0Assigned ID: 3341
----- Attempting Submission 1 (Fri Mar 25 17:09:46 GMT 2022) -----This target is not used in this proposal.
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ORBITAL VISIBILITY OVERRUNThis proposal exclusively uses WFC3/UVIS G280 and associated filters it therefore requires a number of "restricted" settings that have been modeled on previous sucessful proposals.
This has been updated for visits 24, 25, and 26 to increase exposure times and saturate the +1 to use the -1 order as the science spectrum
Target WASP-39b has been removed and two visits for this target have been removed so that there is not duplication with GO 17162
I have opened up the orient constraints for visit 10, 11, and 21 to help with schedualability. The phase constraints for visits 10 and 11 are correct to my calculations.
Added visit 25 in response to HOPR 92406 - repeat of visit 8 due to FGS failure
Toggled to AVAILABLE mode as is required for all observations in this program.
Added visit 26 in response to HOPR 92498 - repeat of visit 13 due to FGS failure
Added in "schedule after" 31 Dec 2023 constraints to visit 23 and 24 to allow for assessment of visit 22 set-up
Added visit 27 in response to HOPR 92540 - repeat of visit 7 due to FGS failure
Adjusted the exposure time and number of exposures for visits 23 and 24 (WASP-189) as discussed with the CS following more thorough calibration and understanding of the shutter speed uncertainty
Adjusted the Y POSTARG position for visit 11 (HAT-P-1b T2) to fully capture the companion star in the subarray.
Visit 10 observations chopped off the companion star meaning it cannot be used as a calibrator as intended.
This second observations will now include that star and will be used to assess the quality of the data and instrument.
In response to PCR 92865 we have removed visit 17 (8 orbits) and replaced it with visit 28 (4 orbits) and visit 29 (4 orbits).
Visit 28 is a duplication of visit 16 with minor changes to the YPOSTARG and SIZEAXIS1.
Visit 29 is a duplication of visit 19 with minor changes to the YPOSTARG and SIZEAXIS1 and SEIZAXIS2.-1711018358----- Attempting Submission 1 (Fri Jul 08 08:36:26 GMT 2022) -----
----- Attempting Submission 2 (Wed Sep 28 15:58:34 GMT 2022) -----
----- Attempting Submission 3 (Fri Oct 28 07:08:09 GMT 2022) -----
----- Attempting Submission 4 (Wed Nov 02 09:37:11 GMT 2022) -----
----- Attempting Submission 5 (Tue Jan 10 10:01:41 GMT 2023) -----
HST Phase II Proposal 17183 successfully submitted.
Receipt: # 17183-5
----- Attempting Submission 6 (Tue Jan 10 16:43:34 GMT 2023) -----
----- Attempting Submission 7 (Fri Apr 21 10:02:46 GMT 2023) -----
----- Attempting Submission 8 (Mon May 22 07:30:24 GMT 2023) -----
----- Attempting Submission 9 (Fri Dec 08 11:19:57 GMT 2023) -----
----- Attempting Submission 10 (Tue Jun 04 13:30:55 GMT 2024) -----
----- Attempting Submission 11 (Thu Jun 06 16:17:33 GMT 2024) -----
----- Attempting Submission 12 (Wed Jun 26 18:52:26 GMT 2024) -----In response to PCR 92865 we have removed visit 17 (8 orbits) and replaced it with visit 28 (4 orbits) and visit 29 (4 orbits).
Visit 28 is a duplication of visit 16 with minor changes to the YPOSTARG and SIZEAXIS1.
Visit 29 is a duplication of visit 19 with minor changes to the YPOSTARG and SIZEAXIS1 and SEIZAXIS2.
Errors in programs already completed are ignored. All upcoming observations are warning free.Hubble Ultraviolet-optical Survey of Transiting Legacy Exoplanets (HUSTLE) treasury programThe UV contains unique constraints on the atmospheric properties of a planet. Yet, the UV is an often overlooked wavelength region for exoplanet studies despite the wealth of information it contains on aerosol scattering properties and unknown absorbers. We propose to conduct a Hubble Ultraviolet-optical Survey of Transiting Legacy Exoplanets (HUSTLE) treasury program using the newly proven capabilities of the WFC3/UVIS G280 grism to produce a spectroscopic survey of 14 exoplanet atmospheres from 200-800nm. G280 has the highest throughput among all Hubble's UV instruments, making it an important instrument for the future of UV exoplanet science. This program targets giant planets from warm Neptunes to ultra hot Jupiters with equilibrium temperatures from 900-2600K, spanning a broad range of chemical, aerosol, and irradiation conditions.
This treasury program will expand Hubble's UV legacy for exoplanet studies, and in doing so, will address several important science questions: 1) place constraints on aerosol particle sizes, altitudes, and vertical mixing of clouds on the planetary limb, 2) identify and constrain the abundance of any Mid to Near-UV absorbers, and 3) leverage these directly measured properties to create legacy datasets to facilitate comparative studies, adding to our understanding of the mechanisms that sculpt these worlds.
Our target list includes a number of well known exoplanets that have formed the basis of our understanding of these extreme atmospheres and are already targets for Webb. The HUSTLE treasury program will provide the critical missing puzzle pieces to ensure that we can view the full picture of exoplanet atmospheres now and in the future.This program uses the WFC3-UVIS G280 grism to measure the transmission spectrum of 14 exoplanets. There are 26 visits in total with between one and four transits per targets to obtain the required SNR. Exposure times have been selected to maximize the number of exposures obtained per HST orbit increasing the overall SNR of the observations. Exposures range between filling 60 - 87% full well. The observations are accompanied by a 300X filter image for wavelength calibration, apart from for HAT-P-12 where we use the clear F200LP filter. Subarrays are used to reduce the overheads and buffer dumps are positioned during Earth occultation events. The target is centered on chip2 of the detector which has a more accurate calibration profile. Each observation is centered around a transit event such that baseling of the star is acquired before and after transit. The first orbit will not be impacted by additional systematics and will be used in the full analysis.
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.
Observational set-up is kept as consistant as possible to enable uniform analysis.
SIZEAXIS1=2100 and SIZEAXIS2=600 are used to minimize data volume (in some cases the Sizeaxis2 is reduced for the same reason), while CENTERAXIS2 is used to center the subarray readout on the target location. CENTERAXIS2 is set to 1208 and CENTERAXIS1 is set to 2148, to place the center of the subarray at the vertical center of chip 2. FLASH is required for a numeber of targets where exposure times are less than 220s and is set according to the required flux. All filter images require a FLASH of 16 to remove warnings. These parameters are based upon similar observations obtained successfully in proposal 16039 and 15288.The team consists of many experts in observations and theory, with specific expertise in exoplanet spectroscopy, UV absorption, and exoplanet modelling. The team has collectively contributed to many high impact papers in the field of exoplanet atmospheres. This broad team of experts has been assembled such that all aspects of this treasury program can be completed and delivered to the community.
Lili Alderson - observer, expert in data analysis and transmission spectroscopy
Dr. Natasha Batalha - theorist, expert on modelling exoplanet transmission spectra, and community software.
Dr. David Grant - observer, expert in data analysis and transit fitting
Prof. Nikole Lewis - observer and theorist, expert in data reduction and interpretation.
Prof. Mercedes Lopez-Morales - observer, expert in stellar monitoring and transmission spectroscopy
Dr Ryan MacDonald - theorist, expert in 1D and 3D modelling of exoplanet atmospheres
Dr. Mark S. Marley - theorist, expert in UV absorbers and giant planet atmospheres.
Dr. Sarah E. Moran - experimentalist and theorist, expert in laboratory generation of cloud particles.
Dr. Kazumasa Ohno - theorist, expert in scattering properties and haze formation.
Dr. Hannah Wakeford - observer and theorist, expert in HST data analysis and cloud physics.
The project will be managed by Dr. Hannah Wakeford.Exoplanets and Exoplanet Formation0falsetruetruefalsefalsefalseAVAILABLESTAREXTRA-SOLAR PLANETNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STAREXTRA-SOLAR PLANETNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STAREXTRA-SOLAR PLANETARY SYSTEMNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STAREXTRA-SOLAR PLANETNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STAREXTRA-SOLAR PLANETNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STAREXTRA-SOLAR PLANETARY SYSTEMNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STAREXTRA-SOLAR PLANETARY SYSTEMNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STAREXTRA-SOLAR PLANETThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STAREXTRA-SOLAR PLANETThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STAREXTRA-SOLAR PLANETARY SYSTEMNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STAREXTRA-SOLAR PLANETARY SYSTEMNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STAREXTRA-SOLAR PLANETThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STAREXTRA-SOLAR PLANETARY SYSTEMNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000WFC3/UVISSpectroscopicNoNoG280WFC3/UVISImagingNoNoF300XWFC3/UVISSpectroscopicNoNoG280WFC3/UVISImagingNoNoF300XWFC3/UVISSpectroscopicNoNoG280WFC3/UVISImagingNoNoF300XWFC3/UVISSpectroscopicNoNoG280WFC3/UVISImagingNoNoF300XWFC3/UVISSpectroscopicNoNoG280WFC3/UVISImagingNoNoF300XWFC3/UVISSpectroscopicNoNoG280WFC3/UVISImagingNoNoF300XWFC3/UVISSpectroscopicNoNoG280WFC3/UVISImagingNoNoF300XWFC3/UVISSpectroscopicNoNoG280WFC3/UVISImagingNoNoF300XWFC3/UVISSpectroscopicNoNoG280WFC3/UVISImagingNoNoF300XWFC3/UVISSpectroscopicNoNoG280WFC3/UVISImagingNoNoF300XWFC3/UVISSpectroscopicNoNoG280WFC3/UVISImagingNoNoF300XWFC3/UVISSpectroscopicNoNoG280WFC3/UVISImagingNoNoF300XWFC3/UVISSpectroscopicNoNoG280WFC3/UVISImagingNoNoF300XWFC3/UVISSpectroscopicNoNoG280WFC3/UVISImagingNoNoF300XThe scheduling data was generated by CASM 32.1.1.CASM was run in Phase II mode.SIZEAXIS2 set to maximize data volume.
Filter F200LP used to minimize time taken with F300X due to dimness of target.
Based on ETC calculations with Castelli-Kurucz Models K2V 4750 4.5 at V mag = 12.8
G280 time to saturation = 1317.13s
No known nearby sources to avoid
Centaxis paramters set based on previous program measurements (16039, 15838, 15288).
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G280 time to saturation = 446.39s
Orient contraints used to limit spectral overlap from one nearby source.
Centaxis paramters set based on previous program measurements (16039, 15838, 15288).
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NEW: We will expose for 2s to reach a peak of 65K e- in the +1 spectral trace. This new strategy was implemented following calibration tests to quantify the effect of jitter confirming that it should not dramatically impact the SNR.
No known nearby sources to avoid
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G280 time to saturation = 2.09s
OLD: For this bright target, we saturate the +1 order in 2.09 s which could potentially introduce jitter issues due to the shutter speed which has a photometric error of 0.004/integration. In order to mitigate for the shutter timing jitter, we will saturate the +1 order and use the -1 spectral order as our many science spectrum. The -1 order has a peak throughput approximately 5x lower than the +1 order (see Fig 8.3 in the WFC3 Handbook and Fig 1 of Wakeford et al. 2020). We therefore increase our exposure time to 9 s to reach 87% full well on the -1 spectral order.
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No known nearby sources to avoid
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