Difference: Pipeline (1 vs. 6)

Revision 62017-01-12 - KarlVyhmeister

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IFU Data Reduction pipeline

Revision 52016-10-17 - DonNeill

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IFU Data Reduction pipeline

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Current version in Nick Konidaris/Don Neills Github.
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Current version in Nick Konidaris/Don Neill's Github.
  Quick Guide for automated pipeline can be found here.

Revision 42016-03-01 - DonNeill

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IFU Data Reduction pipeline

Current version in Nick Konidaris/Don Neills Github.

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Quick Guide for automated pipeline can be found here.
 

Photometric Data Reduction pipeline

Revision 32016-02-29 - NadiaBlagorodnova

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IFU Data Reduction pipeline

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Current version in Nick Konidaris/Don Neills Github.
 

Photometric Data Reduction pipeline

Revision 22016-02-29 - NadiaBlagorodnova

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Data Reduction pipeline

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IFU Data Reduction pipeline

  Current version in Nick Konidaris Github.
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Photometric Data Reduction pipeline

 
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Location

/scr2/nblago/kpy/SEDMrph/rcred.py

Requisites

Ureka must be setup before running the pipeline.

Usage

  • First, reduce the photometry for the night's directory:
python /scr2/nblago/kpy/SEDMrph/rcred.py -d 2016XXXX

  • Second, calibrate the zeropoints:
python /scr2/nblago/kpy/SEDMrph/zeropoint.py -d 2016XXXX/reduced

  • Third, call the aperture photometry:
python /scr2/nblago/kpy/SEDMrph/app_phot.py -d 2016XXXX/reduced

Operation

/scr2/nblago/kpy/SEDMrph/rcred.py

Steps:

  1. Solve astrometry on the entire image.
  2. Compute master bias (if it does not exist) and de-bias the image.
  3. Separate the image into 4 filters.
  4. Compute flat field for each filter (if it does not exist) and apply flat fielding on the image.
  5. Computes cosmic ray rejectionon the entire image.
  6. Compute zeropoint for each image and store in a log file.
  7. Plot zeropoint for the night.
 

-- NadiaBlagorodnova - 27 Oct 2015 \ No newline at end of file

Revision 12015-10-27 - NadiaBlagorodnova

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Data Reduction pipeline

Current version in Nick Konidaris Github.

-- NadiaBlagorodnova - 27 Oct 2015

 
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