Sequencer Site SIRTF IOC Activity c. 2002

CAID: MIPS-112 Title: 160 um On-board Data Processing Algorithms
 
System: MIPS Principal: alberto Deputy: dfrayer, SStolovy
Objective:   
To enusure that the on-board command 
sequences
expand appropriately and that the data
manipulation of
160um array behaves as expected. (e.g. SUR, 
RAW
and CO-ADDing modes).
 
Description: 
Commands wil be iussed that get expanded 
on board
of the spacecrfat. The telemetry will be 
monitored
to ensure that the correct commands were
performed.

A modified  160um Photometry AORs(3sec) 
will be
used to observed the same star in SUR, RAW,
CO-ADD=2,4,8
 
Day:   48.4972222222277 Suggested Order:   H500
 
Must be preceded by these activities (list by CAID):   MIPS-324
 
Place in Schedule:   The telescope has to be cold enough to measure standard stars at 160um
 
Priority:   Critical

Conditions

Maximum telescope temperature: 6.5 K
 
Minimum telescope temperature: 5.5 K
 
Should activity be repeated if focus changes?   No     Repeat if focus changes by 0 mm
 
Maximum absolute pointing uncertainty: 10 arcsec (1 sigma radial)
 
Maximum precision offset uncertainty: 10 arcsec  (1 sigma radial)
 
Observatory configuration:
 
Go/No Go criteria:

Resources

Duration:   15 minutes
 
Real time downlink:   No   

Data Volume (uncompressed): 96 Mbits
 
List Blocks, AORs, SERs, IERs, or unique sequences required (uplink):
 
List Analysis tools required (downlink):   Standard MIPS pipeline.

Outcome

Estimate of data turn around:   0 hours
 
Description: SUR and Raw models are identical in function for the GeGa MIPS arrays, so their BCDs should reflect that. Ratio or difference of the BCDs should be enough to show discrepancy. Co-adding reduces dowlink volume, but otherwise should produce also identical BCDs, so same method will be applied.
 
Can proceed in parallel with other activity: No
 
Must outcome be confirmed before next activity: No
 
Method of Confirmation:   BCDs from the different data taking modes will be compared.
 
 
Success criteria: The BCDs should be pretty much the same. Cosmic Rays will be the source of largest uncertainty, and at this point is impossible to quantify their effect (although we hope is not large).
 
Contingency plan:  (1) If co-adding fails. This is not a big issue for 70um, since this observing mode is not use during normal operation. (2) If either Raw or SUR fails. It can be replaced by either mode. (3) If we can not take data using our commands, this a major issue and should be brought up to the highest decision making level because there is not an obvious "work around".
 
 

Comments

 
References:  
 
Additional Comments:
This task takes very little time, that although is collecting RAW and SUR for the Ge:Ga arrays (which are equivalent), I will keep both modes, since the task is **to test** the on board commands (thanks fto D. Kelly for his comments).
 
This activity last updated: 10/8/2002 9:46:58 AM