KCWI Reduced Products Quicklook (Lev1) and Science Ready (Lev2)
KCWI raw data is processed via the KCWI DRP pipeline. When available, a Quicklook (Lev1) and Science Ready (Lev2) link is shown in the search results "Previews" column for individual koaids. When downloading KCWI data, choose "Include extracted/calibrated data" to receive a script (curl and wget options) to download all the individual products. The products are of the form:
KCWI Reduced Product file types
| File name format | File type | Description |
|---|---|---|
| Processing | ||
| DRPF.log | LOG | Log file created by the DRP framework |
| KCWI.log | LOG | Log file created by the KCWI DRP, info related to reducing the data |
| kcwi.*.cfg | CFG | KCWI RTI DRP configuration file |
| kcwi.proc | LOG | DRP processed filelist |
| Science Files | ||
| KOAID.*_icubed.fits | FITS | Differential atmospheric refraction corrected data |
| KOAID.*_icubes.fits | FITS | Data cube flux calibrated by standard star |
| Images | ||
| arc.*_atlines.png | IMG | ThAr normalized flux |
| arc.*_coef*.png | IMG | ThAr coefficient for individual bars |
| arc.*_nlines.png | IMG | Number of ThAr lines per bar |
| arc.*_resid.png | IMG | ThAr RMS per bar |
| bars.*.png | IMG | Spatial control points |
| bias.*_rdnoise.png | IMG | Bias readnoise per amplifier |
| scat*.png | IMG | Scattered Light Fit |
| sky*.png | IMG | Master Sky |
| arc_*_ThAr_*_*_atoff.png | IMG | Offset wavelength solution for slice 11 fitted atlas emission lines |
| arc_*_ThAr_*_*_*_baroffs.png | IMG | Pixel offsets of cwave at 5 pts across each slice with respect to slice 11 |
| arc_*_ThAr_*_*_cdisp.png | IMG | Dispersion at 5 pts across each slice at the central wavelength |
| arc_*_ThAr_*_*_cwaves.png | IMG | Central wavelength at 5 pts across each slice mapped to the wavelength scale of slice 11 |
| std_*_*_*_*_*_cal.png | IMG | Calibrated flux of the standard star as a function of wavelength, units ergs/s/cm^2/Ang; shows data vs reference |
| std_*_*_*_*_*_eff.png | IMG | Estimated effective efficiency (%) as a function of wavelength; shows data vs fit |
| std_*_*_*_*_*_invsens.png | IMG | Transformation from count rate to flux as a function of wavelength, units flux/e/s; shows data vs fit |
| std_*_*_*_*_*_resid.png | IMG | Residual (calibrated observed spectrum - reference)/reference as a function of wavelength, in % |
Please acknowledge the use of KOA by including this text in your publications:
This research has made use of the Keck Observatory Archive (KOA), which is operated by the W. M. Keck Observatory and the NASA Exoplanet Science Institute (NExScI), under contract with the National Aeronautics and Space Administration.
Please also acknowledge the PI(s) of datasets that have been obtained through KOA, and please contact the KOA Help Desk if you publish archival data.
If your research uses data reduced by the DEIMOS, KCWI, MOSFIRE, or NIRES PypeIt DRP, please use the PypeIt Citation.
If your research uses data reduced by the KPF DRP, please use the citation as described in the README.md.
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The Keck Observatory Archive (KOA) is a collaboration between the NASA Exoplanet Science Institute (NExScI) and the W. M. Keck Observatory (WMKO). NExScI is sponsored by NASA's Exoplanet Exploration Program, and operated by the California Institute of Technology in coordination with the Jet Propulsion Laboratory (JPL).
