Submission 3, 04/10/25. kevin.france@colorado.edu1269690870Assigned ID: 6240
----- Attempting Submission 1 (Wed Apr 09 16:24:59 GMT 2025) -----
HST Phase I Proposal 6240 successfully submitted.
Receipt: # 6240-1
----- Attempting Submission 2 (Thu Apr 10 02:50:42 GMT 2025) -----
HST Phase I Proposal 6240 successfully submitted.
Receipt: # 6240-2
----- Attempting Submission 3 (Thu Apr 10 19:42:49 GMT 2025) -----
HST Phase I Proposal 6240 successfully submitted.
Receipt: # 6240-3Unsupported characters were found in Observing Description and replaced with |*|
For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.
For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.
For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.
For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.
INEFFICIENT ORDERING OF FP-POS POSITIONS
For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.
For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.
For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.
For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.
INEFFICIENT ORDERING OF FP-POS POSITIONS
For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.
For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.
For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.
For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.
INEFFICIENT ORDERING OF FP-POS POSITIONSGO18030 - submission #4. 28 march 2026. Kevin France (kevin.france@colorado.edu)-1830325195----- Attempting Submission 1 (Fri Aug 08 20:21:03 GMT 2025) -----
----- Attempting Submission 2 (Sat Mar 28 12:38:37 GMT 2026) -----Muscles Advanced Library With an Atmospheric Retention EmphasisShoring Up the Cosmic Shoreline: Improving the Cumulative XUV Irradiance Knowledge of Rocky Worlds DDT Targets
The JWST Rocky Worlds Director's Discretionary Time (RW DDT) program is studying whether rocky planets orbiting M dwarf stars can retain their atmospheres. The RW DDT is targeting approximately 10 of the most promising small planets for (1) atmospheric detection observations with JWST and (2) measurements of the far-ultraviolet to infrared stellar spectral energy distributions with HST. The RW program is framed around the concept of the Cosmic Shoreline, where a planet's gravity (escape velocity) is compared with the escape-driving XUV energy input from the star.
We propose to directly support the fundamental goal of the DDT program with a multi-cycle GO+AR program to quantify the stellar XUV environments of the RW target stars and empirically place them on the Cosmic Shoreline. We will do this with (1) new far-ultraviolet + X-ray (Chandra and XMM) observations of the host stars in Cycles 33, 34, and 35 that enable high-quality extreme-ultraviolet calculations and characterization of the full XUV (X-ray + extreme-ultraviolet) irradiance, (2) observation and characterization of stellar flares across the full high-energy spectral band to quantify the contribution of time-variable phenomena to the total ionizing radiation budget, and (3) creation of a high-level stellar data product library to support the community's analysis and interpretation of the terrestrial planet data acquired by the RW DDT program.++Observing Modes and Exposure Times: We propose deep, COS G140L CENWAVE 800
observations of each of the Rocky Worlds targets. The short wavelength coverage compared
to the RW DDT HST plan (monitoring in COS G130M only; Espinoza & Diamond-Lowe
2025) provides access to key spectral diagnostics that |*|fill in|*| plasma temperature coverage
for robust EUV spectral calculations using the DEM method, including the brightest stellar
FUV lines in cool star atmosphere (C III |*|977 |*|A, O VI 1032/1038 |*|A; Redfield et al. 2002)
and high-temperature lines not covered by standard COS G130M CENWAVE 1291
observations (S VI |*|933/944 |*|A, Fe XVIII 974 |*|A, Fe XIX 1118 |*|A; Redfield et al. 2003).
G140L CENWAVE 800 has the additional advantage of being designed specifically to
minimize the astigmatic spectral height on the COS detector at |*| < 1100 |*|A, reducing the
background levels where HST|*|s sensitivity is lower (e.g., Sankrit et al. 2018). We estimate
exposure times for our proposed observations by scaling the observed Si IV flux of LTT1445
A (Diamond Lowe et al. 2024) with line ratios derived from AU Mic observations by FUSE
and HST (Redfield et al., 2002; Feinstein et al., 2022). We find that quiescent S/N per
spectral resolution element |*| 4 |*| 5 in the peaks of key lines (C III, O VI, Fe XIX) can
be achieved in 12 orbit observations (COS.sp.1949954, COS.sp.1949955, COS.sp.1949956),
which we propose to break into 4 visits of 3 orbits each. These observations will also be
sensitive to flares which can raise the FUV flux by factors of 5 |*| 10 and are expected to
be present during |*| 25 |*| 40% of the total observing duration (France et al. 2020). The
majority of our proposed targets have previous UV detections, and UV/X-ray flares have
been observed on several of our proposed targets (e.g., Brown et al. 2022; Behr et al. 2023).
++FUV Spectral Lightcurve Production for Flares |*| The COS FUV XDL detector
records spectra in time-tagged mode as [x (or |*|), y, t] photon lists, where x is the photon|*|s
x-axis arrival position (i.e., wavelength), y is the photon|*|s cross-dispersion location, and t is
the photon arrival time. The CALCOS-provided corrtag files contain the [x, y, t] photon
lists, and the total number of counts in a [|*|x,|*|y] box is integrated over an arbitrary time
step |*|t as part of CalCOS|*|s SplitTag package. Flux-calibrated light curves (in units of
erg cm|*|2 s|*|1) are produced by integrating the SplitTag x1d spectrum over the wavelength
interval |*| of the spectral line of interest.
++COS Instrument Safety & Lifetime Position Usage: All of the spectral estimates for
our targets have been run through the STScI on-line Exposure Time Calculators, including
the |*|M dwarf flare safety margins|*| (COS ISR 2017-01-v3). Our targets are all well within
the safety limits for the COS FUV detector using the G140L grating (including the bright
lines Ly|*|, Si IV, and C IV). The targets have been checked against the new COS Lifetime
Position Usage rules and are well under the 1% guidelines (COS.sp.1958706).PI Kevin France is the PI of the HST MUSCLES Treasury Survey (GO13650) and MEATS (GO16166) Survey to study the UV and X-ray spectral and temporal properties of exoplanet host stars (France et al. 2016, 2018, 2020; Loyd et al. 2016; Youngblood et al. 2016; Behr et al. 2023). He is the co-PI of the follow-on Mega-MUSCLES (GO15071; Brown et al. 2022; Wilson et al. 2025) 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 HST and X-ray observatory observations of cool stars. Dr France has authored over 100 refereed publications on exoplanets, cool stars, and planet-forming disks using UV spectra from HST.
CoI Cynthia Froning is the PI of the HST Mega-MUSCLES Treasury Survey (GO-15071), which extended the original MUSCLES survey to lower-mass and more active M dwarfs in support of JWST rocky planet observations. She is a co-I on the MUSCLES and Mega-MEATS surveys. Dr. Froning was the Project Scientist for the HST-COS instrument and is an expert in UV spectroscopic observations of stellar targets as well as UV instrument development and performance.
Co-I Alexander Brown has over four decades of experience studying the evolution of late-type star outer atmospheres in the UV (including EUV directly), X-ray, radio, and optical spectral regions. He has conducted UV spectroscopic and imaging studies with HST since its launch. He has been a Co-I on the MUSCLES/Mega-MUSCLES/Mega-MEATS sequence of exoplanet host star HST projects and provided X-ray analysis for these projects.
Co-I Girish M. Duvvuri has scientific and technical expertise in the time-series spectroscopy of cool dwarfs observed at X-ray + ultraviolet + optical wavelengths to characterize the variability of stellar activity and in modeling stellar X-ray and extreme ultraviolet radiation.
Co-I David Wilson is an expert in stellar ultraviolet and X-ray observations, having led multiple observing programs with HST and other space telescopes. He has published multiple papers concerning exoplanet host stars and produced high-level science product stellar SEDs for projects such as Mega-MUSCLES.
Co-I Allison Youngblood is the Co-PI of Mega-MEATS (GO-16701), a large joint HST-Chandra-XMM survey to measure the UV and X-ray spectra of the JWST Cycle 1 transiting exoplanet host stars. She has led multiple HST programs studying cool stars, exoplanets, and the interstellar medium with the COS and STIS instruments (GO-15190, GO-15463, GO-15635, GO-15674, GO-16700, GO-16701).Exoplanets and Exoplanet FormationStellar Physics and Stellar Types0falsetruefalsefalsetruefalsefalsefalsefalsefalsetruePRIMARY8760trueSUPPORTEDEXT-STARM V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
SIMBAD listed proper motion for this target. When retrieving targets with PM from SIMBAD, APT requests the coordinates be calculated with an epoch of the year 2000. Do not modify this epoch. Always review coordinates using the Target Confirmation tool, which graphically displays the PM.J2000J2000EXT-STARM V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
SIMBAD listed proper motion for this target. When retrieving targets with PM from SIMBAD, APT requests the coordinates be calculated with an epoch of the year 2000. Do not modify this epoch. Always review coordinates using the Target Confirmation tool, which graphically displays the PM.J2000J2000the above "V" mag is actually Johnson BEXT-STARM V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
SIMBAD listed proper motion for this target. When retrieving targets with PM from SIMBAD, APT requests the coordinates be calculated with an epoch of the year 2000. Do not modify this epoch. Always review coordinates using the Target Confirmation tool, which graphically displays the PM.J2000J2000COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800The scheduling data was generated by CASM 34.0.CASM was run in Phase II mode.(Tic-Visit
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