0 Assigned ID: 3529 ----- Attempting Submission 1 (Fri Mar 25 20:45:58 GMT 2022) ----- HST Phase I Proposal 3529 successfully submitted. Receipt: # 3529-1 ----- Attempting Submission 2 (Fri Mar 25 23:03:39 GMT 2022) ----- HST Phase I Proposal 3529 successfully submitted. Receipt: # 3529-2 ----- Attempting Submission 3 (Fri Mar 25 23:20:53 GMT 2022) ----- The number of orbits used exceeds the number allocated This target is not used in this proposal. This target is not used in this proposal. This target is not used in this proposal. FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser We corrected the POSTARG Y to be -50 arcsec, so the target's spectrum will land inside the subarray as intended. (Visit 01 failed because of that error). Peter and Jennifer Mack double checked and expect Visit 02 to work as we intended Visit 01 to. We picked a new target form those we had pre-selected; the new target's availability begins around Dec 24, so that works well for this program hopefully to get prompt scheduling. 1973493611 ----- Attempting Submission 1 (Thu Nov 03 16:12:11 GMT 2022) ----- ----- Attempting Submission 2 (Mon Dec 12 16:43:19 GMT 2022) ----- All the warnings about lack of FLASH are intentional. I checked the Target Confirmation in Aladin. This time both in the target ACQ and the G280 spectra! We use observations of a stable star with the WFC3 UVIS G280 grism in order to measure the following: 1) measure the UVIS shutter's timing jitter, i.e. the non-repeatability of a commanded exposure time due to the vagaries of the mechanical shutter mechanism (current best estimates are 0.004s rms or 0.006s rms); 2) validate if FLASH is important for very bright stellar spectrophotometric time series with G280; and 3) test effects of shutter BLADE (A or B) for the same. The design of this 1-HST-orbit calibration program is as follows: (Note added 12.07.2022: Program 17265's Visit 01 missed the target in the G280 exposures on 11.21.2022 because the POSTARG Y = -50 was omitted, apparently because we had used as a template Program 17082's Visit 05 which failed on 11.23.2022 for the same reason. We have reviewed our error, copied Visit 01 to Visit 02, changed the POSTARG Y to -50 in all G280 exposures, and swapped the target from HR-7596 (V=5.63, A0III) to HR-5501 (V=5.665, B9.5V); the former's availability ended 11/30 and the latter's begins 12/24.) We observe a bright and stable star with G280 grism in order to spread its light out so we can get good spectrophotometric precision in very short exposures so we can measure the shutter timing jitter, i.e. the non-repeatability of a commanded exposure time due to the vagaries of the mechanical shutter mechanism. We use a subarray to capture the ROI of the +1 and -1 orders of G280 simultaneously. The latter provides approximately 3x dynamic range because the +1 order has ~3x greater throughput than the -1 order; this will allow us to observe the star well into saturation to determine if good spectrophotometry can be obtained even while saturating the spectrum, and bleeding charge. We select spectrophotometric standard stars from the references below, looking for ones with V=6, type = A0V. If our primary target HR-7596 cannot be used for some reason, we have identified four other similar targets. We use a custom subarray, centered on the zeroth order of G280 spectrum. The subarray parameters have been tested in GO programs 16086 and others. Here, we choose a smaller but adequate SIZEAXIS2=340 to allow us to buffer dump at the end during Earth occultation. We test whether FLASH=20 (following the approach adopted in GO 16086 and discussed in the Instrument Science Report WFC3 2021-09) is useful or not with the 2s exposures in the second half of the orbit. The specific value of FLASH=20 is the one recommended by the ETC. The 2s exposure is chosen to optimally expose (but not saturate) the -1 order and also to be long enough that shutter timing jitter will be a small effect. We needed to use a different filter than in GO 16086 to avoid saturating the ACQ REF direct image. The first exposure will be with shutter BLADE=A in order to know which shutter BLADE each exposure is: A, B, A, B, .... We make all exposures in pairs so we will get BLADE=A and BLADE=B, one after the other, for each and every configuration. 2 ACQ exposures, one with FLASH and the other without FLASH; The second one also assures that each of the following series start with BLADE=A. Six exposures in series of 0.5s, 0.7s, 1s, and 4s, then twenty exposures ( five sets of four 2s exposures), as follows do i=1, 5 { 2sA 2sB 2sAFLASH 2sBFLASH } The 2s exposures are interlaced FLASH, NO FLASH, FLASH, NO FLASH so that any environmental changes, e.g. scattered light will be similar throughout each series. ETC runs are listed only for the 1s G280 exposure and the 0.5s F280N direct image for ACQ. References: https://www2.keck.hawaii.edu/inst/esi/flux_stds.html https://www2.keck.hawaii.edu/inst/common/stone_stds_hst.html https://www.eso.org/sci/observing/tools/standards/spectra/stanlis.html Exoplanets and Exoplanet Formation 0 false false RESTRICTED STAR A0-A3 V-IV This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 CALIBRATION PHOTOMETRIC This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 CALIBRATION PHOTOMETRIC This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 CALIBRATION PHOTOMETRIC This object was generated by the targetselector and retrieved from the SIMBAD database. Picked it from the following list, looking for a star close to type A0 and B=6 mag. https://www.eso.org/sci/observing/tools/standards/spectra/stanlis.html J2000 CALIBRATION PHOTOMETRIC This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 WFC3/UVIS Spectroscopic No No G280 WFC3/IR Spectroscopic No No G102 WFC3/IR Spectroscopic No No G141 1667491624709 The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. 1669031186000 67.60343615385281 (Tic-Visit :proposal-id 17265 :visit-id "01" :proposal-version -1 :trans-version "20220630" :date "03-Nov-2022 12:07:03.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 584400 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17265 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17265 :visit-id "01" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2703 :al-overhead-at-end 52 :internal-dur-at-end 675 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) true 1 0 Two exposures in series: BLADE=A with FLASH and BLADE=B with no FLASH. Detector chip 2. We include FLASH=20, as we anticipate < 1 e- of background per science exposure, in order to ensure maximum CTE. Detector chip 2. We include FLASH=20, as we anticipate < 1 e- of background per science exposure, in order to ensure maximum CTE. Detector chip 2. We include FLASH=20, as we anticipate < 1 e- of background per science exposure, in order to ensure maximum CTE. Detector chip 2. We include FLASH=20, as we anticipate < 1 e- of background per science exposure, in order to ensure maximum CTE. Detector chip 2. We include FLASH=20, as we anticipate < 1 e- of background per science exposure, in order to ensure maximum CTE. Detector chip 2. We include FLASH=20, as we anticipate < 1 e- of background per science exposure, in order to ensure maximum CTE. Detector chip 2. We include FLASH=20, as we anticipate < 1 e- of background per science exposure, in order to ensure maximum CTE. Detector chip 2. We include FLASH=20, as we anticipate < 1 e- of background per science exposure, in order to ensure maximum CTE. Detector chip 2. We include FLASH=20, as we anticipate < 1 e- of background per science exposure, in order to ensure maximum CTE. Detector chip 2. We include FLASH=20, as we anticipate < 1 e- of background per science exposure, in order to ensure maximum CTE. Detector chip 2. We include FLASH=20, as we anticipate < 1 e- of background per science exposure, in order to ensure maximum CTE. Detector chip 2. We include FLASH=20, as we anticipate < 1 e- of background per science exposure, in order to ensure maximum CTE. Detector chip 2. We include FLASH=20, as we anticipate < 1 e- of background per science exposure, in order to ensure maximum CTE. Detector chip 2. We include FLASH=20, as we anticipate < 1 e- of background per science exposure, in order to ensure maximum CTE. 1670421685050 The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. (Tic-Visit :proposal-id 17265 :visit-id "02" :proposal-version -1 :trans-version "20220630" :date "07-Dec-2022 09:01:24.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 584400 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17265 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17265 :visit-id "02" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2703 :al-overhead-at-end 52 :internal-dur-at-end 675 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) true 1 0 Two exposures in series: BLADE=A with FLASH and BLADE=B with no FLASH. Detector chip 2. We include FLASH=20, as we anticipate < 1 e- of background per science exposure, in order to ensure maximum CTE. Detector chip 2. We include FLASH=20, as we anticipate < 1 e- of background per science exposure, in order to ensure maximum CTE. Detector chip 2. We include FLASH=20, as we anticipate < 1 e- of background per science exposure, in order to ensure maximum CTE. Detector chip 2. We include FLASH=20, as we anticipate < 1 e- of background per science exposure, in order to ensure maximum CTE. Detector chip 2. We include FLASH=20, as we anticipate < 1 e- of background per science exposure, in order to ensure maximum CTE. Detector chip 2. We include FLASH=20, as we anticipate < 1 e- of background per science exposure, in order to ensure maximum CTE. Detector chip 2. We include FLASH=20, as we anticipate < 1 e- of background per science exposure, in order to ensure maximum CTE. Detector chip 2. We include FLASH=20, as we anticipate < 1 e- of background per science exposure, in order to ensure maximum CTE. Detector chip 2. We include FLASH=20, as we anticipate < 1 e- of background per science exposure, in order to ensure maximum CTE. Detector chip 2. We include FLASH=20, as we anticipate < 1 e- of background per science exposure, in order to ensure maximum CTE. Detector chip 2. We include FLASH=20, as we anticipate < 1 e- of background per science exposure, in order to ensure maximum CTE. Detector chip 2. We include FLASH=20, as we anticipate < 1 e- of background per science exposure, in order to ensure maximum CTE. Detector chip 2. We include FLASH=20, as we anticipate < 1 e- of background per science exposure, in order to ensure maximum CTE. Detector chip 2. We include FLASH=20, as we anticipate < 1 e- of background per science exposure, in order to ensure maximum CTE.