| IOC-MIPS_340a | 10630C | ||||||||
| Title: | Determination of Ultimate MIPS Scattered Light Levels | ||||||||
| Objective: | Determine the level of scattered background light within MIPS when the scan mirror is | ||||||||
| moved to the "dark" position. | |||||||||
| This test will indicate how well the total powermode will work. | |||||||||
| Description: | |||||||||
| including flow / state diagram | |||||||||
| Part 1: | Diffuse light scattered into MIPS | ||||||||
| Point at a high background location (Galactic plane preferably). | |||||||||
| Place the 24um array into the dark with the scan mirror. | |||||||||
| Take 30 30-second integrations. | |||||||||
| Perform a thermal anneal on the 70-um array. | |||||||||
| Place the 70um-array into the first 70um dark position. | |||||||||
| Take 30 10-second integraqtions. | |||||||||
| Move the scan mirror to the other 70um dark position. | |||||||||
| Take 30 10-second integrations. | |||||||||
| Perform a thermal anneal on the 160um array. | |||||||||
| Move the scan mirror to the 160um dark position. | |||||||||
| Take 30 10-second integrations | |||||||||
| Part 2: | Scattered light from stars adjacent to the field of view. | ||||||||
| Repeat the following tests for a bright star placed 5",10", and 20" outside the FOV. | |||||||||
| Place the 24um array in the dark. | |||||||||
| Take 60 30-second integrations with the 24um array while stepping the star by 5" | |||||||||
| along the side of the 24um array as it would project onto the sky if open. | |||||||||
| Repeat moving the star along the other 3 sides of the array. | |||||||||
| Place the 70um array into the first dark position. | |||||||||
| Take 30 10-second integrations with the 70um array while stepping a star by 10" | |||||||||
| along the side of the array projected onto the sky. | |||||||||
| Repeat for the other three sides of the array. | |||||||||
| Place the 70um array into the second dark position. | |||||||||
| Take 30 10-second integrations with the 70um array while stepping a star by 10" | |||||||||
| along the side of the array projected onto the sky. | |||||||||
| Repeat for the other three sides of the array. | |||||||||
| Place the 160um array into the dark position. | |||||||||
| Take 20 10-second integrations while stepping the star by 15" along | |||||||||
| a long side of the 160um array. | |||||||||
| Take 3 10-scond integrations while stepping the star by 15" along | |||||||||
| a short side of the 160um array. | |||||||||
| Repeat the above steps on the other two sides of the 160um array. | |||||||||
| Integration times will allow detection at levels of less than 1% of the incoming flux | |||||||||
| Place in Schedule: | Can begin after aperture door is opened. | ||||||||
| (relative to water shed events) | |||||||||
| Required Conditions: | Basic detector and scan mirror operation must be confirmed before | ||||||||
| executing this program. | |||||||||
| The telescope must be fully cold for this test. | |||||||||
| Resources: | duration (best estimate) | 10 hrs | |||||||
| real time downlink (Y / N) | no | ||||||||
| special post event actions (Y / N) | no | ||||||||
| Generates 120 DCEs in Part 1 and 2340 DCEs in Part 2 | |||||||||
| Outcome: | |||||||||
| description | |||||||||
| can proceed in parallel with other activity | no, requires dedicated pointing | ||||||||
| must outcome be confirmed before next event / test /activity | No | ||||||||
| method of confirmation (sensor TLM, data analysis, etc.) | data analysis | ||||||||
| estimate of data turn around if required for confirmation | N/A | ||||||||
| Unique or included in planned AOT? | |||||||||
| Should be the same as an EOT for measuring dark current | |||||||||
| Contingency Plan: | |||||||||
| "What if..." | If an unusually high background is observed, an analysis of the MIPS/CTA optical path will be needed. | ||||||||
| IOC Critical | Y | ||||||||
| References: | |||||||||
| Template last updated: | 9/7/99 | ||||||||
| M. Rieke | |||||||||