ADASS 2004 PanSTARRS Eugene Magnier PanSTARRS The Image

ADASS 2004 : Pan-STARRS Eugene Magnier Pan-STARRS The Image & Processing Pipeline Eugene Magnier University of Hawaii Institute for Astronomy ADASS XIV - Pasadena, CA October 25, 2004

ADASS 2004 : Pan-STARRS Summary ● ● ● Eugene Magnier of Topics Pan-STARRS Overview IPP within Pan-STARRS Data Analysis Plan IPP System Architecture IPP Data Products

ADASS 2004 : Pan-STARRS The PI: Eugene Magnier Pan-STARRS Nick Kaiser Concept (If. A)

ADASS 2004 : Pan-STARRS Eugene Magnier by the numbers PS-4 system parameters: ● 4 telescopes (1. 8 m each) ● 1 Gigapixel per telescope (each 7. 5 deg 2) ●grizy + w filters ● 40 seconds per exposure ● 5� detection ~ 24. 5 mag ● 100� detection ~ 20. 0 mag ●Observable sky every ~7 nights (including weather) ●~4000 Gigapixel images per night (8 TB) ●~2. 5 PB per year of raw PS-1: images ●Engineering Prototype ●Verification Surveys (MVP & IVP) ●AP Survey in prep for PS-4 PS-1 goes here

ADASS 2004 : Pan-STARRS IPP Eugene Magnier within Pan-STARRS If. A: Nick Kaiser ●Eugene Magnier ●Paul Price ●Josh Hoblitt ●Robert Lupton ●Dave Monet MOPS ● Telescopes Cameras OTIS raw images Preferred Science Clients metad ata, detec tions IDs static sky metadata metad ata, detec tions IDs IPP metadata, imagesdetections PSPS filtered detections metadata static sky MHPCC: ●Bruce Duncan ●Mike Berning ●Robert De. Sonia ●George Science Gusciora Client Legend orbits ●Ross Exte Prefe identifications PS rnal. Harman rred Subsyst Syste Sci em m Client ●Eric van pixel data Alst photons meta & imagesother data World Users Solar System Community & object data commands

ADASS 2004 : Pan-STARRS Data Eugene Magnier Analysis Plan Phase 2 (Image Process) raw stacked image Static Sky Images static sky image + cleaned stacked image Phase 4 (Image Combi difference image (P 4�)

ADASS 2004 : Pan-STARRS Data Eugene Magnier Analysis Data has Details units of: cell, chip, mosa Analysis is staged by data unit: ●Phase 1: analysis preparation (mo ●Phase 2: single image analysis (c ●Phase 3: calibration improvements ●Phase 4: image combinations (fram

ADASS 2004 : Pan-STARRS IPP ● ● ● Image Eugene Magnier Processing Responsibilities: Processing of single images (phase ●remove instrumental signature ●bright object detection / basic c ●initial astrometric & photometric c Merging of image groups (phase 4) ●warp & resample to reference imag ●stack and CR-reject ●subtract static sky image ●measure objects on difference & su ●update static sky Construct Calibrations ●basic calibration images (bias, da ●derived calibration images (fringe ●other calibration data (optical d Analysis Trace & Monitor System Characterization

ADASS 2004 : Pan-STARRS IPP System Eugene Magnier Architecture state machine (not event d system infrastru independent o architectural are stand-al

ADASS 2004 : Pan-STARRS Hardware Eugene Magnier Organization: optimized for

ADASS 2004 : Pan-STARRS IPP Eugene Magnier Software Architecture processing scheduler parallel processing controller processing scripts / Software analysis stages Tools: (phase 0 -4, cal 1 CVS 3, Astrom. Ref, SWIG Photom. Ref) bugzill modules a (debias, convolve, doxygen flatten, findobjects, eups etc) autocon PSLib [includes f wrappers to externals] make (images, vectors, gcc errors, syscalls, etc) External Libraries External Systems (glibc, glib, gsl, (Lustre? , GFS? , CFITSIO, FFTW, SLALIB, Mysql, Apache, etc)

ADASS 2004 : Pan-STARRS IPP ● ● ● Data Eugene Magnier Products Imaging Data Products: ●Static Sky images ●Postage Stamp Images Object Measurements ●P 2, P 4 S, P 4 D, Static Sky ●rudimentary object associations ●photometric / astrometric calibrat Metadata ●image information from summit ●weather & other ancillary summit d ●analysis statistics ●analysis history ●calibration information All external data products are sent MOPS & other science clients also r

ADASS 2004 : Pan-STARRS Phase ● 2 Eugene Magnier Issues Flat-fields are corrected based o

ADASS 2004 : Pan-STARRS Phase ● ● ● 2 Eugene Magnier Issues Flat-fields are corrected based o fringe frames may be built with a fringe correction may be based on

ADASS 2004 : Pan-STARRS Phase ● ● ● 2 Eugene Magnier Issues Flat-fields are corrected based o fringe frames may be built with a fringe correction may be based on minimal object parameters (x, y, high detection threshold (~20 sigm we keep postage-stamp images on a

ADASS 2004 : Pan-STARRS Static ● ● ● Sky Eugene Magnier Analysis Detailed object analysis including ●complex object deblending a la SDS ●simultaneous multi-band analysis Analysis is NOT performed nightly ●Static Sky changes slowly ●Goal is deep science, not variabili ●Analysis is computationally more inte Rolling Analysis: ●~1 degree RA strips per day ●only RA within 10 degrees of solar

ADASS 2004 : Pan-STARRS Phase ● ● 4 Eugene Magnier Issues overlapping pixels are mapped to c Object detections are perfomed on: ●Difference Images (P 4 D) to low thr ●Improved Summed Images (P 4 S) to mo Static Sky is updated note caveat in CR rejection for seq Phase 2 images: 0. 3 arcsec/pix Chip/Cell units Phase 4 images: 0. 2 arcsec/pix Static Sky cells