0Assigned ID: 3859
----- Attempting Submission 1 (Fri Oct 21 22:58:50 GMT 2022) -----
HST Phase I Proposal 3859 successfully submitted.
Receipt: # 3859-1
----- Attempting Submission 2 (Fri Oct 21 23:02:08 GMT 2022) -----
HST Phase I Proposal 3859 successfully submitted.
Receipt: # 3859-2Updated the submission based on advice from instrument scientists:
- changed WFC3 visits to 3x (1xF275W, 1xF280N, 2x225W). Exposures times changed from 600s to 590s to allow scheduling with the increased overhead.
- ACS exposure times increased from 1200s to 1300s to fill orbit.
- Dither added bettwen ACS exposures by adding a POSTARG of 1 arcsecond.
- Minimuim gap between visits increased to 7 days to ensure better coverage of the visibility window.
- Updated program description with above.-1528657598----- Attempting Submission 1 (Wed Dec 28 12:43:01 GMT 2022) -----
----- Attempting Submission 2 (Thu Feb 09 21:47:20 GMT 2023) -----Ultraviolet Photometry of TRAPPIST-1 during the next JWST Observing WindowWith the successful launch of JWST, the atmospheres of rocky exoplanets are finally within reach. The exemplary host star is TRAPPIST-1, orbited by seven Earth-sized planets. Here we seek to obtain time-series ultraviolet photometry of TRAPPIST-1 during the next JWST observing window, providing vital information for interpreting ongoing JWST transit and eclipse spectroscopy.
The TRAPPIST-1 planets experience a radically different ultraviolet flux than the Earth, changing photochemical reaction rates of key molecules and biomarkers such as ozone. Detailed knowledge of the stellar ultraviolet SED is required to correctly interpret upcoming JWST spectroscopy to characterize the atmospheres and potential habitability of the planets. A large investment of HST spectroscopy time into TRAPPIST-1 has returned only low signal detections of a few stellar emission lines, and essentially no constraints on the ultraviolet variability. Here, we will use ultraviolet photometry, which provides high-quality data in multiple bands with much less HST time.
We will observe TRAPPIST-1 three times in five ultraviolet bands. In the NUV, we will characterize the as-yet unconstrained continuum flux that is a key driver of atmospheric chemistry, and measure the 2800A Mg II lines to diagnose the chromospheric structure. In the FUV, we will observe the C IV 1550A doublet to estimate the strength of the total FUV flux. These observations will provide a contemporaneous ultraviolet dataset for each JWST observation and the first constraints on the ultraviolet variability of TRAPPIST-1. Photometric measurements from the observations will be made available as a MAST High Level Science Product.The aim is to obtain ultraviolet photometry of TRAPPIST-1 during the next window where both JWST and HST can observe TRAPPIST-1. The expected return is a single flux meaurement in each filter per visit, not an in-visit light curve.
Three two-vist blocks are requested. The two visits in each block should be scheduled on the same day, ideally one right after the other. The three blocks should be spread across the June 1st - July 23rd window as evenly as possible (I've separated them by a nominal 7 days in the phase two but ideally this should be longer).
If scheduling allows, timing one or more of the visits to be simultaneous with a JWST observation of TRAPPIST-1 would provide enhanced science, but is not a requirement.
Each two-visit block consists of one visit with WFC3-UVIS and one with ACS-SBC.
The WFC visits contain three orbits, each with 2x F225W exposure, 1x F275W exposure and 1x F280N exposure. The W filters probe the NUV continuum and the N filter measures the strength of the Mg II 2800A lines. We expect the F275W and F280N observations to return S/N 10-20 per visit. The expected F225W flux is basically unconstrained and its measurement (or an upper limit) will be a key result of this program.
The ACS visits contain one orbit each of the F150LP and F165LP filters. When subtracted, these will measure the strength of the C IV 1550A lines. We predict S/N 10-20 in each filter, although this is somewhat uncertain due to the low quality of existing COS spectra.David Wilson is a PI of three previous HST programs (13719, 15189, 16449) obtaining ultraviolet spectroscopy of stars using both COS and STIS, and has published multiple first-author papers based on HST data. He has extensive experience with the HST calibration tools to perform the non-standard reductions necessary for studying late-type stars, and has completed bright-object protection checks for multiple programs. Dr Wilson is an expert on the ultraviolet SED of TRAPPIST-1, having constructed and published the Mega-MUSCLES SED of TRAPPIST-1 (Wilson et al. 2021a). He also led the production of the Mega-MUSCLES High Level Science Products and will apply that expertise to the HLSP proposed here.
Dr. Froning is the PI of the HST Mega-MUSCLES Treasury Survey, a large program using HST, Chandra, XMM, Swift, and several ground-based telescopes to obtain pan-chromatic spectroscopy of a broad survey of M stars to evaluate their high energy irradiance environment, exoplanet atmospheric parameters and biomarker production, and the potential for habitability. Dr. Froning is an experienced observer and instrument developer with expertise in stellar astrophysics and the design and development of UV/OIR imagers and spectrographs for ground and space facilities. She was the Project Scientist for the Cosmic Origins Spectrograph and is the lead or co-author on over 20 papers using HST UV spectroscopic observations.
Kevin France is the PI of the HST MUSCLES Treasury Survey (GO13650) and MEATS (GO16166) Survey to
study the spectral and temporal properties of exoplanet host stars (France et al. 2016, 2018, 2020; Loyd et al. 2016; Youngblood et al. 2016). He is the co-PI of the follow-on Mega-MUSCLES (GO15071) and Mega-MEATS (16701) Surveys that focused on activity in stars optimal for planetary characterization with JWST. He was a member of the COS instrument and science teams; he is intimately familiar with HST-COS and -STIS
instrument, data, and analysis procedures. His research group has developed numerous community tools for
spectral and temporal analysis of COS and STIS data. Dr France has authored over 70 refereed publications on
exoplanets, cool stars, and planet-forming disks using UV spectra from HST.
CoI Youngblood is the PI of multiple HST STIS programs to study the UV emission from M dwarfs. She is a member of the MUSCLES and Mega-MUSCLES teams, including program 16701 obtaining ultraviolet spectroscopy of JWST planet target hosts.
Peter Wheatley is the PI of three previous HST programs (12920, 14906, 16487), including STIS observations of TRAPPIST-1. He has particular expertise in characterising the X-ray irradiation of exoplanet atmospheres, including for TRAPPIST-1, which is key to understanding atmospheric escape and survival (e.g. Wheatley et al. 2017).Exoplanets and Exoplanet FormationStellar Physics and Stellar Types0falsefalsetruefalsefalsetruefalseSUPPORTEDEXT-STARLATE-TYPE DEGENERATEJ2000J2000WFC3/UVISImagingNoNoF280NWFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF225WACS/SBCImagingNoNoF150LPACS/SBCImagingNoNoF165LPWFC3/UVISImagingNoNoF280NWFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF225WACS/SBCImagingNoNoF150LPACS/SBCImagingNoNoF165LPWFC3/UVISImagingNoNoF280NWFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF225WACS/SBCImagingNoNoF150LPACS/SBCImagingNoNoF165LP/tmp/OPVisit16951933245829974010.xmlTiming link suitability includes constraints ([02 After 01 by at most 1.0 days])The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.(Tic-Visit
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