0 Assigned ID: 897 ----- Attempting Submission 1 (Fri Apr 07 21:12:53 GMT 2017) ----- HST Phase I Proposal 897 (NUVWFC3.pdf.apt) successfully submitted. Receipt: # 897-1 ----- Attempting Submission 2 (Fri Apr 07 22:34:13 GMT 2017) ----- Hannah Wakeford (13/09/2017) The phase constraints have been expanded from 0.93-0.934 out to 0.93-0.942. We have additionally expanded the orient constraints by 1' in each direction. These should increase the schedualability of this program. 643045320 ----- Attempting Submission 1 (Thu Jul 20 15:01:18 GMT 2017) ----- ----- Attempting Submission 2 (Wed Sep 13 09:12:59 GMT 2017) ----- Progress on addressing two important exoplanet science topics can be made in the near-UV, where transit spectroscopy can measure aerosol scattering from the lower atmosphere, while large atmospheric escape signatures can be detectable in narrow-bands centred around strong Mg and Fe lines. WFC3/UVIS has never been used nor verified for high photometric precision transit observations, though it has the highest throughput among all HST near-UV instruments, making it an important instrument to develop for UV exoplanet science. This program targets the ultra-hot Jupiter HAT-P-41b to measure both the broadband near-UV transmission spectra, and the narrowband escaping atmosphere signatures of Mg. Recent WFC3/IR observations show strong evidence for aerosol haze in HAT-P-41b covering a near-IR H2O feature, making it an ideal target to study near-UV aerosol properties at high altitude. By measuring how high in the atmosphere near-UV scattering signatures can be seen, important constraints can be made on both cloud aerosol sizes and atmospheric vertical mixing rates; both critical parameters needed to explain how exoplanet clouds are suspended to high altitudes. In addition, the strong estimated atmospheric escape rates in HAT-P-41b also make it an ideal target to detect hydrodynamical escape signatures of Mg. Our pilot program will demonstrate the exoplanet capabilities of WFC3/UVIS, expanding Hubble's unique UV access with a potential to probe hundreds of exoplanets. We will use the WFC3 G280 grism to obtain spectra covering 2004 to 4000 Ang (the grim spectra longwords of 4000 Ang contains overlapping spectral orders and will not be used for our primary science objectives). We have estimated the exposure times using the STScI ETC, and will adopt 190 second exposures, which exposes the detector to 2/3 well- depth, resulting in a signal-to-noise per spectra of 300 to 500. As buffer dumps are an important issue with UVIS, we will use sub-arrays to increase duty cycle. Sub-array sizes of 800x2100 limits the overheads between exposures, and contains the entire useable spectra. Using APT, we find 11 exposures-per-orbit can be obtained, and will require 5-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. 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 at the vertical center of chip 2. These parameters are based upon similar observations obtained successfully in proposal 13574. Planets and Planet Formation 0 false true false true false false SUPPORTED STAR EXTRA-SOLAR PLANETARY SYSTEM F3-F9 NO This object was generated by the targetselector and retrieved from the SIMBAD database. TYC-488-2442-1 J2000 J2000 WFC3/UVIS Spectroscopic No No G280 WFC3/UVIS Spectroscopic No No G280 1505293570998 /private/var/folders/y6/nvwqsbrx725gvkz0vjsxcpwr07g5lt/T/OPVisit5866614371315131449.xml The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. Exposures of HAT-P-41 with F300X, and G280. The two visits consist of 5 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 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=2100 and SIZEAXIS2=800 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 HAT-P-41 will occupy only a narrow swath of pixel rows within the field. This also requires the use of optional parameter CENTERAXIS2 in order to "steer" the location of the subarray readout so that it is centered on the target location. 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 CENTERAXIS2=1026, which puts the vertical center of the subarray at the vertical center of chip 2. 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 observatoins to reach the science and technology test goals stated. (Tic-Visit :proposal-id 15288 :visit-id "01" :proposal-version -1 :trans-version "20170613" :date "13-Sep-2017 10:06:08.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 1588848 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15288 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15288 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2806 :al-overhead-at-end 74 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3202 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15288 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2978 :al-overhead-at-end 74 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3202 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15288 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2978 :al-overhead-at-end 74 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3202 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15288 :visit-id "01" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2978 :al-overhead-at-end 74 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3202 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15288 :visit-id "01" :orbit-number 5 :pcs-time 222 :si-vis-utilization 2978 :al-overhead-at-end 74 :internal-dur-at-end 751 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3202 :pcs-gap 0 ) true 5 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=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. 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. 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. 1505293733681 The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. /private/var/folders/y6/nvwqsbrx725gvkz0vjsxcpwr07g5lt/T/OPVisit7823598015029382344.xml Exposures of HAT-P-41 with F300X, and G280. The two visits consist of 5 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 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=2100 and SIZEAXIS2=800 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 HAT-P-41 will occupy only a narrow swath of pixel rows within the field. This also requires the use of optional parameter CENTERAXIS2 in order to "steer" the location of the subarray readout so that it is centered on the target location. 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 CENTERAXIS2=1026, which puts the vertical center of the subarray at the vertical center of chip 2. 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 observatoins to reach the science and technology test goals stated. (Tic-Visit :proposal-id 15288 :visit-id "02" :proposal-version -1 :trans-version "20170613" :date "13-Sep-2017 10:08:52.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 1588848 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15288 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15288 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2806 :al-overhead-at-end 74 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3202 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15288 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2978 :al-overhead-at-end 74 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3202 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15288 :visit-id "02" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2978 :al-overhead-at-end 74 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3202 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15288 :visit-id "02" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2978 :al-overhead-at-end 74 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3202 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15288 :visit-id "02" :orbit-number 5 :pcs-time 222 :si-vis-utilization 2978 :al-overhead-at-end 74 :internal-dur-at-end 751 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3202 :pcs-gap 0 ) true 5 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=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. 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. 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.