Notes on MIPS IOC/SV campaign structures: General philosophies: 1) Seek consistency in the timing of calibration measurements 2) Place tasks that are sensitive to telescope and electronics temperature changes (focus check, focal plane survey) towards the ends of campaigns 3) Schedule all Ge tasks with an awareness of the time since the last thermal anneal. For 70um, data should ideally be taken within about 4h after an anneal, for 160um within 2h. For Ge tasks less sensitive to cosmic ray induced responsivity changes, these times increase to 6h and 3h. 4) When possible, minimize slew overheads 5) If an extra downlink is scheduled during a campaign, identify tasks for which the data turnaround time is demanding and run those tasks before the first downlink 6) Schedule tasks to minimize risk. If a tricky AOT or IER is to be run, place it towards the end of the campaign. When there are no other criteria for ordering tasks, schedule the ones that have been run successfully before to run first. The thinking here is that new tasks introduce some risk of an instrument suspend, and we would like to complete as much of a campaign as possible before this unfortunate event. --------------------------------------------------------------------- Standard MIPS CAMPAIGN Calibration Activities Time since Start-up activities, Si and Ge MIPS-905 40 Ge anneal - 10m R70 R160 IOC Darks, 160um MIPS-912 16.5 14.5 1.06 1.40 IOC Darks, 70um MIPS-911 32.5 31 1.12 1.80 IOC Darks, 24um MIPS-910 17.2 63.5 1.23 2.53 24um Flat - routine, Scan AOR MIPS-914 14.3 80.7 1.29 2.86 160um IC - routine, Scan AOR MIPS-916 12.7 95 1.33 3.13 70um IC - routine, Scan AOR MIPS-915 12.7 107.7 1.38 3.39 70um NF Illumination correction MIPS-313 18.5 120.4 1.42 3.63 SED Slit Illumination Correction MIPS-299 19.3 138.9 70um Flux standards MIPS-922 6.6 158.2 1.24 2.57 Ge Anneal and recovery MIPS-930 15 165 160um Flux standards MIPS-924 11.2 0 1.00 1.00 Routine 24um Flux standard MIPS-920 8.2 11.2 1.08 1.56 Comments: Our usual Ge anneal activity includes 10m of settling time after the completion of the anneals. For purposes of this discussion, I assume that the responsivity at that time has a value of 1.0 and that it increases as R(t) = R0 + 7R0[1-exp(-t/Tau)], where Tau=240m at 160um and as R(t) = R0 + 2R0[1-exp(-t/Tau)], where Tau=480m at 70um. This functional form is probably right, but the time constants are highly uncertain. The UC Davis 160um data are fit very well by this function with a time constant of 60m. However, the energy deposition and hit rate were each about 2-3x too high there. At 70um, only about half of the response change comes from cosmic rays, and the detector relaxation time constant and the cosmic ray time constants are probably different from each other, so the true formula is probably more complicated. There is 10m of settling time after the end of the Vrst calibration in the startup activities. The darks should be done in sequence to reduce pointing overheads and to minimize latency effects. Cosmic ray effects are minimized by doing the 160um darks first, followed by the 70um and 24um darks. By measuring the darks this soon after the anneal, we get a better measure of the zero-point dark current and we get darks that are less affected by stray light. In standard MIPS operations, we measure point sources and stim flashes in the Ge detector quick response regime, while sky backgrounds and flatfields/illumination corrections are measured in the slow response regime. Chad Engelbracht did an analysis of Ge data taken with a modest background and with regular stim flashes. He found that the stim flashes did a poor job of tracking the responsivity of the background for a short time after a thermal anneal, but after about 15m at 160um and an hour at 70um the stim flashes were quite effective at calibrating the background. Based on this result, it appears beneficial to wait at least an hour and preferably longer after a thermal anneal before collecting our 70um and 160um IC data. The worry here is that the shape of the measured IC will change during the first hour after an anneal due to pixel-to-pixel differences in the settling time. The IC measured after an hour should be fairly stable and should be good for correcting both point sources and backgrounds. Most of our science data will be taken in this "settled" regime, so it is beneficial to measuring the ICs in this same regime. To accomplish these goals, it is best to delay the IC measurements by measuring the 24um flats first. The 160um settling time is quick, so the 160um IC comes next. The 70um ICs are saved for last. The flux standards come last. For the flux calibrators, there are two important issues. The first is the calibration repeatability of the stim flashes after an anneal, which Chad found to be good immediately after an anneal at 160um and good after about 10m at 70um. The other factor is the stability of the stim/source ratio, which has a settling time akin to the stim/background ratio for any source not equal in brightness to the stim. The 70um flux calibrators are measured first. The responsivity should still be reasonable, and the stim/source ratio should be well settled. An anneal is performed before the 160um flux calibrators to reset the responsivity. Ground-based tests suggest a drop in 24um responsivity by 1% during the first hour of operations, followed by recovery over the next two hours. By placing the 24um calibrators last, the responsivity should be very close to its final value. --------------------------------------------------------------------- MIPS CAMPAIGN D1 Start-up activities, Si MIPS-900 32 Scattered background monitor MIPS-950 23.6 24um First Light MIPS-100 13.1 24um Detector Response to Stims MIPS-115 3.25 24um Voffset Adjustment test MIPS-125 4.9 24um Flat -- Routine, Phot AOR MIPS-917Z 11.5 Shutdown activities, Si only MIPS-990 13 Comments: The scattered background monitor was the only task between startup and shutdown in campaigns B and C. Putting it first after power-up provides consistency in the timing of this task within a campaign. The 24um first light test involves the first MIPS-PCS interactions and the first use of an AOT, so it introduces some risk of failure. I put it second anyway since it is the driving task for this campaign. I place the stim response test next since it is a first-light activity. The Voffset test is unaffected by stim latents, so it is placed next to provide a little latency recovery time before the running of mips-917. The nominal requirement for this campaign is a telescope temperature of 40K or lower, which would give a background flux rate of about 8% full well per second. The first light task can probably be run successfully at up to 45K, where the background flux is about 40% full-well per second. If this criterion is not met, the campaign should be deferred until the telescope gets below 45K. --------------------------------------------------------------------- MIPS CAMPAIGN D2 Start-up activities, Si MIPS-900 32 Scattered background monitor MIPS-950 23.6 IOC Darks, 24um MIPS-910 17.2 24um Onboard data processing algorithms MIPS-110 36 24um Flat - routine, Phot AOR, field 1 MIPS-917 11.5 24um Flat - routine, Phot AOR, field 2 MIPS-917 11.5 24um Ph/SR AOT validation, preliminary MIPS-320 24.4 24um Focus confirmation MIPS-121 29.3 24um Flux Standards MIPS-920Z 6.8 Dark Verification, 24um MIPS-190Z 28.1 Shutdown activities, Si only MIPS-990 13 Comments: Calibration task mips-950 is performed first, the same as in earlier campaigns. mips-910 and mips-110 use the same pointing as mips-950, so they come next. The two flat fields are probably relatively close to each other on the sky so they are scheduled back-to-back. The Ph/SR AOT validation comes next because it is high priority and because mips-121 is being deferred to ensure good stability. mips-920 and mips-190 come last since they are filler tasks; mips-920 comes first because it involves similar pointing to the previous two tasks. A telescope temperature of 33K (250 DN/s) or lower is desired for this campaign. The focus check is the only temperature-sensitive task in this campaign, but there is time pressure to obtain a focus confirmation, so we will probably execute this campaign as long as the telescope temperature is 35K (750 DN/s) or lower. The sky background is expected to be of order 400 DN/s. No assessment has been made yet of the affect of high background on the focus measurement. --------------------------------------------------------------------- MIPS CAMPAIGN E Start-up activities, Si MIPS-900 32.2 Scattered background monitor MIPS-950 23.55 IOC Darks, 24um MIPS-910 17.2 24um Flat - routine, Phot AOR, field 1 MIPS-917 11.5 24um Flat - routine, Phot AOR, field 2 MIPS-917 11.5 24um Stim cal. with celestial sources MIPS-120 35 24um Flux linearity vs background MIPS-315Z 31 24um Focus confirmation MIPS-121 29.3 ERO MIPS-500 19 Shutdown activities, Si only MIPS-990 13.2 Comments: Again, it makes sense to put MIPS-950 and MIPS-910 back-to-back, and likewise for the two runnings of MIPS-917. The focus check is again placed last to maximize settling time. Other than that, there is no compelling reason for any of the task ordering in this campaign, so we can shuffle the tasks to reduce slew overheads. --------------------------------------------------------------------- MIPS CAMPAIGN F Start-up activities, Si MIPS-900 32.2 Scattered background monitor MIPS-950 23.55 IOC Darks, 24um MIPS-910 17.2 24um Flat - routine, Phot AOR MIPS-917 11.5 24um Photometry Flat MIPS-917Z 11.5 24um Flux Standards MIPS-920 6.8 24um Focal plane survey (coarse) MIPS-130 81 24um Focus confirmation MIPS-121 29.3 24um Optimum bias setting MIPS-245 103 24um Photometry Flat MIPS-917Z 11.5 24um Photometry Flat MIPS-917Z 11.5 24um Dark Verification MIPS-190Z 28.1 24um Latent Images and Sat. Sources MIPS-155Z 46 ERO MIPS-500 19 Shutdown activities, Si only MIPS-990 13.2 Comments: This campaign starts with darks, flats, and flux standards, the same as in previous campaigns. The FPS is placed next. I would prefer to place the FPS later in the campaign to ensure better stability, but mips-245 and mips-155 are disruptive to the array and introduce some risk, and mips-917 and mips-190 are low priority. mips-130 is a coarse FPS survey, so we can tolerate a small amount of instability. The focus check requires better stability, so it is placed after mips-130. The bias optimization is our only remaining high priority task, so it comes next. Among the remaining tasks, the dark comparison is deferred until after the flats in case the bias test causes some instabilities in the array. The latents and saturation test is saved for last since it disrupts the array. This campaign includes our only focus check after the focus change, so MIPS-121 should be deferred to a later campaign if the focus is not updated before this campaign. --------------------------------------------------------------------- MIPS CAMPAIGN G time since Start-up activities, Si and Ge MIPS-905 40 Ge anneal Scattered background monitor MIPS-950 23.6 24 70um Darks MIPS-911 32.6 48 70um IC - routine, Phot AOR MIPS-918 24.3 81 70um NF IC MIPS-313 23 105 70um First light and Ph/SR AOT val.(Prel)MIPS-322 27.4 128 70um Stim response MIPS-247 13.5 155 70um Voffset adjustment test MIPS-126 5.1 169 70um On-board data processing algorithms MIPS-111 10.4 174 70um Flux Standards MIPS-922Z 6.6 184 70um WF Candidate Star MIPS-965 15.3 191 70um NF Candidate Star MIPS-966 12.2 204 24um Spectral leak check MIPS-240 19.7 216 24um Flux Standards MIPS-920 7.0 236 24um Flat - routine, Phot AOR MIPS-917 11.5 243 24um Focal plane survey (coarse) MIPS-130 83 255 Shutdown activities, Ge and Si MIPS-992 23 338 Comments: I made an effort in this campaign to follow what will later become the standard sequence of calibration activities. Darks come first, then ICs. I deferred all of the 24um tasks until the end of the campaign so that the 70um tasks could be completed without needing a thermal anneal. The calibration tasks are followed by the first light activities and then by a set of three standard star measurements. Among the 24um tasks, the stellar observations are placed right after the 70um stellar observations to minimize slew overheads. The FPS is scheduled last to ensure good thermal stability. With luck, we will see sources on the 70um array during the FPS that will allow us to get a first look at the effects of cosmic rays on the 70um array 4-5.5 hours after a thermal anneal. The telescope should be about 9K during this campaign. If the telescope is still above 15K, the 70um tasks should be postponed. --------------------------------------------------------------------- MIPS CAMPAIGN H time since Start-up activities, Si and Ge MIPS-905 40 Ge anneal Routine 24um flux standard MIPS-920 7 24 Scattered background monitor MIPS-950 24 31 Routine 24um flux standard MIPS-920 7 55 160um IC - routine, Phot AOR MIPS-919 24 62 Routine 24um flux standard MIPS-920 7 86 160um On-board data processing algorithmsMIPS-112 10 93 160um Stim response MIPS-248 9 103 160um Voffset adjustment test MIPS-127 3 112 Routine 24um flux standard MIPS-920 7 115 160um First light and Ph/SR AOT val.(Prel)MIPS-324 37 122 Routine 24um flux standard MIPS-920 7 159 70um Spectral leak check MIPS-241 21 166 Ge Anneal and recovery MIPS-930 15 187 IOC Darks, 160um MIPS-912 16 10 IOC Darks, 70um MIPS-911 33 26 IOC Darks, 24um MIPS-910 17 59 24um Flat - routine, Phot AOR MIPS-917 12 76 24um Flat - routine, Phot AOR MIPS-917 12 88 70um IC - routine, Phot AOR MIPS-918 24 100 Calibration stars against different bkgdsMIPS-921 67 124 Ge Anneal and recovery MIPS-930 15 191 70um WF Focal plane survey (coarse) MIPS-132 107 10 24um Scan AOT validation (Preliminary) MIPS-326 17 117 24um Frame table update sanity check MIPS-960 5 315 Shutdown activities, Ge and Si MIPS-992 23 320 Periodic IRU Calibration updates PCS-055 36 Periodic PCRS/STA alignment filter updatesPCS-105 12 Comments: The driving factor at the start of this campaign is the multiple runs of MIPS-920. These 5 repeats are designed to study the stability of the 24um array response over the first several hours after instrument power-up. To accomplish this, we need to run MIPS-920 right after MIPS-905 and then again at semi-regular intervals over the next several hours. I tried to schedule short tasks between the mips-920 tasks to provide good and regular sampling. The 37m long first light task is placed last in this sequence since we do not need very good time sampling this long after power-up. It is soon enough after power-up that the 160um response should still be reasonable. The second anneal block is very close in structure to our normal startup calibration sequence. The FPS is placed last to ensure good thermal stability. The remaining 24um tasks are placed last in the campaign. This campaign involves the first 160um operations and the last scattered light measurement. It will be difficult to do much at 160um if the telescope temperature is above 7K. The scattered light test should possibly be deferred if the telescope is not yet close to its final temperature. I see no good way for me to schedule the PCS activities. They should not be permitted to break up the anneal blocks, so they can be placed after mips-241, mips-921, or mips-992. --------------------------------------------------------------------- MIPS CAMPAIGN I time since Start-up activities, Si and Ge MIPS-905 40 70um/160um anneal 70um and 160um Optimum bias setting MIPS-246 677 24 Anneals done in here. 70um IC - routine, Scan AOR MIPS-915 14 70/10 70um IC - routine, Phot AOR MIPS-918 24 84/24 70um NF Illumination correction MIPS-313 23 108/48 70um SED Slit IC MIPS-299 19 131/71 160um IC - routine, scan AOR MIPS-916Z 14 150/90 160um IC - routine, phot AOR MIPS-919 24 164/104 IOC Darks, 70um MIPS-911 33 188/128 IOC Darks, 24um MIPS-910 17 221/161 24um Flat - routine, Scan AOR MIPS-914 14 238/178 24um Flat - routine, Phot AOR MIPS-917 12 252/192 Ge Anneal and recovery MIPS-930 15 264/204 24um Optimum operating temperature MIPS-345 72 10 160um Flux Standards MIPS-924 11 82 24um Flux Standards MIPS-920 7 93 70um Flux Standards MIPS-922 7 100 160um FPS Candidate Star MIPS-967 14 107 70um WF Focal plane survey (coarse) MIPS-132 104 121 Ge Anneal and recovery MIPS-930 15 225 70um NF Focal plane survey (coarse) MIPS-137 164 10 SED Slit location and orientation MIPS-139 75 174 70um NF IC MIPS-313Z 23 249 Shutdown activities, Ge and Si MIPS-992 19 272 Periodic PCRS/STA alignment filter updatesPCS-105 12 Periodic PCRS/STA alignment filter updatesPCS-105 12 Periodic PCRS/STA alignment filter updatesPCS-105 12 Periodic IRU Calibration updates PCS-055 36 Comments: The Ge bias optimization is the dominant task in this campaign. I made a mistake when I wrote it by not performing a thermal anneal at the start of the task. This is corrected by scheduling this task first in the campaign, after the thermal anneals in MIPS-905. There is a 70um thermal anneal 70m before the end of MIPS-246 and a 160um anneal 10m before the end of the task. The next anneal block consists of calibration tasks. It was not possible to match the startup sequence for these tasks, but I matched the timings of the tasks relative to their respective anneal as best I could. The 24um optimum temperature test is essentially a 160um dark test, so it was placed first after an anneal. The flux standards tasks were placed next, making sure that the 70um standards were taken at least an hour after the preceding anneal. One of the 70um FPS tasks was placed next. It is timed well relative to the anneal, and enough time has elapsed since the start of the campaign that the stability should be good. I scheduled the NF FPS next in hopes that this will cut down on slew overheads. The final 70 NF IC is poorly timed relative to the anneal, but it put it there anyway since it is a filler task. --------------------------------------------------------------------- MIPS CAMPAIGN J Time since Start-up activities, Si and Ge MIPS-905 40 Ge anneal IOC Darks, 160um MIPS-912 17 24 IOC Darks, 70um MIPS-911 33 41 IOC Darks, 24um MIPS-910z 17 74 24um Flat - routine, Scan AOR MIPS-914 14 91 160um IC - routine, Scan AOR MIPS-916 14 105 70um IC - routine, Scan AOR MIPS-915 14 119 70um NF Illumination correction MIPS-313 23 133 70um Flux standards MIPS-922 7 156 Ge Anneal and recovery MIPS-930 15 163 160um Flux standards MIPS-924 11 10 Routine 24um Flux standard MIPS-920 7 21 Flux Nonlinearity Calibration, Ge MIPS-600 146 28 Ge Anneal and recovery MIPS-930 15 174 160um Array location and orientation MIPS-234 142 10 SED Slit location and orientation MIPS-139 75 152 70um WF Frame table update sanity check MIPS-961 5 227 Ge Anneal and recovery MIPS-930 15 232 70um NF Focal plane survey (coarse) MIPS-137 164 10 160um Flux standards MIPS-924 11 174 70um Flux standards MIPS-922 7 185 Shutdown activities, Ge and Si MIPS-992 23 192 Periodic PCRS/STA alignment filter updatesPCS-105 12 Periodic PCRS/STA alignment filter updatesPCS-105 12 Periodic IRU Calibration updates PCS-055 36 Comments: This campaign opens with the standard calibration sequence. The Ge flux nonlinearity calibration comes immediately after the flux standards. This is soon enough after the anneal to get good 160um data. The FPS tasks are placed in the latter two anneal cycles to ensure good thermal stability. The two flux standards repeats are placed last in the campaign to provide a good timeline for stability checks. --------------------------------------------------------------------- MIPS CAMPAIGN K Time since Start-up activities, Si and Ge MIPS-905 40 Ge anneal Startup Transients, 24um and Ge Arrays MIPS-226 61 24 160um IC - routine, Scan AOR MIPS-916 14 85 160um IC - routine, Phot AOR MIPS-919 24 99 70um IC - routine, Scan AOR MIPS-915 14 123 70um IC - routine, Phot AOR MIPS-918 24 137 70um NF Illumination correction MIPS-313 23 161 24um Flat - routine, Scan AOR MIPS-914 14 184 24um Flat - routine, Phot AOR MIPS-917 12 198 Ge Anneal and recovery MIPS-930 15 210 Flux Calibration 1 MIPS-350 76 10 160um Spectral Leak Check MIPS-242 13 86 160um Flux standards MIPS-924 11 99 70um Flux standards MIPS-922 7 110 Routine 24um Flux standard MIPS-920 7 117 SED Mode Wavelength Calibration MIPS-145 39 124 70um and 160um Thermal Anneal Behavior MIPS-160a 168 163/2 SED Slit Illumination Function MIPS-299 19 170 SED Skeleton AOT Validation MIPS-300 58 189 70um and 160um Thermal Anneal Behavior MIPS-160b 110 247 Ge Anneal and recovery MIPS-930 15 357 IOC Darks, 160um MIPS-912 17 10 160um Array Location and Orientation MIPS-234 145 27 IOC Darks, 70um MIPS-911 33 172 IOC Darks, 24um MIPS-910 17 205 Shutdown activities, Ge and Si MIPS-992 23 222 Periodic PCRS/STA alignment filter updatesPCS-105 12 Periodic PCRS/STA alignment filter updatesPCS-105 12 Periodic IRU Calibration updates PCS-055 36 Comments: A big part of this campaign is checking the stability and behavior of the Ge arrays following startup and following a thermal anneal. MIPS-226 has to come right away to address this need, and MIPS-160 has to come much later in the campaign, when startup transients are not a factor. Since MIPS-160 was shortened, I split it into two segments: MIPS-160a has the thermal anneal and three calibration cycles; MIPS-160b has two calibration cycles. The flats after MIPS-226 somewhat approximate the timing of the standard startup sequence, with the 24um flats deferred until last. The next anneal block consists mostly of stellar calibration data. MIPS-160 comes in the third anneal block, with a pair of 70um FPS tasks placed between the two halves. The total time between anneals ends up being about 6 hours, which was our original target. The 160um FPS and the darks come in the final anneal block. ---------------------------------------------------------------------