Heather - Here's my phase-2-craft for 13501. I am uploading it now. It sometimes takes 24 hours for the STSCI database to move it to the public domain that APT can retrieve. So I have attached it to this email.
Beth – can you fit either visit 4 or visit 3 into Visit 1's Jan 7, 2014 slot? If so, then it will only require Heather to give the A-OK and we're done. (It may also require Claus Leitherer or his deputy or John MacKenty to approve the use of the F132N filter, or your replacement of that with a BLANK). If you have trouble reaching people, I may have their cell phone numbers.
I realize this is a very late change, but we only got the data 3 days ago (from the Dec 19, 2013 transit) that showed that we could improve the phase 2 by making this change. We really appreciate your efforts both in crafting the phase 2 and shoe-horning it into the schedule for the Jan 7 date. I hope this one can drop right in and replace that one – I tuned it with that in mind.
- Peter-1026753144----- Attempting Submission 4 (Mon Dec 23 16:58:19 GMT 2013) -----The Visit 4 and Visit 3 are two alternates for Visit 1 to be executed Jan 7, 2014. That's why it trips the "using too many orbits" error.Characterizing the Atmosphere of Benchmark Super-Earth HD 97658bSuper-Earth planets are ubiquitous, diverse, and poorly characterized. Kepler has discovered several thousand planet candidates with radii intermediate between the Earth and Neptune, yet to date only one nearby super-Earth, GJ 1214b, has been studied in detail. We propose to measure the atmospheric scale height of HD 97658b, a recently detected close analogue of GJ 1214b in bulk mass and radius. HD 97658b is the only other super-Earth aside from GJ 1214b that can be easily characterized with HST, and is likely to be the target of multiple observing proposals in Cycle 22. By investing a small amount of telescope time now, we can ensure that the proposing teams and the HST TAC are able to make informed decisions about how best to use scarce observing resources. Our WFC3 measurement will cleanly distinguish a large scale-height, hydrogen-dominated atmosphere from a compact, water steam atmosphere. The measurement will also be the first and most important step toward characterizing the planet's bulk composition. Currently, the mass and radius measurements of HD 97658 are compatible with widely divergent interior compositions: a water world of half rock and half water, a mini-Neptune, or a planet of terrestrial composition with outgassed hydrogen. The detection of a low scale-height water atmosphere would strongly suggest a water world bulk composition, and a birth near or beyond the ice line of the protoplanetary disk. We will directly compare the atmospheres of HD 97658b and GJ 1214b, providing the first measure of the diversity of super-Earth atmospheres prior to the era of JWST.We will observe two transits of HD 97658 in scan mode, with five orbits per visit. The timing windows were selected so the third orbit would end around the mid-transit time in the first visit, and the fourth orbit would begin around the mid-transit time in the second visit. This ensures near-total coverage of the 178 minute transit over the two visits.
We use a scan rate of 1.4"/s and an initial position of -17", which should ensure that the full 21" long vertical scan is contained within the 256x256 subarray.Visit 1 of program 13501, set to execute on Jan 7, 2014, as currently prescribed has irregular pattern of exposures which is bad practice for the WFC3 IR detector for precision time series. Visit 2 (executed on Dec 19, 2013) had a similar layout and the light curve has lots of systematics that will be unlikely or impossible to remove well.
Here are two alternates for Visit 1: Only one visit should be executed, commensurate with the number of orbits allocated to this program. Use Visit 4 if it schedules; use Visit 3 if Visit 4 cannot be made to work. The padding exposures are F132N filters. That will throw a flag because we did not specify F132N in our phase 1; we chose F139M. However, F132N is a better choice because it will not saturate the detector as much as the 4x wider F139M. A BLANK would be preferable to F132N, but that will require special commanding because GOs are not allowed to specify the BLANK. (If you replace F132N with BLANK, do not also replace F139M with BLANK - we should have one direct image of the star).EXTRA-SOLAR PLANETS0falsefalse0.00.0falsefalsefalseSUPPORTEDSTARK V-IVThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000WFC3/IRSpectroscopicNoNoG141The scheduling data was generated by CASM 21.2.CASM was run in Phase II mode.52(Tic-Visit
:proposal-id 13501
:visit-id "01"
:proposal-version -1
:trans-version "20130502"
:date "23-Dec-2013 08:53:39.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 5
:saa-model "30"
:si-bright-earth-limb-angle 20.0
:data-volume 994848
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
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:pcs-mode "FGS"
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(Tic-Obset
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:dark-utilization 0
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:low-sky "N"
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)
(Tic-Orbit
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:orbit-number 2
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(Tic-Orbit
:proposal-id 13501
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(Tic-Orbit
:proposal-id 13501
:visit-id "01"
:orbit-number 4
:pcs-time 176
:si-vis-utilization 2909
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:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
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(Tic-Orbit
:proposal-id 13501
:visit-id "01"
:orbit-number 5
:pcs-time 176
:si-vis-utilization 2790
:al-overhead-at-end 0
:internal-dur-at-end 375
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
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)false50The scheduling data was generated by CASM 21.2.CASM was run in Phase II mode.52Visit 3 (second-choice alternate for Visit 1):
The buffer dumps are being triggered when the number of headers = 304. We have NSAMP=3, so 4 headers per exposure. I put 38 exposures into each orbit, so a buffer dump is forced every other orbit (76 exposures times 4 headers per exposure = 304 headers). I managed the first orbit's asymmetry (due to the direct image) by making it NSAMP=7 (8 headers) and asking for only a total of 37 exposures in that orbit. We have 188 scans total; 188=36+4*38. That's to be compared with Visit 1's 36+39+47+36+45=203 scans. That implies a loss of Poisson-limited S/N of only 4%; sqrt(203./188.) = 1.04. It might be better or worse in terms of in-transit photon collection compared to Visit 1 depending on when buffer dumps line up with the transit. The point is that it's not a large factor (4%).
We could tune the first orbit to either have the buffer dump come after the 2nd orbit, or at the start of visibility of the 3rd orbit, depending on where we wanted to phase up the exposures on the ephemeris of the transit on Jan 7, 2014. Or there may be a way to have the system "hold in place" to phase shift the pattern in the visibility window. However, a fixed pattern at fixed 96-min cadence may be preferable in terms of empirical modeling of detector systematics.(Tic-Visit
:proposal-id 13501
:visit-id "03"
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:date "23-Dec-2013 09:42:59.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 5
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:data-volume 912048
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(Tic-Obset
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(Tic-Orbit
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(Tic-Orbit
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(Tic-Orbit
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(Tic-Orbit
:proposal-id 13501
:visit-id "03"
:orbit-number 4
:pcs-time 176
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(Tic-Orbit
:proposal-id 13501
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:orbit-number 5
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:dark-offset NIL
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)false50The scheduling data was generated by CASM 21.2.CASM was run in Phase II mode.52Visit 4 (first choice alternate for visit 1):
This one forces a buffer dump each orbit so we can use more of the available time. It took some iterative craftsmanship with APT. We use the requirement that the buffer dumps after the equivalent of two full-frame images, each NSAMP=15 (I.e. 16 samples). We pad each orbit with some direct narrow-band images to fill the buffer, then iterate on the NSAMP of the last exposure until it packs properly into exactly one orbit. We require that the first orbit's unused visibility ends before 42:33 (from visit 1, which we know schedules on Jan 7, 2014). We also require that orbits 2,3,4, and 5's unused visibilities begin before 51:21, 51:30, 51:25, and 49:26. We find that a pattern of 42 GRISM exposures (plus a set of direct images for padding) has unused visibility beginning at 50:11, so we use that for the last four orbits, and then for the final orbit, we trim off the last IR direct images (the pads) and replace them with grism pairs, since at that point we don't need to worry about buffer management since it's the program's last orbit.
This visit has 32+42+42+42+46=204 scans (one more than Visit 1's 203 scans). As designed, Visit 4 (like Visit 3) has a fixed pattern of scans, each one uninterrupted in the visibility period.(Tic-Visit
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(Tic-Orbit
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)false50The scheduling data was generated by CASM 21.2.CASM was run in Phase II mode.501387478399000298.08995484978277(Tic-Visit
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:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 5
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:data-volume 994848
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(Tic-Orbit
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