| CAID: MIPS-131 | Title: 24 um Focal Plane Survey (Fine) #1 | |
| System: MIPS | Principal: jkeene | Deputy: |
| Objective: | To measure the pixel locations ( i.e., array orientation, scale and distortion) as a function of scan mirror angle for the 24 um array to an accuracy of 0.14 arcsec. |
| Description: | Use the 24 um photometry AOT to measure the locations on the sky of several
positions on the array as a function of scanning mirror angle.
1) Adjust the IPPs to position the two extreme images (#2 and #7; see Figure 8-17
in the SIRTF Observer's Manual V.2.1) at the extremes of the allowable mirror
deflections with the remaining images evenly spaced between them.
2) Set the S/C offset between AOT halves to be slightly less than half of the array width.
3) Perform a PCRS peak-up with the star on PCRS 1.
4) Offset the star to PCRS 2 and make a measurement.
5) Offset the star so that the central image (#1) is near but within the lower left-hand
corner of the array.
6) Execute the AOT and repeat steps 3 & 4.
7) Offset the star so that image #1 is at the center and near but within bottom edge of
the array.
8) Execute the AOT and repeat steps 3 & 4.
9) Offset the star so that image #1 is near but within the upper left of the array.
10) Execute the AOT and repeat steps 3 & 4.
11) Offset the star so that image #1 is near but within the center top of the array.
12) Execute the AOT and repeat steps 3 & 4.
13) Offset the star so that image #1 is near the middle of the array.
14) Execute the AOT and repeat steps 3 & 4.
15) Offset the star so that the lowest image (#2) is near but within the lower left-hand
corner of the array.
16) Execute the AOT and repeat steps 3 & 4.
17) Offset the star so that image #2 is near but within the center bottom of the array.
18) Execute the AOT and repeat steps 3 & 4.
19) Offset the star so that image #2 is near but within the upper left of the array.
20) Execute the AOT and repeat steps 3 & 4.
21) Offset the star so that image #2 is near but within the center top of the array.
22) Execute the AOT and repeat steps 3 & 4.
23) Offset the star so that image #2 is near the middle of the array.
24) Execute the AOT and repeat steps 3 & 4.
25) Offset the star so that the uppermost image (#7) is near but within the lower left-hand
corner of the array.
26) Execute the AOT and repeat steps 3 & 4.
27) Offset the star so that image #7 is near but within the center bottom of the array.
28) Execute the AOT and repeat steps 3 & 4.
29) Offset the star so that image #7 is near but within the upper left of the array.
30) Execute the AOT and repeat steps 3 & 4.
31) Offset the star so that image #7 is near but within the center top of the array.
32) Execute the AOT and repeat steps 3 & 4.
33) Offset the star so that image #7 is near the middle of the array.
34) Execute the AOT and repeat steps 3 & 4.
35) Ge anneal and wait.
This whole procedure will be repeated 3 times for this task and the task itself will need
to be repeated at least a total of 3 times. |
| Day: 68.3756944444467 | Suggested Order: Q300 | ||
| Must be preceded by these activities (list by CAID): MIPS-130 | |||
| Place in Schedule: The telescope must be focussed. The S/C must be pointing and tracking optimally. The PCS, PCRS, and IRU must be calibrated. The 24 um array and scan mirror must be fully operational. The 24 um photometry AOT must be validated. The FP coarse survey must have been done successfully. This procedure should be done when the telescope and electronics are in temperature equilibrium so that the pointing performance is optimal. | |||
| Priority: Desired | |||
Conditions | |||
| Maximum telescope temperature: | 33 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: | 3 arcsec (1 sigma radial) | ||
| Maximum precision offset uncertainty: | 0.4 arcsec (1 sigma radial) | ||
| Observatory configuration: | IPP files must be adjusted to optimize the scan mirror motion and image placement. | ||
| Go/No Go criteria: | Telescope must be pointing and tracking optimally. Scan mirror must be stable. | ||
Duration: 402 minutes
| | Real time downlink:
No | | |||
| Data Volume (uncompressed): 69 Mbits | |||
| List Blocks, AORs, SERs, IERs, or unique sequences required (uplink): 24 um PT/SR AOT with modified IPP files. | |||
| List Analysis tools required (downlink): Standard data reduction software (e.g., IRAF) for centroiding star images. Specialized software for calculating transformation of pixel number and mirror angles into location on sky. | |||
| Estimate of data turn around: 48 hours | |||
| Description: Maps of the pixel locations as a function of scan mirror angle. | |||
| Can proceed in parallel with other activity: No | |||
| Must outcome be confirmed before next activity: No | |||
| Method of Confirmation: Examination of data. | |||
| Success criteria: 1) Star images visible. 2) Sufficient S/N in each image (>30) to centroid each image to better than 0.1 pixel. | |||
| Contingency plan: Repeat with different stars, integrating longer, using different S/C offsets, IPP files. | |||
Comments | |||
| References: | |||
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Additional Comments:
The same procedure will be used for the coarse and fine focal plane mappings. It will be repeated many times (~10) to achieve the accuracy needed for the fine survey. The time required and data volume assume 3 repeats. | |||
| This activity last updated: 1/2/2002 4:58:00 PM | |||