0
Assigned ID: 2171
----- Attempting Submission 1 (Fri Apr 09 19:54:13 GMT 2021) -----
The number of orbits used exceeds the number allocated
Added repeat visit for HD 80606 (HOPR 92516)
1757858310
----- Attempting Submission 1 (Wed Jul 28 19:03:02 GMT 2021) -----
----- Attempting Submission 2 (Thu Aug 12 21:49:01 GMT 2021) -----
----- Attempting Submission 3 (Wed Sep 29 23:54:35 GMT 2021) -----
HST Phase II Proposal 16701 successfully submitted.
Receipt: # 16701-3
----- Attempting Submission 4 (Thu Sep 30 16:13:22 GMT 2021) -----
----- Attempting Submission 5 (Wed Oct 06 23:58:13 GMT 2021) -----
----- Attempting Submission 6 (Mon Nov 08 17:31:50 GMT 2021) -----
----- Attempting Submission 7 (Mon Nov 15 23:18:46 GMT 2021) -----
----- Attempting Submission 8 (Fri Nov 19 22:30:21 GMT 2021) -----
----- Attempting Submission 9 (Mon Jan 24 23:11:21 GMT 2022) -----
----- Attempting Submission 10 (Tue Jan 25 20:20:46 GMT 2022) -----
----- Attempting Submission 11 (Thu Feb 10 21:35:53 GMT 2022) -----
----- Attempting Submission 12 (Wed Feb 16 16:53:48 GMT 2022) -----
----- Attempting Submission 13 (Wed Jul 20 16:25:13 GMT 2022) -----
----- Attempting Submission 14 (Fri Oct 28 18:19:18 GMT 2022) -----
----- Attempting Submission 15 (Sun Feb 12 16:13:15 GMT 2023) -----
----- Attempting Submission 16 (Thu Apr 27 22:20:42 GMT 2023) -----
N/A
Essential Ultraviolet Stellar Characterization for Cycle 1 JWST Transiting Planet Targets
Atmospheric spectroscopy of an exciting array of exoplanets (warm rocky planets, sub-Neptune, and Jupiter-mass planets) will be obtained during JWST's Cycle 1. 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 atmospheric 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 UV 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 A) and X-ray stellar spectroscopy of the 23 JWST Cycle 1 targets without UV characterization data in the HST archive. Our proposed observations will provide the high-energy 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 efficient observations of the 22 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-alpha 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 M dwarf targets that are sufficiently bright, we will also observe using G140M with the 52x0.2 arcsec slit to measure the Ly-alpha profile for our targets (the 0.2" slit is chosen to maximize throughput and mitigate pointing drift). Ly-alpha 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 field from cool stars (France et al. 2012). Medium-resolution (R ~ 10,000; G140M) observations can produce high quality reconstructed measurements of the local Ly-alpha flux (France et al. 2013; Youngblood et al. 2016). For FGK stars whose Ly-alpha line widths are intrinsically broader, we will reconstruct the Ly-alpha line from the G140L spectra. For those targets where Ly-alpha and/or general FUV 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), 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, pi Men, HD 85512, and GJ 832), scaled to the distance and radius of the target star. Note that during Phase 2, four of our targets' STIS G140L exposures were switched to COS G130M for instrument safety reasons (GJ 367, GJ 341, TOI-260, and TOI-134).
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.
Allison Youngblood is a member of the MUSCLES and Mega-MUSCLES teams (GO-13650 and GO-15071) and has led multiple HST proposals as PI studying the UV emission of exoplanet host stars (GO-15190, GO-15643). She has published a number of papers focused on the quiescent and flare properties of M and K stars, especially regarding their Lyman alpha emission and reconstruction techniques.
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), a large SNAP program on UV emission from exoplanet host stars (GO14633), and the PI of an active HST project to acquire UV spectra of JWST targets on the GTO and ERS lists (GO16166). He is the co-PI of the Mega-MUSCLES Survey (GO15071) that focused on activity in later-type M dwarfs. He and his research group have developed numerous community tools for spectral and temporal analysis of COS and STIS data, and has authored over 70 refereed publications on cool stars, exoplanets, and planet-forming disks using UV spectra from HST.
Cynthia 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 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 latetype stars, and has completed bright-object protection checks for multiple programs.
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.
Thomas Mikal-Evans is an expert in designing space-based observations of transiting exoplanets and analyzing the data, and will ensure the data products of this program are best applied to atmospheric datasets.
Yamila Miguel is 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.
Sebastian 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).
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. Patrick Behr is a graduate student performing the STIS data analysis and X-ray spectral modeling for HST-GO-16166, a program focused on obtaining UV and X-ray spectroscopy of the JWST ERS/GTO targets.
Eliza Kempton is an expert in the theoretical modeling of exoplanet atmospheres, specifically focusing on photochemistry, radiative transfer, and spectroscopic observables. She and her team at UMD (Matej Malik and DJ Teal) will provide guidance to the team on how to best incorporate the UV data products into exoplanet atmosphere models and will lead an effort to perform photochemical calculations with VULCAN and Atmos for planets orbiting the observed host stars. She has been a theorist co-I on 13 HST programs totaling over 300 orbits, and she serves as PI or co-PI on two selected JWST Cycle 1 observing programs.
Matej Malik is an expert in the theory and numerical modeling of radiative transfer in exoplanetary atmospheres. He is well versed in interpreting and simulating spectroscopic observations of exoplanets with theoretical models. He is also experienced in thermochemical and photochemical modeling of a wide range of exoplanets, ranging from super-Earths to ultra-hot Jupiters. He will support the atmospheric modeling efforts for the planets orbiting the observed stars.
Alexander Brown has decades of UV and X-ray observational experience studying the chromospheres, transition regions, and coronae of late-type stars, including
many HST and Chandra/XMM projects from the launch of these space observatories to the present day. He will work extensively on the coordinated X-ray observations proposed here.
Christian Schneider has more than 10 years of experience studying X-ray emission of various kinds of stars (from young stars over solar type to evolved stars) with XMM-Newton, Chandra, Swift, and eROSITA (an ongoing German-Russian X-ray all-sky survey).
Exoplanets and Exoplanet Formation
0
false
false
true
false
false
false
false
180
90
true
SUPPORTED
STAR
M V-IV
NO
Coordinates from Gaia EDR3. V-magnitude from Winters et al. 2019
LTT-1445A
J2000
J2000
STAR
M V-IV
NO
Coordinates from Gaia EDR3.
GJ-486
J2000
J2000
STAR
M V-IV
NO
Coordinates from Gaia EDR3.
GJ-367
J2000
J2000
STAR
M V-IV
NO
Coordinates from Gaia EDR3.
GJ-341
J2000
J2000
STAR
M V-IV
NO
Coordinates from Gaia EDR3.
GJ-4102
J2000
J2000
STAR
M V-IV
NO
Coordinates from Gaia EDR3.
TOI-260
J2000
J2000
STAR
M V-IV
NO
Coordinates from Gaia EDR3.
TOI-134
J2000
J2000
STAR
M V-IV
NO
Coordinates from Gaia EDR3.
TOI-776
J2000
J2000
STAR
K V-IV
NO
Coordinates from Gaia EDR3.
TOI-836
J2000
J2000
STAR
M V-IV
NO
Coordinates from Gaia EDR3.
J2000
J2000
STAR
K V-IV
NO
Coordinates from Gaia EDR3.
TOI-402
J2000
J2000
STAR
K V-IV
NO
Coordinates from Gaia EDR3.
K2-141
J2000
J2000
STAR
K V-IV
NO
Coordinates from Gaia EDR3.
TOI-178
J2000
J2000
STAR
G V-IV
NO
Coordinates from Gaia EDR3.
J2000
J2000
STAR
G V-IV
NO
Coordinates from Gaia EDR3.
TOI-421
J2000
J2000
STAR
F3-F9
NO
Coordinates from Gaia EDR3.
WASP-166
J2000
J2000
STAR
G V-IV
NO
Coordinates from Gaia EDR3.
HIP-67522
J2000
J2000
STAR
K V-IV
NO
Coordinates from Gaia EDR3.
J2000
J2000
STAR
F3-F9
NO
Coordinates from Gaia EDR3.
WASP-121
J2000
J2000
STAR
G V-IV
NO
Coordinates from Gaia EDR3.
WASP-63
J2000
J2000
STAR
K V-IV
NO
Coordinates from Gaia EDR3.
J2000
J2000
STAR
G V-IV
K V-IV
NO
Coordinates from Gaia EDR3.
J2000
J2000
STIS/FUV-MAMA
Spectroscopic
No
No
G140L
1425
STIS/FUV-MAMA
Spectroscopic
No
No
G140M
1222
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/CCD
Spectroscopic
No
No
G430L
4300
STIS/FUV-MAMA
Spectroscopic
No
No
G140L
1425
STIS/FUV-MAMA
Spectroscopic
No
No
G140M
1222
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/CCD
Spectroscopic
No
No
G430L
4300
STIS/FUV-MAMA
Spectroscopic
No
No
G140L
1425
STIS/FUV-MAMA
Spectroscopic
No
No
G140M
1222
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/CCD
Spectroscopic
No
No
G430L
4300
STIS/FUV-MAMA
Spectroscopic
No
No
G140L
1425
STIS/FUV-MAMA
Spectroscopic
No
No
G140M
1222
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/CCD
Spectroscopic
No
No
G430L
4300
STIS/FUV-MAMA
Spectroscopic
No
No
G140L
1425
STIS/FUV-MAMA
Spectroscopic
No
No
G140M
1222
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/CCD
Spectroscopic
No
No
G430L
4300
STIS/FUV-MAMA
Spectroscopic
No
No
G140L
1425
STIS/FUV-MAMA
Spectroscopic
No
No
G140M
1222
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/CCD
Spectroscopic
No
No
G430L
4300
STIS/FUV-MAMA
Spectroscopic
No
No
G140L
1425
STIS/FUV-MAMA
Spectroscopic
No
No
G140M
1222
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/CCD
Spectroscopic
No
No
G430L
4300
STIS/FUV-MAMA
Spectroscopic
No
No
G140L
1425
STIS/FUV-MAMA
Spectroscopic
No
No
G140M
1222
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/CCD
Spectroscopic
No
No
G430L
4300
STIS/FUV-MAMA
Spectroscopic
No
No
G140L
1425
STIS/FUV-MAMA
Spectroscopic
No
No
G140M
1222
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/CCD
Spectroscopic
No
No
G430L
4300
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/CCD
Spectroscopic
No
No
G430L
4300
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/CCD
Spectroscopic
No
No
G430L
4300
STIS/FUV-MAMA
Spectroscopic
No
No
G140L
1425
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/CCD
Spectroscopic
No
No
G430L
4300
STIS/FUV-MAMA
Spectroscopic
No
No
G140L
1425
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/CCD
Spectroscopic
No
No
G430L
4300
STIS/FUV-MAMA
Spectroscopic
No
No
G140L
1425
STIS/FUV-MAMA
Spectroscopic
No
No
G140M
1222
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/CCD
Spectroscopic
No
No
G430L
4300
STIS/FUV-MAMA
Spectroscopic
No
No
G140L
1425
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/CCD
Spectroscopic
No
No
G430L
4300
STIS/FUV-MAMA
Spectroscopic
No
No
G140L
1425
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/CCD
Spectroscopic
No
No
G430L
4300
STIS/FUV-MAMA
Spectroscopic
No
No
G140L
1425
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/CCD
Spectroscopic
No
No
G430L
4300
STIS/FUV-MAMA
Spectroscopic
No
No
G140L
1425
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/CCD
Spectroscopic
No
No
G430L
4300
STIS/FUV-MAMA
Spectroscopic
No
No
G140L
1425
STIS/CCD
Spectroscopic
No
No
G430L
4300
STIS/FUV-MAMA
Spectroscopic
No
No
G140L
1425
STIS/CCD
Spectroscopic
No
No
G430L
4300
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/CCD
Spectroscopic
No
No
G430L
4300
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/CCD
Spectroscopic
No
No
G430L
4300
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
The scheduling data was generated by CASM 31.0.
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true
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The scheduling data was generated by CASM 31.0.
CASM was run in Phase II mode.
/private/var/folders/51/d9fx8d_x10s7sp3fbpfns04cs2q3k7/T/OPVisit12685207649729735301.xml
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