planetary atmospheric scale height, by default None
planet_R0float; optional: The reference radius for the scale height, by default None

S6_planet_spectra.s6_spectra

eureka.S6_planet_spectra.s6_spectra.compute_scale_height(meta, log)[source]

Compute the atmospheric scale height for a planet.

Parameters

metaeureka.lib.readECF.MetaClass: The current meta data object.
loglogedit.Logedit: The open log in which notes from this step can be added.

Returns

metaeureka.lib.readECF.MetaClass: The updated meta data object.

eureka.S6_planet_spectra.s6_spectra.compute_timescale(meta)[source]

Convert the fitted r1 or r4 value to a timescale.

Parameters

metaeureka.lib.readECF.MetaClass: The current meta data object.

Returns

metaeureka.lib.readECF.MetaClass: The updated meta data object.

eureka.S6_planet_spectra.s6_spectra.compute_transit_depth(meta)[source]

Convert the fitted rp values to transit depth.

Parameters

metaeureka.lib.readECF.MetaClass: The current meta data object.

Returns

metaeureka.lib.readECF.MetaClass: The updated meta data object.

eureka.S6_planet_spectra.s6_spectra.load_model(meta, log, x_unit)[source]

Load in a model to plot above/below the fitted data.

Parameters

metaeureka.lib.readECF.MetaClass: The current meta data object.
loglogedit.Logedit: The open log in which notes from this step can be added.
x_unitstr: The astropy.units unit that will be used in the plot.

Returns

metaeureka.lib.readECF.MetaClass: The updated meta data object.

Raises

AssertionError: Unknown conversion between y_param and model_y_param.

eureka.S6_planet_spectra.s6_spectra.load_specific_s5_meta_info(meta)[source]

Load in the MetaClass object from the particular aperture pair being used.

Parameters

metaeureka.lib.readECF.MetaClass: The current meta data object.

Returns

metaeureka.lib.readECF.MetaClass: The current meta data object with values from earlier stages.

eureka.S6_planet_spectra.s6_spectra.parse_s5_saves(meta, log, fit_methods, channel_key='shared')[source]

Load in an S5 save file.

Parameters

metaeureka.lib.readECF.MetaClass: The current meta data object.
loglogedit.Logedit: The open log in which notes from this step can be added.
fit_methodslist: The fitting methods used in S5.
channel_keystr; optional: A string describing the current channel (e.g. ch0), by default ‘shared’.

Returns

medians: The best-fit values from S5.
errs: The uncertainties from a sampling algorithm like dynesty or emcee.

eureka.S6_planet_spectra.s6_spectra.parse_unshared_saves(meta, log, fit_methods)[source]

Load in the many S5 save files for an unshared fit.

Parameters

metaeureka.lib.readECF.MetaClass: The current meta data object.
loglogedit.Logedit: The open log in which notes from this step can be added.
fit_methodslist: The fitting methods used in S5.

Returns

metaeureka.lib.readECF.MetaClass: The updated meta data object.

eureka.S6_planet_spectra.s6_spectra.plot_spectra(eventlabel, ecf_path=None, s5_meta=None)[source]

Gathers together different wavelength fits and makes transmission/emission spectra.

Parameters

eventlabelstr: The unique identifier for these data.
ecf_pathstr; optional: The absolute or relative path to where ecfs are stored. Defaults to None which resolves to ‘./’.
s5_metaeureka.lib.readECF.MetaClass; optional: The metadata object from Eureka!’s S5 step (if running S5 and S6 sequentially). Defaults to None.

Returns

metaeureka.lib.readECF.MetaClass: The metadata object with attributes added by S6.

Notes

History:

Feb 14, 2022 Taylor Bell
Original version

eureka.S6_planet_spectra.s6_spectra.roundToDec(x, nDec=2)[source]

Round a value to a requested number of decimals.

Parameters

xnumerical type: A float or int to be rounded.
nDecint: The number of decimals desired, by default 2.

Returns

outputstr: x formatted as a string with the requested number of decimals.

Notes

History:

2022-08-22, Taylor J Bell
Imported code written for SPCA, and optimized for Python3.

eureka.S6_planet_spectra.s6_spectra.roundToSigFigs(x, sigFigs=2)[source]

Round a value to a requested number of significant figures.

Parameters

xnumerical type: A float or int to be rounded.
sigFigsint; optional: The number of significant figures desired, by default 2.

Returns

nDecint: The number of decimals corresponding to sigFigs where nDec = -1 for a value rounded to the ten’s place (e.g. 101 -> 100 if nDec = -1).
outputstr: x formatted as a string with the requested number of significant figures.

Notes

History:

2022-08-22, Taylor J Bell
Imported code written for SPCA, and optimized for Python3.

eureka.S6_planet_spectra.s6_spectra.save_table(meta, log)[source]

Clean y_param for filenames and save the table of values.

Also calls transit_latex_table().

Parameters

metaeureka.lib.readECF.MetaClass: The current meta data object.
loglogedit.Logedit: The open log in which notes from this step can be added.

eureka.S6_planet_spectra.s6_spectra.transit_latex_table(meta, log)[source]

Write a nicely formatted LaTeX table for each plotted value.

Parameters

metaeureka.lib.readECF.MetaClass: The current meta data object.
loglogedit.Logedit: The open log in which notes from this step can be added.

lib

lib.apphot

eureka.lib.apphot.apphot(meta, image, ctr, photap, skyin, skyout, betahw, targpos, mask=None, imerr=None, skyfrac=0.0, med=False, nochecks=False, expand=1, order=1, aperr=False, nappix=False, skylev=False, skyerr=False, nskypix=False, nskyideal=False, status=False, isbeta=False, betaper=False)[source]

Perform aperture photometry on the input image.

Parameters

image2D ndimage: Float array containing object to measure.
ctr2 elements tuple: x,y location of object’s center.
photapScalar: Size of photometry apperture in pixels.
skyinScalar: Inner sky annulus edge, in pixels.
skyoutScalar: Outer sky annulus edge, in pixels.
betahwScalar: Half-width of box size around centroid for beta calculation.
targpos2 elements tuple: x,y location of object’s center calculated from mean image.
mask2D ndimage: Byte array giving status of corresponding pixel in Image: bad pixel=0, good pixel=1. Default: all pixels are good. Same shape as image.
imerr2D ndimage: Error estimate for each pixel in the image. Suggest sqrt(image/flat/gain+rdnoise^2), with proper adjustment if a sky, dark, or bias frame has been removed. Same shape as image.
skyfracScalar: Minimum fraction of sky pixels required to be good. Must be in range 0 < skyfrac < 1.
medBoolean: If True use median rather than mean in sky level estimation.
nochecksBoolean: Set to True to skip checks of input sanity.
expandInteger scalar: Positive integer factor by which to blow up image, for more accurate aperture arithmetic. If expand=5, each pixel becomes a 5x5 block of pixels. If the pixel is on the edge of an aperture or annulus radius, some of the 5x5 block will be counted and some will not.
orderInteger scalar: Set order to 0 to do nearest-neighbor interpolation if expand. Default: 1, bilinear interpolation.
aperrBoolean: Set to True to return flux error.
nappixBoolean: Set to True to return number of total pixels in aperture.
skylevBoolean: Set to True to return the sky level.
skyerrBoolean: Set to True to return the error in the sky level.
nskypixboolean: Set to True to return the number of good pixels in sky annulus.
nskyideal: Boolean: Set to True to return the number of pixels that should be in sky annulus.
statusBoolean: Set to True to return a status flag. If status = 0, result is good. Bits: 0 = there are NaN(s) in the photometry aperture 1 = there are masked pixel(s) in the photometry aperture 2 = the aperture is off the edge of the image 3 = a fraction less than skyfrac of the sky annulus pixels is in the image and not masked
isbetaboolean: If True photometric extraction aperture scales with noise pixel parameter (beta).
betaperScalar: Returns aperture size used for beta.

Returns

This function returns the flux within Photap pixels of
[Cx,Cy], after subtracting the average per-pixel flux in the
sky annulus. See POCEDURE for details of the calculation.

Notes

The sky level is the mean, error-weighted mean (if errors are present), or median (if /med is set) of the non-masked Image pixels in the sky annulus. NaN values and values whose errors are zero (for the error-weighted mean) are not included in the average. No flagging is done if these values are found in the sky annulus. SKYERR is the error in the mean, even for the median calculation. Errors in the median can only be estimated using the compute-intensive bootstrap Monte-Carlo method.

The sky value is subtracted from the Image. The photometric flux is then the total of Image pixels in the aperture, whether in the Mask or not. NaN values are not included in the calculation, and set the STATUS flag. It would be much better for the user to pass an interpolated image instead.

For expansion, it is recommended to use bilinear interpolation, which is flux-conserving:

sz = [50, 50] expand = 4 a = dblarr(sz) a[25, 25] = 1 b = rebin(a, expand * sz) / expand^2 print, total(b) 1.0000000 a[25, 26] = 1 b = rebin(a, expand * sz) / expand^2 print, total(b) 2.0000000 a[26, 26] = 3 b = rebin(a, expand * sz) / expand^2 print, total(b) 5.0000000

Of course, pixels on the high-indexed edge will not follow that. Neither will integer-arithmetic images, particularly at low integer values (such as masks).

If either the entire sky annulus or the entire aperture is bad or filled with NaNs, the function sets a flag and returns NaN for all incalculable values.

History:

27-02-2004: Joseph Harrington, Cornell. jh@oobleck.astro.cornell.edu
Initial version
18-03-2004: jh
Added nochecks keyword.
19-03-2004: jh
Added error calculation.
13-01-2005: jh
Fixed header comment. Added NAN keyword.
14-10-2005: jh
Found and fixed major bug in sky mask calculation (needed parens around subtraction next to mask multiplication). Added skyfrac.
07-11-2005: shl35
Added STATUS keyword, error-weighted sky mean.
16-11-2005: jh
Rewrote, using meanerr. Fixed major bug in error calc. Added scaling and test cases.
24-11-2005: jh
Return NAPPIX, NSKYPIX, NSKYIDEAL (all renamed).
30-11-2005: jh
Changed NAPPIX, NSKYPIX, NSKYIDEAL to give fractional, unexpanded pixels.
21-07-2010: patricio
Converted to python.

Examples

This being one of my most important routines, and being also complex, the following examples are also its test suite. Any changes should produce exactly the same numerical results. These tests should also be available in the accompanying file apphottest.pro.

eureka.lib.apphot.apphot_status(data)[source]

Prints a warning if aperture step had errors. Bit flag definitions from the apphot function:

statnan = 2 ** 0

statbad = 2 ** 1

statap = 2 ** 2

statsky = 2 ** 3

E.g., If the flag is 6 then is was created by a flag in

statap and statbad as 2 ** 2 + 2 ** 1 = 6.

This function is converting the flags back to binary

and checking which flags were triggered.

Parameters

dataXarray Dataset: The Dataset object.

lib.astropytable

eureka.lib.astropytable.readtable(filename)[source]

Read in a saved ECSV file.

Parameters

filenamestr: The fully qualified filename of the file to read.

Returns

astropy.table.QTable: The table previously saved by savetable_S5 or savetable_S6.

eureka.lib.astropytable.savetable_S5(filename, time, wavelength, bin_width, lcdata, lcerr, model, residuals)[source]

Save the results from Stage 5 as an ECSV file.

Parameters

filenamestr: The fully qualified filename that the results will be stored in.
timendarray (1D): The times for each data point.
wavelengthndarray (1D): The wavelengths of each data point.
bin_widthndarray (1D): The width of each wavelength bin.
lcdatandarray (1D): The normalized flux measurements for each data point.
lcerrndarray (1D): The normalized uncertainties for each data point.
modelndarray (1D): The predicted values from the fitted model.
residualsndarray (1D): The residuals from lcdata - model.

Raises

ValueError: There was a shape mismatch between your arrays

eureka.lib.astropytable.savetable_S6(filename, key, wavelength, bin_width, value, error)[source]

Save the results from Stage 6 as an ECSV.

Parameters

filenamestr: The fully qualified filename that the results will be stored in.
keystr: The parameter being saved.
wavelengthndarray (1D): The wavelengths of each data point.
bin_widthndarray (1D): The width of each wavelength bin.
valuendarray (1D): The fitted value at each wavelength.
errorndarray (1D): The uncertainty on each value.

Raises

ValueError: There was a shape mismatch between your arrays

lib.centerdriver

eureka.lib.centerdriver.centerdriver(method, data, guess, trim, radius, size, mask=None, uncd=None, fitbg=1, maskstar=True, expand=5.0, psf=None, psfctr=None, i=None, m=None, meta=None)[source]

Use the center method to find the center of a star in data, starting from position guess.

Parameters

method: string: Name of the centering method to use.
data: 2D ndarray: Array containing the star image.
guess: 2 elements 1D array: y, x initial guess position of the target.
trim: integer: Semi-lenght of the box around the target that will be trimmed.
radius: float: least asymmetry parameter. See err_fasym_c.
size: float: least asymmetry parameter. See err_fasym_c.
mask: 2D ndarray: A mask array of bad pixels. Same shape of data.
uncd: 2D ndarray: An array containing the uncertainty values of data. Same shape of data.

Returns

A y,x tuple (scalars) with the coordinates of center of the target
in data.

Notes

History:

23-11-2010 patricio Written by Patricio Cubillos: pcubillos@fulbrightmail.org

lib.centroid

eureka.lib.centroid.ctrgauss(data, guess=None, mask=None, indarr=None, trim=None)[source]

Finds and records the stellar centroid of a set of images by fitting a two dimensional Gaussian function to the data.

It does not find the average centroid, but instead records the centroid of each image in the supplied frame parameters array at the supplied indices. The frame parameters array is assumed to have the same number of rows as the number of frames in the data cube.

Parameters

datandarray (2D): The stellar image.
guessarray_like: The initial guess of the position of the star. Has the form (y, x) of the guess center.
maskndarray (2D): The stellar image.
indarrarray_like: The indices of the x and y center columns of the frame parameters and the width index. Defaults to 4, 5, and 6 respectively.
trimScalar (positive): If trim!=0, trims the image in a box of 2*trim pixels around the guess center. Must be !=0 for ‘col’ method.

Returns

centery, x: The updated frame parameters array. Contains the centers of each star in each image and their average width.

Notes

History:

2010-06-23, Patricio E. Cubillos
Adapted to POET from Chris’ routines.
2009-10-30, Christopher J. Campo
Initial version.

eureka.lib.centroid.ctrguess(data, mask=None, guess=None)[source]

Calculates crude initial guesses of parameters required for Gaussian centroiding of stellar images.

Speciffically, this function guesses the flux of the center of a star, the array indices of this location, and a rough guess of the width of the associated PSF. This method is not robust to bad pixels or any other outlying values.

Parameters

datandarray (2D): The image in the form of a 2D array containing the star to be centroided. Works best if this is a small subarray of the actual data image.
maskndarray (2D): The image in the form of a 2D array containing the star to be centroided. Works best if this is a small subarray of the actual data image.

Returns

ghtscalar: The rough estimate of the height (or max flux) of the stars PSF.
gwdtuple: The guessed width of the PSF, in the form (gwdy, gwdx) where gwdy and gwdx are the y and x widths respectively.
gcttuple: The guessed center of the PSF, in the form (gcty, gctx) where gcty and gctx are the y and x center indices respectively.

Notes

Logic adapted from gaussian.py

History:

2009-10-27, Christopher Campo
Initial Version

lib.clipping

eureka.lib.clipping.clip_outliers(data, log, wavelength, wavelength_units='microns', mask=None, sigma=10, box_width=5, maxiters=5, boundary='extend', fill_value='mask', verbose=False)[source]

Find outliers in 1D time series.

Be careful when using this function on a time-series with known astrophysical variations. The variable box_width should be set to be significantly smaller than any astrophysical variation timescales otherwise these signals may be clipped.

Parameters

datandarray (1D): The input array in which to identify outliers
loglogedit.Logedit: The open log in which notes from this step can be added.
wavelengthfloat: The wavelength currently under consideration.
wavelength_unitsfloat: The wavelength units currently under consideration.
maskndarray (1D); optional: A mask array to use if data is not a masked array. Defaults to None in which case only the invalid values of data will be masked.
sigmafloat; optional: The number of sigmas a point must be from the rolling mean to be considered an outlier. Defaults to 10.
box_widthint; optional: The width of the box-car filter (used to calculated the rolling median) in units of number of data points. Defaults to 5.
maxitersint; optional: The number of iterations of sigma clipping that should be performed. Defaults to 5.
boundarystr; optional: The boundary argument to pass to astropy.convolution.convolve. Defaults to ‘extend’.
fill_valuestr or float; optional: Either the string ‘mask’ to mask the outlier values, ‘boxcar’ to replace data with the mean from the box-car filter, or a constant float-type fill value. Defaults to ‘mask’.
verbosebool; optional: If True, log details about the outliers found at this wavelength. Defaults to False.

Returns

datandarray (1D): An array with the same dimensions as the input array with outliers replaced with fill_value.
outliersndarray (1D): A boolean array where True for values that were clipped.
noutliersint: The number of outliers identified.

Notes

History:

Jan 29-31, 2022 Taylor Bell
Initial version, added logging

eureka.lib.clipping.gauss_removal(img, mask, linspace, where='bkg')[source]

An additional step to remove cosmic rays.

This fits a Gaussian to the background (or a skewed Gaussian to the orders) and masks data points which are above a certain sigma.

Parameters

imgnp.ndarray: Single exposure image.
masknp.ndarray: An approximate mask for the orders.
linspacearray: Sets the lower and upper bin bounds for the pixel values. Should be of length = 2.
wherestr; optional: Sets where the mask is covering. Default is bkg. Other option is order.

Returns

imgnp.ndarray: The same input image, now masked for newly identified outliers.

lib.disk

eureka.lib.disk.disk(r, ctr, size, status=False)[source]

This function returns a byte array containing a disk.

The disk is centered at (ctr[0], ctr[1]), and has radius r. The array is (size[0], size[1]) in size and has byte type. Pixel values of 1 indicate that the center of a pixel is within r of (ctr[0], ctr[1]). Pixel values of 0 indicate the opposite. The center of each pixel is the integer position of that pixel.

Parameters

rfloat: The radius of the disk.
ctrtuple, list, or array: The x,y position of the center of the disk, 2-element vector.
sizetuple, list, or array: The x,y size of the output array, 2-element vector.
statusbool; optional: If True, return the status optional output.

Returns

retndarray: A boolean array where False if outside the disk or True if inside the disk.
retstatusint; optional: Set to 1 if any part of the disk is outside the image boundaries. Only returned if status==True.

Notes

History:

2003 April 4; Joseph Harrington, jh@oobleck.astro.cornell.edu
Initial version.
2004 Feb 27; jh
Added alternate input method
2005 Nov 16; jh
Added STATUS, simplified disk calculation, use double precision

lib.gaussian

eureka.lib.gaussian.fitgaussian(y, x=None, bgpars=None, fitbg=0, guess=None, mask=None, weights=None, maskg=False, yxguess=None)[source]

Fits an N-dimensional Gaussian to (value, coordinate) data.

Parameters

yndarray: Array giving the values of the function.
xndarray: (optional) Array (any shape) giving the abcissas of y (if missing, uses np.indices(y). The highest dimension must be equal to the number of other dimensions (i.e., if x has 6 dimensions, the highest dimension must have length 5). The rest of the dimensions must have the same shape as y. Must be sorted ascending (which is not checked), if guess is not given.
bgparsndarray or tuple, 3-elements: Background parameters, the elements determine a X- and Y-linearly dependant level, of the form: f = Y*bgparam[0] + X*bgparam[1] + bgparam[2] (Not tested for 1D yet).
fitbgInteger: This flag indicates the level of background fitting: fitbg=0: No fitting, estimate the bg as median(data). fitbg=1: Fit a constant to the bg (bg = c). fitbg=2: Fit a plane as bg (bg = a*x + b*y + c).
guesstuple, (width, center, height): Tuple giving an initial guess of the Gaussian parameters for the optimizer. If supplied, x and y can be any shape and need not be sorted. See gaussian() for meaning and format of this tuple.
maskndarray: Same shape as y. Values where its corresponding mask value is 0 are disregarded for the minimization. Only values where the mask value is 1 are considered.
weightsndarray: Same shape as y. This array defines weights for the minimization, for scientific data the weights should be 1/sqrt(variance).
maskgbool; optional: If true, mask the gaussian.
yxguesstuple; optional: A guess at just the centroid. Defaults to None which uses the data point with the highest value.

Returns

paramsndarray: This array contains the best fitting values parameters: width, center, height, and if requested, bgpars. with: width : The fitted Gaussian widths in each dimension. center : The fitted Gaussian center coordinate in each dimension. height : The fitted height.
errndarray: An array containing the concatenated uncertainties corresponding to the values of params. For example, 2D input gives np.array([widthyerr, widthxerr, centeryerr, centerxerr, heighterr]).

Notes

If the input does not look anything like a Gaussian, the result might not even be the best fit to that.

Method: First guess the parameters (if no guess is provided), then call a Levenberg-Marquardt optimizer to finish the job.

History:

2007-09-17 Joe jh@physics.ucf.edu
Initial version, portions adapted from http://www.scipy.org/Cookbook/FittingData.
2007-11-13 Joe
Made N-dimensional.
2008-12-02 Nate nlust@physics.ucf.edu
Included error calculation, and return Fixed a bug in which if the initial guess was None, and incorrect shape array was generated. This caused gaussian guess to fail.
2009-10-25
Converted to standard doc header, fixed examples to return 4 parameters.
2011-05-03 patricio pcubillos@fulbrightmail.org
Added mask, weights, and background-fitting options.

Examples

>>> import matplotlib.pyplot as plt
>>> import gaussian as g

>>> # parameters for X
>>> lx = -3.  # low end of range
>>> hx = 5.   # high end of range
>>> dx = 0.05 # step

>>> # parameters of the noise
>>> nc = 0.0  # noice center
>>> ns = 1.0  # noise width
>>> na = 0.2  # noise amplitude

>>> # 1D Example

>>> # parameters of the underlying Gaussian
>>> wd = 1.1  # width
>>> ct = 1.2  # center
>>> ht = 2.2  # height

>>> # x and y data to fit
>>> x  = np.arange(lx, hx + dx / 2., dx)
>>> x += na * np.random.normal(nc, ns, x.size)
>>> y  = g.gaussian(x, wd, ct, ht)+na*np.random.normal(nc, ns, x.size)
>>> s  = x.argsort()   # sort, in case noise violated order
>>> xs = x[s]
>>> ys = y[s]

>>> # calculate guess and fit
>>> (width, center, height)     = g.gaussianguess(ys, xs)
>>> (fw,    fc,     fh,    err) = g.fitgaussian(ys, xs)

>>> # plot results
>>> plt.clf()
>>> plt.plot(xs, ys)
>>> plt.plot(xs, g.gaussian(xs, wd, ct, ht))
>>> plt.plot(xs, g.gaussian(xs, width, center, height))
>>> plt.plot(xs, g.gaussian(xs, fw, fc, fh))
>>> plt.title('Gaussian Data, Guess, and Fit')
>>> plt.xlabel('Abcissa')
>>> plt.ylabel('Ordinate')
>>> # plot residuals
>>> plt.clf()
>>> plt.plot(xs, ys - g.gaussian(xs, fw, fc, fh))
>>> plt.title('Gaussian Fit Residuals')
>>> plt.xlabel('Abcissa')
>>> plt.ylabel('Ordinate')

>>> # 2D Example

>>> # parameters of the underlying Gaussian
>>> wd = (1.1, 3.2)  # width
>>> ct = (1.2, 3.1)  # center
>>> ht = 2.2         # height

>>> # x and y data to fit
>>> nx = (hx - lx) / dx + 1
>>> x  = np.indices((nx, nx)) * dx + lx
>>> y  = g.gaussian(x, wd, ct, ht) + na * np.random.normal(nc, ns,
                                                        x.shape[1:])

>>> # calculate guess and fit
>>> #(width, center, height) = g.gaussianguess(y, x) # not in 2D yet...
>>> (fw, fc, fh, err) = g.fitgaussian(y, x, (wd, ct, ht))

>>> # plot results
>>> plt.clf()
>>> plt.title('2D Gaussian Given')
>>> plt.xlabel('X')
>>> plt.ylabel('Y')
>>> plt.imshow(    g.gaussian(x, wd, ct, ht))
>>> plt.clf()
>>> plt.title('2D Gaussian With Noise')
>>> plt.xlabel('X')
>>> plt.ylabel('Y')
>>> plt.imshow(y)
>>> #plt.imshow(g.gaussian(x, width, center, height))  # not in 2D yet
>>> plt.clf()
>>> plt.title('2D Gaussian Fit')
>>> plt.xlabel('X')
>>> plt.ylabel('Y')
>>> plt.imshow(    g.gaussian(x, fw, fc, fh))
>>> plt.clf()
>>> plt.title('2D Gaussian Fit Residuals')
>>> plt.xlabel('X')
>>> plt.ylabel('Y')
>>> plt.imshow(y - g.gaussian(x, fw, fc, fh))

>>> # All cases benefit from...

>>> # show difference between fit and underlying Gaussian
>>> # Random data, your answers WILL VARY.
>>> np.array(fw) - np.array(wd)
array([ 0.00210398, -0.00937687])
>>> np.array(fc) - np.array(ct)
array([-0.00260803,  0.00555011])
>>> np.array(fh) - np.array(ht)
0.0030143371034774269

>>> # Last Example:
>>> x = np.indices((30,30))
>>> g1 = g.gaussian(x, width=(1.2, 1.15), center=(13.2,15.75),
>>>                 height=1e4, bgpars=[0.0, 0.0, 100.0])
>>> error = np.sqrt(g1) * np.random.randn(30,30)
>>> y = g1 + error
>>> var = g1

>>> plt.figure(1)
>>> plt.clf()
>>> plt.imshow(y, origin='lower_left', interpolation='nearest')
>>> plt.colorbar()
>>> plt.title('2D Gaussian')
>>> plt.xlabel('X')
>>> plt.ylabel('Y')

>>> guess = ((1.2,1.2),(13,16.),1e4)
>>> reload(g)
>>> fit = g.fitgaussian(y, x, bgpars=[0.0, 0.0, 110.], fitbg=1,
                        guess=guess, mask=None, weights=1/np.sqrt(var))
>>> print(fit[0])

eureka.lib.gaussian.fitgaussians(y, x=None, guess=None, sigma=1.0)[source]

Fit position and flux of a data image with gaussians, same sigma is applied to all directions.

Parameters

yarray_like: Array giving the values of the function.
xarray_like: (optional) Array (any shape) giving the abcissas of y (if missing, uses np.indices(y).
guess2D-tuple: [[width1, center1, height1], [width2, center2, height2], … ] Tuple giving an initial guess of the Gaussian parameters for the optimizer. If supplied, x and y can be any shape and need not be sorted. See gaussian() for meaning and format of this tuple.

eureka.lib.gaussian.gaussian(x, width=1.0, center=0.0, height=None, bgpars=[0.0, 0.0, 0.0])[source]

Evaluates the Gaussian and a background with given parameters at locations in x.

Parameters

xndarray (any shape): Abcissa values. Arranged as the output of np.indices() but may be float. The highest dimension must be equal to the number of other dimensions (i.e., if x has 6 dimensions, the highest dimension must have length 5, and each of those must give the coordinate along the respective axis). May also be 1-dimensional. Default: np.indices(y.shape).
widtharray_like; optional: The width of the Gaussian function, sometimes called sigma. If scalar, assumed constant for all dimensions. If array, must be linear and the same length as the first dimension of x. In this case, each element gives the width of the function in the corresponding dimension. Defaults to 1.0.
centerarray_like; optional: The mean value of the Gaussian function, sometimes called x0. Same scalar/array behavior as width. Defaults to 0.0.
heightscalar; optional: The height of the Gaussian at its center. If not set, initialized to the value that makes the Gaussian integrate to 1. If you want it to integrate to another number, leave height alone and multiply the result by that other number instead. Must be scalar. Defaults to None which resolves to [product(1./sqrt(2 * pi * width**2))].
bgparsndarray or tuple, 3-element; optional: Background parameters, the elements determine a X- and Y-linearly dependant level, of the form: f = Y*bgparam[0] + X*bgparam[1] + bgparam[2] (Not tested for 1D yet). Defaults to [0.0, 0.0, 0.0].

Returns

resultsndarray: Same shape as x (or first element of x if multidimensional) This function returns the Gaussian function of the given width(s), center(s), and height applied to its input plus a linear background level. The Gaussian function is: f(x) = 1./sqrt(2 * pi * width**2) * exp(-0.5 * ((x - center) / width)**2). It is defined in multiple dimensions as the product of orthogonal, single-dimension Gaussians.

Notes

History:

2007-09-17 0.1 jh@physics.ucf.edu
Initial version.
2007-10-02 0.2 jh@physics.ucf.edu
Started making N-dimensional, put width before center in args.
2007-11-13 0.3 jh@physics.ucf.edu
Fixed docs, bugs, added param, made N-dimensional.
2009-10-01 0.4 jh@physics.ucf.edu
Fixed docs.
2009-10-25 0.5 jh@physics.ucf.edu
Added examples and plot labels.
2011-05-03 patricio
Params option no longer sopported, Added bgpars to add a background.
2017-XX-XX bbrooks@stsci.edu
Added Patricio centering method.

Examples

>>> import matplotlib.pyplot as plt
>>> import gaussian as g

>>> x = np.arange(-10., 10.005, 0.01)
>>> plt.plot(x, g.gaussian(x))
>>> plt.title('Gaussian')
>>> plt.xlabel('Abcissa')
>>> plt.ylabel('Ordinate')

>>> # use an array [3] as a single parameter vector
>>> z = np.array([2., 2, 3])
>>> plt.plot(x, g.gaussian(x, *z))

>>> # Test that it integrates to 1.
>>> a = np.indices([100, 100]) - 50
>>> print(np.sum(g.gaussian(a, 3, 3)))
0.999999999999997
>>> print(np.sum(g.gaussian(a, np.array([1,2]), np.array([2,3]))))
1.0000000107

>>> plt.clf()
>>> plt.imshow(g.gaussian(a, [3,5], [7,3]))
>>> plt.title('2D Gaussian')
>>> plt.xlabel('X')
>>> plt.ylabel('Y')

>>> A gaussian + a linear background level:
>>> g2 = g.gaussian(x, width=(1.2, 1.15), center=(13.2,15.75),
>>>                 height=4.3, bgpars=[0.05, 0.01, 1.0])
>>> plt.figure(1)
>>> plt.clf()
>>> plt.imshow(g2, origin='lower_left', interpolation='nearest')
>>> plt.colorbar()
>>> plt.title('2D Gaussian')
>>> plt.xlabel('X')
>>> plt.ylabel('Y')

>>> plt.figure(2)
>>> plt.clf()
>>> plt.plot(g2[13,:])
>>> plt.title('X slice of 2D Gaussian')
>>> plt.xlabel('X')
>>> plt.ylabel('Z')

>>> plt.figure(3)
>>> plt.clf()
>>> plt.plot(g2[:,16])
>>> plt.title('Y slice of 2D Gaussian')
>>> plt.xlabel('Y')
>>> plt.ylabel('Z')

eureka.lib.gaussian.gaussianguess(data, mask=None, yxguess=None)[source]

Used by fitgaussian to get an initial guess at the parameters for a Gaussian fit.

Parameters

datandarray (2D): The data to which a Gaussian is being fit.
maskndarray (2D); optional: An integer mask array where 1 is unmasked and 0 is masked. Defaults to None which leaves all data unmasked.
yxguesstuple; optional: A guess at the centroid. Defaults to None which uses the data point with the highest value.

Returns

gwidthtuple: The guess for the Gaussian width in each direction.
gcentertuple: The guess for the centroid. Returns yxguess if it is not None, else uses the data point with the highest value.
gheightfloat: The guess for the Gaussian amplitude.

eureka.lib.gaussian.gaussians(x, param)[source]: Evaluate more than 1 gaussian.

eureka.lib.gaussian.resids(param, x, ngauss, y)[source]

Get the residuals of a Gaussian compared to data for fitting.

Parameters

paramndarray (1D): The fitted parameters raveled into a 1D array.
xndarray (1D): The x-positions of the values y.
ngaussint: The number of Gaussians being fitted.
yndarray (1D): The values to which a Gaussian should be fitted.

Returns

ndarray (1D): The difference between y and the Gaussian.

eureka.lib.gaussian.residuals(params, x, data, mask, weights, bgpars, fitbg)[source]

Calculates the residuals between data and a gaussian model determined by the rest of the parameters. Used in fitgaussian.

Parameters

params1D ndarray: This array contains the parameters desired to fit with fitgaussian, depending on fitbg, the number of elements varies.
xndarray: Array (any shape) giving the abcissas of data.
datandarray: Array giving the values of the function.
maskndarray: Same shape as data. Values where its corresponding mask value is 0 are disregarded for the minimization. Only values where the mask value is 1 are considered.
weightsndarray: Same shape as data. This array defines weights for the minimization, for scientific data the weights should be 1/sqrt(variance).
bgparsndarray or tuple, 3-elements: Background parameters, the elements determine a X- and Y-linearly dependant level, of the form: background = Y*bgparam[0] + X*bgparam[1] + bgparam[2]
fitbgInteger: This flag indicates the level of background fitting: fitbg=0: No fitting, estimate the bg as median(data). fitbg=1: Fit a constant to the bg (bg = c). fitbg=2: Fit a plane as bg (bg = a*x + b*y + c).

Returns

residuals1D ndarray: An array of the (unmasked) weighted residuals between data and a gaussian model determined by params (and bgpars when necessary).

Notes

History:

2011-05-03 patricio pcubillos@fulbrightmail.org
Initial version.

lib.gelmanrubin

eureka.lib.gelmanrubin.convergetest(pars, nchains)[source]

Driver routine for gelmanrubin.

Perform convergence test of Gelman & Rubin (1992) on a MCMC chain.

Parameters

parsndarray: A 2D array containing a separate parameter MCMC chain per row.
nchainsscalar: The number of chains to split the original chain into. The length of each chain MUST be evenly divisible by nchains.

Returns

psrfndarray: The potential scale reduction factors of the chain. If the chain has converged, each value should be close to unity. If they are much greater than 1, the chain has not converged and requires more samples. The order of psrfs in this vector are in the order of the free parameters.
meanpsrfscalar: The mean of psrf. This should be ~1 if your chain has converged.

Notes

History:

2010-08-20 ccampo: Initial version.

Examples

Consider four MCMC runs that has already been loaded. The individual fits are located in the fit list. These are for channels 1-4.

>>> import gelmanrubin
>>> import numpy as np
>>> # channels 1/3 free parameters
>>> ch13pars = np.concatenate((fit[0].allparams[fit[0].freepars],
>>>                            fit[2].allparams[fit[2].freepars]))

>>> # channels 2/4 free parameters
>>> ch24pars = np.concatenate((fit[1].allparams[fit[1].freepars],
>>>                            fit[3].allparams[fit[3].freepars]))

>>> # number of chains to split into
>>> nchains = 4

>>> # test for convergence
>>> ch13conv  = gelmanrubin.convergetest(ch13pars, nchains)
>>> ch24conv  = gelmanrubin.convergetest(ch24pars, nchains)

>>> # show results
>>> print(ch13conv)
(array([1.02254252, 1.00974035, 1.04838778, 1.0017869 , 1.7869707,
        2.15683239, 1.00506215, 1.00235165, 1.06784124, 1.04075207,
        1.01452032]), 1.1960716427734874)
>>> print(ch24conv)
(array([1.01392515, 1.00578357, 1.03285576, 1.13138702, 1.0001787,
        3.52118005, 1.10592542, 1.05514509, 1.00101459]),
        1.3185994837687156)

eureka.lib.gelmanrubin.gelmanrubin(chain, nchains)[source]

Perform convergence test of Gelman & Rubin (1992) on a MCMC chain.

Parameters

chainndarray: A vector of parameter samples from a MCMC routine.
nchainsscalar: The number of chains to split the original chain into. The length of chain WILL BE MODIFIED if NOT evenly divisible by nchains.

Returns

psrfscalar: The potential scale reduction factor of the chain. If the chain has converged, this should be close to unity. If it is much greater than 1, the chain has not converged and requires more samples.

Notes

History:

2010-08-20 ccampo: Initial version.
2011-07-07 kevin: Removed chain length constraint.

lib.imageedit

eureka.lib.imageedit.pasteimage(data, subim, dy_, syx=(None, None))[source]

Inserts the subim array into data, the data coordinates (dyc,dxc) will match the subim coordinates (syc,sxc). The arrays can have not overlapping pixels.

Parameters

data2D ndarray: Image where subim will be inserted.
subim2D ndarray: Image so be inserted.
dy_2 elements scalar tuple: dyc, dxc. Position in data that will match the (syc,sxc) position of subim.
syx: 2 elements scalar tuple: syc, sxc. Semi-length of the extracted image. if not specified, (syc,sxc) will be the center of subim.

Returns

The data array with the subim array inserted, according to the
given coordinates.

Notes

History:

2010-07-11 patricio pcubillos@fulbrightmail.org
Added documentation.
2022-08-03 szieba
changed (syc, sxc) is (None, None) to (syc, sxc) == (None, None)

Examples

eureka.lib.imageedit.trimimage(data, c, r, mask=None, uncd=None, oob=0)[source]

Extracts a rectangular area of an image masking out of bound pixels.

Parameters

data2D ndarray: Image from where extract a sub image.
c: 2-elements tuple: yc, xc. Position in data, where the extracted image will be centered. yc and xc must have integer values.
r2-elements tuple: yr, xr. Semi-length of the extracted image. Integer values.
mask2D ndarray: If specified, this routine will extract the mask subimage as well. out of bound pixels values will have value oob.
uncd2D ndarray: If specified, this routine will extract the uncd subimage as well.
oobscalar: Value for out of bound pixels in the mask. Default is 0.

Returns

Tuple, up to 3 2D-ndarray images containing the extracted image,
its mask (if specified) and a uncd array (if specified). The shape
of each array is (2*yr+1, 2*xr+1).

Notes

History:

2010-07-11 patricio, pcubillos@fulbrightmail.org
Added documentation.

Examples

lib.interp2d

eureka.lib.interp2d.interp2d(image, expand=5, y=None, x=None, yi=None, xi=None)[source]

This function oversamples a 2D frame (image) which can be used if the user decides that the resolution of the image is not enough and they want to split a pixel into more subpixels.

Parameters

image2D numpy array: Contains the 2D frame which will be oversampled in pixels
expandint: The factor by which a pixel should be oversampled. E.g., if set to 5, a pixel will turn into 25 subpixels.
y1D numpy array: np.arange(ny), with ny being the number of pixels in the y direction
x1D numpy array: np.arange(nx), with nx being the number of pixels in the x direction
yi1D numpy array: np.linspace(0, ny - 1, isz[0]), with isz = np.array(sz, dtype=int) + (np.array(sz, dtype=int)-1)*(expand-1) and sz = np.shape(image)
xi1D numpy array: np.linspace(0, ny - 1, isz[0]), with isz = np.array(sz, dtype=int) + (np.array(sz, dtype=int)-1)*(expand-1) and sz = np.shape(image)

lib.logedit

class eureka.lib.logedit.Logedit(logname, read=None)[source]

Bases: object

This object handles writing text outputs into a log file and to the screen as well.

Notes

History:

2010-07-10 Patricio Cubillos
Initial version
2010-11-24 Patricio Cubillos
logedit converted to a class.

Examples

>>> from logedit import Logedit
>>> message1 = 'This message will be logged and displayed.'
>>> message2 = 'This message too.'
>>> message3 = 'This one is Not going to delete previous lines.'
>>> message4 = ('This one copies previous lines and keeps previous '
                'log, but saves to new log.')
>>> message5 = 'This one deletes previous lines.'

>>> logname = 'out.log'
>>> logname2 = 'out2.log'

>>> # Create and print lines to a log
>>> log = Logedit(logname)
>>> log.writelog(message1)
This message will be logged and displayed.
>>> log.writelog(message2)
This message too.
>>> log.closelog()

>>> # Edit log without overiding previous lines
>>> log = Logedit(logname, read=logname)
>>> log.writelog(message3)
This one is Not going to delete previous lines.
>>> log.closelog()

>>> # copy a pre-existing log on a new log, and edit it.
>>> log = Logedit(logname2, read=logname)
>>> log.writelog(message4)
This one copies previous lines and keeps previous log, but saves to
new log.
>>> log.closelog()

>>> # overite a pre-existing log
>>> log = Logedit(logname)
>>> log.writelog(message5)
This one deletes previous lines.
>>> log.closelog()

>>> # See the output files: 'out.log' and 'out2.log' to see results.

Methods

`closelog`()	Closes an existing log file.
`writeclose`(message[, mute, end])	Print message in terminal and log, then close log.
`writelog`(message[, mute, end])	Prints message in the terminal and stores it in the log file.

closelog()[source]: Closes an existing log file.

writeclose(message, mute=False, end='\n')[source]

Print message in terminal and log, then close log.

Parameters

messagestr: The message to log.
mutebool; optional: If True, only log and do not pring. Defaults to False.
endstr; optional: Can be set to ‘\r’ to have the printed line overwritten which is useful for progress bars. Defaults to ‘\n’.

writelog(message, mute=False, end='\n')[source]

Prints message in the terminal and stores it in the log file.

Parameters

messagestr: The message to log.
mutebool; optional: If True, only log and do not pring. Defaults to False.
endstr; optional: Can be set to ‘\r’ to have the printed line overwritten which is useful for progress bars. Defaults to ‘\n’.

lib.manageevent

eureka.lib.manageevent.findevent(meta, stage, allowFail=False)[source]

Loads in an earlier stage meta file.

Parameters

metaeureka.lib.readECF.MetaClass: The new meta object for the current processing.
stagestr: The previous stage (e.g. “S2” for Stage 3).
allowFailbool; optional: Whether to allow the code to find no previous stage metadata files (for S2, S3) or throw an error if no metadata files are found. Default is False.

Returns

old_metaeureka.lib.readECF.MetaClass: The old metadata object.
inputdirstr: The new inputdir to use (based on the present location of the located metadata file).
inputdir_rawstr: The new inputdir_raw to use (based on the present location of the located metadata file).

Raises

AssertionError: Unable to find a metadata save file and allowFail was False.

Notes

History:

April 25, 2022 Taylor Bell
Initial version.

eureka.lib.manageevent.loadevent(filename, load=[], loadfilename=None)[source]

Loads an event stored in .dat and .h5 files.

Parameters

filenamestr: The string contains the name of the event file.
loadstr tuple; optional: The elements of this tuple contain the parameters to read. We usually use the values: ‘data’, ‘uncd’, ‘head’, ‘bdmskd’, ‘brmskd’ or ‘mask’. Defaults to [].
loadfilenamestr; optional: The filename of the .h5 save file (excluding the file extension). Defaults to None which uses filename.

Returns

eureka.lib.readECF.MetaClass: The requested metadata object.

Notes

The input filename should not have the .dat nor the .h5 extentions.

History:

2010-07-10 patricio
Added documentation.
2010-11-12 patricio
reimplemented using exec()

eureka.lib.manageevent.mergeevents(new_meta, old_meta)[source]

Merge the current MetaClass data into the MetaClass object from a previous stage.

Parameters

new_metaeureka.lib.readECF.MetaClass: The metadata object for the current stage.
old_metaeureka.lib.readECF.MetaClass: The metadata object for the previous stage.

Returns

new_metaeureka.lib.readECF.MetaClass: The current metadata object containing the details from the previous metadata object.

Notes

History:

April 25, 2022 Taylor Bell
Initial version.

eureka.lib.manageevent.saveevent(event, filename, save=[], delete=[], protocol=3)[source]

Saves an event in .dat (using cpickle) and .h5 (using h5py) files.

Parameters

eventeureka.lib.readECF.MetaClass: The meta data object to save.
filenamestr: The string contains the name of the event file.
savestr tuple: The elements of this tuple contain the parameters to save. We usually use the values: ‘data’, ‘uncd’, ‘head’, ‘bdmskd’, ‘brmksd’ or ‘mask’.
deletestr tuple: Parameters to be deleted.

Notes

The input filename should not have the .dat nor the .h5 extentions. Side effect: This routine deletes all parameters except ‘event’ after saving it.

History:

2010-07-10 patricio
Added documentation.
2010-11-12 patricio
reimplemented using exec()

eureka.lib.manageevent.updateevent(event, filename, add)[source]

Adds parameters given by add from filename to event.

Parameters

eventeureka.lib.readECF.MetaClass: The metadata object to update.
filenamestr: The string contains the name of the event file.
addstr tuple: The elements of this tuple contain the parameters to add. We usually use the values: ‘data’, ‘uncd’, ‘head’, ‘bdmskd’, ‘brmaskd’ or ‘mask’.

Returns

eureka.lib.readECF.MetaClass: The updated metadata object.

Notes

The input filename should not have the .dat nor the .h5 extentions.

History:

2010-07-10 patricio
Initial version.
2010-11-12 patricio
reimplemented using exec()

lib.mastDownload

eureka.lib.mastDownload.cleanup(download_dir='.')[source]

Remove empty folders from download directory.

Parameters

download_dirstr; optional: Temporary download directory specified for mastDownload.download(). Defaults to ‘.’.

Notes

History:

June 2022 Kevin Stevenson
Initial version

eureka.lib.mastDownload.columnNames()[source]

Print column names from MAST Observation table.

Notes

History:

June 2022 Kevin Stevenson
Initial version

eureka.lib.mastDownload.consolidate(result, final_dir)[source]

Consolidate downloaded files into a single directory

Parameters

resultAstroPy Table: The manifest of files downloaded, returned from mastDownload.download().
final_dirstr: Final destination of files.

Notes

History:

June 2022 Kevin Stevenson
Initial version

eureka.lib.mastDownload.downloadHST(proposal_id, visit, inst='WFC3', download_dir='.', subgroup='IMA')[source]

Download observation visit number from specified proposal ID.

Parameters

proposal_idstr or int: HST proposal/program ID (e.g., 13467).
visitstr or int: HST visit number listed on the Visit Status Report (e.g., 60). See https://www.stsci.edu/cgi-bin/get-visit-status?id=XXXXX, where XXXXX is the proposal/program ID.
inststr; optional: HST instrument name, can be upper or lower case. Supported options include: WFC3, STIS, COS, or FGS. Defaults to ‘WFC3’.
download_dirstr; optional: Temporary download directory will be ‘download_dir’/mastDownload/… Defaults to ‘.’.
subgroupstr; optional: FITS file type (usually IMA, sometimes FLT). Defaults to ‘IMA’.

Returns

resultAstroPy Table: The manifest of files downloaded.

Notes

History:

June 2022 Kevin Stevenson
Initial version

eureka.lib.mastDownload.filterJWST(proposal_id, observation, visit, calib_level, subgroup)[source]

Find JWST data products by applying standard filters.

Parameters

proposal_idstr or int: JWST proposal/program ID (e.g., 1366).
observationstr or int: JWST observation number listed on the Visit Status Report (e.g., 2). See www.stsci.edu/cgi-bin/get-visit-status?id=XXXXX&observatory=JWST, where XXXXX is the proposal/program ID.
visitstr or int: JWST visit number listed on the Visit Status Report (e.g., 2). See www.stsci.edu/cgi-bin/get-visit-status?id=XXXXX&observatory=JWST, where XXXXX is the proposal/program ID.
calib_levellist or int: Product Calibration Level (0 = raw, 1 = uncalibrated, 2 = calibrated, 3 = science product, 4 = contributed science product)
subgroupstr: FITS file type, varies by calib_level. 1: UNCAL, GS-ACQ1, GS-ACQ2, GS-FG, GS-ID, GS-TRACK 2: CAL, CALINTS, RATE, RATEINTS, X1DINTS, ANNNN_CRFINTS, GS-ACQ1, GS-ACQ2, GS-FG, GS-ID, GS-TRACK, RAMP 3: X1DINTS, WHTLT

Returns

tableAstroPy Table: The filtered table of data products.

Notes

History:

July 2022 Kevin Stevenson
Initial version

eureka.lib.mastDownload.login(mast_token=None)[source]

Log into the MAST portal.

Parameters

mast_tokenstr; optional: The token to authenticate the user. Default is None. This can be generated at https://auth.mast.stsci.edu/token. If not supplied, it will be prompted for if not in the keyring or set via $MAST_API_TOKEN.

Notes

History:

July 2022 Kevin Stevenson
Initial version

eureka.lib.mastDownload.logout()[source]

Log out of current MAST session.

Notes

History:

July 2022 Kevin Stevenson
Initial version

eureka.lib.mastDownload.sortHST(final_dir, sci_dir='sci', cal_dir='cal')[source]

Sort files into science and calibration subdirectories.

Parameters

final_dirstr: Final destination of files.
sci_dirstr; optional: Name of science subdirectory within ‘final_dir’. Defaults to ‘sci’.
cal_dirstr; optional: Name of calibration subdirectory within ‘final_dir’. Defaults to ‘cal’.

Notes

History:

June 2022 Kevin Stevenson
Initial version

eureka.lib.mastDownload.sortJWST(source_dir, target_dir, filetype)[source]

eureka.lib.mastDownload.writeTable_JWST(proposal_id, observation, visit, filename, format='csv')[source]

Write all products from specified visit to an ASCII file

Parameters

proposal_idstr or int: JWST proposal/program ID (e.g., 1366).
observationstr or int: JWST observation number listed on the Visit Status Report (e.g., 2). See www.stsci.edu/cgi-bin/get-visit-status?id=XXXXX&observatory=JWST, where XXXXX is the proposal/program ID.
visitstr or int: JWST visit number listed on the Visit Status Report (e.g., 1). See www.stsci.edu/cgi-bin/get-visit-status?id=XXXXX&observatory=JWST, where XXXXX is the proposal/program ID.
filenamestr; optional: The file format to use. Defaults to ‘csv’.

Notes

History:

July 2022 Kevin Stevenson
Initial version

lib.meanerr

eureka.lib.meanerr.meanerr(data, derr, mask=None, err=False, status=False)[source]

Calculate the error-weighted mean and the error in the error-weighted mean of the input data, omitting masked data, NaN data or errors, and data whose errors are zero.

Parameters

data: ndarray: The data to average.
derr: ndarray: The 1-sigma uncertainties in data, same shape as data.
mask: ndarray: A 1 indicates the corresponding element of Data is good, a 0 indicates it is bad, same shape as data.
err: boolean: Set to True to return error in the mean.
status: boolean: Set to True to return a bit flag. If value=0, result is good. Bits: 0 = NaN(s) in data. 1 = some errors equal zero. 2 = masked pixel(s) in data.

Returns

This function returns the error-weighted mean of the unmasked
elements of Data. If err or status were set to True, return a
tuple.

Notes

Follows maximum likelihood method (see, e.g., Bevington and Robinson 2003, Data Reduction and Error Analysis for the Physical Sciences, 3rd ed, McGraw Hill, Ch. 4.).

History:

2005-11-15: jh. Joseph Harrington, Cornell. jh@oobleck.astro.cornell.edu
Initial version
2010-11-18 patricio. pcubillos@fulbrightmail.org
Wrote in python, docstring added.

Examples

lib.medstddev

eureka.lib.medstddev.medstddev(data, mask=None, medi=False, axis=0)[source]

Compute the stddev with respect to the median.

This is rather than the standard method of using the mean.

Parameters

datandarray: An array from which to caculate the median standard deviation.
mask1D ndarray: Mask indicating the good values (ones) and bad values (zeros). Same shape as data. Defaults to None.
mediboolean; optional: If True return a tuple with (stddev, median) of data. Defaults to False.
axisint; optional: The axis along wich the median std deviation is calculated. Defaults to 0.

Returns

float: The stadard deviation.
float; optional: The median; only returned if medi==True.

Notes

MEANSTDDEV calculates the median, subtracts it from each value of X, then uses this residual to calculate the standard deviation.

The numerically-stable method for calculating the variance from moment.pro doesn’t work for the median standard deviation. It only works for the mean, because by definition the residuals from the mean add to zero.

History:

2005-01-18 statia
Written by Statia Luszcz.
2005-01-19 statia
Updated variance calculation according to algorithm in moment.pro, added medi keyword.
2005-01-20 Joe Harrington, Cornell, jh@oobleck.astro.cornell.edu
Header update. Removed algorithm from moment.pro because it doesn’t work for the median. Added /double.
2010-11-05 patricio pcubillos@fulbrightmail.org
Converted to python, documented.
2022-04-11 Taylor James Bell
Efficiently using numpy axes

Examples

>>> import medstdev as m
>>> a  = np.array([1,3,4,5,6,7,7])
>>> std, med = m.medstddev(a, medi=True)
>>> print(median(a))
5.0
>>> print(med)
5.0
>>> print(std)
2.2360679775

>>> # use masks
>>> a    = np.array([1,3,4,5,6,7,7])
>>> mask = np.array([1,1,1,0,0,0,0])
>>> std, med = m.medstddev(a, mask, medi=True)
>>> print(std)
1.58113883008
>>> print(med)
3.0

>>> # automatically mask invalid values
>>> a = np.array([np.nan, 1, 4, np.inf, 6])
>>> std, med = m.medstddev(a, medi=True)
>>> print(std, med)
(2.5495097567963922, 4.0)

>>> # critical cases:
>>> # only one value, return std = 0.0
>>> a    = np.array([1, 4, 6])
>>> mask = np.array([0, 0, 1])
>>> std, med = m.medstddev(a, mask, medi=True)
>>> print(std, med)
(0.0, 6.0)

>>> # no good values, return std = nan, med = nan
>>> mask[-1] = 0
>>> std, med = m.medstddev(a, mask, medi=True)
>>> print(std, med)
(nan, nan)

lib.plots

eureka.lib.plots.set_rc(style='preserve', usetex=False, filetype='.png', from_scratch=False, **kwargs)[source]

Function to adjust matplotlib rcParams for plotting procedures.

Parameters

stylestr; optional: Your plotting style from (“custom”, “eureka”, “preserve”, or “default”). Custom passes all kwargs to the ‘font’ rcParams group at the moment. Eureka sets some nicer rcParams settings recommended by the Eureka team. Preserve leaves all rcParams as-is and can be used to toggle the usetex parameter. By default uses ‘preserve’.
usetexbool; optional: Do you want to use LaTeX fonts (which requires LaTeX to be installed), by default False
filetypestr: The file type that all Eureka figures should be saved as (e.g. .png, .pdf).
from_scratchbool; optional: Should the rcParams first be set to rcdefaults? By default False.
**kwargsdict: Any additional parameters to be passed to rcParams.update.

Raises

ValueError: Ensures that usetex and from_scratch arguments are boolean
ValueError: Ensures that input style is one of: “custom”, “eureka”, “preserve”, or “default”

lib.readECF

class eureka.lib.readECF.MetaClass(folder=None, file=None, **kwargs)[source]

Bases: object

A class to hold Eureka! metadata.

This class loads a Eureka! Control File (ecf) and lets you query the parameters and values.

Notes

History:

2009-01-02 Christopher Campo
Initial Version.
2010-03-08 Patricio Cubillos
Modified from ccampo version.
2010-10-27 Patricio Cubillos
Docstring updated
2011-02-12 Patricio Cubillos
Merged with ccampo’s tepclass.py
2022-03-24 Taylor J Bell
Significantly modified for Eureka

Methods

`copy_ecf`()	Copy an ECF file to the output directory to ensure reproducibility.
`read`(folder, file)	A function to read ECF files
`write`(folder)	A function to write an ECF file based on the current MetaClass settings.

copy_ecf()[source]

Copy an ECF file to the output directory to ensure reproducibility.

NOTE: This will update the inputdir of the ECF file to point to the exact inputdir used to avoid ambiguity later and ensure that the ECF could be used to make the same outputs.

Notes

History:

Mar 2022 Taylor J Bell
Initial Version based on old readECF code.

read(folder, file)[source]

A function to read ECF files

Parameters

folderstr: The folder containing an ECF file to be read in.
filestr: The ECF filename to be read in.

Notes

History:

Mar 2022 Taylor J Bell
Initial Version based on old readECF code.
April 25, 2022 Taylor J Bell
Joining topdir and inputdir/outputdir here.

write(folder)[source]

A function to write an ECF file based on the current MetaClass settings.

NOTE: For now this only rewrites the input ECF file to a new ECF file in the requested folder. In the future this function should make a full ECF file based on any adjusted parameters.

Parameters

folderstr: The folder where the ECF file should be written.

Notes

History:

Mar 2022 Taylor J Bell
Initial Version.

lib.readEPF

class eureka.lib.readEPF.Parameter(name, value, ptype, priorpar1=None, priorpar2=None, prior=None)[source]

Bases: object

A generic parameter class

Attributes

ptype: Getter for the ptype
values: Return all values for this parameter

property ptype: Getter for the ptype

property values

Return all values for this parameter

Returns

list

[self.name, self.value, self.ptype, self.priorpar1,: self.priorpar2, self.prior] excluding any values which are None.

class eureka.lib.readEPF.Parameters(param_path=None, param_file=None, **kwargs)[source]

Bases: object

A class to hold the Parameter instances

This class loads a Eureka! Parameter File (epf) and lets you query the parameters and values.

Notes

History:

2022-03-24 Taylor J Bell
Based on readECF with significant edits for Eureka

Methods

`read`(folder, file)	A function to read EPF files
`write`(folder)	A function to write an EPF file based on the current Parameters settings.

read(folder, file)[source]

A function to read EPF files

Parameters

folderstr: The folder containing an EPF file to be read in.
filestr: The EPF filename to be read in.

Notes

History:

Mar 2022 Taylor J Bell
Initial Version based on old readECF code.

write(folder)[source]

A function to write an EPF file based on the current Parameters settings.

NOTE: For now this only rewrites the input EPF file to a new EPF file in the requested folder. In the future this function should make a full EPF file based on any adjusted parameters.

Parameters

folderstr: The folder where the EPF file should be written.

Notes

History:

Mar 2022 Taylor J Bell
Initial Version.

lib.smooth

eureka.lib.smooth.medfilt(x, window_len)[source]

Apply a length-k median filter to a 1D array x. Boundaries are extended by repeating endpoints.

Parameters

xndarray (1D): The data to be smoothed.
window_lenint: The smoothing window length.

Returns

ndarray: A smoothed copy of x.

eureka.lib.smooth.smooth(x, window_len=10, window='hanning')[source]

Smooth the data using a window with requested size.

This method is based on the convolution of a scaled window with the signal. The signal is prepared by introducing reflected copies of the signal (with the window size) in both ends so that transient parts are minimized in the begining and end part of the output signal.

Parameters

xndarray: The input signal.
window_lenint; optional: The dimension of the smoothing window. Defaults to 10.
windowstr; optional: The type of window from ‘flat’, ‘hanning’, ‘hamming’,’bartlett’, or ‘blackman’. flat window will produce a moving average smoothing. Defaults to ‘hanning’.

Returns

ndarray: the smoothed signal

lib.sort_nicely

eureka.lib.sort_nicely.alphanum_key(s)[source]

Turn a string into a list of string and number chunks.: “z23a” -> [“z”, 23, “a”]

Parameters

sstr: The string to break into a list.

Returns

list: The string broken into a list of strings and ints.

eureka.lib.sort_nicely.sort_nicely(list1)[source]

Sort the given list in the way that humans expect.

Parameters

list1list: The list to sort nicely.

Returns

list: The nicely sorted list.

eureka.lib.sort_nicely.tryint(s)[source]

Turn a string into an int if possible.

Parameters

sstr: The string to try to convert to an int.

Returns

int OR str: An int if s was numeric, otherwise just returns s.

lib.splinterp

eureka.lib.splinterp.splinterp(x2, x, y)[source]

This function implements the methods splrep and splev of the module scipy.interpolate

Parameters

x21D array_like: array of points at which to return the value of the smoothed spline or its derivatives
xarray_like: The x data points defining a curve y = f(x).
yarray_like: The y data points defining a curve y = f(x).

Returns

array_like: An array of values representing the spline function or curve. If tck was returned from splrep, then this is a list of arrays representing the curve in N-dimensional space.

Examples

>>> import numpy as np
>>> import matplotlib.pyplot as plt

>>> x = np.arange(21)/20.0 * 2.0 * np.pi
>>> y = np.sin(x)
>>> x2 = np.arange(41)/40.0 *2.0 * np.pi

>>> y2 = splinterp(x2, x, y)
>>> plt.plot(x2,y2)

lib.suntimecorr

eureka.lib.suntimecorr.getcoords(file)[source]

Use regular expressions to extract X,Y,Z, and time values from the horizons file.

Parameters

filestrs list: A list containing the lines of a horizons file.

Returns

list: A four elements list containing the X, Y, Z, and time arrays of values from file.

Notes

History:

2010-11-01, Patricio Cubillos
Initial version

Examples

>>> start_data = '$$SOE'
>>> end_data   = '$$EOE'

>>> # Read in whole table as an list of strings, one string per line
>>> ctable = open('/home/esp01/ancil/horizons/all_spitzer.vec', 'r')
>>> wholetable = ctable.readlines()
>>> ctable.close()

>>> # Find start and end line
>>> i = 0
>>> while wholetable[i].find(end_data) == -1:
>>>     if wholetable[i].find(start_data) != -1:
>>>        start = i + 1
>>>     i += 1

>>> # Chop table
>>> data = wholetable[start:i-2]

>>> # Find values:
>>> x, y, z, t = getcoords(data)

>>> print(x, y, z, t)

eureka.lib.suntimecorr.suntimecorr(ra, dec, obst, coordtable, verbose=False)[source]

This function calculates the light-travel time correction from observer to a standard location. It uses the 2D coordinates (RA and DEC) of the object being observed and the 3D position of the observer relative to the standard location. The latter (and the former, for solar-system objects) may be gotten from JPL’s Horizons system.

Parameters

rafloat: Right ascension of target object in radians.
decfloat: Declination of target object in radians.
obstfloat or numpy float array: Time of observation in Julian Date (may be a vector)
coordtablestr: Filename of output table from JPL HORIZONS specifying the position of the observatory relative to the standard position.
verbosebool: If True, print X,Y,Z coordinates.

Returns

np.array: This function returns the time correction in seconds to be ADDED to the observation time to get the time when the observed photons would have reached the plane perpendicular to their travel and containing the reference position.

Notes

The position vectors from coordtable are given in the following coordinate system: Reference epoch : J2000.0 xy-plane : plane of the Earth’s mean equator at the reference epoch x-axis : out along ascending node of instantaneous plane of the Earth’s orbit and the Earth’s mean equator at the reference epoch z-axis : along the Earth mean north pole at the reference epoch

Ephemerides are often calculated for BJD, barycentric Julian date. That is, they are correct for observations taken at the solar system barycenter’s distance from the target. The BJD of our observation is the time the photons we observe would have crossed the sphere centered on the object and containing the barycenter. We must thus add the light-travel time from our observatory to this sphere. For non-solar-system observations, we approximate the sphere as a plane, and calculate the dot product of the vector from the barycenter to the telescope and a unit vector to from the barycenter to the target, and divide by the speed of light.

Properly, the coordinates should point from the standard location to the object. Practically, for objects outside the solar system, the adjustment from, e.g., geocentric (RA-DEC) coordinates to barycentric coordinates has a negligible effect on the trig functions used in the routine.

History:

2005-12-01, Statia Luszcz
Initial version.
2006-03-09, jh
Corrected 90deg error in algorithm, renamed, updated header, made Coordtable a positional arg since it’s required, switched to radians.
2007-06-28, jh
Renamed to suntimecorr since we now use barycentric Julian date.
2009-01-28, jh
Change variables to long, use spline instead of linfit so we can use one HORIZONS file for the whole mission.
2009-02-22, jh
Reshape spline results to shape of obst. Make it handle unsorted unput data properly. Header update.
2010-07-10, patricio
Converted to python.
2010-11-01, patricio
Docstring updated.

Examples

>>> # Spitzer is in nearly the Earth's orbital plane.  Light coming
>>> # from the north ecliptic pole should hit the observatory and
>>> # the sun at about the same time.

>>> import suntimecorr as sc
>>> ra  = 18.0 * np.pi /  12 # ecliptic north pole coords in radians
>>> dec = 66.5 * np.pi / 180 # "
>>> obst = np.array([2453607.078])  # Julian date of 2005-08-24 14:00
>>> print(sc.suntimecorr(
>>>           ra, dec, obst,
>>>           '/home/esp01/ancil/horizons/cs41_spitzer.vec'))
1.00810877 # about 1 sec, close to zero

>>> # If the object has the RA and DEC of Spitzer, light time should be
>>> # about 8 minutes to the sun.
>>> obs  = np.array([111093592.8346969, -97287023.315796047,
>>>                  -42212080.826677799])
>>> # vector to the object
>>> obst = np.array([2453602.5])

>>> print( np.sqrt(np.sum(obs**2.0)) )
153585191.481 # about 1 AU, good
>>> raobs  = np.arctan(obs[1]/ obs[0])
>>> decobs = np.arctan(obs[2]/ np.sqrt(obs[0]**2 + obs[1]**2))
>>> print(raobs, decobs)
-0.7192383661, -0.2784282118
>>> print(sc.suntimecorr(raobs, decobs, obst,
>>>                      '/home/esp01/ancil/horizons/cs41_spitzer.vec')
>>>       / 60.0)
8.5228630 # good, about 8 minutes light time to travel 1 AU

lib.utc_tt

eureka.lib.utc_tt.leapdates(rundir, log)[source]

Generates an array of leap second dates.

The array is automatically updated every six months. Uses a local leap second file, but retrieves a leap second file from NIST if the current file is missing or out of date.

Parameters

rundirstr: The folder in which to cache the leapdates array.
loglogedit.Logedit: The current log.

Returns

ndarray: The Julian dates of leap seconds.

eureka.lib.utc_tt.leapseconds(jd_utc, dates)[source]

Computes the difference between UTC and TT for a given date.

Parameters

jd_utcfloat: UTC Julian date.
datesarray_like: An array of Julian dates on which leap seconds occur.

Returns

float: The difference between UTC and TT for a given date.

eureka.lib.utc_tt.utc_tdb(jd_utc, leapdir, log)[source]

Converts UTC Julian dates to Barycentric Dynamical Time (TDB).

Formula taken from USNO Circular 179, based on that found in Fairhead and Bretagnon (1990). Accurate to 10 microseconds.

Parameters

jd_utcarray-like: UTC Julian date.
leapdirstr: The folder containing leapdir save files.
loglogedit.Logedit: The current log.

Returns

array-like: time in JD_TDB.

eureka.lib.utc_tt.utc_tt(jd_utc, leapdir, log)[source]

Converts UTC Julian dates to Terrestrial Time (TT).

Parameters

jd_utcarray-like: UTC Julian date.
leapdirstr: The folder containing leapdir save files.
loglogedit.Logedit: The current log.

Returns

array-like: Time in TT.

lib.util

eureka.lib.util.check_nans(data, mask, log, name='')[source]

Checks where a data-like array is invalid (contains NaNs or infs).

Parameters

datandarray: a data-like array (e.g. data, err, dq, …).
maskndarray: Input mask.
loglogedit.Logedit: The open log in which NaNs/Infs will be mentioned, if existent.
namestr; optional: The name of the data array passed in (e.g. SUBDATA, SUBERR, SUBV0). Defaults to ‘’.

Returns

maskndarray: Output mask where 0 will be written where the input data array has NaNs or infs.

eureka.lib.util.find_fits(meta)[source]

Locates S1 or S2 output FITS files if unable to find an metadata file.

Parameters

metaeureka.lib.readECF.MetaClass: The new meta object for the current stage processing.

Returns

metaeureka.lib.readECF.MetaClass: The meta object with the updated inputdir pointing to the location of the input files to use.

Notes

History:

April 25, 2022 Taylor Bell
Initial version.

eureka.lib.util.get_mad(meta, log, wave_1d, optspec, optmask=None, wave_min=None, wave_max=None)[source]

Computes variation on median absolute deviation (MAD) using ediff1d for 2D data.

The computed MAD is the average MAD along the wavelength direction. In otherwords, the MAD is computed in the spectral direction for each integration, and then the returned value is the average of those MAD values.

Parameters

metaeureka.lib.readECF.MetaClass: Unused. The metadata object.
loglogedit.Logedit: The current log.
wave_1dndarray: Wavelength array (nx) with trimmed edges depending on xwindow and ywindow which have been set in the S3 ecf
optspecndarray: Optimally extracted spectra, 2D array (time, nx)
optmaskndarray (1D); optional: A mask array to use if optspec is not a masked array. Defaults to None in which case only the invalid values of optspec will be masked.
wave_minfloat; optional: Minimum wavelength for binned lightcurves, as given in the S4 .ecf file. Defaults to None which does not impose a lower limit.
wave_maxffloat; optional: Maximum wavelength for binned lightcurves, as given in the S4 .ecf file. Defaults to None which does not impose an upper limit.

Returns

madfloat: Single MAD value in ppm

eureka.lib.util.get_mad_1d(data, ind_min=0, ind_max=None)[source]

Computes variation on median absolute deviation (MAD) using ediff1d for 1D data.

Parameters

datandarray: The array from which to calculate MAD.
int_minint: Minimum index to consider.
ind_maxint: Maximum index to consider (excluding ind_max).

Returns

madfloat: Single MAD value in ppm

eureka.lib.util.interp_masked(data, meta, i, log)[source]

Interpolates masked pixels. Based on the example here: https://docs.scipy.org/doc/scipy/reference/generated/scipy.interpolate.griddata.html

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.
iint: The current integration.
loglogedit.Logedit: The current log.

Returns

dataXarray Dataset: The updated Dataset object with requested pixels masked.

eureka.lib.util.makedirectory(meta, stage, counter=None, **kwargs)[source]

Creates a directory for the current stage.

Parameters

metaeureka.lib.readECF.MetaClass: The metadata object.
stagestr: ‘S#’ string denoting stage number (i.e. ‘S3’, ‘S4’).
counterint; optional: The run number if you want to force a particular run number. Defaults to None which automatically finds the run number.
**kwargsdict: Additional key,value pairs to add to the folder name (e.g. {‘ap’: 4, ‘bg’: 10}).

Returns

runint: The run number

eureka.lib.util.manmask(data, meta, log)[source]

Manually mask input bad pixels.

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The current log.

Returns

dataXarray Dataset: The updated Dataset object with requested pixels masked.

eureka.lib.util.manual_clip(lc, meta, log)[source]

Manually clip integrations along time axis.

Parameters

lcXarray Dataset: The Dataset object containing light curve and time data.
metaeureka.lib.readECF.MetaClass: The current metadata object.
loglogedit.Logedit: The open log in which notes from this step can be added.

Returns

lcXarray Dataset: The updated Dataset object containing light curve and time data with the requested integrations removed.
metaeureka.lib.readECF.MetaClass: The updated metadata object.
loglogedit.Logedit: The updated log.

eureka.lib.util.normalize_spectrum(meta, optspec, opterr=None, optmask=None)[source]

Normalize a spectrum by its temporal mean.

Parameters

metaeureka.lib.readECF.MetaClass: The new meta object for the current stage processing.
optspecndarray: The spectrum to normalize.
opterrndarray; optional: The noise array to normalize using optspec, by default None.
optmaskndarray (1D); optional: A mask array to use if optspec is not a masked array. Defaults to None in which case only the invalid values of optspec will be masked.

Returns

normspec: The normalized spectrum.
normerrndarray; optional: The normalized error. Only returned if opterr is not none.

eureka.lib.util.pathdirectory(meta, stage, run, old_datetime=None, **kwargs)[source]

Finds the directory for the requested stage, run, and datetime (or old_datetime).

Parameters

metaeureka.lib.readECF.MetaClass: The metadata object.
stagestr: ‘S#’ string denoting stage number (i.e. ‘S3’, ‘S4’)
runint: run #, output from makedirectory function
old_datetimestr; optional: The date that a previous run was made (for looking up old data). Defaults to None in which case meta.datetime is used instead.
**kwargsdict: Additional key,value pairs to add to the folder name (e.g. {‘ap’: 4, ‘bg’: 10}).

Returns

pathstr: Directory path for given parameters

eureka.lib.util.phot_arrays(data)[source]

Setting up arrays for the photometry routine.

These arrays will be populated by the returns coming from centerdriver.py and apphot.py

Parameters

dataXarray Dataset: The Dataset object.

Returns

dataXarray Dataset: The updated Dataset object with new arrays where the outputs from the photometry routine will be saved in.

eureka.lib.util.read_time(meta, data, log)[source]

Read in a time CSV file instead of using the FITS time array.

Parameters

metaeureka.lib.readECF.MetaClass: The metadata object.
dataXarray Dataset: The Dataset object with the fits data stored inside.
loglogedit.Logedit: The current log.

Returns

timendarray: The time array stored in the meta.time_file CSV file.

eureka.lib.util.readfiles(meta, log)[source]

Reads in the files saved in topdir + inputdir and saves them into a list.

Parameters

metaeureka.lib.readECF.MetaClass: The metadata object.
loglogedit.Logedit: The current log.

Returns

metaeureka.lib.readECF.MetaClass: The metadata object with added segment_list containing the sorted data fits files.

eureka.lib.util.trim(data, meta)[source]

Removes the edges of the data arrays.

Parameters

dataXarray Dataset: The Dataset object.
metaeureka.lib.readECF.MetaClass: The metadata object.

Returns

subdataXarray Dataset: A new Dataset object with arrays that have been trimmed, depending on xwindow and ywindow as set in the S3 ecf.
metaeureka.lib.readECF.MetaClass: The metadata object.