Principal: Deborah Padgett
Deputy: Chad Engelbracht
Data Monkey(s):
Priority: Critical
Downlink Priority: Normal
Analysis Time: 24 hours
Last
Updated: Mon Nov 04 2002, 10:43:21
Confirm that MIPS 24 µm photometry works as expected in a rudamentary
way
Description
Execute MIPS 24 µm photometry AOT for a few parameter selections.
For the preliminary validation, only the small field option is tested.
This task is implemented by commanding one cycle of 24 µm small field
photometry for each exposure time (3, 10, 30 seconds). In addition, 3 cycles
of the same AOT are commanded for only the 3 s exposure time.
Data Collected
This task is implemented by commanding one cycle of 24 µm small field
photometry for each exposure time (3, 10, 30 seconds). In addition, 3 cycles
of the same AOT are commanded for only the 3 s exposure time. The target
star was carefully selected to be unsaturated in 30 s exposures, but detetable
in 3 s exposures.
Data Reformatting Requirements
Array Data Desired:
24 µm
Data Reformatting Option:
NONE
1 FITS file per DCE per array
NORMAL
1 FITS file per AOR per array.
Special Instructions:
Task Dependencies
MIPS-110
Calibration Dependencies
CSMM parameters known
distortion correction applied
Output and Deliverable Products
This task will confirm that the combination of FOV offsets and mirror parameters
used in the MIPS Ph/SR AOT places the target in the expected positions
on the array. The output product for this task will be altered versions
of the IPP files and FOV table positions for MIPS 24 µm small field
photometry.
Data Analysis
The data analysis for this task involves comparing the positions of the
stellar image on the array to the positions expected based on the input
CSMM parameters and FOV table.
Software Requirements
DAT and/or SSC BCD/Post-BCD pipeline
ATV - IDL image viewer
IDP3 or other centrioding package
"fv" - Goddard "lheasoft" package
plotting package (SM, IRAF, IDL)
Actions Following Analysis
The FOV table and MIPS configuration IPPs will be updated to place imaged
in the desired pixel locations on the array.
Failure Modes and Responses
Presuming that data is fully obtained, the most likely failure mode of
this task is saturation of the star at the longest exposure times or lack
of detection at the shortest exposure times. bright source.