0 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 high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long 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 high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long 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 high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long 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 have copied the failed visit 6 into visit 56 (HOPR 93049). A minor change was made to all remaining visits, increasing the SIZEAXIS2=300 to 310. This is to provide more room for the direct image, as the target in the direct image was very near the bottom of the subarray with 300. There is no noticable change in the overheads or the total duration. In addition, in visit 4 the F300X direct image filter was corrected from a larger subarray to the same sub-array size as the G280 spectra. -1550243620 ----- Attempting Submission 1 (Thu Apr 04 20:49:28 GMT 2024) ----- ----- Attempting Submission 2 (Thu Jan 09 14:08:14 GMT 2025) ----- We are following the recomended post-flash of 12 e-/pixel from STScI, but this value can be adjusted if need be. JWST's Exoplanet Grand Tour Spectroscopic Survey During their Grand Tour, the Voyager spacecraft revolutionized our view of the solar system, making more fundamental discoveries about different planetary environments than any mission before or since. Thousands of exoplanets are now known, and with the transformative capabilities of JWST, a Grand Tour of the exoplanets can now begin. How exoplanets form and their overall composition and chemical makeup remain major outstanding issues, and we seek to make progress on the underlying physical processes of these topics by unlocking the rich spectra of exoplanetary atmospheres, synergizing JWST's capabilities with HST. Here, we propose a first-generation JWST-HST exoplanet statistical survey covering giant planets from Neptune to Jupiter sizes. With a wide comprehensive survey across the major giant planet types and temperatures, our Grand Tour will establish a legacy dataset of high-quality exoplanet spectra early in JWST's lifetime. Without this frame of reference, the multitude of single-planet JWST studies will be hard to place in the context of the wider perspective, and rich areas of discovery can be easily overlooked. This program synthesizes the discordant Cycle 1 & 2 observations by carefully selecting 142 hours of complimentary key targets and wavelengths, leveraging the entire set into a 1st generation 350-hour Treasury-level 25 planet survey, a true exoplanet Grand Tour. A statistically significant number of planets will be available in JWST's first few cycles, enabling comparison studies which will provide immediate progress in answering several longstanding key questions relevant to all exoplanet types regarding their atmospheric chemistry and formation. This program uses HST/WFC3 UVIS slitless spectrograph with the G280 grism to obtain an exoplanet transmission spectra of HATS-72b, NGTS-2b, and HAT-P-30b covering 0.2 to 1.0 microns. Three transits of HATS-72b (requiring four consecutive orbits), one transit of HATS-72b (requiring six consecutive orbits), and two transits of HAT-P-30b (requiring three consecutive orbits) will be done, for a total of 24 orbits. Though HST is operating in reduced gyro mode, for each transit the orbits must be executed consecutively in order to measure both the transit and have sufficient baseline flux out of transit. This is critical in order to accurately characterize telescope systematics and determine the true wavelength-dependent transit depth. Other than this, because UVIS does not use spatial scanning, this impact of RGM will not affect these observations. Phase constraints have been set in the aquisition image of each visit to observe the transit near the middle of the visits. Orient restrictions have been added such that the spectra of nearby stars (or, in the case of HAT-P-30, a binary companion about 4" away) will not overlap the target spectra. We have estimated the exposure times using the STScI ETC, and will adopt 175, 118, and 71 second exposures for HATS-72b, NGTS-2b, and HAT-P-30, respectively. We use a post-flash of 12 electrons/pixel, as is recommended by STScI to reduced the impact of charge trapping. As buffer dumps are an important issue with UVIS, we will use sub-arrays to increase duty cycle. Sub-array sizes of 300x1700 limits the overheads between exposures, and contains the entire useable spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. Using APT, we found 11, 16, and 20 exposures per orbit can be obtained for the three systems, respectively (with the first orbit typically having one fewer exposure due to target acquisition). Prof. Sing is an expert in the analysis and interpretation of transiting exoplanets, leading many HST observing programs targeting transiting planets over the last 10 cycles including small, large, and Treasury programs. He has published 43 refereed papers over the last 12 years on space-based transiting exoplanet data. Prof. Sing has additional expertise in retrieval analyses of exoplanet atmosphere data. Prof. Greg Henry is a senior research scientist with the Automated Astronomy Group at Tennessee State University. In that capacity, he oversees a network of robotic telescopes that conduct a wide variety of astronomical Dr. Lopez-Morales is the Co-PI of The HST PanCET program (HST GO 16767) which observed the atmospheres of 20 gas giants at UV, Visible and near-IR wavelengths with all current instruments on HST. Lopez-Morales is also the PI of the ACCESS Survey on the Magellan telescopes, which is obtaining a large database of optical transmission spectra of Jupiter-to-Neptune size exoplanets. Dr. Lothringer is an expert in both observing exoplanet atmospheres with HST and the modeling of atmospheres with PHOENIX. He has extensive experience studying the highly irradiated class of ultra-hot Jupiters and is PI of 4 HST programs and is co-I on 6 other programs. Prof. N. Mayne, Dr. P. Tremblin, Dr. J. Goyal are experts in the 1D/3D (and lower dimensionality) modelling of exoplanet climates, including dynamics, radiative transfer, chemistry, clouds, and generation of synthetic observables. Maria Zamyatina is an expert in atmospheric chemistry, including analysis of chemical networks and pathways, and the simulation of planetary climates including chemical kinetics. Z. Rustamkulov, Natalie Allen, K Bennett, & L. Ramos-Rosado are PhDs student at JHU advised by Prof. Sing and are focusing their PhDs on the observations of transiting exoplanets. Prof. Kevin Schlaufman is an expert in the use of the characteristics of planets and the abundance of their host stars to uncover the unobservable properties of protoplanetary disks and the planet formation process. Dr. K. Stevenson and Dr. Fu are experts in transit observations and data analysis. Dr. Henrique Reggiani is an expert in precision stellar spectroscopy and stellar characterization. He has extensive experience in the analysis of stellar atmospheric parameters and abundances, including non-LTE modelling of spectral features. He is co-Pi in other 3 JWST programs as the stellar characterization expert. Exoplanets and Exoplanet Formation 0 false false false false false false false false AVAILABLE STAR EXTRA-SOLAR PLANET EXTRA-SOLAR PLANETARY SYSTEM K III-I This object was generated by the targetselector and retrieved from the SIMBAD database. SIMBAD listed proper motion for this target. When retrieving targets with PM from SIMBAD, APT requests the coordinates be calculated with an epoch of the year 2000. Do not modify this epoch. Always review coordinates using the Target Confirmation tool, which graphically displays the PM. J2000 J2000 STAR EXTRA-SOLAR PLANET EXTRA-SOLAR PLANETARY SYSTEM F3-F9 This object was generated by the targetselector and retrieved from the SIMBAD database. SIMBAD listed proper motion for this target. When retrieving targets with PM from SIMBAD, APT requests the coordinates be calculated with an epoch of the year 2000. Do not modify this epoch. Always review coordinates using the Target Confirmation tool, which graphically displays the PM. J2000 J2000 STAR EXTRA-SOLAR PLANET EXTRA-SOLAR PLANETARY SYSTEM F3-F9 This object was generated by the targetselector and retrieved from the SIMBAD database. SIMBAD listed proper motion for this target. When retrieving targets with PM from SIMBAD, APT requests the coordinates be calculated with an epoch of the year 2000. Do not modify this epoch. Always review coordinates using the Target Confirmation tool, which graphically displays the PM. J2000 J2000 WFC3/UVIS Spectroscopic No No G280 WFC3/UVIS Spectroscopic No No G280 WFC3/UVIS Spectroscopic No No G280 /Users/davidsing/Library/CloudStorage/OneDrive - Johns Hopkins 2/PROPOSALS/JWST_props/JWST_Cycle_3/Treasury_transit_survey_05924/OP-cache/HST_apt_8jan_25-v01.xml The scheduling data was generated by CASM 32.1.3. CASM was run in Phase II mode. The optional parameters SIZEAXIS1=1700 and SIZEAXIS2=300 are used for all exposures to minimize the data volume and hence time lost to buffer dumps. This is fine for the data that needs to be obtained because the spectum will occupy only a narrow swath of pixel rows within the field. This also requires the use of optional parameters CENTERAXIS1 and CENTERAXIS2 in order to "steer" the location of the subarray readout so that it is centered on the target spectrum. If we were positioning on chip 1 we could set CENTERAXIS2=TARGET. However, for the field center (nominal "UVIS" aperture) location on chip 2, we cannot center the subarray on the target because this would cause the subarray to extend into the chip gap, so we hardwire CENTERAXIS1=2136 and CENTERAXIS2=1216, which is intende to put the vertical center of the subarray on the zeroth order of the target spectrum. Chip 2 biases are taken at the end of the visit because the grism exposures use custom subarrays, which will not have matching biases from the WFC3 bias calibration program. For each visit we have phase constraints around the event of the planetary transit, both the orbital period of the planet and the phasing needed are placed on the first exposure in the sequence for each visit. Each exposure in the visit must be observed sequentially with no interruption. 1720303300000 254.48537129364746 (Tic-Visit :proposal-id 17612 :visit-id "01" :proposal-version -1 :trans-version "20240604" :date "09-Jan-2025 08:46:59.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 407056 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17612 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17612 :visit-id "01" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2493 :al-overhead-at-end 43 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2913 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17612 :visit-id "01" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2503 :al-overhead-at-end 43 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2913 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17612 :visit-id "01" :orbit-number 3 :pcs-time 380 :si-vis-utilization 2503 :al-overhead-at-end 43 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2913 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17612 :visit-id "01" :orbit-number 4 :pcs-time 380 :si-vis-utilization 2503 :al-overhead-at-end 43 :internal-dur-at-end 692 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2913 :pcs-gap 0 ) true 4 0 Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=300 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=300 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Exposure times of 173 seconds have been chosen to optimize between exposure time and number of subexposures. Though the target can be observed longer per exposure without saturating, roughly 10 subexposures per orbit are needed to fully characterize UVIS systematics. Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=300 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Exposure times of 173 seconds have been chosen to optimize between exposure time and number of subexposures. Though the target can be observed longer per exposure without saturating, roughly 10 subexposures per orbit are needed to fully characterize UVIS systematics. Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=300 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Exposure times of 173 seconds have been chosen to optimize between exposure time and number of subexposures. Though the target can be observed longer per exposure without saturating, roughly 10 subexposures per orbit are needed to fully characterize UVIS systematics. Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=300 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Exposure times of 173 seconds have been chosen to optimize between exposure time and number of subexposures. Though the target can be observed longer per exposure without saturating, roughly 10 subexposures per orbit are needed to fully characterize UVIS systematics. /Users/davidsing/Library/CloudStorage/OneDrive - Johns Hopkins 2/PROPOSALS/JWST_props/JWST_Cycle_3/Treasury_transit_survey_05924/OP-cache/HST_apt_8jan_25-v02.xml The scheduling data was generated by CASM 32.1.3. CASM was run in Phase II mode. The optional parameters SIZEAXIS1=1700 and SIZEAXIS2=300 are used for all exposures to minimize the data volume and hence time lost to buffer dumps. This is fine for the data that needs to be obtained because the spectum will occupy only a narrow swath of pixel rows within the field. This also requires the use of optional parameters CENTERAXIS1 and CENTERAXIS2 in order to "steer" the location of the subarray readout so that it is centered on the target spectrum. If we were positioning on chip 1 we could set CENTERAXIS2=TARGET. However, for the field center (nominal "UVIS" aperture) location on chip 2, we cannot center the subarray on the target because this would cause the subarray to extend into the chip gap, so we hardwire CENTERAXIS1=2136 and CENTERAXIS2=1216, which is intende to put the vertical center of the subarray on the zeroth order of the target spectrum. Chip 2 biases are taken at the end of the visit because the grism exposures use custom subarrays, which will not have matching biases from the WFC3 bias calibration program. For each visit we have phase constraints around the event of the planetary transit, both the orbital period of the planet and the phasing needed are placed on the first exposure in the sequence for each visit. Each exposure in the visit must be observed sequentially with no interruption. (Tic-Visit :proposal-id 17612 :visit-id "02" :proposal-version -1 :trans-version "20240604" :date "09-Jan-2025 08:58:55.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 420880 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17612 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17612 :visit-id "02" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2493 :al-overhead-at-end 43 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2913 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17612 :visit-id "02" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2503 :al-overhead-at-end 43 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2913 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17612 :visit-id "02" :orbit-number 3 :pcs-time 380 :si-vis-utilization 2503 :al-overhead-at-end 43 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2913 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17612 :visit-id "02" :orbit-number 4 :pcs-time 380 :si-vis-utilization 2503 :al-overhead-at-end 43 :internal-dur-at-end 707 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2913 :pcs-gap 0 ) true 4 0 Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=300 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=310 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Exposure times of 173 seconds have been chosen to optimize between exposure time and number of subexposures. Though the target can be observed longer per exposure without saturating, roughly 10 subexposures per orbit are needed to fully characterize UVIS systematics. Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=310 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Exposure times of 173 seconds have been chosen to optimize between exposure time and number of subexposures. Though the target can be observed longer per exposure without saturating, roughly 10 subexposures per orbit are needed to fully characterize UVIS systematics. Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=310 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Exposure times of 173 seconds have been chosen to optimize between exposure time and number of subexposures. Though the target can be observed longer per exposure without saturating, roughly 10 subexposures per orbit are needed to fully characterize UVIS systematics. Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=310 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Exposure times of 173 seconds have been chosen to optimize between exposure time and number of subexposures. Though the target can be observed longer per exposure without saturating, roughly 10 subexposures per orbit are needed to fully characterize UVIS systematics. /Users/davidsing/Library/CloudStorage/OneDrive - Johns Hopkins 2/PROPOSALS/JWST_props/JWST_Cycle_3/Treasury_transit_survey_05924/OP-cache/HST_apt_8jan_25-v03.xml The scheduling data was generated by CASM 32.1.3. CASM was run in Phase II mode. The optional parameters SIZEAXIS1=1700 and SIZEAXIS2=300 are used for all exposures to minimize the data volume and hence time lost to buffer dumps. This is fine for the data that needs to be obtained because the spectum will occupy only a narrow swath of pixel rows within the field. This also requires the use of optional parameters CENTERAXIS1 and CENTERAXIS2 in order to "steer" the location of the subarray readout so that it is centered on the target spectrum. If we were positioning on chip 1 we could set CENTERAXIS2=TARGET. However, for the field center (nominal "UVIS" aperture) location on chip 2, we cannot center the subarray on the target because this would cause the subarray to extend into the chip gap, so we hardwire CENTERAXIS1=2136 and CENTERAXIS2=1216, which is intende to put the vertical center of the subarray on the zeroth order of the target spectrum. Chip 2 biases are taken at the end of the visit because the grism exposures use custom subarrays, which will not have matching biases from the WFC3 bias calibration program. For each visit we have phase constraints around the event of the planetary transit, both the orbital period of the planet and the phasing needed are placed on the first exposure in the sequence for each visit. Each exposure in the visit must be observed sequentially with no interruption. (Tic-Visit :proposal-id 17612 :visit-id "03" :proposal-version -1 :trans-version "20240604" :date "09-Jan-2025 08:58:58.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 420880 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17612 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17612 :visit-id "03" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2493 :al-overhead-at-end 43 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2913 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17612 :visit-id "03" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2503 :al-overhead-at-end 43 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2913 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17612 :visit-id "03" :orbit-number 3 :pcs-time 380 :si-vis-utilization 2503 :al-overhead-at-end 43 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2913 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17612 :visit-id "03" :orbit-number 4 :pcs-time 380 :si-vis-utilization 2503 :al-overhead-at-end 43 :internal-dur-at-end 707 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2913 :pcs-gap 0 ) true 4 0 Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=300 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=310 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Exposure times of 173 seconds have been chosen to optimize between exposure time and number of subexposures. Though the target can be observed longer per exposure without saturating, roughly 10 subexposures per orbit are needed to fully characterize UVIS systematics. Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=310 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Exposure times of 173 seconds have been chosen to optimize between exposure time and number of subexposures. Though the target can be observed longer per exposure without saturating, roughly 10 subexposures per orbit are needed to fully characterize UVIS systematics. Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=310 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Exposure times of 173 seconds have been chosen to optimize between exposure time and number of subexposures. Though the target can be observed longer per exposure without saturating, roughly 10 subexposures per orbit are needed to fully characterize UVIS systematics. Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=310 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Exposure times of 173 seconds have been chosen to optimize between exposure time and number of subexposures. Though the target can be observed longer per exposure without saturating, roughly 10 subexposures per orbit are needed to fully characterize UVIS systematics. /Users/davidsing/Library/CloudStorage/OneDrive - Johns Hopkins 2/PROPOSALS/JWST_props/JWST_Cycle_3/Treasury_transit_survey_05924/OP-cache/HST_apt_8jan_25-v04.xml The scheduling data was generated by CASM 32.1.3. CASM was run in Phase II mode. The optional parameters SIZEAXIS1=1700 and SIZEAXIS2=300 are used for all exposures to minimize the data volume and hence time lost to buffer dumps. This is fine for the data that needs to be obtained because the spectum will occupy only a narrow swath of pixel rows within the field. This also requires the use of optional parameters CENTERAXIS1 and CENTERAXIS2 in order to "steer" the location of the subarray readout so that it is centered on the target spectrum. If we were positioning on chip 1 we could set CENTERAXIS2=TARGET. However, for the field center (nominal "UVIS" aperture) location on chip 2, we cannot center the subarray on the target because this would cause the subarray to extend into the chip gap, so we hardwire CENTERAXIS1=2136 and CENTERAXIS2=1216, which is intended to put the vertical center of the subarray on the zeroth order of the target spectrum. Chip 2 biases are taken at the end of the visit because the grism exposures use custom subarrays, which will not have matching biases from the WFC3 bias calibration program. For each visit we have phase constraints around the event of the planetary transit, both the orbital period of the planet and the phasing needed are placed on the first exposure in the sequence for each visit. Each exposure in the visit must be observed sequentially with no interruption. (Tic-Visit :proposal-id 17612 :visit-id "04" :proposal-version -1 :trans-version "20240604" :date "09-Jan-2025 08:59:04.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 6 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 876896 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17612 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17612 :visit-id "04" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2615 :al-overhead-at-end 43 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3034 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17612 :visit-id "04" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2639 :al-overhead-at-end 43 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3034 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17612 :visit-id "04" :orbit-number 3 :pcs-time 380 :si-vis-utilization 2639 :al-overhead-at-end 43 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3034 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17612 :visit-id "04" :orbit-number 4 :pcs-time 380 :si-vis-utilization 2639 :al-overhead-at-end 43 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3034 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17612 :visit-id "04" :orbit-number 5 :pcs-time 380 :si-vis-utilization 2639 :al-overhead-at-end 43 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3034 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17612 :visit-id "04" :orbit-number 6 :pcs-time 380 :si-vis-utilization 2639 :al-overhead-at-end 43 :internal-dur-at-end 822 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3034 :pcs-gap 0 ) true 6 0 Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=300 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=310 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Exposure times have been chosen to achieve 2/3 well-depth and limit the amount of unused time per orbit. Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=310 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Exposure times have been chosen to achieve 2/3 well-depth and limit the amount of unused time per orbit. Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=310 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Exposure times have been chosen to achieve 2/3 well-depth and limit the amount of unused time per orbit. Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=310 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Exposure times have been chosen to achieve 2/3 well-depth and limit the amount of unused time per orbit. Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=310 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Exposure times have been chosen to achieve 2/3 well-depth and limit the amount of unused time per orbit. Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=310 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Exposure times have been chosen to achieve 2/3 well-depth and limit the amount of unused time per orbit. /Users/davidsing/Library/CloudStorage/OneDrive - Johns Hopkins 2/PROPOSALS/JWST_props/JWST_Cycle_3/Treasury_transit_survey_05924/OP-cache/HST_apt_8jan_25-v05.xml The scheduling data was generated by CASM 32.1.3. CASM was run in Phase II mode. The optional parameters SIZEAXIS1=1700 and SIZEAXIS2=300 are used for all exposures to minimize the data volume and hence time lost to buffer dumps. This is fine for the data that needs to be obtained because the spectum will occupy only a narrow swath of pixel rows within the field. This also requires the use of optional parameters CENTERAXIS1 and CENTERAXIS2 in order to "steer" the location of the subarray readout so that it is centered on the target spectrum. If we were positioning on chip 1 we could set CENTERAXIS2=TARGET. However, for the field center (nominal "UVIS" aperture) location on chip 2, we cannot center the subarray on the target because this would cause the subarray to extend into the chip gap, so we hardwire CENTERAXIS1=2136 and CENTERAXIS2=1216, which is intende to put the vertical center of the subarray on the zeroth order of the target spectrum. Chip 2 biases are taken at the end of the visit because the grism exposures use custom subarrays, which will not have matching biases from the WFC3 bias calibration program. For each visit we have phase constraints around the event of the planetary transit, both the orbital period of the planet and the phasing needed are placed on the first exposure in the sequence for each visit. Each exposure in the visit must be observed sequentially with no interruption. 1729546255000 281.7401341238288 (Tic-Visit :proposal-id 17612 :visit-id "05" :proposal-version -1 :trans-version "20240604" :date "09-Jan-2025 08:47:20.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 542736 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17612 :visit-id "05" :obset-id "05" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17612 :visit-id "05" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2452 :al-overhead-at-end 43 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2913 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17612 :visit-id "05" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2511 :al-overhead-at-end 43 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2913 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17612 :visit-id "05" :orbit-number 3 :pcs-time 380 :si-vis-utilization 2511 :al-overhead-at-end 43 :internal-dur-at-end 841 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2913 :pcs-gap 0 ) true 3 0 Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=2250 and SIZEAXIS2=590 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574 & 15288 but have been adjusted to better center the zeroth order spectrum on the sub-array. Exposure times have been chosen to achieve 2/3 well-depth. Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=300 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Exposure times have been chosen to achieve 2/3 well-depth and limit the amount of unused time per orbit. Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=300 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Exposure times have been chosen to achieve 2/3 well-depth and limit the amount of unused time per orbit. Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=300 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Exposure times have been chosen to achieve 2/3 well-depth and limit the amount of unused time per orbit. /Users/davidsing/Library/CloudStorage/OneDrive - Johns Hopkins 2/PROPOSALS/JWST_props/JWST_Cycle_3/Treasury_transit_survey_05924/OP-cache/HST_apt_8jan_25-v06.xml The scheduling data was generated by CASM 32.1.3. CASM was run in Phase II mode. The optional parameters SIZEAXIS1=1700 and SIZEAXIS2=300 are used for all exposures to minimize the data volume and hence time lost to buffer dumps. This is fine for the data that needs to be obtained because the spectum will occupy only a narrow swath of pixel rows within the field. This also requires the use of optional parameters CENTERAXIS1 and CENTERAXIS2 in order to "steer" the location of the subarray readout so that it is centered on the target spectrum. If we were positioning on chip 1 we could set CENTERAXIS2=TARGET. However, for the field center (nominal "UVIS" aperture) location on chip 2, we cannot center the subarray on the target because this would cause the subarray to extend into the chip gap, so we hardwire CENTERAXIS1=2136 and CENTERAXIS2=1216, which is intende to put the vertical center of the subarray on the zeroth order of the target spectrum. Chip 2 biases are taken at the end of the visit because the grism exposures use custom subarrays, which will not have matching biases from the WFC3 bias calibration program. For each visit we have phase constraints around the event of the planetary transit, both the orbital period of the planet and the phasing needed are placed on the first exposure in the sequence for each visit. Each exposure in the visit must be observed sequentially with no interruption. 1731732108000 287.8655580986226 (Tic-Visit :proposal-id 17612 :visit-id "06" :proposal-version -1 :trans-version "20240604" :date "09-Jan-2025 08:47:23.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 542736 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17612 :visit-id "06" :obset-id "06" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17612 :visit-id "06" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2452 :al-overhead-at-end 43 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2913 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17612 :visit-id "06" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2511 :al-overhead-at-end 43 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2913 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17612 :visit-id "06" :orbit-number 3 :pcs-time 380 :si-vis-utilization 2511 :al-overhead-at-end 43 :internal-dur-at-end 841 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2913 :pcs-gap 0 ) true 3 0 Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=2250 and SIZEAXIS2=590 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574 & 15288 but have been adjusted to better center the zeroth order spectrum on the sub-array. Exposure times have been chosen to achieve 2/3 well-depth. Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=300 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Exposure times have been chosen to achieve 2/3 well-depth and limit the amount of unused time per orbit. Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=300 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Exposure times have been chosen to achieve 2/3 well-depth and limit the amount of unused time per orbit. Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=300 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Exposure times have been chosen to achieve 2/3 well-depth and limit the amount of unused time per orbit. The scheduling data was generated by CASM 32.1.3. CASM was run in Phase II mode. /Users/davidsing/Library/CloudStorage/OneDrive - Johns Hopkins 2/PROPOSALS/JWST_props/JWST_Cycle_3/Treasury_transit_survey_05924/OP-cache/HST_apt_8jan_25-v56.xml The optional parameters SIZEAXIS1=1700 and SIZEAXIS2=300 are used for all exposures to minimize the data volume and hence time lost to buffer dumps. This is fine for the data that needs to be obtained because the spectum will occupy only a narrow swath of pixel rows within the field. This also requires the use of optional parameters CENTERAXIS1 and CENTERAXIS2 in order to "steer" the location of the subarray readout so that it is centered on the target spectrum. If we were positioning on chip 1 we could set CENTERAXIS2=TARGET. However, for the field center (nominal "UVIS" aperture) location on chip 2, we cannot center the subarray on the target because this would cause the subarray to extend into the chip gap, so we hardwire CENTERAXIS1=2136 and CENTERAXIS2=1216, which is intende to put the vertical center of the subarray on the zeroth order of the target spectrum. Chip 2 biases are taken at the end of the visit because the grism exposures use custom subarrays, which will not have matching biases from the WFC3 bias calibration program. For each visit we have phase constraints around the event of the planetary transit, both the orbital period of the planet and the phasing needed are placed on the first exposure in the sequence for each visit. Each exposure in the visit must be observed sequentially with no interruption. (Tic-Visit :proposal-id 17612 :visit-id "56" :proposal-version -1 :trans-version "20240604" :date "09-Jan-2025 08:59:10.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 561168 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17612 :visit-id "56" :obset-id "56" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17612 :visit-id "56" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2452 :al-overhead-at-end 43 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2913 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17612 :visit-id "56" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2511 :al-overhead-at-end 43 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2913 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17612 :visit-id "56" :orbit-number 3 :pcs-time 380 :si-vis-utilization 2511 :al-overhead-at-end 43 :internal-dur-at-end 861 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2913 :pcs-gap 0 ) true 3 0 Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=2250 and SIZEAXIS2=590 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574 & 15288 but have been adjusted to better center the zeroth order spectrum on the sub-array. Exposure times have been chosen to achieve 2/3 well-depth. Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=310 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Exposure times have been chosen to achieve 2/3 well-depth and limit the amount of unused time per orbit. Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=310 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Exposure times have been chosen to achieve 2/3 well-depth and limit the amount of unused time per orbit. Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2. SIZEAXIS1=1700 and SIZEAXIS2=310 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574, 15288, and 17162 but have been adjusted to better center the zeroth order spectrum on the sub-array. We use FLASH=12 to meet the nominal count level. Exposure times have been chosen to achieve 2/3 well-depth and limit the amount of unused time per orbit.