The COMBO-17 project status:
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project definition & preparation: | 100% done | |
development & test of reduction pipeline: | 100% done | |
development of calibration & classification: | 100% done | |
observations: | 100% done | |
data reduction (fields AXAF, A901, S11): | 100% done | |
data reduction (fields A226, SGP): | 100% done | |
science analysis: | 80% done | |
publication: | 75% done | |
II. Project definition and preparation:
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The COMBO-17 project was started after three inspiring prerequisites came together:
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III. Development of reduction pipeline, calibration and classification:
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A reduction pipeline for dithered WFI survey images has been developed for the MIDAS environment with participation by S. Dye, M. Kleinheinrich, K. Meisenheimer and C. Wolf in the years 1999 and 2000. This pipeline is installed as a MIDAS context file named WFI and makes use of the other context packages MPIAPHOT and CADIS, which were developed by the CADIS team from 1997 to 1999. All elements of the pipeline have been tested and work as desired. The pipeline consists of two main parts:
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IV. Observations:
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All observations were performed with the Wide-Field Imager at the MPG/ESO 2.2-m telescope at La Silla observatory, Chile, and finished by January 2001. A total of 48.5 nights have been used for COMBO observations, with 38 usably clear nights in seeing below 1.4 arcsec. A dither pattern with 2'x 3' size is used for cosmic correction, compensation of CCD cosmetics and for the construction of science flats. The latter are needed any time in the far-red filters and for all filters observed before Feb, 4, 2000 due to scattered light in the flatfields. | |
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run | code | date period | nights | turnout | fields | observers | |
Feb 99 | A | 11.02.-22.02.1999 | 9 | ~75% | A901, S11 | CW, RW | |
Jun 99 | B | 03.06.-17.06.1999 | 2 | ~90% | S11 | JE, SW | |
Aug 99 | C | 04.08.-08.08.1999 | 2.5 | ~90% | SGP | JG | |
Oct 99 | D | 07.10.-22.10.1999 | 12 | ~50% | SGP, FDF, AXAF | CW, TK | |
Jan 00 | E | 28.01.-11.02.2000 | 15 | ~90% | AXAF, A901, S11 | CW, MK, KM | |
Oct 00 | F | 00.09.-00.09.2000 | 5 | ~90% | SGP, FDF, AXAF | MK | |
Jan 01 | G | 19.01.-20.01.2001 | 2 | ~90% | AXAF, A901, S11 | CW, KM | |
May 02 | H | 00.05.-30.05.2002 | 1 | ~90% | S11 | service | |
Aug 02 | I | 16.08.-13.09.2002 | FDF, A226 | service | |||
Oct 02 | O | Periode P69 | SGP | service | |||
Aug 03 | J | 08.08.-28.08.2003 | AXAF, A226 | service | |||
Dec 03 | K | 02.12.-20.12.2003 | SGP, A226 | service | |||
Dec 04 | L | 01.12.-19.12.2004 | SGP, A226 | service | |||
Aug 05 | M | 08.08.-12.08.2005 | SGP, A226 | service | |||
Dec 05 | N | 20.11.-04.12.2005 | SGP, A226 | service | |||
Nov 06 | P | 13.11.-28.11.2007 | 2 | ~95% | SGP, A226 | CW, MZ (MPIA service) | |
V. Data reduction:
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Data reduction is now complete and has been performed with MIDAS image processing software on SUN Enterprise workstations. Many additional routines are used and installed as context environments CADIS, MPIAPHOT and WFI. Disk space includes a Terabyte raid system, where individual frames needed for accurate photometric error calculation can reside on disk. For details on the reduction procedure we refer to our WFI processing cookbook. Data quality control includes inspection of flatfields, success of cosmic correction, depth and background properties of the sum images, precision checks for the coordinate projection onto all individual frames, and finally checking error distributions and calibrations in the final flux table of the object catalog. |
VI. Results:
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see Results & Papers page |
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Last update May 10, 2007, CT/CW