wiki:DM/ReferenceDesign/ApplicationStatus
Last modified 8 years ago Last modified on 07/12/2011 12:47:04 PM

Application Reference Design Status =

Apps Developers,

Update the table for the packages/use cases for which you are responsible. The 'Functional / Algorithmic Description' will be used in the EA Description of the object.

If you note a missing object, please insert its details appropriately.

For reference, you can access a copy of the UML Domain model here.

"WBS Code" "UML Production " " UML Pipeline " " UML Stage " "Module.Class" "Guru" " Functional / Algorithmic Description " "Started in DC?" "Implementation Maturity {Empty: no DC, Basic: 1 DC, Alternates: 2+ DC, Complete: done}" "Comparative Status" "Science Validation" "Reference"
"02.04" "Data Release" " " "Reprocess Archive Exposure data"
"02.03.01.01" "Data Release" " ISR " "ip.isr, ip.pipeline, ip.utils" "Krughoff" "Instrument Signature Removal removes the instrument signature and standardizes the input image and metadata into LSST format. " "DC2 " "Alternates" "Supported by: LSST / 2MASS / SDSS" "Examination of corrected exposures"
"02.03.01.01" "Data Release" " ISR" " Remove Saturation " "ip.isr, ip.pipeline. IsrSaturationStage?" "Krughoff" "The pixel values are examined to detect saturation (which will naturally also identify bleed trails near saturated targets, and the strongest cosmic rays). These values, along with pixels that are identified in the list of static bad pixels, are flagged in the DQ mask of the science image. All pixels in the science array identified as “bad” in this sense are interpolated over, in order to avoid problems with source detection and with code optimization for other downstream pipeline processing," "DC3bPT1.0" "Alternates"
"02.03.01.01" "Data Release" " ISR" " Remove Overscans " "ip.pipeline. IsrOverscan?" "Krughoff" "The bias and overscan correction is applied to remove the (additive) electronic bias that is present in the signal chain. The bias is, for the most part, composed of a constant pedestal, but it has structure that is related to the electronic stability of the bias during read-out of the detector segment. The processing pipeline removes the bias and overscan contribution in a two-step process.
In this first step, the median value of non-flagged pixels in the over-scan region is subtracted from the image."
"DC3bPT1.0" "Alternates"
"02.03.01.01" "Data Release" " ISR" "Bias Correction " "ip.pipeline. IsrBiasStage?" "Krughoff" "The bias and overscan correction is applied to remove the (additive) electronic bias that is present in the signal chain. The bias is, for the most part, composed of a constant pedestal, but it has structure that is related to the electronic stability of the bias during read-out of the detector segment. The processing pipeline removes the bias and overscan contribution in a two-step process.
In the first step, the median value of non-flagged pixels in the over-scan region is subtracted from the image.
In this second step, the reference bias image is subtracted from the science image to remove higher-order structure.
Following the bias correction, the pixels are scaled by the gain factor for the appropriate CCD and normalized to unit exposure time. The brightness units are electrons s-1 (or equivalently for unit gain, detected photons s-1) for calibrated images."
"DC3bPT1.0" "Alternates"
"02.03.01.01" "Data Release" " ISR" "Cross-Talk Correction" "The cross-talk effect, when present, is to introduce a small fraction of the signal from one CCD into the signal chain of the CCD that shares the same electronics, such that “ghosts” of bright objects appear in the paired CCD. This is an additive effect, and is most noticeable for sources that are at or near saturation. The pipeline has a placeholder for this correction, should it be necessary, but no cross-talk correction is implemented at this time." "Not yet"
"02.03.1.01" "Data Release" " ISR" " Add Variance " "ip.pipeline. IsrVarianceStage?" "Krughoff" "The bias correction is applied to remove the (additive) electronic bias that is present in the signal chain. The bias is, for the most part, composed of a constant pedestal, but it has structure that is related to the electronic stability of the bias during read-out of the detector segment. The processing pipeline removes the bias contribution in a two-step process. In the first step, the median value of non-flagged pixels in the over-scan region is subtracted from the image. In the second step, the reference bias image is subtracted from the science image to remove higher-order structure. Following the bias correction, the pixels are scaled by the gain factor for the appropriate CCD and normalized to unit exposure time. The brightness units are electrons s-1 (or equivalently for unit gain, detected photons s-1) for calibrated images." "DC3bPT1.0" "Alternates"
"02.03.1.01" "Data Release" " ISR" " Apply Darks " "ip.pipeline. IsrDarkStage?" "Krughoff" "Dark correction is applied by subtracting a reference Dark calibration frame that has been scaled to the exposure time of the visit image." "DC3bPT1.0" "Alternates"
"02.03.01.01" "Data Release" " ISR" " Linearity " "The response of the CCD detectors to radiation is highly linear for pixels that are not near saturation. Currently, no linearity correction is applied in the pipelines. Were a correction necessary it would be implemented with a look-up table, and executed following the dark correction but prior to fringe correction." "Not yet"
"02.03.01.01" "Data Release" " ISR" " Defringe " "The details of the fringe pattern depend mostly upon the spatial variation in thickness of the top layer of the substrate, but also depend upon a number of other factors including the wavelengths(s) of the incident emission lines, the composition of the substrate, the temperature of the CCD, and the focal ratio of the incident beam. The amplitude of the fringe pattern background varies with time and telescope pointing. No fringe pattern correction is currently implemented" "Not yet"
"02.03.01.01" "Data Release" " ISR" " Flatten " "ip.pipeline. IsrFlatStage?" "Krughoff" "The flat-field correction removes the variations in the pixel-to-pixel response of the detectors. The Flat field corrects approximately for vignetting across the CCD. The flat-field correction is performed by dividing each science frame by a normalized, reference flat-field for the corresponding filter." "DC3bPT1.0" "Alternates"
"02.03.01.01" "Data Release" " ISR" "sdqa.pipeline.IsrSdqaStage?" " AWOL -> ???" "DC3a" "Basic"
"02.03.01.01" "Data Release" "CCD Assembly " " "ip.isr, ip.pipeline, ip.utils" "CCD Assembly Pipeline assembles amplifiers from ISR into CCD Exposures. " "Basic"
"02.03.01.01" "Data Release" "CCD Assembly" " CCD Assembly " "ip.pipeline. IsrCcdAssemblyStage?" "Krughoff" " " "DC3bPT1.0" "Basic"
"02.03.01.01" "Data Release" "CCD Assembly" "Defect Removal" "ip.pipeline. IsrCcdDefectStage?" "Krughoff" "DC3bPT1.0" "Alternates"
"02.03.01.01" "Data Release" "CCD Assembly" " SDQA per Exposure" "ip.pipeline. IsrCcdSdqaStage?" " AWOL -> ???" "DC3a" "Basic"
"02.03.01.01" "Data Release" "CCD Assembly" " SDQA " "ip.pipeline. IsrSdqaStage?" " AWOL -> ???" "DC3a" "Basic"
"02.03.01.01" "Data Release" "CR Split Handling (Alias: CrSplit?)" "Cosmic Ray Split Handling handles cosmic ray removal using the two ""split"" exposures per visit, algorithmically rejecting cosmics on each one, then taking their difference to find more cosmics. Background estimation is in this pipeline because it is required before CrReject?. Cosmic rays (CRs) are detected in two stages: in the first pass sources that are not similar in shape to a PSF are recorded. When pairs of images for a visit are processed together, a difference image is created from which additional CRs are recorded. Following CR detection, a flag is set in the quality mask of the calibrated images for all pixels that are affected by CRs, and the corresponding pixels in the individual science frames are then interpolated over. The pair of visit exposures are then averaged to create a single science image." "DC3b" "Basic"
"02.03.01.01" "Data Release" " CR Split Handling" " Background Estimation Snap 1 & 2" "meas.pipeline. BackgroundEstimationStage?" "Lupton" "Background estimation is in this pipeline because it is required before CR Rejection. The background for an exposure is first estimated and then possibly subtracted from the image. ." "DC3bPT1.0" "Basic" "Comparison with simulations"
"02.03.01.01" "Data Release" " CR Split Handling" " Find and Mask CRs Snap 1 & 2" "ip.pipeline. CrRejectStage?" "Krughoff/Lupton?" "In the first CR Rejection pass, sources that are not similar in shape to a PSF masked." "DC3bPT1.0" "Basic"
"02.03.01.01" "Data Release" " CR Split Handling" " Simple Image Differencing " "ip.pipeline. SimpleDiffImStage?" "Lupton" "Subtract two almost identical exposures to find and mask additional Crs" "DC3bPT1.0" "Basic"
"02.03.01.02" "Data Release" " Image Characterization (Alias: ImChar?)" "Image Characterization Pipeline handles image characterization, including determination of PSF and WCS. It also handles initial CCD-exposure-level photometric calibration and background subtraction. It combines all of this information into a single Exposure" "DC3b" "Alternates"
"02.04.07" "Data Release" " Image Characterization" " Bright Star Detection " "meas.pipeline. SourceDetectionStage?" "Lupton/Bickerton?" "Detection of bright sources on an exposure. If more than one exposure are provided, the exposures will be added first to create a stacked exposure." "DC3b" "Alternates"
"02.04.07" "Data Release" " Image Characterization" " Bright Star Measurement " "meas.pipeline. SourceMeasurementStage?" "Robert/Bickerton?" "Measurement of bright sources on an exposure. The resulting measurements (position, brightness, shape, orientation, and errors on those parameters) are recorded in the source catalog of the science database." "DC3b" "Alternates"
"02.03.01.02" "Data Release" " Image Characterization" "PSF Measurement" "meas.pipeline. PsfDeterminationStage?" "Lupton" "The size and shape of the point-spread function is determined from well isolated, relatively bright stellar sources in the visit image. The procedure is the following: 1. From a list of candidate detected sources, retain only those with fluxes that exceed a relatively bright (configurable) threshold. 2. Measure the second moments of these sources and exclude those that deviate significantly from the central locus (which are assumed to be populated by point sources). 3. Perform PSF photometry on the remaining sources." "DC3a" "Alternates" "Aperture and PSF fluxes agree to 1.5% on both HSC and LSSTImSim. Examination of PSF models, accuracy of PSF photometry"
"02.03.01.02" "Data Release" " Image Characterization" "Aperture Correction " "meas.pipeline. ApertureCorrectionStage?" "Bickerton" "The PSF stars are also used to determine empirically the aperture correction and it’s spatial dependence on each image. This step determines the correction needed to measured system magnitudes using a finite aperture. The procedure is the following: 1. Perform aperture photometry on the PSF stars, using a pre-configured radius (3.0 arcsec). 2. Determine the aperture correction, defined as the ratio of Flux(PSF)/Flux(Aper), using a second-order polynomial to account for the spatial variation across the image. The aperture correction will be applied to all point sources that are identified." "DC3b" "Alternates" "Generated WCS solutions for LSST ImSim, HSC sims, SuprimeCam?"
"02.03.01.02" "Data Release" " Image Characterization" " WCS Determination " "meas.pipeline. WcsDeterminationStage?" "Dubcovsky" "The WCS calibration for science images is described by a two-dimensional polynomial (the function type and coefficients are found in the header) of a tangentplane projection of stellar coordinates to the image pixel grid. The lower-order terms relate to the location of the reference pixel on the sky, the plate scale, and the rotation of the image, while the distortion terms relate to nonlinear effects of the optical system and differential atmospheric refraction. The magnitude of the terms in the second-order function varies with the filter and with the airmass of the observation. The per-CCD WCS solution is based on the Astrometry.net code. Briefly, the approach is to find asterisms composed of a few stars (typically 4) in the image, and search for similar asterisms (i.e., with similar relative geometry, invariant to position, rotation, and scale) in a reference catalog. This generates hypotheses about where the image might be on the sky. Each hypothesis is checked by predicting where other stars should be found, and evaluating this prediction using Bayesian decision theory. If the image already has a complete WCS, it is possible to skip the first stage and go straight to evaluating whether it is correct. Knowledge about the plate scale and an estimate of the pointing can be used to constrain (and thus speed up) the search." "DC3a" "Alternates" "Generated WCS solutions for LSST ImSim, HSC sims, SuprimeCam?"
"02.03.01.02" "Data Release" " Image Characterization" " WCS Determination " "meas.pipeline. WcsVerificationStage?" "Dubcovsky" "Evaluating whether WCS is correct." "DC3b" "Alternates"
"02.03.01.02" "Data Release" " Image Characterization" " CCD Photometric Calibration " "meas.pipeline. PhotoCalStage?" "AWOL -> Lupton" "An estimate is made of the magnitude zero-point of each science image by comparing the published magnitudes in a reference photometric catalog to their instrumental magnitudes, applying color transformations as necessary. The result of the photometric calibration is to populate the science header with keywords—the pixel values remain unchanged, and have units of detected photons s-1." "DC3b" "Basic"
"02.03.01.02" "Data Release" " Image Characterization" "Exposure Generation " "???" "Create Science Exposure with instrument signature removal" "DC3b" "Alternates"
02/04/07 "Data Release" " Single Frame Source Measurement (Alias SFM)" "Detects and Measures Sources on a single frame. Each slice operates on a single science CCD Exposure." "DC3bPT1.0" "Alternates"
"02.04.07" "Data Release" " Single Frame Source Measurement (Alias SFM)" "SF Source Detection" "meas.pipeline. SourceDetectionStage?" "The calibrated, background-subtracted image is examined for sources, or astrophysical targets in the field of view. A copy of the image is first convolved with a Gaussian function that has the same width in each dimension as the PSF for that image. Pixels above a configurable threshold in this smoothed image are flagged." "DC3bPT1.0" "Alternates"
"02.04.07" "Data Release" " Single Frame Source Measurement" "SF Source Measurement" "meas.pipeline. SourceMeasurementStage?" "From the pixels just flagged, groups of contiguous pixels are measured to determine the centroids, fluxes, and shape parameters of (possibly overlapping) sources. This step is limited to detecting targets smaller than ~10 arcmin in size (i.e., somewhat smaller than the area of sky covered by a single CCD). The resulting measurements (position, brightness, shape, orientation, and errors on those parameters) are recorded in the source catalog of the science database." "DC3bPT1.0" "Alternates"
"02.04.03" "Data Release" " Single Frame Source Measurement" "SF Aperture Correction " "meas.pipeline. ApertureCorrectionApplyStage?" "Bickerton" "Given a set of sources measured, and an apertureCorrection object, apply the aperture correction to the sourceSet." "DC3bPT1.0" "Alternates"
"02.04.03" "Data Release" " Single Frame Measurement" " Compute Source Sky Coordinates " "meas.pipeline. ComputeSourceSkyCoordsStage?" "Lupton/Bickerton?" " Converts pixel coordinates (X,Y) to sky coordinates (ra,dec) (in radians) for all sources in a SourceSet?." "DC3bPT1.0" "Alternates"
"02.04.04" "Data Release" "PSF Match" "PSF Match" "coadd.pipeline.PsfMatchStage?, coadd.pipeline. PsfMatchToModelStage?" "Becker" "PSF-match an Exposure to a model PSF." "DC3bPT1.2" "Alternates"
"02.04.04" "Data Release" "PSF Match" "Warp Exposure" "coadd.pipeline.WarpExposureStage?" "Owen" "Warp (astrometrically remap) an Exposure to a desired WCS." "DC3bPT1.2" "Alternates"
"02.04.04" "Data Release" "PSF Match" "Build Exposure Stack" "coadd.pipeline. coaddGenerationStage" "Owen" "Add Exposures to a coadd Exposure using a weighted sum." "DC3bPT1.2" "Alternates"
"02.04.04" "Data Release" "PSF Match" "Reject Outliers" "coadd.pipeline. OutlierRejectionStage?" "Owen" "Compute an outlier-rejected coadd Exposure: a pixel-by-pixel robust mean of a collection of Exposures. The Exposures must already have the WCS of the coadd" "DC3bPT1.2" "Alternates"
"02.04.04" "Data Release" " Template Generation" "Template Generation (TemplateGen?) Pipeline builds coadded Sky Map Image to be used to construct Template Exposure" "DC3bPT2.0" "Alternates"
"02.04.04" "Data Release" "Template Generation" "Convert Coadd Exposure to Sky Map Image" "Owen" "Given a coadd Exposure generate the appropriate Sky Map Image. This is a null operation if Russell's sky pixelization design is accepted" "DC3bPT2.0" "Alternates"
"02.03.1.03" "Data Release" "Difference Imaging" "Difference Imaging Pipeline handles computation of Difference Exposures by subtracting Template Exposures from Exposures. It also detects and measures DiaSources? on the resulting Difference Images. " "DC3a" "Alternates"
"02.03.1.03" "Data Release" "Difference Imaging" "Identify SkyTile?" "Owen" "Given a Sky Region, identify a SkyTile? that contains data for the region" "DC3bPT2.0" "Alternates"
"02.03.1.03" "Data Release" "Difference Imaging" "Extract Sky Map Image" "Owen" "Given a Sky Region, return a Sky Map Image that contains data for the region" "DC3bPT2.0" "Alternates"
"02.03.1.03" "Data Release" "Difference Imaging" "Convert Sky Map Image to Exposure" "Owen" "Convert a Sky Map Image to an Exposure. This is a null operation if Russell's sky pixelization design is accepted" "DC3bPT2.0" "Alternates"
"02.03.1.03" "Data Release" "Difference Imaging" "Image Differencing" "ip.pipeline.SimpleDiffImStage?" "Becker" "Subtract two almost identical exposures to find and mask additional Crs" "DC3a" "Alternates" "Examination of difference images"
"02.03.1.03" "Data Release" " Difference Imaging" " Difference Detection " "Lupton/Bickerton?" "Detection of bright sources on an exposure. If more than one exposure are provided, the exposures will be added first to create a stacked exposure." "DC3bPT1.0" "Alternates"
"02.04.07" "Data Release" " Difference Imaging" " Difference Measurement " "meas.pipeline. SourceMeasurementStage?" "Measurement of bright sources on an exposure. The resulting measurements (position, brightness, shape, orientation, and errors on those parameters) are recorded in the source catalog of the science database." "DC3bPT1.0" "Alternates"
"02.03.05" "Data Release" " DayMOPS" "DayMOPS generates the predicted ephemerides for the current exposure's sky position" "DC3bPT2.0"
"02.03.05" "Data Release" " DayMOPS" " Setup DayMOPS " "mops.daymops. SetupStage?" "Myers/Jones?" "Determine linking work to be done and set up temporary tables" "DC3bPT2.0"
"02.03.05" "Data Release" " DayMOPS" "Link Intra-Night" "mops.daymops. IntraNightLinkingStage?" "Myers/Jones?" "Link detections from oldest unprocessing night to form tracklets" "DC3bPT2.0"
"02.03.05" "Data Release" " DayMOPS" " Link Inter-Night " "mops.daymops. InterNightLinkingStage?" "Myers/Jones?" "Look for inter-night tracks between unprocessed tracklets and tracklets from previous nights" "DC3bPT2.0"
"02.03.05" "Data Release" " DayMOPS" " Determine Orbits " "mops.daymops. OrbitDeterminationtStage?" "Myers/Jones?" "Attempt to find orbits for all unprocessed tracks" "DC3bPT2.0"
"02.03.05" "Data Release" " DayMOPS" " Manage Orbits " "mops.daymops. OrbitManagementStage?" "Myers/Jones?" "Find and merge redundant orbits" "DC3bPT2.0"
"02.04.05" "Data Release" " Mask Moving Objects" "Mask Moving Objects (MaskMovers?) Pipeline handles the masking of moving objects from science CCD Exposures that are to be used for deep detection and Galaxy multifit measurement. Each slice operates on a single science CCD Exposure as well as (some type of) footprints for all moving objects that appear within that Exposure. " "DC3bPT2.0"
"02.04.05" "Data Release" " Mask Moving Objects" " Mask Moving Object Footprints in Exposure " "???" "DC3bPT2.0"
"02.04.04" "Data Release" " Deep Coadd Generation" "Deep Coadd Generation Pipeline (aka CoaddGen?) handles the co-addition of masked Exposures to form deep templates. " "DC3bPT2.0"
"02.04.04" "Data Release" " Deep Coadd Generation" "Generate Deep Coadds" "coadd.pipeline. ChiSquaredStage?" "Owen" "Create a chi-squared coadd by adding Exposures using the chi-squared algorithm. The exposures must already be warped to the coadd's WCS. This stage generates multi-color coadds that will be used for deep detection/force photometry" "DC3bPT2.0" "Alternates"
"02.04.05" "Data Release" " Deep Detection" "Deep Detection Pipeline (DeepDet?) handles the generation of the deep panchromatic chi-square co-add and detection and measurement on that co-add. Each slice operates on a single sky tile." "DC3bPT2.0"
"02.04.05" "Data Release" "Deep Detection" " Acquire Sky Tile Metadata " " " "DC3bPT2.0"
"02.04.05" "Data Release" "Deep Detection" " Generate ChiSquared? Coadd " "coadd.pipeline. ChiSquaredStage?" "Create a chi-squared coadd" "DC3bPT2.0"
"02.04.07" "Data Release" "Deep Detection" " Detect Sources " "meas.pipeline. SourceDetectionStage?" "Detection of bright sources on an exposure. If more than one exposure are provided, the exposures will be added first to create a stacked exposure." "DC3b"
"02.04.07" "Data Release" "Deep Detection" " Measure Sources " "meas.pipeline. SourceMeasurementStage?" "Measurement of bright sources on an exposure. The resulting measurements (position, brightness, shape, orientation, and errors on those parameters) are recorded in the source catalog of the science database." "DC3b"
"02.03.02" "Data Release" " Source Association Phase 1" "Until deep detection is implemented, Source Association Phase 1 creates Objects by clustering sources." "DC3bPT1.0" "Alternates"
"02.03.02" "Data Release" " Source Association Phase 1" " Cluster Sources " "ap.cluster. SourceClustering?" "Monkewitz" "Discards input sources falling outside the current sky tile and runs the OPTICS clustering algorithm over the remaining sources. The algorithm takes 2 parameters, epsilon and MinPts?, and operates on the set of all sources falling into a sky-tile. These sources are taken from all the CCDs containing at least one raw amp that is within some padding distance P of the sky-tile, where P is chosen based on an estimate of the maximum error in the raw WCSes, and is currently ~15 arcsec. The algorithm visits each source S in the sky-tile (in some arbitrary order). If the epsilon neighborhood of a source S contains at least MinPts? other sources and S has not already been placed into a cluster: 1. Create a new cluster C. 2. Add all the epsilon-neighbors of S that don't already belong to a cluster to C; 3. Recursively perform 2 for each epsilon-neighbor S' of S that has an epsilon neighborhood containing at least MinPts? other sources. If the epsilon neighborhood of S contains less than MinPts? other sources, it is called a noise source and is discarded" "DC3bPT1.0" "Alternates"
"02.03.02" "Data Release" " Source Association Phase 1" " Determine Source Cluster Attributes " "ap.cluster. SourceClusterAttributes?" "Monkewitz" "Computes and outputs source cluster attributes, i.e. Objects." "DC3bPT1.0" "Alternates"
"02.04.02" "Data Release" "Astrometric Model Generation Calibration" "Each slice operates on all Sources within a given sky tile across all epochs. Before the astrometric model for a source can be generated, a Source must be associated with a deep Detection."
"02.04.02" "Data Release" "Astrometric Model Generation Calibration" " Associate Detections and Sources " "Monkewitz" " Associate deep detections with Single Frame Measurement sources with a spatial match" " " "
"02.04.02" "Data Release" "Astrometric Model Generation Calibration" " Calibrate Object Astrometry " "???" "For each Object, fit the Time/Sky? Coordinates for the astrometric parameters, creating a new Astrometric Model containing a goodness-of-fit metric as well as the model parameters" " "
"02.04.06" "Data Release" "Galaxy Model Generation " "Galaxy Model Generation, aka Multifit Pipeline, handles the projection of a detection from a coadd to all the exposures that overlap it, using the list of projected detections to input a stack of ""postage stamp"" images, and fitting of a model using the multifit algorithm. This includes forced photometry of the resulting shape (prototype Object) on each image of the stack to form ForcedSources?." "DC3bPT1.2"
"02.04.06" "Data Release" "Galaxy Model Generation " "Transform Detections" "meas.pipeline. TransformDetectionStage?" "Dubcovsky/Bosch?" "Takes a detection. Computes the image space bounding box for that object for each exposure. Used in postage stamp generation" " DC3bPT1.2" "Empty"
"02.04.06" "Data Release" "Galaxy Model Generation " "Generate Postage Stamps " "Dubcovsky/Bosch?" "Use computed bounding boxes to load postage stamps cutouts from each overlapping exposure." " DC3bPT1.2" "Empty"
"02.04.06" "Data Release" "Galaxy Model Generation " " Multifit " "meas.pipeline. MultifitStage?" "Dubcovsky/Bosch?" "Given a set of postage stamps and a detection, fit a model to all exposures simultaneously. Algorithms: multifit" " DC3bPT1.2" "Empty" "Comparison to simulation inputs"
"02.04.06" "Data Release" "Galaxy Model Generation " " Forced Photometry " "meas.pipeline. ForcedPhotometryStage?" "Dubcovsky/Bosch?" "Given model(s) for an object, measure the flux on each exposure. Algorithm: forced photometry" " DC3bPT1.2" "Empty" "Comparison to simulation inputs"
"02.03.02" "Data Release" " DIA Source Association" "DiaSource? Association (DiaSourceAssoc?) Pipeline handles association of DiaSources? that have not already been associated with MovingObjects? by DayMOPS. It associates them with prototype Objects from Deep Detection and Galaxy Model Generation. Unassociated DiaSources? are taken to be transients and new Objects are created for them."
"02.04.01" "Data Release" "Difference Forced Photometry " "Perform Forced Photometry for Moving & Transient Sources in the Difference Image"
"02.04.01" "Data Release" "Difference Forced Photometry" " NightMOPS " "Predict locations of known objects expected to appear in difference image. " "DC3a"
"02.04.01" "Data Release" "Difference Forced Photometry" " Measure Sources " "???" "Measure predicted objects in difference image" " "
"???" "Data Release" "Object Merge/Association?" "???" "Associate transient objects created by DiaSourceAssoc? with Sources (via a spatial match), and Sources with moving objects. Merge together transient, moving, and deep-detection objects with object measurements and astrometry to produce final objects for ingestion into the data release Object catalogs"
"????" "Data Release" "Generate Astrometric Models" "???" "Calibrate Astrometric Measurements"
"02.04.01" "Data Release" " Photometric Calibration" "Recalibrate Data Release Photometry"
"02.04.01" "Data Release" " Photometric Calibration" " Find Non-gray Extinction " "???" " " " "
"02.04.01" "Data Release" " Photometric Calibration" " Correct for Atmospheric Extinction " "???" " " " "
"02.04.01" "Data Release" " Photometric Calibration" "Assess TOA Mag Distributions" "???" " " " "
"02.04.01" "Data Release" " Photometric Calibration" " Compare Grey Atm with IR Camera Data" "???" " " " "
"02.04.01" "Data Release" " Photometric Calibration" " Calculate Photometric Calibration SDQA Metrics" "???" " " " "
"02.01.03.01" "Data Release" "Assess Data Quality for Data Release" "???" "Summarize quality metrics "
"02.03" "Calibration" "Build Calibration Products"
"02.03.04" "Calibration" "Pre-sequence Exposure Catalog" "Axelrod"
"02.03.04" "Calibration" "Produce Crosstalk Matrix" "Axelrod"
"02.03.04" "Calibration" "Produce Illumination Correction Exposure" "Axelrod"
"02.03.04" "Calibration" "Produce Master Bias Exposure" "Axelrod"
"02.03.04" "Calibration" "Produce Master Dark Current Exposure" "Axelrod"
"02.03.04" "Calibration" "Produce Master Flat Exposure" "Axelrod"
"02.03.04" "Calibration" "Produce Master Fringe" "Axelrod"
"02.03.04" "Calibration" "Produce Pupil Ghost Exposure" "Axelrod"
"02.03" "Alert" "Process Raw Images to Alerts"
"02.03.05" "Alert" "Compute Coarse Ephemerides" "???" "Myers" "Build Ephemerides for night's processingDC3a" "DC2 " "Alternates"
"02.03.05" "Alert" "NightMOPS" "NightMOPS takes time and coordinate information from the exposure and creates a catalog of known solar system objects predicted to be within the exposure FOV." "DC2 " "Alternates"
"02.03.05" "Alert" "NightMOPS" "NightMOPS" "mops.nightMops" "Myers/Jones?" "Select solar system objects whose orbit can intersect the image's FoV. Compute precise ephemerides (with positional uncertainties) at MJD of image. The Forced Sources are those whose ephemerides are inside the image's FoV. "
"02.03.1.01" "Alert" " ISR "
"02.03.1.01" "Alert" "CCD Assembly
" " "
"02.03.1.02" "Alert" "CR Split Handling (Alias: CrSplit?)"
"02.03.1.02" "Alert" " Image Characterization (Alias: ImChar?)"
"02.03.02" "Alert" "Source Association" "Monkewitz" Correlates difference sources with known objects -- either fixed or moving objects predicted to be within the FOV -- to determine whether new objects have been detected, in which case a new object is created, stored and made available for association in future visits. The associations can be used to avoid issuing an alert for a difference source matching a known moving, variable or transient object. "DC2" "Basic"
"02.03.1.03" "Alert" "Difference Imaging"
"02.03.03" "Alert" "Alert Generation Pipeline" "Post Alerts on selected Objects found during processing"
"02.03.03" "Alert" "Alert Generation Pipeline" "Process Alerts" "???"
"02.01.03.01" "Alert" "Alert Production SDQA Monitoring" "Perform DQA on each visit exposure and each exposure's derived products"
"02.01.03.01" "Alert" "Alert Production SDQA Monitoring" "SDQA Pipeline per Exposure" "???" "DC3a"
"02.01.03.01" "Alert" "Generate SDQA Summary for Entire Alert Production Run"
"02.01.03.01" "Alert" "Generate SDQA Summary for Entire Alert Production Run" "Retrieve SDQA Flags and Status for all Exposures" "???"
"02.01.03.01" "Alert" "Generate SDQA Summary for Entire Alert Production Run" "Compute Selected Summary SDQA Information" "???"
" "
"Deprecated"
"02.03.1.01" "Data Release" " ISR" " Acquire Visit Metadata " "subsumed in Butler" "DC3bPT1.0" "Basic"
"02.03.1.01" "Data Release" " ISR" " Transform Metadata " "subsumed in Butler" "DC3bPT1.0" "Basic"
"02.03.1.01" "Data Release" " ISR" " Validate Metadata " "subsumed in Butler" "DC3bPT1.0" "Basic"
"02.03.1.01" "Data Release" " ISR" " Identify Calibration Product " "subsumed in Butler" "DC3bPT1.0" "Basic"
"02.03.1.02" "Data Release" " CR Split Handling" " Difference Detection " "<Img Char subsumed>" " " "DC3bPT1.0" "Basic"
"02.03.1.02" "Data Release" " CR Split Handling" " Mask and Sum " "<Img Char subsumed>" " " "DC3bPT1.0" "Basic"
"Note"
"ISR, CCD Assembly, CRSplit Handling, Image Characterization, Difference Imaging, and nightMOPS are shared w/o significant change with DR Release and Alert Production"
"Implementation Maturity (col H):
* Empty: possibly no UML design, definitely not implemented in Data Challenge.
* Basic: similar to UML Basic Course spec; may not have design 'alternate courses' or error recovery gracefully implemented.
* Alternates: design includes alternate courses and implementation handles exceptional data and events gracefully.
* Complete: Design meets science requirements and implementation meets design requirements."