0 Assigned ID: 1068 ----- Attempting Submission 1 (Fri Apr 07 23:02:41 GMT 2017) ----- LONG SU LIKELY TO INTERSECT THE SAA Unschedulable Visit Unschedulable Visit You must specify an Exposure level Phase Special Requirement when using the Visit level Period Special Requirement. LONG SU LIKELY TO INTERSECT THE SAA Unschedulable Visit Unschedulable Visit You must specify an Exposure level Phase Special Requirement when using the Visit level Period Special Requirement. Comments for re-submission on 13 Oct 2017: 1. Removed the phase constraints on visits 2 and 4. This removed the overrun problem, so I have left the 'schedulability' setting at 90 (i.e. it was not necessary to change it to 80). 2. Removed the anomalous 0-0 phase constraints that Kevin noticed (not sure how they got in there). 3. Added two additional orbits to the end of visits 3 and 4, to bring the total up to 2x26 = 52 orbits. THESE HAVE BEEN UPDATED (SEE ABOVE): Comments for re-submission on 13 Oct 2017: 1. Removed the phase constraints on visits 2 and 4. This removed the overrun problem, so I have left the 'schedulability' setting at 90 (i.e. it was not necessary to change it to 80). 2. Removed the anomalous 0-0 phase constraints that Kevin noticed (not sure how they got in there). 3. Added two additional orbits to the end of visits 3 and 4, to bring the total up to 2x26 = 52 orbits. Comments for re-submission on 12 Oct 2017: Set nsamp=15 for all science exposures and number of iterations to 16 for science orbits. Comments for re-submission on 5 Oct 2017: Reduced scan rate from 0.12 arcsec/sec to 0.073 arcsec/sec following advice from Kevin Stevenson to achieve max-counts of 30k electrons per exposure. Here are the new comments from a previous re-submission: Some further comments were added on the subject of splitting the 26-orbit visits into a 19-orbit visit plus a 7-orbit visit due to APT limitations. These comments from the original submission still apply: Please try to schedule the 52 orbits as 2x visits of 26-orbits each. Due to APT limitations, we have had to implement this in Phase 2 by splitting each 26-orbit visit into a 19-orbit visit plus a 7-orbit visit. Please ensure that these "visits" are scheduled back-to-back to ensure a contiguous 26-orbit visit. Further notes are provided in the Proposal Description. -354204926 ----- Attempting Submission 1 (Thu Jul 20 17:47:41 GMT 2017) ----- HST Phase II Proposal 15134 (P2_phasecurve.apt) successfully submitted. Receipt: # 15134-1 ----- Attempting Submission 2 (Thu Jul 20 17:52:52 GMT 2017) ----- ----- Attempting Submission 3 (Thu Oct 05 12:53:08 GMT 2017) ----- ----- Attempting Submission 4 (Thu Oct 12 05:13:15 GMT 2017) ----- ----- Attempting Submission 5 (Fri Oct 13 13:09:15 GMT 2017) ----- HST Phase II Proposal 15134 (P2_phasecurve_v4.apt) successfully submitted. Receipt: # 15134-5 ----- Attempting Submission 6 (Fri Oct 13 13:12:59 GMT 2017) ----- This resubmission is the same as the previous one but I edited the 'Submission comments' slightly to hopefully minimize confusion. A global map of thermal inversions for an ultra-hot planet WASP-121b is one of the standout exoplanets available for atmospheric characterization, both in transmission and emission, due to its large radius (1.8 Rjup), high temperature (~2400K), and bright host star (H=9.4mag). Recent WFC3/G141 transit and eclipse observations of WASP-121b by our group show clear detections of water at 1.4 micron that are in absorption on the nightside and emission on the dayside, implying that the planet has a dayside thermal inversion. Combined, these factors make WASP-121b the best target available to observationally probe the variation of thermal inversions with longitude. Here we propose spectroscopic phase-curve measurements of WASP-121b over a full orbital period with WFC3/G141. Given the measurement precision demonstrated by our previous transit and eclipse observations with WFC3, we anticipate an unprecedented signal-to-noise for a near-infrared exoplanet phase curve. Combined with state-of-the-art atmospheric retrieval analysis and circulation models, our data will produce a longitudinally-resolved map of the atmospheric thermal structure, and will track the thermal inversion with longitude by measuring the 1.4 micron H2O feature as it transitions from absorption to emission. This information-rich dataset will provide valuable new insight into the long-standing mystery of thermal inversions in hot gas giants, which will provide critical constraints for the global circulation and the molecular sources that produce thermal inversions. We are observing two full-orbit phase curves of WASP-121b using WFC3 G141 in spatial scanning mode over two visits. We will adopt the same observing setup as was used successfully for our previous observations of WASP-121b as part of Programs 14468 and 14767. Each visit will include two consecutive secondary eclipses of the planet as well as the intervening primary transit. We have specified different phase constraints for each visit to maximize the phase coverage achieved for the transits and eclipses. We request that two 26-orbit visits be performed. Due to problems encountered with APT when trying to specify 26-orbit visits, for the purpose of Phase 2 we have split each 26-rbit visit into a 19-orbit "visit A" and 7-orbit "visit B". We request that these visits be performed back-to-back, to achieve a single 26-orbit visit: i.e. Full visit = "visit A" + "visit B" We have correctly phase-constrained the Acquisition image for "visit A". We have also added a phase-constraint to the first exposure in "visit B", which is simply the phase-constraint for "visit A" *plus 20 HST orbits*. We did this with the aim of trying to ensure the orbits of "visit A" and "visit B" are contifuous. But hopefully there is a safer way to ensure this occurs as part of the scheduling (it was the best way we could come up with using APT). The primary technical challenge of our observations is the long duration of each visit, both of which consists of 26 contiguous HST orbits. In particular, SAA crossings pose a challenge for these observations, but hopefully this can be mitigated somewhat by the short 30.6 hour period of our target which allows for a relatively large number of scheduling opportunities. Following consultation with our STSCI support contact, the following points outline the steps we have taken in APT and the requests we have in allowing these observations to be scheduled succesfully: 1. We require a gyro bias update every HST orbit. To accommodate this, we have left 5 minutes of unused FGS visibility at the end of each orbit. In practice, we achieved this in APT by setting SCHED 100 orbits, as recommended by our STSCI support contact. 2. We will likely require a second full GS Acq at some point during each visit, probably about 14 orbits in. This is in addition to the first full GS Acq done automatically at the start of the first orbit. 3. Ideally, we would like the observations to be scheduled without being affected by SAA crossings (i.e. an "SAA hider"). However, given the length of our visits, this may not be achievable, in which case we request that orbits are scheduled such that any SAA crossings occur at close to the *end* of target visibility as possible. This will allow the GS Reacq (plus the full Acqs) to be performed at the start of the affected orbits before dropping to gyro part way through. If we are unlucky and it is unavoidable for SAA crossings to occur in the first half of orbits, we will presumably be forced to gyro guiding for the affected orbits. 4. For orbits affected by SAA crossings, we request that they do not coincide with the planetary primary transit and secondary eclipse. Specifically, we request that they occur *outside* the phase ranges -0.12 to +0.12 (primary transit) and +0.38 to +0.62 (secondary eclipse). Planets and Planet Formation 6 false false false false false false false SUPPORTED EXT-STAR EXTRA-SOLAR PLANETARY SYSTEM F3-F9 J2000 J2000 WFC3/IR Spectroscopic No No G141 WFC3/IR Spectroscopic No No G141 Timing link suitability includes constraints ([02 After 01 by 1.2 to 1.2 days]) The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. Please see Proposal Description for important notes on SAA crossing. We have defined each HST orbit within a non-interruptible sequence, to ensure that all exposures defined within the sequence are taken during the same HST orbit. We will use forward spatial scanning mode to avoid saturation on relatively long exposures and increase observing efficiency. Visit orientation requirements have been defined to avoid spectra from nearby stars overlapping the target spectrum. Phase constraints have been specified to maximize phase coverage of the primary transits and secondary eclipses achieved by the two visits of our program. 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:al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3096 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15134 :visit-id "03" :orbit-number 18 :pcs-time 222 :si-vis-utilization 2707 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3096 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15134 :visit-id "03" :orbit-number 19 :pcs-time 222 :si-vis-utilization 2707 :al-overhead-at-end 0 :internal-dur-at-end 457 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3096 :pcs-gap 0 ) false 19 0 Phase-constrained Timing link suitability includes constraints ([04 After 03 by 1.2 to 1.2 days]) The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. Please see Proposal Description for important notes on SAA crossing. We have defined each HST orbit within a non-interruptible sequence, to ensure that all exposures defined within the sequence are taken during the same HST orbit. We will use forward spatial scanning mode to avoid saturation on relatively long exposures and increase observing efficiency. Visit orientation requirements have been defined to avoid spectra from nearby stars overlapping the target spectrum. Phase constraints have been specified to maximize phase coverage of the primary transits and secondary eclipses achieved by the two visits of our program. 1520984523000 50.0 (Tic-Visit :proposal-id 15134 :visit-id "04" :proposal-version -1 :trans-version "20171009" :date "16-Feb-2018 11:07:53.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 7 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 2150912 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15134 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15134 :visit-id "04" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2707 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3096 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15134 :visit-id "04" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2707 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3096 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15134 :visit-id "04" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2707 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3096 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15134 :visit-id "04" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2707 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3096 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15134 :visit-id "04" :orbit-number 5 :pcs-time 222 :si-vis-utilization 2707 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3096 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15134 :visit-id "04" :orbit-number 6 :pcs-time 222 :si-vis-utilization 2707 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3096 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15134 :visit-id "04" :orbit-number 7 :pcs-time 222 :si-vis-utilization 2707 :al-overhead-at-end 0 :internal-dur-at-end 478 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3096 :pcs-gap 0 ) true 7 0 Visit 04 should follow directly from Visit 03 in a contiguous sequence of 26 HST orbits in total.