1. MIPS Data Processing for SINGS George J. Bendo & Chad Engelbracht (A ''George's Adventures in Learning OpenOffice'' Presentation)

2. Overview ● Brief review of MIPS ● Description of observational data ● Data checks ● Mosaicing data ● Parallel pipeline processing

3. MIPS Overview Three detector arrays – 128x128 24  m array – 32x32 70  m array – 2x20 160  m array Will provide – Photometric maps – Low-resolution spectra in 55 - 95  m range

4. MIPS Observing Modes for SINGS Scan Mapping (or Photometry Mode for smaller targets) – Telescope drifts by targets as mirror in MIPS keeps image steady for multiple adjacent BCDs – Each AOR may contain tens to thousands of individual BCDs – Each observation consists of 2 AORs (for spatial sampling and asteroid rejection) SED Mode – Telescope slit is pointed at a series of adjacent locations to form data cube

5. Example Data: NGC 3184 Generated simulated data for demonstration – Started with U-band image from NED – Convolved image with MIPS PSFs – Flux calibrated data with IRAS data – Added images to backgrounds provided by H. Dole et al.

6. Scanned region of NGC 3184 (70  m)

7. Example of MIPS Scan Map Data

8. Data Checks Fits header checks – Basic header keywords – Proposal & observer name – Target name – AOT & AOR information – Observing mode – Integration time – Coordinates – Map or SED observing parameters Pipeline data checks – Number of BCDs – BCD image size – Movement of target from BCD to BCD – Noise levels per BCD

9. List of Fits Header Keywords in Check General Keywords ● KEYWORD ● NAXIS ● NAXIS1 ● NAXIS2 ● TELESCOP ● INSTRUME ● CHNLNUM ● AOT_TYPE ● AORLABEL ● FILETYPE ● FOVID ● FOVNAME ● ISPRIME ● RDOUTMOD Scan Map Keywords ● SCANRATE ● REQ160 ● FASTRES ● NMAPCYCL ● NSCANLEG ● SCANLEN ● STEPFOR ● STEPREV ● OBSRVR ● PROGID ● SAMPTIME ● OBJECT ● RA_HMS ● DEC_DMS ● RA_CMD ● DEC_CMD Photometry Super- Resolution Keywords ● LARGE24 ● NCYCL24 ● LARGE70 ● NCYCL70 ● LARGE160 ● NCYCL160 SED Keywords ● CHOPDIST ● NCYCLES ● COLSTEP ● ROWSTEP

10. Mosaicing The individual frames will be combined with the mips_enhancer software, which will produce a mosaic of the images as well as enhancing the data. Further checks of the observations will include checking the signal-to-noise ratio of the final data product, checking the quality of the PSF, and comparing the fluxes to IRAS fluxes. The final data products will include the straight mips_enhancer output and trimmed, background-subtracted, resampled versions.

11. Comparison of Input and Output 24  m Data

12. Comparison of Input and Output 70  m Data

13. Comparison of Input and Output 160  m Data

14. Parallel Pipeline Processing To check the data products from the SSC pipeline, the raw MIPS data will also be processed with developmental software written by the MIPS group ● mips_sloper – Processes charge ramps into slopes for all pixels – Removes cosmic rays – Performs transient correction ● mips_caler – Data calibrated – Dark current subtracted

15. Example of Output from mips_sloper

16. Summary ● Prepared series of checks on data output to check observations ● Have software for producing simulated data ● Have software for mosaicing pipeline data from SSC ● Have developmental software for additional parallel pipeline processing

17. Mosaicer Schedule 5 Sep 2002 (Version 1) – No interpolation (directly from BCD to final mosaicked image) – Distortion correction and outlier rejection Late 2003 (Version 1.n) – MIPS/SINGS review of progress and possible decision to use an intermediate version for SINGS MIPS deliveries – May decide to continue to use version 1 2003-2004 – Add instrumental signatures removal based on redundancy – Iterative approach driven by actual MIPS data – Stim flash latents, long-term drift,... Late 2004 (Version 2) – Will be used to create the final MIPS SINGS data products

18. Simulator Schedule Jun 2002 – Given AOR and image, will produce input for mips_enchancer Aug 2002 – Produce input for full MIPS pipeline (charge ramps) including distortions Sep 2002 – Add the capability to do SED AORs Dec 2002 – Add instrumental signatures ● Cosmic rays ● Stim flash latents ● Long term drift