0 Assigned ID: 1034 ----- Attempting Submission 1 (Sat Mar 07 00:41:09 GMT 2020) ----- HST Phase I Proposal 1034 successfully submitted. Receipt: # 1034-1 0 The Life and Death of Ultra-Hot Jupiter WASP-12b A new class of exoplanets called ultra-hot Jupiters has recently been recognized; these gas-giant exoplanets are on extremely close orbits around their host stars and have dayside atmospheres which reach >2500 K. Ultra-hot Jupiters are so strongly irradiated that many of the molecules, including the dominant constituent hydrogen, will thermally dissociate on their daysides and may recombine on their cooler nightsides. Significant mass loss and tidal distortion have also been predicted for some ultra-hot Jupiters. However, there are currently few ultra-hot Jupiters whose entire atmospheres are well characterized, and additional high precision observations are required to test recent model predictions. We therefore propose to collect one HST/WFC3 G141 spectroscopic full-orbit phasecurve of WASP-12b - the prototypical ultra-hot Jupiter - in order to create longitudinally resolved temperature and chemical maps, to understand the enormous ellipsoidal variations seen at 4.5 microns, and to better constrain the planet's orbital decay rate and the stellar tidal quality factor. Full-orbit phasecurve observation of the exoplanet WASP-12b using WFC3 G141, containing two secondary eclipses and one transit. We have placed stringent orientation constraints which are necessary to avoid overlapping spectra from nearby stellar objects 1 and 10 arcsec away at PA=250 and 238, respectively. We intend to use the differences between individual non-destructive reads to remove the contamination from the nearby M-dwarfs, using the technique as was tested for HAT-P-32Ab using data from GO 14767 (Nikolov et al., 2018). To guarantee that we are able to subtract the companion spectra, we will also collect 10 staring mode observations during the first, stabilizing orbit (as was done by Kreidberg et al., 2015). We enforce a phase constraint on the first exposure of the first orbit to ensure that we acquire our two baseline orbits before the first secondary eclipse and two baseline orbits after the final secondary eclipse. We have placed our 22 orbits into 3 "visits" with timing constraints on the second and third visits to ensure they follow immediately after each other. We have had to use 3 visits instead of one to solve two error messages from the APT software: (PHASE CRITICAL VISIT HAS PHASE WINDOW LARGER THAN PERIOD; and TOO MANY SUBEXPOSURES IN ONE GROUP (REQUEST HELP FROM YOUR PC)). We have also placed a constraint on the second and third "visits" to ensure that all 22 orbits be collected at the same orientation angle as the first orbit to increase our ability to decorrelate detector systematics and to allow for subtraction of the nearby companion stars. We anticipate there being a need for gyro bias updates and SAA crossing(s), but have not entered any parameters related to this into the APT software. However, two good opportunities for brief interruptions in the observations are at the breaks between visits which are at times not expected to impact the transit, eclipse, or maximum/minimum points of the phasecurve. PI Bell has expertise in the decorrelation of detector systematics through experience in analyzing a HST/STIS secondary eclipse observation of WASP-12b and Spitzer/IRAC phasecurve observations of WASP-12b. PI Bell is a Ph.D. student studying ultra-hot Jupiter atmospheres, both observationally and theoretically, under the supervision of Co-I Cowan who is an expert on using thermal phasecurves to map exoplanetary atmospheres. PI Bell will lead the reduction, analysis, and publication(s) resulting from these proposed observations. Co-Is Stevenson and Kreidberg are experts in HST/WFC3 phasecurve observations: the technique and instrument used in these proposed observations. Co-I Sing is also an expert in exoplanetary observations with HST. These Co-Is have assisted in the planning of our proposed observations and will assist in the reduction and analysis of the data. Co-Is Cubillos, Line, Todorov, and Zellem have expertise in transit/eclipse spectroscopy, the modelling of exoplanetary spectra, and/or spectral retrieval. Co-I Zellem also has experience in phasecurve observations as well as assessing and correcting for the impact of stellar activity on transiting exoplanet spectroscopy. These Co-Is will interpret the observed spectral variations with orbital phase using models with varying chemical composition and/or thermal structure. Co-I Dobbs-Dixon has expertise in numerical modelling of hydrodynamical and radiative processes. Co-I Fortney has expertise with modelling planetary atmospheres, interiors, and thermal evolution. These Co-Is will provide theoretical models to aid in the interpretation of our proposed observations. Co-I Fossati is an expert with HST/COS observations whose research focuses on the observational and theoretical study of atmospheric escape from planets and of star--planet interactions; they will provide theoretical insight into the findings of our proposed observations. Co-I Winn has expertise in transit/eclipse timing and the orbital evolution of exoplanets, and they will use the occultation timings from our observations to constrain the orbital evolution of our proposed target, WASP-12b. Co-I Knutson is an expert in thermal phasecurve observations, having published the very first such observation in 2007. Co-I Dang has expertise in the analysis of Spitzer/IRAC thermal phasecurves. Co-I Zhang has experience in the analysis of Spitzer/IRAC thermal phasecurves and HST/WFC3 spectra. Co-Is Crossfield and Deming are experts in observational atmospheric characterization of exoplanets. These Co-Is will assist in the analysis of our proposed observations. Exoplanets and Exoplanet Formation 6 false false false false false false false SUPPORTED EXT-STAR EXTRA-SOLAR PLANET G V-IV This object was generated by the targetselector and retrieved from the SIMBAD database.This object was generated by the targetselector and retrieved from the SIMBAD database. Edited to include Proper Motion, RV, and Parallax J2000 J2000 WFC3/IR Spectroscopic No No G141 Timing link suitability includes constraints ([Sequence (01 02 03 04 05 06 07) within 1.2 days] [02 After 01]) Hst Same orient constraint links visits (01 02 03 04 05 06 07) The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. /private/var/folders/0b/qbp4bysx6vdbfxvp_xw3dyxw00023y/T/OPVisit16956370952301414103.xml The stringent orientation constraints are necessary to avoid overlapping spectra from nearby stellar objects 1 and 10 arcsec away at PA=250 and 238. We calculate the central values for our orient ranges using Detector Offset+PA=135+250=25 or 205. We calculate the width of our orient range to ensure that after each non-destructive read the two stars' spectra are still separated by >4 FWHM to try to allow for our mildly experimental technique to subtract the comanion flux using the differences between non-destructive reads (tested for HAT-P-32Ab using data from GO 14767; Nikolov et al., 2018). To guarantee that we are able to subtract the companion spectra, we will also collect 10 staring mode observations during the first, stabilizing orbit (as was done by Kreidberg et al., 2015); our orient ranges ensure that the spectra will be separated by >5.6 FWHM for these staring-mode spectra. We enforce a phase constraint on the first exposure to ensure that we acquire our two baseline orbits before the first secondary eclipse and two baseline orbits after the final secondary eclipse. (Tic-Visit :proposal-id 203 :visit-id "01" :proposal-version -1 :trans-version "20220630" :date "05-Oct-2022 15:37:13.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 930176 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 203 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 203 :visit-id "01" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2297 :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 3049 :pcs-gap 0 ) (Tic-Orbit :proposal-id 203 :visit-id "01" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2332 :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 3049 :pcs-gap 0 ) (Tic-Orbit :proposal-id 203 :visit-id "01" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2332 :al-overhead-at-end 0 :internal-dur-at-end 462 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3049 :pcs-gap 0 ) false 3 0 F126N was selected as a narrow band filter to avoid saturation while determining the wavelength solution. This filter was also previously successfully used in GO program 13467 (Kreidberg et al., 2015). No spatial scan desired here to ensure the separation between WASP-12A and the nearby M-dwarf companions WASP-12B,C. Our scan rate, SAMP-SEQ, and NSAMP ere jointly optimized to provide high observing efficiency, a peak per-pixel count of ~35,000 to ensure rapid charge-trapping equilibriation within the first orbit, and the ability to separate the contaminating flux from the nearby M-dwarf companions at PA=250 while also not excessively limiting the ORIENT range of the observations. F126N was selected as a narrow band filter to avoid saturation while determining the wavelength solution. This filter was also previously successfully used in GO program 13467 (Kreidberg et al., 2015). Our scan rate, SAMP-SEQ, and NSAMP ere jointly optimized to provide high observing efficiency, a peak per-pixel count of ~35,000 to ensure rapid charge-trapping equilibriation within the first orbit, and the ability to separate the contaminating flux from the nearby M-dwarf companions at PA=250 while also not excessively limiting the ORIENT range of the observations. F126N was selected as a narrow band filter to avoid saturation while determining the wavelength solution. This filter was also previously successfully used in GO program 13467 (Kreidberg et al., 2015). Our scan rate, SAMP-SEQ, and NSAMP ere jointly optimized to provide high observing efficiency, a peak per-pixel count of ~35,000 to ensure rapid charge-trapping equilibriation within the first orbit, and the ability to separate the contaminating flux from the nearby M-dwarf companions at PA=250 while also not excessively limiting the ORIENT range of the observations. Timing link suitability includes constraints ([Sequence (01 02 03 04 05 06 07) within 1.2 days] [02 After 01] [03 After 02]) Hst Same orient constraint links visits (01 02 03 04 05 06 07) The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. /System/Volumes/Data/solaris/user1/enance/working/hst/OP-cache/203-v02.xml The stringent orientation constraints are necessary to avoid overlapping spectra from nearby stellar objects 1 and 10 arcsec away at PA=250 and 238. We calculate the central values for our orient ranges using Detector Offset+PA=135+250=25 or 205. We calculate the width of our orient range to ensure that after each non-destructive read the two stars' spectra are still separated by >4 FWHM to try to allow for our mildly experimental technique to subtract the comanion flux using the differences between non-destructive reads (tested for HAT-P-32Ab using data from GO 14767; Nikolov et al., 2018). To guarantee that we are able to subtract the companion spectra, we will also collect 10 staring mode observations during the first, stabilizing orbit (as was done by Kreidberg et al., 2015); our orient ranges ensure that the spectra will be separated by >5.6 FWHM for these staring-mode spectra. We enforce a phase constraint on the first exposure to ensure that we acquire our two baseline orbits before the first secondary eclipse and two baseline orbits after the final secondary eclipse. (Tic-Visit :proposal-id 203 :visit-id "02" :proposal-version -1 :trans-version "20220630" :date "05-Oct-2022 12:30:18.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 1401904 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 203 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 203 :visit-id "02" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2616 :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 3049 :pcs-gap 0 ) (Tic-Orbit :proposal-id 203 :visit-id "02" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2616 :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 3049 :pcs-gap 0 ) (Tic-Orbit :proposal-id 203 :visit-id "02" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2616 :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 3049 :pcs-gap 0 ) (Tic-Orbit :proposal-id 203 :visit-id "02" :orbit-number 4 :pcs-time 392 :si-vis-utilization 2616 :al-overhead-at-end 0 :internal-dur-at-end 458 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3049 :pcs-gap 0 ) false 4 0 F126N was selected as a narrow band filter to avoid saturation while determining the wavelength solution. This filter was also previously successfully used in GO program 13467 (Kreidberg et al., 2015). Our scan rate, SAMP-SEQ, and NSAMP ere jointly optimized to provide high observing efficiency, a peak per-pixel count of ~35,000 to ensure rapid charge-trapping equilibriation within the first orbit, and the ability to separate the contaminating flux from the nearby M-dwarf companions at PA=250 while also not excessively limiting the ORIENT range of the observations. F126N was selected as a narrow band filter to avoid saturation while determining the wavelength solution. This filter was also previously successfully used in GO program 13467 (Kreidberg et al., 2015). Our scan rate, SAMP-SEQ, and NSAMP ere jointly optimized to provide high observing efficiency, a peak per-pixel count of ~35,000 to ensure rapid charge-trapping equilibriation within the first orbit, and the ability to separate the contaminating flux from the nearby M-dwarf companions at PA=250 while also not excessively limiting the ORIENT range of the observations. F126N was selected as a narrow band filter to avoid saturation while determining the wavelength solution. This filter was also previously successfully used in GO program 13467 (Kreidberg et al., 2015). Our scan rate, SAMP-SEQ, and NSAMP ere jointly optimized to provide high observing efficiency, a peak per-pixel count of ~35,000 to ensure rapid charge-trapping equilibriation within the first orbit, and the ability to separate the contaminating flux from the nearby M-dwarf companions at PA=250 while also not excessively limiting the ORIENT range of the observations. F126N was selected as a narrow band filter to avoid saturation while determining the wavelength solution. This filter was also previously successfully used in GO program 13467 (Kreidberg et al., 2015). Our scan rate, SAMP-SEQ, and NSAMP ere jointly optimized to provide high observing efficiency, a peak per-pixel count of ~35,000 to ensure rapid charge-trapping equilibriation within the first orbit, and the ability to separate the contaminating flux from the nearby M-dwarf companions at PA=250 while also not excessively limiting the ORIENT range of the observations. Timing link suitability includes constraints ([Sequence (01 02 03 04 05 06 07) within 1.2 days] [03 After 02] [04 After 03]) Hst Same orient constraint links visits (01 02 03 04 05 06 07) The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. /System/Volumes/Data/solaris/user1/enance/working/hst/OP-cache/203-v03.xml We must maintain the same orientation as in "visit" 1 to increase our ability to decorrelate the detector systematics and to allow us to subtract the companion star's spectrum. We also have placed an After Visit requirement to try to ensure that Visit 2 will follow immediately after Visit 1. See the Proposal Description for more details. (Tic-Visit :proposal-id 203 :visit-id "03" :proposal-version -1 :trans-version "20220630" :date "05-Oct-2022 12:30:24.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 700912 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 203 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 203 :visit-id "03" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2616 :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 3049 :pcs-gap 0 ) (Tic-Orbit :proposal-id 203 :visit-id "03" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2616 :al-overhead-at-end 0 :internal-dur-at-end 458 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3049 :pcs-gap 0 ) false 2 0 F126N was selected as a narrow band filter to avoid saturation while determining the wavelength solution. This filter was also previously successfully used in GO program 13467 (Kreidberg et al., 2015). Our scan rate, SAMP-SEQ, and NSAMP ere jointly optimized to provide high observing efficiency, a peak per-pixel count of ~35,000 to ensure rapid charge-trapping equilibriation within the first orbit, and the ability to separate the contaminating flux from the nearby M-dwarf companions at PA=250 while also not excessively limiting the ORIENT range of the observations. F126N was selected as a narrow band filter to avoid saturation while determining the wavelength solution. This filter was also previously successfully used in GO program 13467 (Kreidberg et al., 2015). Our scan rate, SAMP-SEQ, and NSAMP ere jointly optimized to provide high observing efficiency, a peak per-pixel count of ~35,000 to ensure rapid charge-trapping equilibriation within the first orbit, and the ability to separate the contaminating flux from the nearby M-dwarf companions at PA=250 while also not excessively limiting the ORIENT range of the observations. Timing link suitability includes constraints ([Sequence (01 02 03 04 05 06 07) within 1.2 days] [04 After 03] [05 After 04]) Hst Same orient constraint links visits (01 02 03 04 05 06 07) The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. /System/Volumes/Data/solaris/user1/enance/working/hst/OP-cache/203-v04.xml We must maintain the same orientation as in "visit" 1 to increase our ability to decorrelate the detector systematics and to allow us to subtract the companion star's spectrum. We also have placed an After Visit requirement to try to ensure that Visit 2 will follow immediately after Visit 1. See the Proposal Description for more details. (Tic-Visit :proposal-id 203 :visit-id "04" :proposal-version -1 :trans-version "20220630" :date "05-Oct-2022 12:30:32.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 1051408 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 203 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 203 :visit-id "04" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2616 :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 3049 :pcs-gap 0 ) (Tic-Orbit :proposal-id 203 :visit-id "04" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2616 :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 3049 :pcs-gap 0 ) (Tic-Orbit :proposal-id 203 :visit-id "04" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2616 :al-overhead-at-end 0 :internal-dur-at-end 458 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3049 :pcs-gap 0 ) false 3 0 F126N was selected as a narrow band filter to avoid saturation while determining the wavelength solution. This filter was also previously successfully used in GO program 13467 (Kreidberg et al., 2015). Our scan rate, SAMP-SEQ, and NSAMP ere jointly optimized to provide high observing efficiency, a peak per-pixel count of ~35,000 to ensure rapid charge-trapping equilibriation within the first orbit, and the ability to separate the contaminating flux from the nearby M-dwarf companions at PA=250 while also not excessively limiting the ORIENT range of the observations. F126N was selected as a narrow band filter to avoid saturation while determining the wavelength solution. This filter was also previously successfully used in GO program 13467 (Kreidberg et al., 2015). Our scan rate, SAMP-SEQ, and NSAMP ere jointly optimized to provide high observing efficiency, a peak per-pixel count of ~35,000 to ensure rapid charge-trapping equilibriation within the first orbit, and the ability to separate the contaminating flux from the nearby M-dwarf companions at PA=250 while also not excessively limiting the ORIENT range of the observations. F126N was selected as a narrow band filter to avoid saturation while determining the wavelength solution. This filter was also previously successfully used in GO program 13467 (Kreidberg et al., 2015). Our scan rate, SAMP-SEQ, and NSAMP ere jointly optimized to provide high observing efficiency, a peak per-pixel count of ~35,000 to ensure rapid charge-trapping equilibriation within the first orbit, and the ability to separate the contaminating flux from the nearby M-dwarf companions at PA=250 while also not excessively limiting the ORIENT range of the observations. Timing link suitability includes constraints ([Sequence (01 02 03 04 05 06 07) within 1.2 days] [05 After 04] [06 After 05]) Hst Same orient constraint links visits (01 02 03 04 05 06 07) The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. /System/Volumes/Data/solaris/user1/enance/working/hst/OP-cache/203-v05.xml We must maintain the same orientation as in "visit" 1 to increase our ability to decorrelate the detector systematics and to allow us to subtract the companion star's spectrum. We also have placed an After Visit requirement to try to ensure that Visit 2 will follow immediately after Visit 1. See the Proposal Description for more details. (Tic-Visit :proposal-id 203 :visit-id "05" :proposal-version -1 :trans-version "20220630" :date "05-Oct-2022 12:30:40.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 1051408 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 203 :visit-id "05" :obset-id "05" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 203 :visit-id "05" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2616 :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 3049 :pcs-gap 0 ) (Tic-Orbit :proposal-id 203 :visit-id "05" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2616 :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 3049 :pcs-gap 0 ) (Tic-Orbit :proposal-id 203 :visit-id "05" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2616 :al-overhead-at-end 0 :internal-dur-at-end 458 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3049 :pcs-gap 0 ) false 3 0 F126N was selected as a narrow band filter to avoid saturation while determining the wavelength solution. This filter was also previously successfully used in GO program 13467 (Kreidberg et al., 2015). Our scan rate, SAMP-SEQ, and NSAMP ere jointly optimized to provide high observing efficiency, a peak per-pixel count of ~35,000 to ensure rapid charge-trapping equilibriation within the first orbit, and the ability to separate the contaminating flux from the nearby M-dwarf companions at PA=250 while also not excessively limiting the ORIENT range of the observations. F126N was selected as a narrow band filter to avoid saturation while determining the wavelength solution. This filter was also previously successfully used in GO program 13467 (Kreidberg et al., 2015). Our scan rate, SAMP-SEQ, and NSAMP ere jointly optimized to provide high observing efficiency, a peak per-pixel count of ~35,000 to ensure rapid charge-trapping equilibriation within the first orbit, and the ability to separate the contaminating flux from the nearby M-dwarf companions at PA=250 while also not excessively limiting the ORIENT range of the observations. F126N was selected as a narrow band filter to avoid saturation while determining the wavelength solution. This filter was also previously successfully used in GO program 13467 (Kreidberg et al., 2015). Our scan rate, SAMP-SEQ, and NSAMP ere jointly optimized to provide high observing efficiency, a peak per-pixel count of ~35,000 to ensure rapid charge-trapping equilibriation within the first orbit, and the ability to separate the contaminating flux from the nearby M-dwarf companions at PA=250 while also not excessively limiting the ORIENT range of the observations. Timing link suitability includes constraints ([Sequence (01 02 03 04 05 06 07) within 1.2 days] [06 After 05] [07 After 06]) Hst Same orient constraint links visits (01 02 03 04 05 06 07) The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. /System/Volumes/Data/solaris/user1/enance/working/hst/OP-cache/203-v06.xml We must maintain the same orientation as in "visit" 1 to increase our ability to decorrelate the detector systematics and to allow us to subtract the companion star's spectrum. We also have placed an After Visit requirement to try to ensure that Visit 3 will follow immediately after Visit 2. See the Proposal Description for more details. (Tic-Visit :proposal-id 203 :visit-id "06" :proposal-version -1 :trans-version "20220630" :date "05-Oct-2022 12:30:48.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 1051408 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 203 :visit-id "06" :obset-id "06" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 203 :visit-id "06" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2616 :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 3049 :pcs-gap 0 ) (Tic-Orbit :proposal-id 203 :visit-id "06" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2616 :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 3049 :pcs-gap 0 ) (Tic-Orbit :proposal-id 203 :visit-id "06" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2616 :al-overhead-at-end 0 :internal-dur-at-end 458 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3049 :pcs-gap 0 ) false 3 0 F126N was selected as a narrow band filter to avoid saturation while determining the wavelength solution. This filter was also previously successfully used in GO program 13467 (Kreidberg et al., 2015). Our scan rate, SAMP-SEQ, and NSAMP ere jointly optimized to provide high observing efficiency, a peak per-pixel count of ~35,000 to ensure rapid charge-trapping equilibriation within the first orbit, and the ability to separate the contaminating flux from the nearby M-dwarf companions at PA=250 while also not excessively limiting the ORIENT range of the observations. F126N was selected as a narrow band filter to avoid saturation while determining the wavelength solution. This filter was also previously successfully used in GO program 13467 (Kreidberg et al., 2015). Our scan rate, SAMP-SEQ, and NSAMP ere jointly optimized to provide high observing efficiency, a peak per-pixel count of ~35,000 to ensure rapid charge-trapping equilibriation within the first orbit, and the ability to separate the contaminating flux from the nearby M-dwarf companions at PA=250 while also not excessively limiting the ORIENT range of the observations. F126N was selected as a narrow band filter to avoid saturation while determining the wavelength solution. This filter was also previously successfully used in GO program 13467 (Kreidberg et al., 2015). Our scan rate, SAMP-SEQ, and NSAMP ere jointly optimized to provide high observing efficiency, a peak per-pixel count of ~35,000 to ensure rapid charge-trapping equilibriation within the first orbit, and the ability to separate the contaminating flux from the nearby M-dwarf companions at PA=250 while also not excessively limiting the ORIENT range of the observations. Timing link suitability includes constraints ([Sequence (01 02 03 04 05 06 07) within 1.2 days] [07 After 06]) Hst Same orient constraint links visits (01 02 03 04 05 06 07) The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. /System/Volumes/Data/solaris/user1/enance/working/hst/OP-cache/203-v07.xml We must maintain the same orientation as in "visit" 1 to increase our ability to decorrelate the detector systematics and to allow us to subtract the companion star's spectrum. We also have placed an After Visit requirement to try to ensure that Visit 3 will follow immediately after Visit 2. See the Proposal Description for more details. (Tic-Visit :proposal-id 203 :visit-id "07" :proposal-version -1 :trans-version "20220630" :date "05-Oct-2022 12:31:00.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 1401904 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 203 :visit-id "07" :obset-id "07" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 203 :visit-id "07" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2616 :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 3049 :pcs-gap 0 ) (Tic-Orbit :proposal-id 203 :visit-id "07" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2616 :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 3049 :pcs-gap 0 ) (Tic-Orbit :proposal-id 203 :visit-id "07" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2616 :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 3049 :pcs-gap 0 ) (Tic-Orbit :proposal-id 203 :visit-id "07" :orbit-number 4 :pcs-time 392 :si-vis-utilization 2616 :al-overhead-at-end 0 :internal-dur-at-end 458 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3049 :pcs-gap 0 ) false 4 0 F126N was selected as a narrow band filter to avoid saturation while determining the wavelength solution. This filter was also previously successfully used in GO program 13467 (Kreidberg et al., 2015). Our scan rate, SAMP-SEQ, and NSAMP ere jointly optimized to provide high observing efficiency, a peak per-pixel count of ~35,000 to ensure rapid charge-trapping equilibriation within the first orbit, and the ability to separate the contaminating flux from the nearby M-dwarf companions at PA=250 while also not excessively limiting the ORIENT range of the observations. F126N was selected as a narrow band filter to avoid saturation while determining the wavelength solution. This filter was also previously successfully used in GO program 13467 (Kreidberg et al., 2015). Our scan rate, SAMP-SEQ, and NSAMP ere jointly optimized to provide high observing efficiency, a peak per-pixel count of ~35,000 to ensure rapid charge-trapping equilibriation within the first orbit, and the ability to separate the contaminating flux from the nearby M-dwarf companions at PA=250 while also not excessively limiting the ORIENT range of the observations. F126N was selected as a narrow band filter to avoid saturation while determining the wavelength solution. This filter was also previously successfully used in GO program 13467 (Kreidberg et al., 2015). Our scan rate, SAMP-SEQ, and NSAMP ere jointly optimized to provide high observing efficiency, a peak per-pixel count of ~35,000 to ensure rapid charge-trapping equilibriation within the first orbit, and the ability to separate the contaminating flux from the nearby M-dwarf companions at PA=250 while also not excessively limiting the ORIENT range of the observations. F126N was selected as a narrow band filter to avoid saturation while determining the wavelength solution. This filter was also previously successfully used in GO program 13467 (Kreidberg et al., 2015). Our scan rate, SAMP-SEQ, and NSAMP ere jointly optimized to provide high observing efficiency, a peak per-pixel count of ~35,000 to ensure rapid charge-trapping equilibriation within the first orbit, and the ability to separate the contaminating flux from the nearby M-dwarf companions at PA=250 while also not excessively limiting the ORIENT range of the observations.