| IOC-MIPS_205a | 10560C,10700C | ||||||||
| Title: | Determination of MIPS Radiometric Throughput at 70 and 160um | ||||||||
| Objective: | Measure the fluxes of known celestial objects to calibrate the absolute throughput at 70 and 160um. | ||||||||
| Description: | |||||||||
| including flow / state diagram | |||||||||
| For each module and mode in MIPS, a celestial standard will be observed. | |||||||||
| At 70 microns a nominal sensitivity of 100:1 will be achieved. | |||||||||
| 160um at least 10:1 will be achieved. The observed fluxes will be compared to | |||||||||
| the modelled throughput of MIPS and will be used to update subsequent | |||||||||
| estimates of sensitivity and integration times required . | |||||||||
| See attached page for listing of events | |||||||||
| Place in Schedule: | |||||||||
| (relative to water shed events) | |||||||||
| CTA and instrument at nominal operational temperature (below). | |||||||||
| Required Conditions: | |||||||||
| Telescope must be at 5.5K | |||||||||
| Location of MIPS apertures must be completed. | |||||||||
| Basic instrument comanding and functionality must have been confirmed. | |||||||||
| At least one of the candidate stars (alpha Tau,alpha Aur, alpha Hya, alpha Boo, gamma Dra for | |||||||||
| 70 and 160um) must be observable. | |||||||||
| Resources: | |||||||||
| duration (best estimate) | 2 hrs | ||||||||
| real time downlink (Y / N) | No | ||||||||
| special post event actions (Y / N) | No | ||||||||
| Generates ~1500 DCEs depending on overscan distance | |||||||||
| Outcome: | |||||||||
| description | Revised throughput numbers | ||||||||
| can proceed in parallel with other activity | No, dedicated observing. | ||||||||
| must outcome be confirmed before next event / test /activity | Outcome must be confirmed before tests of ultimate sensitivity can | ||||||||
| be executed. | |||||||||
| method of confirmation (sensor TLM, data analysis, etc.) | Data analysis | ||||||||
| estimate of data turn around if required for confirmation | 48 hrs | ||||||||
| Unique or included in planned AOT? | |||||||||
| Planned AOTs but with non-standard pipeline processing as calibration data | |||||||||
| will not yet be available | |||||||||
| Contingency Plan: | |||||||||
| "What if..." | If throughput is radically different than pre-launch estimates, further analysis and | ||||||||
| tests to pin point the nature of the problem will be required (eg., are other instruments | |||||||||
| affected similarly, are backgrounds as expected and so on). | |||||||||
| IOC Critical | Y | ||||||||
| References: | |||||||||
| Template last updated: | 7-Sep-99 | ||||||||
| M. Rieke | |||||||||
| Events: | |||||||||
| I. Throughput in Scan Map mode | |||||||||
| Make scan maps at each scan rate (slow,medium,fast) such that the star | |||||||||
| traverses each array. Repeat fast scan 4x to get enough integration at 160um. | |||||||||
| Use the scan map AOT. | |||||||||
| II. Throughput in Photometry mode | |||||||||
| Place star on each array (70um,160um) in turn. Take data in a 12 position | |||||||||
| dither pattern at 70um using the coarse scale and exposing for a total of 30 seconds at each position | |||||||||
| Take data in an 8 position dither at 160um and 60 seconds total exposure | |||||||||
| All patterns should be repeated using both 3 and 10 second exposure times | |||||||||
| Use the photometry/superreolution AOT. | |||||||||
| III. Throughput in Superresolution Mode | |||||||||
| Switch 70um module to fine plate scale. Take data in a 12-position dither pattern | |||||||||
| with a total integration time of ~100 secs per position. Repeat using each of the base integration | |||||||||
| times of 3 and 10 sec. | |||||||||
| Use the photometry/superresolution AOT. | |||||||||
| IV. Throughput in SED Mode | |||||||||
| Place star near one end of the SED slit. Take a series of exposures totalling | |||||||||
| 150 secs at each of five positions along the slit. Repeat for each of the basic | |||||||||
| integration times (3 and 10 secs). | |||||||||