sings and smart
DESCRIPTION
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 - PowerPoint PPT PresentationTRANSCRIPT
SINGS and SMART
3 April 2001
Tucson, AZ
L. ArmusSIRTF Science Center
Mar 01LA - 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
Mar 01LA - 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
Mar 01LA - 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
Mar 01LA - 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.
Mar 01LA - 6
SMART Legacy Contacts
Program PI Contacts
Formation and Evolutionof Planetary Systems
Michael [email protected]
Dean [email protected]
SINGS Rob Kennicutt Claus Leitherer
Lee Armus
From Molecular Clouds toPlanets
Neil Evans [email protected]
Geoff [email protected]
Ewine van [email protected]
Mar 01LA - 7
IRS Slits (details)
54.6 “54.6 “
Short-Low2nd Order 1st Order
3.6 “
23 “
(5.3 –7.5 m)
Short-High11.8 “
5.3 “ Long-High
22.4 “
11.1 “
(7.5 –14.2 m)
(10.0–19.5 m) (19.3–37.0 m)
9.7 “
Long-Low
151.3 “ 151.3 “
2nd Order 1st Order(14.2 – 21.8 m) (20.6 – 40.0 m)
43 “
[1st Order (7.5 –8.5 m)]
Mar 01LA - 8
IRS Peakup
72“ 72”
60”Blue Red
37 “
Peak-UpApertures
Short-Low Array
128 x 128 pixels(1.8 arcsec /pxl)
2nd
Ord
er
5.3
7.5
m
1st
Ord
er s
pect
rum
7.5
14.
2m
Bluepeakup
Redpeakup
(13.318.7 m) (18.526 m)
VignettedField
1st Order7.5-8.5
Mar 01LA - 9
IRS High-res Maps
15.7
11.85.3
23.6
Short-HI
33.5
22.4
11.1
44.8
Long-HI
The current plan is that for both SH and LH we use 3x5 grids whosedimensions are indicated above. Steps are 1/2 slit width or length. The blue boxes indicate the size of a single slit wrt the grid.
Mar 01LA - 10
IRS Wavelength Coverage
IRS Low-Res
IRS High-Res