Orbit number missing (probably due to addition of this sub-exposure after previous Orbit Planner processing). To learn more about orbit numbers, please read the full error text in the Diagnostic Report.
Orbit number missing (probably due to addition of this sub-exposure after previous Orbit Planner processing). To learn more about orbit numbers, please read the full error text in the Diagnostic Report.Divided visits to avoid errors with number of exposures. Visits 1 and 2 must be scheduled consecutively to observe the exoplanet transit. Also visits 3,4 and 5 must be scheduled consecutively.
Widened the phase constraints for easier scheduling.
Scan parameters were adjusted.
Adjusted exposured for SAA avoidance following Januszewski's recommendations.
Adjusted again.-659655271----- Attempting Submission 1 (Thu Jul 29 18:55:03 GMT 2021) -----
HST Phase II Proposal 16695 successfully submitted.
Receipt: # 16695-1
----- Attempting Submission 2 (Thu Jul 29 20:40:41 GMT 2021) -----
----- Attempting Submission 3 (Fri Feb 10 15:47:09 GMT 2023) -----
----- Attempting Submission 4 (Thu Dec 07 20:59:52 GMT 2023) -----reduced number of iterationsCloudy mornings and clear afternoons: mapping atmospheric dynamics at the limbs of an exceptional hot SaturnTwo decades of modeling and observations have revealed hot Jupiter atmospheres to be incredibly dynamic worlds, with extreme circulation patterns, strong day-night temperature contrast, and complex cloud feedback processes. While much of our understanding of hot Jupiter atmospheres is derived from information-rich transmission spectroscopy with HST, such observations spatially blend the inhomogeneous atmosphere, introducing strong biases to the retrieved mean molecular weight, temperature, and molecular abundances. Spatial, vertical, and even temporal aerosol inhomogeneities compound these uncertainties, further complicating our interpretations of traditional, blended transmission spectra. Observations that can spatially resolve both the morning and evening terminators are therefore extremely valuable to illuminate a deeper, more holistic portrait of a hot Jupiter's atmosphere with less degeneracy. We propose to measure NUV-to-IR transmission spectra of both terminators of a highly exceptional target to measure each lim'bs aerosol properties, temperature, and chemical abundances in order to trace its dynamics. Our proposed observations will be sensitive to even subtle differences between the limbs, providing an entirely novel and unprecedented dataset which can be used to test models of atmospheric dynamics, aerosol formation, and radiative processes.We will measure the NUV-to-IR transmission spectra of both terminators of a highly exceptional target to measure each limbs aerosol properties, temperature, and chemical abundances in order to trace its dynamics. Our proposed observations will be sensitive to even subtle differences between the limbs, providing an entirely novel and unprecedented dataset which can be used to test models of atmospheric dynamics, aerosol formation, and radiative processes. During an exoplanet transit, the precise shape of the light curve during transit ingress and egress (T12 and T34, respectively) contains radius information of the two terminators, en- abling studies of limb-to-limb variations. In particular, sections T1-1.5 and T3.5-4 contain information about the leading terminator, and sections T1.5-2 and T3-3.5 capture the trailing terminator (see Fig. 1). This is because the change in flux during these phases of the light curve is dominated by the respective terminator entering or leaving the stellar limb.
The spirit of exoplanet transit/eclipse observations is to attempt to gather as many spectra as possible before, during, and after a transit event with each image as identical as possible. As a transit observation consists of measuring a differential drop in stellar flux during the event, identical exposures are resistant to uncertainties in flat-fielding and very high photometric precisions are achievable. The WFC3 UVIS and IR observations require 11 to 12 orbit visits, as the baseline stellar flux and instrument systematics need to be measured before and after the transit/eclipse event, with the transit/eclipse event taking about 2.5 orbits orbits and is phase constrained to occur mid-way through the visit.
We place phase constraints such that ingress and egress are fully observed, such that the limb differences can be seen.
We would like to work with the scheduler to find a set a of orbits that minimally impact the observation. In general SAA hiding can be used which does not impact the observations, or the SAA can occur during the latter half of certain orbits. In general, orbits 4 through 8 for G280 and 5 through 9 for G141 occur during the exoplanet transit and would idealy use SAA hiding or not have SAA ipact those orbits. The rest of the baseline orbits could have some SAA imact with minimal science loss. Similar long programs with visits of 9 to 20 orbits with minimal SAA impact have recently been observed (e.g. GO15255, GO15134).Zafar Rustamkulov is an expert in exoplanet atmosphere observations and data analysis.
Prof. David Sing has significant experience and expertise in the setup and reduction of HST/WFC3 observations. Prof. Sing is also an expert in exoplanet transit observations, leading many HST observing programs targeting transiting planets over the last 10 cycles. He has published 43 refereed papers over the last 12 years on HST-collected transiting exoplanet data. Prof. Sing has additional expertise in retrieval analyses of exoplanet atmosphere data.
Dr. Lothringer is an expert in both observing with HST, as well as atmosphere modeling and retrieval with PHOENIX. Dr. Lothringer has extensive experience studying the highly irradiated class of ultra-hot Jupiters and is PI and co-I of several HST programs.
Guangwei Fu is a graduate student at UMD working with Prof. Drake Deming on the observations of transiting exoplanets.
Sarah Moran is an expert in cloud and haze formation processes and forward modeling of their effect on transmission spectra.
Jessica Spake is an expert in WFC3 data reduction and in the interpretation of transit data.
Ryan MacDonald is an expert in atmospheric retrievals and theoretical modeling of exoplanet transmission spectra.
Kevin Stevenson is an expert in WFC3 data reduction and in the modeling of clouds in transiting exoplanets.
Lili Alderson is an expert in observational analysis and interpretation of exoplanet spectra.
Dr Wakeford is an expert in time series data analysis from Hubble, and the leader in UVIS G280 reduction for exoplanet spectroscopy. She is also an expert on exoplanet aerosols and their impact on measured exoplanet spectra.Exoplanets and Exoplanet Formation6falsefalsetruefalsefalsefalsefalsefalseAVAILABLESTARF3-F9This object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000WFC3/UVISSpectroscopicNoNoG280WFC3/IRSpectroscopicNoNoG141Timing link suitability includes constraints ([02 After 01 by 0.4 to 0.4 days])The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.Visits 1 and 2 must be observed consecutively.
The optional parameters SIZEAXIS1=1700 and SIZEAXIS2=170 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-67 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=1221, 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 target acq exposure.
To avoid any contamination by several dim, nearby stars, we have placed Orient Ranges for the observations to reach our science goals.169399510800096.11466286576888(Tic-Visit
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)false60For target acq, saturation in 3.5 seconds. 3.3 seconds gives SNR > 500.
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=1600 and SIZEAXIS2=170 are used to collect a wide acquisition image of the field, 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 16039 & 16086 but have been adjusted to better center the zeroth order spectrum on the sub-array.
We use FLASH=20 to meet the nominal count level.For target acq, saturation in 14 seconds. 12 seconds gives SNR of >500.
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=1600 and SIZEAXIS2=170 are used to minimize overheads, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of the G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 16039 & 16086 but have been adjusted to better center the zeroth order spectrum on the sub-array.
We use FLASH=20 to meet the nominal count level.We add a FLASH of 14, which when combined with the natural background of about 6 e- per exposure will result in 20 e- and better CTE.We add a FLASH of 14, which when combined with the natural background of about 6 e- per exposure will result in 20 e- and better CTE.We add a FLASH of 14, which when combined with the natural background of about 6 e- per exposure will result in 20 e- and better CTE.We add a FLASH of 14, which when combined with the natural background of about 6 e- per exposure will result in 20 e- and better CTE.We add a FLASH of 14, which when combined with the natural background of about 6 e- per exposure will result in 20 e- and better CTE.We add a FLASH of 14, which when combined with the natural background of about 6 e- per exposure will result in 20 e- and better CTE.Timing link suitability includes constraints ([02 After 01 by 0.4 to 0.4 days])The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.169402930900096.11466286576888(Tic-Visit
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)false50We add a FLASH of 14, which when combined with the natural background of about 6 e- per exposure will result in 20 e- and better CTE.We add a FLASH of 14, which when combined with the natural background of about 6 e- per exposure will result in 20 e- and better CTE.We add a FLASH of 14, which when combined with the natural background of about 6 e- per exposure will result in 20 e- and better CTE.We add a FLASH of 14, which when combined with the natural background of about 6 e- per exposure will result in 20 e- and better CTE.We add a FLASH of 14, which when combined with the natural background of about 6 e- per exposure will result in 20 e- and better CTE.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.Timing link suitability includes constraints ([04 After 03 by 0.3 to 0.3 days])Hst Same orient constraint links visits (03 04 05)The scheduling data was generated by CASM 31.1.CASM was run in Phase II mode./private/var/folders/cv/0p6mxhdj5r95k60smwh6_qpw0000gp/T/OPVisit15198242454697651411.xmlRoll constraints have been added to avoid a nearby red companion star located 9.7" north east of the target (visible in a SDSS image).
Visits 3, 4 and 5 must be observed consecutively.(Tic-Visit
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