How hot is the inside of a young planet?

0 Assigned ID: 999 ----- Attempting Submission 1 (Fri Apr 05 23:52:37 GMT 2019) ----- HST Phase I Proposal 999 (phase1-GO_v1FINAL2apt.pdf.apt) successfully submitted. Receipt: # 999-1 ----- Attempting Submission 2 (Fri Apr 05 23:58:46 GMT 2019) ----- HST Phase I Proposal 999 (phase1-GO_v1FINAL2apt.pdf.apt) successfully submitted. Receipt: # 999-2 ----- Attempting Submission 3 (Sat Apr 06 00:00:41 GMT 2019) ----- HST Phase I Proposal 999 (phase1-GO_v1FINAL2apt.pdf.apt) successfully submitted. Receipt: # 999-3 ----- Attempting Submission 4 (Sat Apr 06 00:05:43 GMT 2019) ----- HST Phase I Proposal 999 (phase1-GO_v1FINAL2apt.pdf.apt) successfully submitted. Receipt: # 999-4 ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN 0 ----- Attempting Submission 1 (Thu Jul 25 03:42:35 GMT 2019) ----- ----- Attempting Submission 2 (Fri Apr 08 22:17:39 GMT 2022) ----- Visits 1-3 are complete How hot is the inside of a young planet? We propose to test the following hypothesis: the gas-giant exoplanet WASP-107b is unusually inflated, and methane-depleted, because it is young, and therefore has a high internal temperature. If this is correct, the temperature throughout its atmosphere should be high enough for sodium and potassium to be in the gas phase, and show absorption signatures in WASP-107b's transmission spectrum. We therefore propose to use measurements of sodium and potassium as thermometers of WASP-107b's internal temperature. Our proposed observations will also tell us whether or not a low C/O ratio is required to explain the methane depletion previously observed for WASP-107b. This is useful because C/O ratios can tell us where planets form in their protoplanetary disks. WASP-107b is an outstanding target for atmospheric characterisation, which, combined with its apparent youth, makes it an ideal exoplanet for linking planet formation and evolution theories to observations of its present-day atmosphere. This kind of atmospheric archaeology has so far been difficult for individual planets. HST is the only telescope that can achieve the required precision and wavelength coverage to achieve our science goals. We will use the WFC3 G280 grism to obtain spectra covering 2004 to 10000 Ang. We have estimated the exposure times using the STScI ETC, and will adopt 231 second exposures, which exposes the detector to 2/3 well- depth, resulting in a signal-to-noise per spectra of 4 to 500. As buffer dumps are an important issue with UVIS, we will use sub-arrays to increase duty cycle. Sub-array sizes of 500x1500 limits the overheads between exposures, and contains the entire useable spectrum. Using APT, we found 10 exposures-per-orbit can be obtained, and we will require 4-orbit long visits to measure both the transit and have sufficient baseline flux out of transit to characterize potential detector 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 chip 2, at an approximate XY position of (2048,1024). SIZEAXIS1=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the target spectrum, which will be displaced from the direct image of the target by approximately +100 in X and +175 in Y. Therefore we set CENTERAXIS1 = 2048+100 = 2148 and CENTERAXIS2 = 1024 + 176 = 1200. These parameters are based upon similar observations obtained successfully in proposals 13574 and 15288. Our team has successfully analysed the first exoplanet transmission spectrum using WFC3/UVIS, and has extensive experience in reducing HST/WFC3 infrared and HST/STIS optical transit spectra (e.g. Nikolov et al. 2015, Sing et al. 2016, Spake et al 2018); in both detailed forward modelling and retrieval analysis (e.g. Sing et al 2016; in interpreting cloud/haze chemistry (e.g. Wakeford et al. 2015; 2017). Co-Is Spake, Sing, Wakeford, Nikolov, Evans and Ballester are experts in the analysis of transiting exoplanet data, covering wavelengths from the UV to the near-infrared. Co-I Goyal is an expert in the modelling of exoplanet atmospheres. Co-I Rackham is an expert in correcting exoplanet transmission spectra for the effects of stellar activity. Co-I Thorngren is an expert in the modelling of exoplanet interiors. Planets and Planet Formation 6 false false true false false false false AVAILABLE STAR EXTRA-SOLAR PLANETARY SYSTEM K V-IV This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 WFC3/UVIS Spectroscopic No No G280 1564026138702 The scheduling data was generated by CASM 27.2. CASM was run in Phase II mode. Exposures of WASP-107 with F300X, and G280. The four visits consist of four orbits each with repeated exopsures on the same target and in the same position for each orbit. The first orbit of each visit contains the F300X direct image for wavelength calibration. Field positions are set to the reccommended position near the center of the second CCD chip (chip 2). As the only aperture allowed to be used with the G280 is the "UVIS", we must use POSTARGS to move the target to the chip center position. The nominal "UVIS" aperture puts the target 10" above the chip gap on chip 1. A Y-POSTARG of about 30" will put the target near the center of chip 1 and a Y-postarg of about -50" will put it near the center of chip 2 with a pixel position of (2048, 1026). The optional parameters SIZEAXIS1=1500 and SIZEAXIS2=500 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 of WASP-107b 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=2148 and CENTERAXIS2=1200, which puts 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. As this target has a number of potential contamination sources we have placed Orient Ranges for the observations to reach our science goals. 1591108306000 109.92991212202878 (Tic-Visit :proposal-id 15838 :visit-id "01" :proposal-version -1 :trans-version "20190514" :date "24-Jul-2019 23:42:17.0" :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 548432 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15838 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15838 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2656 :al-overhead-at-end 46 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3149 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15838 :visit-id "01" :orbit-number 2 :pcs-time 302 :si-vis-utilization 2840 :al-overhead-at-end 46 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3149 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15838 :visit-id "01" :orbit-number 3 :pcs-time 302 :si-vis-utilization 2840 :al-overhead-at-end 46 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3149 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15838 :visit-id "01" :orbit-number 4 :pcs-time 302 :si-vis-utilization 2840 :al-overhead-at-end 46 :internal-dur-at-end 895 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3149 :pcs-gap 0 ) false 4 0 The 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, at an approximate XY position of (2048,1024). SIZEAXIS1=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the target spectrum, which will be displaced from the direct image of the target. The zeroth order is expected to be about 175 pixels above the target in Y, and about 100 pixels to the right of the target in X. Therefore we set CENTERAXIS1 = 2048+100 = 2148 and CENTERAXIS2 = 1024 + 176 = 1200. We set the AMP to D as in previously-sucessful campaigns. We use FLASH=12 to meet the nominal count level. These parameters are based upon similar observations obtained successfully in proposal 13574. 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=2100 and SIZEAXIS2=800 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). We set the AMP to D as in previous-sucessful campaigns. These parameters are based upon similar observations obtained successfully in proposal 13574. 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=2100 and SIZEAXIS2=800 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). We set the AMP to D as in previous-sucessful campaigns. These parameters are based upon similar observations obtained successfully in proposal 13574. 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=2100 and SIZEAXIS2=800 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). We set the AMP to D as in previous-sucessful campaigns. These parameters are based upon similar observations obtained successfully in proposal 13574. 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=2100 and SIZEAXIS2=800 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). We set the AMP to D as in previous-sucessful campaigns. These parameters are based upon similar observations obtained successfully in proposal 13574. We set up the bias frames based on previously sucessful program 11934 and are using the same Aperture and subarray size and position as the observations for direct calibration. 1564026142426 The scheduling data was generated by CASM 27.2. CASM was run in Phase II mode. Exposures of WASP-107 with F300X, and G280. The four visits consist of four orbits each with repeated exopsures on the same target and in the same position for each orbit. The first orbit of each visit contains the F300X direct image for wavelength calibration. Field positions are set to the reccommended position near the center of the second CCD chip (chip 2). As the only aperture allowed to be used with the G280 is the "UVIS", we must use POSTARGS to move the target to the chip center position. The nominal "UVIS" aperture puts the target 10" above the chip gap on chip 1. A Y-POSTARG of about 30" will put the target near the center of chip 1 and a Y-postarg of about -50" will put it near the center of chip 2 with a pixel position of (2048, 1026). The optional parameters SIZEAXIS1=1500 and SIZEAXIS2=500 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 of WASP-107b 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=2148 and CENTERAXIS2=1200, which puts 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. As this target has a number of potential contamination sources we have placed Orient Ranges for the observations to reach our science goals. 1587647733000 102.0 (Tic-Visit :proposal-id 15838 :visit-id "02" :proposal-version -1 :trans-version "20190514" :date "24-Jul-2019 23:42:21.0" :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 548432 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15838 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15838 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2656 :al-overhead-at-end 46 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3149 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15838 :visit-id "02" :orbit-number 2 :pcs-time 302 :si-vis-utilization 2840 :al-overhead-at-end 46 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3149 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15838 :visit-id "02" :orbit-number 3 :pcs-time 302 :si-vis-utilization 2840 :al-overhead-at-end 46 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3149 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15838 :visit-id "02" :orbit-number 4 :pcs-time 302 :si-vis-utilization 2840 :al-overhead-at-end 46 :internal-dur-at-end 895 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3149 :pcs-gap 0 ) false 4 0 The 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, at an approximate XY position of (2048,1024). SIZEAXIS1=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the target spectrum, which will be displaced from the direct image of the target. The zeroth order is expected to be about 175 pixels above the target in Y, and about 100 pixels to the right of the target in X. Therefore we set CENTERAXIS1 = 2048+100 = 2148 and CENTERAXIS2 = 1024 + 176 = 1200. We set the AMP to D as in previously-sucessful campaigns. We use FLASH=12 to meet the nominal count level. These parameters are based upon similar observations obtained successfully in proposal 13574. 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=2100 and SIZEAXIS2=800 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). We set the AMP to D as in previous-sucessful campaigns. These parameters are based upon similar observations obtained successfully in proposal 13574. 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=2100 and SIZEAXIS2=800 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). We set the AMP to D as in previous-sucessful campaigns. These parameters are based upon similar observations obtained successfully in proposal 13574. 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=2100 and SIZEAXIS2=800 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). We set the AMP to D as in previous-sucessful campaigns. These parameters are based upon similar observations obtained successfully in proposal 13574. 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=2100 and SIZEAXIS2=800 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). We set the AMP to D as in previous-sucessful campaigns. These parameters are based upon similar observations obtained successfully in proposal 13574. We set up the bias frames based on previously sucessful program 11934 and are using the same Aperture and subarray size and position as the observations for direct calibration. 1649451608368 The scheduling data was generated by CASM 29.0. CASM was run in Phase II mode. /private/var/folders/cw/rz8llv897sdg_p02ht5h6t2w0000gr/T/OPVisit18103533550264748984.xml Exposures of WASP-107 with F300X, and G280. The four visits consist of four orbits each with repeated exopsures on the same target and in the same position for each orbit. The first orbit of each visit contains the F300X direct image for wavelength calibration. Field positions are set to the reccommended position near the center of the second CCD chip (chip 2). As the only aperture allowed to be used with the G280 is the "UVIS", we must use POSTARGS to move the target to the chip center position. The nominal "UVIS" aperture puts the target 10" above the chip gap on chip 1. A Y-POSTARG of about 30" will put the target near the center of chip 1 and a Y-postarg of about -50" will put it near the center of chip 2 with a pixel position of (2048, 1026). The optional parameters SIZEAXIS1=1500 and SIZEAXIS2=500 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 of WASP-107b 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=2148 and CENTERAXIS2=1200, which puts 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. As this target has a number of potential contamination sources we have placed Orient Ranges for the observations to reach our science goals. 1619779669000 102.34111406449739 (Tic-Visit :proposal-id 15838 :visit-id "03" :proposal-version -1 :trans-version "20200619" :date "08-Apr-2022 14:00:05.0" :trans-errors '(:WARNINGS 3 :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 548432 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15838 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15838 :visit-id "03" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2656 :al-overhead-at-end 46 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3149 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15838 :visit-id "03" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2840 :al-overhead-at-end 46 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3149 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15838 :visit-id "03" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2840 :al-overhead-at-end 46 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3149 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15838 :visit-id "03" :orbit-number 4 :pcs-time 392 :si-vis-utilization 2840 :al-overhead-at-end 46 :internal-dur-at-end 895 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3149 :pcs-gap 0 ) true 4 3 The 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, at an approximate XY position of (2048,1024). SIZEAXIS1=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the target spectrum, which will be displaced from the direct image of the target. The zeroth order is expected to be about 175 pixels above the target in Y, and about 100 pixels to the right of the target in X. Therefore we set CENTERAXIS1 = 2048+100 = 2148 and CENTERAXIS2 = 1024 + 176 = 1200. We set the AMP to D as in previously-sucessful campaigns. We use FLASH=12 to meet the nominal count level. These parameters are based upon similar observations obtained successfully in proposal 13574. 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=2100 and SIZEAXIS2=800 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). We set the AMP to D as in previous-sucessful campaigns. These parameters are based upon similar observations obtained successfully in proposal 13574. 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=2100 and SIZEAXIS2=800 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). We set the AMP to D as in previous-sucessful campaigns. These parameters are based upon similar observations obtained successfully in proposal 13574. 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=2100 and SIZEAXIS2=800 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). We set the AMP to D as in previous-sucessful campaigns. These parameters are based upon similar observations obtained successfully in proposal 13574. 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=2100 and SIZEAXIS2=800 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). We set the AMP to D as in previous-sucessful campaigns. These parameters are based upon similar observations obtained successfully in proposal 13574. We set up the bias frames based on previously sucessful program 11934 and are using the same Aperture and subarray size and position as the observations for direct calibration. 1649451772479 The scheduling data was generated by CASM 29.0. CASM was run in Phase II mode. /private/var/folders/cw/rz8llv897sdg_p02ht5h6t2w0000gr/T/OPVisit2051502818125518679.xml Exposures of WASP-107 with F300X, and G280. The four visits consist of four orbits each with repeated exopsures on the same target and in the same position for each orbit. The first orbit of each visit contains the F300X direct image for wavelength calibration. Field positions are set to the reccommended position near the center of the second CCD chip (chip 2). As the only aperture allowed to be used with the G280 is the "UVIS", we must use POSTARGS to move the target to the chip center position. The nominal "UVIS" aperture puts the target 10" above the chip gap on chip 1. A Y-POSTARG of about 30" will put the target near the center of chip 1 and a Y-postarg of about -50" will put it near the center of chip 2 with a pixel position of (2048, 1026). The optional parameters SIZEAXIS1=1500 and SIZEAXIS2=500 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 of WASP-107b 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=2148 and CENTERAXIS2=1200, which puts 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. As this target has a number of potential contamination sources we have placed Orient Ranges for the observations to reach our science goals. (Tic-Visit :proposal-id 15838 :visit-id "04" :proposal-version -1 :trans-version "20200619" :date "08-Apr-2022 14:02:51.0" :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 548432 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15838 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15838 :visit-id "04" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2575 :al-overhead-at-end 46 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3149 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15838 :visit-id "04" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2750 :al-overhead-at-end 46 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3149 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15838 :visit-id "04" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2750 :al-overhead-at-end 46 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3149 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15838 :visit-id "04" :orbit-number 4 :pcs-time 392 :si-vis-utilization 2750 :al-overhead-at-end 46 :internal-dur-at-end 895 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3149 :pcs-gap 0 ) true 4 0 The 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, at an approximate XY position of (2048,1024). SIZEAXIS1=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the target spectrum, which will be displaced from the direct image of the target. The zeroth order is expected to be about 175 pixels above the target in Y, and about 100 pixels to the right of the target in X. Therefore we set CENTERAXIS1 = 2048+100 = 2148 and CENTERAXIS2 = 1024 + 176 = 1200. We set the AMP to D as in previously-sucessful campaigns. We use FLASH=12 to meet the nominal count level. These parameters are based upon similar observations obtained successfully in proposal 13574. 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=2100 and SIZEAXIS2=800 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). We set the AMP to D as in previous-sucessful campaigns. These parameters are based upon similar observations obtained successfully in proposal 13574. 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=2100 and SIZEAXIS2=800 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). We set the AMP to D as in previous-sucessful campaigns. These parameters are based upon similar observations obtained successfully in proposal 13574. 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=2100 and SIZEAXIS2=800 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). We set the AMP to D as in previous-sucessful campaigns. These parameters are based upon similar observations obtained successfully in proposal 13574. 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=2100 and SIZEAXIS2=800 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). We set the AMP to D as in previous-sucessful campaigns. These parameters are based upon similar observations obtained successfully in proposal 13574. We set up the bias frames based on previously sucessful program 11934 and are using the same Aperture and subarray size and position as the observations for direct calibration.