FgcmFitCycleTask¶
FgcmFitCycleTask runs a single fgcm fit on the star observations generated from lsst.fgcmcal.fgcmBuildStars.FgcmBuildStarsTask using the look-up table generated from FgcmMakeLutTask. This code is meant to be run multiple times until convergence, and the results output from one “fit cycle” are used as an input to the subsequent fit cycle. One final cleanup run is performed to generate the tables required for input to FgcmOutputProductsTask.
This is the third task in a typical fgcmcal processing chain. The first is FgcmMakeLutTask, the second is FgcmBuildStarsTableTask or lsst.fgcmcal.fgcmBuildStars.FgcmBuildStarsTask, and the fourth is FgcmOutputProductsTask.
Processing summary¶
FgcmFitCycleTask reads in the star observations and the look-up table, performs an atmosphere and instrument fit, and outputs fit parameters as well as a comprehensive list of QA plots. If the config option isFinalCycle is set to True then additional datafiles are output that are used by FgcmOutputProductsTask.
FgcmFitCycleTask will output a new config file in the current working directory with recommended settings for the subsequent fit cycle. Furthermore, there are a wide range of diagnostic QA plots that are output by the task. For details on the contents of these QA plots, please see the cookbook as well as Burke, Rykoff, et al. 2018.
Python API summary¶
from lsst.fgcmcal.fgcmFitCycle import FgcmFitCycleTask
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class
FgcmFitCycleTask Run Single fit cycle for FGCM global calibration
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attribute
config Access configuration fields and retargetable subtasks.
See also
See the FgcmFitCycleTask API reference for complete details.
Retargetable subtasks¶
No subtasks.
Configuration fields¶
aperCorrFitNBins¶
Number of aperture bins used in aperture correction fit. When set to 0no fit will be performed, and the config.aperCorrInputSlopes will be used if available.
aperCorrInputSlopeDict¶
Per-band specification of aperture correction input slope parameters. These are used on the first fit iteration, and aperture correction parameters will be updated from the data if config.aperCorrFitNBins > 0. It is recommended to set this when there is insufficient data to fit the parameters (e.g. tract mode).
applyRefStarColorCuts¶
Apply color cuts defined in
starColorCuts to reference stars? These cuts are in addition to any cuts defined in refStarColorCutsapproxThroughputDict¶
Per-band specification of the approximate overall throughput at the start of calibration observations. Must have one entry per band. Typically should be 1.0.
autoHighCutNSig¶
Number of sigma for automatic computation of (high) outlier cut. Cut is based on exposure gray width (per band), unless useRepeatabilityForExpGrayCuts is set, in which case the star repeatability is used (also per band).
autoPhotometricCutNSig¶
Number of sigma for automatic computation of (low) photometric cut. Cut is based on exposure gray width (per band), unless useRepeatabilityForExpGrayCuts is set, in which case the star repeatability is used (also per band).
brightObsGrayMax¶
Maximum gray extinction to be considered bright observation
ccdGrayFocalPlaneChebyshevOrder¶
Order of the 2D chebyshev polynomials for focal plane fit.
ccdGrayFocalPlaneDict¶
Per-band specification on whether to compute focal-plane residual (‘ccd gray’) corrections.
ccdGrayFocalPlaneFitMinCcd¶
Minimum number of ‘good’ CCDs required to perform focal-plane gray corrections. If there are fewer good CCDs then the gray correction is computed per-ccd.
ccdGrayMaxStarErr¶
Maximum error on a star observation to use in ccd gray (achromatic residual) computation
ccdGraySubCcdChebyshevOrder¶
Order of the 2D chebyshev polynomials for sub-ccd gray fit.
ccdGraySubCcdDict¶
Per-band specification on whether to compute achromatic per-ccd residual (‘ccd gray’) on a sub-ccd scale.
ccdGraySubCcdTriangular¶
Should the sub-ccd gray chebyshev matrix be triangular to suppress high-order cross terms?
colorSplitBands¶
Band names to use to split stars by color. Must have 2 entries.
connections¶
- Data type
lsst.pipe.base.config.Connections- Field type
ConfigField
Configurations describing the connections of the PipelineTask to datatypes
cycleNumber¶
FGCM fit cycle number. This is automatically incremented after each run and stage of outlier rejection. See cookbook for details.
defaultCameraOrientation¶
Default camera orientation for QA plots.
deltaAperFitMinNgoodObs¶
Minimum number of good observations to use mean delta-aper values in fits.
deltaAperFitPerCcdNx¶
Number of x bins per ccd when computing delta-aper background offsets. Only used when
doComputeDeltaAperPerCcd is True.deltaAperFitPerCcdNy¶
Number of y bins per ccd when computing delta-aper background offsets. Only used when
doComputeDeltaAperPerCcd is True.deltaAperFitSpatialNside¶
Healpix nside to compute spatial delta-aper background offset maps.
deltaAperInnerRadiusArcsec¶
Inner radius used to compute deltaMagAper (arcseconds). Must be positive and less than
deltaAperOuterRadiusArcsec if any of doComputeDeltaAperPerVisit, doComputeDeltaAperPerStar, doComputeDeltaAperMap, doComputeDeltaAperPerCcd are set.deltaAperOuterRadiusArcsec¶
Outer radius used to compute deltaMagAper (arcseconds). Must be positive and greater than
deltaAperInnerRadiusArcsec if any of doComputeDeltaAperPerVisit, doComputeDeltaAperPerStar, doComputeDeltaAperMap, doComputeDeltaAperPerCcd are set.deltaMagBkgOffsetPercentile¶
Percentile brightest stars on a visit/ccd to use to compute net offset from local background subtraction.
deltaMagBkgPerCcd¶
Compute net offset from local background subtraction per-ccd? Otherwise, use computation per visit.
doComputeDeltaAperMap¶
Do the computation of delta-aper spatial maps? This is only used if
doComputeDeltaAperPerStar is True,doComputeDeltaAperPerCcd¶
Do the computation of per-ccd delta-aper background offsets?
doComputeDeltaAperPerStar¶
Do the computation of delta-aper mean values per star?
doComputeDeltaAperPerVisit¶
Do the computation of delta-aper background offsets per visit? Note: this option can be very slow when there are many visits.
doReferenceCalibration¶
Use reference catalog as additional constraint on calibration
expGrayErrRecoverCut¶
Maximum exposure gray error to be able to recover bad ccds via interpolation. Visits with more gray variance will only get CCD zeropoints if there are sufficient star observations (minStarPerCcd) on that CCD.
expGrayHighCutDict¶
Per-band specification on maximum (positive) achromatic exposure residual (‘gray term’) for a visit to be considered photometric. Must have one entry per band. Broad-band filters should be 0.2.
expGrayInitialCut¶
Maximum exposure/visit gray value for initial selection of possible photometric observations.
expGrayPhotometricCutDict¶
Per-band specification on maximum (negative) achromatic exposure residual (‘gray term’) for a visit to be considered photometric. Must have one entry per band. Broad-band filters should be -0.05.
expGrayRecoverCut¶
Maximum (negative) exposure gray to be able to recover bad ccds via interpolation. Visits with more gray extinction will only get CCD zeropoints if there are sufficient star observations (minStarPerCcd) on that CCD.
expVarGrayPhotometricCutDict¶
Per-band specification on maximum exposure variance to be considered possibly photometric. Must have one entry per band. Broad-band filters should be 0.0005.
fitBands¶
Bands to use in atmospheric fit. The bands not listed here will have the atmosphere constrained from the ‘fitBands’ on the same night. Must be a subset of
config.bandsfocalPlaneSigmaClip¶
Number of sigma to clip outliers per focal-plane.
freezeStdAtmosphere¶
Freeze atmosphere parameters to standard (for testing)
instrumentParsPerBand¶
Model instrumental parameters per band? Otherwise, instrumental parameters (QE changes with time) are shared among all bands.
instrumentSlopeMinDeltaT¶
Minimum time change (in days) between observations to use in constraining instrument slope.
isFinalCycle¶
Is this the final cycle of the fitting? Will automatically compute final selection of stars and photometric exposures, and will output zeropoints and standard stars for use in fgcmOutputProducts
maxCcdGrayErr¶
Maximum error on CCD gray offset to be considered photometric
maxIterBeforeFinalCycle¶
Maximum fit iterations, prior to final cycle. The number of iterations will always be 0 in the final cycle for cleanup and final selection.
minCcdPerExp¶
Minimum number of good CCDs per exposure/visit to be used in calibration fit. Visits with fewer good CCDs will have CCD zeropoints estimated where possible.
minExpPerNight¶
Minimum number of good exposures/visits to consider a partly photometric night
minStarPerCcd¶
Minimum number of good stars per CCD to be used in calibration fit. CCDs with fewer stars will have their calibration estimated from other CCDs in the same visit, with zeropoint error increased accordingly.
minStarPerExp¶
Minimum number of good stars per exposure/visit to be used in calibration fit. Visits with fewer good stars will have CCD zeropoints estimated where possible.
modelMagErrors¶
Should FGCM model the magnitude errors from sky/fwhm? (False means trust inputs)
multipleCyclesFinalCycleNumber¶
- Default
5- Field type
intRangeField- Range
- [2,10]
Final cycle number in multiple cycle mode. The initial cycle is 0, with limited parameters fit. The next cycle is 1 with full parameter fit. The final cycle is a clean-up with no parameters fit. There will be a total of (multipleCycleFinalCycleNumber + 1) cycles run, and the final cycle number cannot be less than 2.
outputStandardsBeforeFinalCycle¶
Output standard stars prior to final cycle? Used in debugging.
outputZeropointsBeforeFinalCycle¶
Output standard stars prior to final cycle? Used in debugging.
physicalFilterMap¶
Mapping from ‘physicalFilter’ to band.
precomputeSuperStarInitialCycle¶
Precompute superstar flat for initial cycle
randomSeed¶
Random seed for fgcm for consistency in tests.
refStarColorCuts¶
Encoded star color cuts specifically to apply to reference stars. This is a list with each entry a string of the format
band1,band2,low,high such that only stars of color low < band1 - band2 < high will be used as reference stars.refStarOutlierNSig¶
Number of sigma compared to average mag for reference star to be considered an outlier. Computed per-band, and if it is an outlier in any band it is rejected from fits.
refStarSnMin¶
Reference star signal-to-noise minimum to use in calibration. Set to <=0 for no cut.
requiredBands¶
Bands that are required for a star to be considered a calibration star. Must be a subset of
config.bandssaveLogOutput¶
Flag to enable/disable saving of log output for a task, enabled by default.
saveMetadata¶
Flag to enable/disable metadata saving for a task, enabled by default.
sedboundaryterms¶
- Data type
lsst.fgcmcal.sedterms.SedboundarytermDict- Field type
ConfigField
Mapping from bands to SED boundary term names used is sedterms.
sedterms¶
- Data type
lsst.fgcmcal.sedterms.SedtermDict- Field type
ConfigField
Mapping from terms to bands for fgcm linear SED approximations.
sigFgcmMaxEGrayDict¶
Per-band specification for maximum (absolute) achromatic residual (gray value) for observations in sigma_fgcm (raw repeatability). Broad-band filters should be 0.05.
sigmaCalFitPercentile¶
Magnitude percentile range to fit systematic error floor
sigmaCalPlotPercentile¶
Magnitude percentile range to plot systematic error floor
sigmaCalRange¶
Allowed range for systematic error floor estimation
starColorCuts¶
Encoded star-color cuts (using calibration star colors). This is a list with each entry a string of the format
band1,band2,low,high such that only stars of color low < band1 - band2 < high will be used for calibration.superStarSigmaClip¶
Number of sigma to clip outliers when selecting for superstar flats
superStarSubCcdChebyshevOrder¶
Order of the 2D chebyshev polynomials for sub-ccd superstar fit. Global default is first-order polynomials, and should be overridden on a camera-by-camera basis depending on the ISR.
superStarSubCcdDict¶
Per-band specification on whether to compute superstar flat on sub-ccd scale. Must have one entry per band.
superStarSubCcdTriangular¶
Should the sub-ccd superstar chebyshev matrix be triangular to suppress high-order cross terms?
useExposureReferenceOffset¶
Use per-exposure (visit) offsets between calibrated stars and reference stars for final zeropoints? This may help uniformity for disjoint surveys.
useQuadraticPwv¶
Model PWV with a quadratic term for variation through the night?
useRepeatabilityForExpGrayCutsDict¶
Per-band specification on whether to use star repeatability (instead of exposures) for computing photometric cuts. Recommended for tract mode or bands with few visits.