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SINGS and SMART

SINGS and SMART. 3 April 2001 Tucson, AZ. L. Armus SIRTF Science Center. SMART. SMART is an IRS data reduction and analysis tool being written by the IRS GTO team with support from the SSC. The basic functionality of SMART will allow it to: read and write FITS files and ASCII tables

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SINGS and SMART

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  1. SINGS and SMART 3 April 2001 Tucson, AZ L. Armus SIRTF Science Center

  2. SMART SMART is an IRS data reduction and analysis tool being written by the IRS GTO team with support from the SSC. The basic functionality of SMART will allow it to: • read and write FITS files and ASCII tables • display and examine 2D and 1D data files • calculate statistics and modify data interactively • combine data sets • provide for optimal extraction of point and extended sources • fit and/or subtract a variety of continuua and lines

  3. SMART General guidelines • Joint development with Legacy teams is desirable • SMART will be written in IDL, and take advantage of existing procedures/packages (e.g. ISAP) as much as possible • SMART will use the ATV display program (http://cfa-www.harvard.edu/~abarth/atv/atv.html) • A fully tested version of SMART will be available by launch • It is a goal (not a requirement) of the IRS GTO team to make SMART available to the GO’s • The SSC will provide user support (distribution, trouble-shooting, etc.) and be involved in all stages of the development

  4. SMART Schedule 06/2001 – Delivery of pipeline processed test frames to IRS team from the SSC 07/2001 – Detailed definition of SMART development plans, team contributions and schedule = following Legacy WG meeting 12/2001 – Preliminary beta-test version of SMART available 04/2002 – SMART enters primary test phase 06/2002 – Functional version of SMART available to the Legacy teams and the SSC

  5. A Plan for SINGS In order to take full advantage of SMART we should : 1. Provide a clear outline of what we need before the Legacy WG meeting – step/stare (high-res) = analysis tools and map (cube) assembly – spectral mapping (low-res) = cube assembly removing all the “peculiarities” of the mode (i.e. drop outs, synchronization, etc.) 2. Commit 0.5–1 FTE to SMART development (focusing on spectral mapping mode data) during the 8–12/2001 period. 3. Provide a high level of SINGS team involvment during the SMART testing phase from 1–5/2002. 4. Commit a full FTE to SMART development for the 4–6/2002 period.

  6. SMART Legacy Contacts

  7. IRS Slits (details) 54.6 “ 54.6 “ 23“ Short-Low 3.6 “ 2nd Order 1st Order (7.5 –14.2 m) (5.3 –7.5 m) [1st Order (7.5 –8.5 m)] 151.3 “ 151.3 “ 43“ 9.7 “ 2nd Order 1st Order Long-Low (20.6 – 40.0 m) (14.2 – 21.8 m) 22.4“ 11.8“ Long-High Short-High 5.3“ 11.1“ (19.3–37.0 m) (10.0–19.5 m)

  8. IRS Peakup 72“ 72” 37“ Peak-Up Apertures Vignetted Field Red Blue 60” (18.526 m) (13.318.7 m) 1st Order 7.5-8.5 Red peakup Short-Low Array 128 x 128 pixels (1.8 arcsec /pxl) 1st Order spectrum 7.5  14.2m 2nd Order 5.3  7.5m Blue peakup

  9. Long-HI Short-HI 33.5 5.3 11.8 11.1 23.6 22.4 44.8 IRS High-res Maps 15.7 The current plan is that for both SH and LH we use 3x5 grids whose dimensions are indicated above. Steps are 1/2 slit width or length. The blue boxes indicate the size of a single slit wrt the grid.

  10. IRS Wavelength Coverage IRS High-Res IRS Low-Res

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