Science Pipelines Walkthrough: DRP Jim Bosch, DRP Scientist Future - - PowerPoint PPT Presentation

Science Pipelines Walkthrough: DRP

Jim Bosch, DRP Scientist

Future Pipeline Flow Overview

LSSTJTM - 2017-03-06 - Glendale, CA 2

ImChar

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Image Characterization ISR, PSF moding, initial background estimation, initial astrometric and photometric calibration, and Sources visits are independent, CCDs are mostly independent

JointCal

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Joint Calibration refine astrometric and photometric calibration refine PSF star positions all visits in an area of sky

Coaddition and Difference Imaging

LSSTJTM - 2017-03-06 - Glendale, CA 5

Make coadds (including templates) Find junk Refine background estimation Measure DIASources

Coadd Processing

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Define Objects by associating DIASources and detection from a variety of coadds. Deblend pixels using a set of coadds. Measure Objects on the coadds.

MultiFit

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Fit individual Objects or groups of Objects using all visit-level images that overlap their position. Includes galaxy model and moving point-source model for every Object. Includes Forced Photometry.

Postprocessing

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• Estimate photometric redshifts.
• Find Solar System Objects, estimate orbits.
• Generate geometric depth/completeness masks.
• Run star/galaxy classification and variability characterization metrics.
• Apply calibrations to raw measurements.

Lower Levels

• All of these pipelines are (conceptually) CmdLineTasks (or

SuperTasks, in the future).

• Below that level, LDM-151 also describes reusable "Algorithmic

Components" that can generally be mapped to regular Tasks: e.g. source detection, image subtraction, astrometric matching.

• And below that level, we have "Software Primitives": low-level

data structures like Images and Psfs.