Coverage for .test/JointcalTestCFHTMinimal/test_jointcalTask_2_visits_photometry/config/jointcal.py : 100%

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# Fit astrometry and write the fitted result.
# Fit photometry and write the fitted result.
# Type of coadd, typically deep or goodSeeing
# Systematic term to apply to the measured position error (pixels)
# Systematic term to apply to the measured error on flux or magnitude as a fraction of source flux or magnitude delta (e.g. 0.05 is 5% of flux or +50 millimag).
# Matching radius between fitted and reference stars (arcseconds)
# Minimum number of associated measured stars for a fitted star to be included in the fit
# Minimum number of measuredStars per ccdImage before printing warnings
# Minimum number of measuredStars per ccdImage before printing warnings
# Allow a line search during minimization, if it is reasonable for the model (models with a significant non-linear component, e.g. constrainedPhotometry).
# Polynomial order for fitting the simple astrometry model.
# Order of the per-chip transform for the constrained astrometry model.
# Order of the per-visit transform for the constrained astrometry model.
# Use the input calexp WCSs to initialize a SimpleAstrometryModel.
# Type of model to fit to astrometry
# Type of model to fit to photometry
# Apply photometric color terms to reference stars?Requires that colorterms be set to a ColortermLibrary
# Order of the per-visit polynomial transform for the constrained photometry model.
# Do the rank update step during minimization. Skipping this can help deal with models that are too non-linear.
# Do the rank update step during minimization (should not change the astrometry fit). Skipping this can help deal with models that are too non-linear.
# How many sigma to reject outliers at during minimization.
# Maximum number of minimize iterations to take when fitting photometry.
# Maximum number of minimize iterations to take when fitting photometry.
# Padding to add to 4 all edges of the bounding box (pixels)
# Default reference catalog filter to use if filter not specified in exposure; if blank then filter must be specified in exposure
# Mapping of camera filter name: reference catalog filter name; each reference filter must exist
# Require that the fields needed to correct proper motion (epoch, pm_ra and pm_dec) are present?
# Name of the ingested reference dataset
# Padding to add to 4 all edges of the bounding box (pixels)
# Default reference catalog filter to use if filter not specified in exposure; if blank then filter must be specified in exposure
# Mapping of camera filter name: reference catalog filter name; each reference filter must exist
# Require that the fields needed to correct proper motion (epoch, pm_ra and pm_dec) are present?
# Name of the ingested reference dataset
# Apply flux limit?
# Apply flag limitation?
# Apply unresolved limitation?
# Apply signal-to-noise limit?
# Apply isolated limitation?
# Select objects with value greater than this
# Select objects with value less than this
# Name of the source flux field to use.
# List of source flag fields that must be set for a source to be used.
# List of source flag fields that must NOT be set for a source to be used.
# Select objects with value greater than this
# Select objects with value less than this
# Name of column for star/galaxy separation
# Select objects with value greater than this
# Select objects with value less than this
# Name of the source flux field to use.
# Name of the source flux error field to use.
# Name of column for parent
# Name of column for nChild
# Apply magnitude limit?
# Apply flag limitation?
# Apply unresolved limitation?
# Apply signal-to-noise limit?
# Apply magnitude error limit?
# Select objects with value greater than this
# Select objects with value less than this
# Name of the source flux field to use.
# List of source flag fields that must be set for a source to be used.
# List of source flag fields that must NOT be set for a source to be used.
# Select objects with value greater than this
# Select objects with value less than this
# Name of column for star/galaxy separation
# Select objects with value greater than this
# Select objects with value less than this
# Name of the source flux field to use.
# Name of the source flux error field to use.
# Select objects with value greater than this
# Select objects with value less than this
# Name of the source flux error field to use.
# Apply flux limit to Psf Candidate selection?
# specify the minimum psfFlux for good Psf Candidates
# specify the maximum psfFlux for good Psf Candidates (ignored if == 0)
# Apply signal-to-noise (i.e. flux/fluxErr) limit to Psf Candidate selection?
# specify the minimum signal-to-noise for good Psf Candidates
# specify the maximum signal-to-noise for good Psf Candidates (ignored if == 0)
# minimum width to include in histogram
# maximum width to include in histogram
# Name of field in Source to use for flux measurement
# Standard deviation of width allowed to be interpreted as good stars
# Keep objects within this many sigma of cluster 0's median
# List of flags which cause a source to be rejected as bad
# Name of a flag field that is True for Sources that should be used.
# List of flags which cause a source to be rejected as bad
# Type of source flux; typically one of Ap or Psf
# Minimum allowed signal-to-noise ratio for sources used for matching (in the flux specified by sourceFluxType); <= 0 for no limit
# Type of source flux; typically one of Ap or Psf
# Minimum allowed signal-to-noise ratio for sources used for matching (in the flux specified by sourceFluxType); <= 0 for no limit
# Exclude objects that have saturated, interpolated, or edge pixels using PixelFlags. For matchOptimisticB set this to False to recover previous matcher selector behavior.
# Apply magnitude limit?
# Apply flag limitation?
# Apply unresolved limitation?
# Apply signal-to-noise limit?
# Apply magnitude error limit?
# Select objects with value greater than this
# Select objects with value less than this
# Name of the source flux field to use.
# List of source flag fields that must be set for a source to be used.
# List of source flag fields that must NOT be set for a source to be used.
# Select objects with value greater than this
# Select objects with value less than this
# Name of column for star/galaxy separation
# Select objects with value greater than this
# Select objects with value less than this
# Name of the source flux field to use.
# Name of the source flux error field to use.
# Select objects with value greater than this
# Select objects with value less than this
# Name of the source flux error field to use.
# Apply magnitude limit?
# Apply flag limitation?
# Apply unresolved limitation?
# Apply signal-to-noise limit?
# Apply magnitude error limit?
# Select objects with value greater than this
# Select objects with value less than this
# Name of the source flux field to use.
# List of source flag fields that must be set for a source to be used.
# List of source flag fields that must NOT be set for a source to be used.
# Select objects with value greater than this
# Select objects with value less than this
# Name of column for star/galaxy separation
# Select objects with value greater than this
# Select objects with value less than this
# Name of the source flux field to use.
# Name of the source flux error field to use.
# Select objects with value greater than this
# Select objects with value less than this
# Name of the source flux error field to use.
# Write the pre/post-initialization Hessian and gradient to text files, for debugging.The output files will be of the form 'astrometry_preinit-mat.txt', in the current directory.Note that these files are the dense versions of the matrix, and so may be very large.
# Write .csv files containing the contributions to chi2 for the initialization and final fit.
# Write .csv files containing the contributions to chi2 for the outer fit loop.
# Source flux field to use in source selection and to get fluxes from the catalog.
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