0Assigned ID: 260
----- Attempting Submission 1 (Thu Mar 05 17:58:04 GMT 2020) -----
HST Phase I Proposal 260 successfully submitted.
Receipt: # 260-1This target is not used in this proposal.
This target is not used in this proposal.Please contact Kevin France (410-340-8651, kevin.france@colorado.edu) with questions/corrections.
This version updates visits 03 and 04 with new offset target for TA.
Submitted Feb 09 2022-349161760----- Attempting Submission 1 (Wed Jun 24 21:43:30 GMT 2020) -----
----- Attempting Submission 2 (Thu Oct 15 21:57:35 GMT 2020) -----
----- Attempting Submission 3 (Fri Oct 16 22:55:22 GMT 2020) -----
----- Attempting Submission 4 (Fri Dec 04 03:48:02 GMT 2020) -----
----- Attempting Submission 5 (Sat Feb 06 22:35:08 GMT 2021) -----
----- Attempting Submission 6 (Wed Feb 24 21:08:08 GMT 2021) -----
HST Phase II Proposal 16166 successfully submitted.
Receipt: # 16166-6
----- Attempting Submission 7 (Thu Feb 25 18:03:46 GMT 2021) -----
----- Attempting Submission 8 (Tue Apr 13 16:37:50 GMT 2021) -----
----- Attempting Submission 9 (Wed Feb 09 19:18:53 GMT 2022) -----MUSCLES Extension for Atmospheric Transmission Spectroscopy: Essential Ultraviolet Stellar Characterization for Guaranteed JWST Transiting Planet TargetsJWST will launch during HST cycle 28 and begin an unprecedented era in atmospheric characterization for all types of exoplanets. Atmospheric spectroscopy of warm rocky planets, sub-Neptune, and Jupiter-mass planets will be obtained through a robust set of guaranteed transiting planet observations (the JWST ERS and GTO programs). To accurately model and interpret observations of these planets' atmospheres, we must understand the high-energy SED of their host stars: FUV and NUV-driven photochemistry shapes an atmosphere's molecular abundances and the formation of hazes, EUV irradiation can erode a planet's gaseous envelope, and flares can affect long term stability.
A number of recent surveys have used HST's UV capabilities to characterize the energetic irradiance spectra across a range of stellar masses, ages, and activity levels. While these surveys have proven invaluable for predicting photochemical tracers and evolution of an exoplanet's atmosphere, they have also shown scatter in behavior and irradiance properties for stars of similar type. As a result, direct UV observations remain the gold standard for understanding the effects of the stellar irradiance on a specific exoplanet. We propose to obtain temporally-resolved UV (1150-3200 Ang) stellar spectroscopy of the 13 JWST guaranteed time targets with no UV characterization data in the HST archive. Our proposed observations will provide the UV context necessary to determine the likelihood of atmospheric formation and retention, the identification and interpretation of atmospheric chemistry, and the impacts of stellar activity on the exoplanet atmospheric stability.A complete census of the UV emission incident on the exoplanets ideally comprises spectral coverage from 1150-3100 A, plus X-ray observations to allow a complete estimation of the unobservable EUV component (100 - 911A). To obtain ecient observations of the 13 targets, we will rely on STIS G140L and G230L to cover the FUV and NUV at moderate spectral resolution (R 500-1000). FUV emission (1150A - 1700 A) from Ly and other strong chromospheric lines (CII, SiIII, SiIV, CIV, etc.) are particularly
interesting because these lines provide constraints on the Lyman continuum/EUV (100 - 900 A) irradiance in these systems (Linsky et al. 2014). At NUV wavelengths, we will use STIS G230L (1800 A - 3100 A) to cover the NUV continuum, Fe II 2400 and 2600, and Mg II 2800) HST is the only active observing facility with a spectroscopic capability at FUV and NUV wavelengths and is required for the proposed program.
For targets that are suciently bright, we will also observe using G140M with the 5200 0:200 slit to measure the Ly prole for our targets (the 0.200 slit is chosen to maximize throughput and mitigate pointing drift). Ly experiences absorption from the intervening
local ISM and the line must be reconstructed to provide a reliable measure of the local Ly-alpha field that dominates the FUV radiation eld from cool stars (France et al. 2012). Medium-resolution (R ~ 10,000; G140M) observations can produce high quality reconstructed mea-
surements of the local Ly-alpha flux (France et al. 2013; Youngblood et al. 2016). For those targets where Ly-alpha observations are infeasible, we will rely on scaling relations (based on MgII, for example) to estimate the HI emission (Wood et al. 2005; Youngblood et al. 2017). Finally,
in order to calibrate the UV data to visible/IR photospheric models and the ground-based spectra, we will also acquire short optical observations with the STIS G430L.
Exposure Time Calculations: We estimated exposure times based on the minimum
amount of time required to achieve S/N -10 per resolution element in the characteristic line
and continuum regions: Ly-alpha (STIS G140M, meas = 1216.0 A), C II (STIS G140L), and
NUV continuum (STIS G230L, 2820 A, longward of MgII). We estimated S/N>20 in the
optical (STIS G430L). We create simulated spectra for exposure time estimates by taking
stars of similar spectral types from the HST archive (Procyon, alpha Cen A, eps Eri, HD 85512,
and GJ 832), scaled to the V magnitude of the target star.
All targets were run through the APT Bright Object Tool software. The only violations reported were cases where the target star was mis-identified as an O5V star.Title: Essential Ultraviolet Stellar Characterization for Guaranteed JWST Transiting Planet Targets
Kevin France was the PI of the HST MUSCLES Treasury Survey (GO13650) to study the spectral and temporal properties of red dwarf stars (France et al. 2016; Loyd et al. 2016; Youngblood et al. 2016). He is the co-PI of the follow-on Mega-MUSCLES Survey (GO15071) that focused on activity in later-type M dwarfs. He was also a member of the COS instrument and science teams, developing numerous community tools for spectral and temporal analysis of COS data, and has authored over 50 refereed publications on cool stars, exoplanets, and planet-forming disks using UV spectra from HST.
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 habitabilty. 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 an the lead or co-author on over 20 papers using HST UV spectroscopic observations.
David Wilson is a PI of two previous HST programs (13719, 15189) 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.
Allison Youngblood was a member of the MUSCLES team and has published a number of papers focused on the quiescent and flare properties of M stars. Girish Duvvuri has developed a new method of estimating the EUV properties of M stars by applying Differential Emission Measure calculations based on X-ray and FUV observations. Zachory Berta-Thompson has been the PI of Lyman-alpha transit spectrosopy programs targeting planets around cool stars. Both he and Jacob Bean are leaders of the large JWST ERS program targeting exoplanetary systems, and will provide guidance on optimization of the HST dataset for supporting future JWST programs. Jacob Bean is an expert in the characterization of exoplanet atmospheres using ground- and space-based telescopes. He has led HST programs totaling 247 orbits and has published more than 20 papers utilizing HST data. He is a Co-PI on the JWST Transiting Exoplanet Community ERS program, and the science lead for a further 80 hours of JWST GTO transit observations.
Yamila Miguel ia a member members of the MUSCLES and Mega-MUSCLES teams and are experts in using the M star spectral and flare information provided by UV observations to model the atmospheres and photochemistry/biomarker tracers of exoplanets around low mass stars.
Co-I Pineda is an expert in the magnetic activity of low-mass stars and brown dwarfs (e.g., Pineda et al. 2017). He is the PI of the FUMES project (HST GO - 14640) targeting the FUV emissions of active early M-dwarfs with STIS. He has worked on the optical spectroscopy and HST UV analysis of quiescent and flaring M-dwarfs, including X-ray programs with XMM-Newton (XMM-086356).Exoplanets and Exoplanet FormationStellar Physics and Stellar Types6falsefalsetruefalsefalsefalse7560trueSUPPORTEDEXT-STARK V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000EXT-STARG V-IVThis object was generated by the targetselector and retrieved from the SIMBAD database.
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Other name: CD-385670J2000J2000EXT-STARM V-IVThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000EXT-STARM V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.GJ357J2000J2000EXT-STARK V-IVThis object was generated by the targetselector and retrieved from the SIMBAD database.TYC-3215-1935-1J2000EXT-STARG V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
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