Version 2.4 (implemented August 2017) :
More information coming soon.
Version 2.3 (implemented February 2017) :
2) There is fix to a bug introduced in version 2.2 where the header keyword RADESYS was set incorrectly defined as '''ICRS''' (using triple quotes instead of single quotes), causing issues with the usability of the WCS solution in the image header. Also included is a change to the definition of the WCS CTYPE keyword from TAN to TPV for improved compatibility with iraf post-processing workflows. Lastly the swarpstack function will now define the RA and DEC keywords in image stacks.
3) Minor internal bug fixes. Reduced images should be unaffected by these changes.
Version 2.2 (implemented December 2016) :
!!!!Warning [Feb 16 2017]: A revised WCS template was introduced in version 2.2. Unfortunately, the new WCS template introduced contained a bug, where the header keywords RADESYS, CTYPE1, and CTYPE2 were populated incorrectly. This error is corrected as of quick reduce version 2.3.
If your data has been processed by QuickReduce v2.2 (as indicated by the header keyword GITBRNCH, please contact the PPA team for instructions on how to either: 1) fix the keywords in your data, or 2) reprocess your data.
2) Where available, SDSS DR13 is used for photometric calibration.
Version 2.1 (implemented October 2016) :
First QuickReduce deployment from Github. This release is primarily a technical release to improve robustness of pipeline operation. Impact on actual scientific data products is minimal compared to the previous version (2.0).
1) Various internal improvements for debugging and logging
2) New header keywords added:
GITBRNCH- QuickReduce version/branch name
GITCOMIT- Code revision commit hash (allows pull of exact version- for advanced github users)
3) Enables comparison of MasterCals with fiducial references (for Pipeline Operator)
4) Improved fringe template generation and fringe removal
5) Improved SExtractor catalog generation
Version 2.0 (July 2015; previous data reprocessed) :
1) Improved pupil ghost template
2) Improved WCS calibration, in particular in denser fields or for narrow-band exposures
3) Stacking improvements: Added illumination correction generation and application; more flexible photometric zeropoints; background normalization
4) Reduction log included in image headers
5) Support for twilight flats in creating mastercals
6) Improved cross-talk correction
Sub-versions to v2.0: These are relatively minor changes implemented in the pipeline, but data taken previous to their release were not reprocessed:
Version 2.0.5 (July 2016)
1) 5x6 fringe templates implemented in i- and z-band
Version 2.0.4 (June 2016)
1) New pupil ghost template and scaling for improved removal of pupil ghost from flat fields
2) New bad pixel mask which includes more regions affected by hot/dead pixels
3) Added support for a new narrow band filter, odi_NB695
Version 2.0.3 (May 2016)
1) Reworked internal communication to improve stability inside PPA (no changes to science functionality)
2) Improved stray-light mitigation during mastercal flat-field generation
Version 2.0.2 (Feb 2016)
1) u-band support
2) Stacking Improvements: Minimized memory demands, support for improved cleaning and rejection of guide-OTAs and broken cells
Version 2.0.1 (Nov 2015)
1) Added support to handle TFLATs and DFLATs simultaneously but separately
Version 1.1 (implemented May 2014; previous data reprocessed; final release for pODI data):
1) Illumination correction added
2) Photometric zeropoint plots and maps added to data products
3) When SDSS coverage is not available, the Pan-STARRs IPPRef catalog is used.
4) PSF shape calculations and diagnostic plots added
5) Persistency masking improvements
6) New WCS algorithm
7) Improvements to exposure scaling when stacking
QuickReduce Version 1.0
An upper-level flow description of the functionality in the QuickReduce pipeline is as follows:
1) Pixels affected by persistency and trailing are masked as non-usable. A catalog of saturated pixels is created
2) Defective cells are masked out. A cell is defined as the 512x512 pixel subsection, 64 of which comprise an OTA.
3) Cross-talk between cells in the same row is corrected.
4) Static bad pixels are masked out.
5) Overscan levels are calculated and subtracted for each cell.
6) Bias and dark-current are subtracted.
7) Non-linearity is corrected.
8) All cells in an OTA are collected into a monolithic frame.
9) Cosmic rays are identified and removed.
10) Fringe affects are removed in the i’ and z’ bands, using a template.
11) Sources are extracted and a catalog is created for each OTA, using SorceExtractor.
12) Astrometric calibration is performed using 2MASS as the astrometric reference catalog.
13) Source photometry is matched to SDSS, where available, and photometric zeropoints are calculated.
14) Output images, metadata, FITS tables, and diagnostic plots are created.
QuickReduce also includes support for stacking of ODI exposures using SWarp. For a more detailed description of any/all of these steps, please refer to:
Kotulla and Harbeck (ref.)