Presentation on theme: "MIPS Data Processing for SINGS George J. Bendo & Chad Engelbracht (A ''George's Adventures in Learning OpenOffice'' Presentation)"— Presentation transcript:
MIPS Data Processing for SINGS George J. Bendo & Chad Engelbracht (A ''George's Adventures in Learning OpenOffice'' Presentation)
Overview ● Brief review of MIPS ● Description of observational data ● Data checks ● Mosaicing data ● Parallel pipeline processing
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
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
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.
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
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.
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
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
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
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