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