0Assigned ID: 6104
----- Attempting Submission 1 (Fri Apr 04 19:22:57 GMT 2025) -----
HST Phase I Proposal 6104 successfully submitted.
Receipt: # 6104-1
----- Attempting Submission 2 (Tue Apr 08 15:49:40 GMT 2025) -----
HST Phase I Proposal 6104 successfully submitted.
Receipt: # 6104-2updated buffer times for remaining FUV visits-1543606121----- Attempting Submission 1 (Fri Aug 08 20:54:00 GMT 2025) -----
HST Phase II Proposal 18001 successfully submitted.
Receipt: # 18001-1
----- Attempting Submission 4 (Tue Mar 03 16:23:00 GMT 2026) -----
HST Phase II Proposal 18001 successfully submitted.
Receipt: # 18001-4
----- Attempting Submission 5 (Fri Mar 13 20:47:38 GMT 2026) -----Completing Panchromatic Spectra for High Priority HWO Target StarsThe Habitable Worlds Observatory (HWO) will enable the first direct imaging and spectral characterization of terrestrial exoplanets in the habitable zones of nearby stars. However, interpreting these spectra and assessing planetary habitability requires a complete understanding of the high-energy stellar radiation that drives atmospheric chemistry and photochemistry. While some HWO target stars have existing X-ray or UV observations, most lack high-quality data across the full high-energy spectrum. Only 1/3 have either FUV or NUV HST spectra and 1/5 have both. Likewise, only a fraction have X-ray measurements, limiting our ability to construct comprehensive stellar SEDs. We propose FUV and NUV spectroscopy of 10 key stars that currently lack full UV coverage but have existing X-ray data, enabling self-consistent panchromatic SEDs for a subset of HWO's most promising targets.
These observations will provide critical missing constraints on stellar radiation environments, allowing for improved exoplanet atmosphere modeling, photochemical studies, and biosignature detectability assessments. Specifically, this dataset will: (1) establish a high-energy spectral library for a representative sample of HWO-relevant stars, (2) refine stellar atmosphere models to improve planetary atmospheric retrievals, (3) constrain interstellar medium attenuation for Lyman alpha and EUV reconstructions, and (4) lay the groundwork for future studies on stellar activity, atmospheric escape, and exoplanet habitability. By securing these data now, we ensure that HWO operates with the most complete empirical understanding of its target stars, maximizing its scientific return.We will use two observing modes on STIS to measure a complete UV dataset for each of the proposed target stars, requesting a total of 37 orbits:
The NUV observations will be taken with the E230H high resolution echelle (R = 114,000), centered at 2713 A, which includes Fe II lines at 2586 and 2600 A and the Mg II doublet at 2796 and 2803 A. We choose the 0".2x0".09 slit to optimize resolution, similar to what has been done for most HWO target stars with existing NUV observations. Beta Com and GL 117 have archival measurements with this mode, so we do not seek to re-observe these two targets. Two additional targets, eta Crv and beta Vir, exceed the bright object limits
with the 0".2x0".09 slit, so we opt to use a neutral density filter (0".2x0".05 ND) to reduce the UV throughput.
The FUV observations will be taken with the E140M medium resolution echelle (R = 45,800), centered at 1425 A. The 1144-1730 A wavelength range samples several emission lines, including Lyman alpha (1215.67 A) and the N V (1240 A), Si IV (1400 A), and C IV (1550 A) doublets. We choose the 0."2x0".2 slit for these observations because they have been used successfully for similar HWO target stars with existing FUV observations.Dr. Sarah Peacock is an expert in modeling stellar atmospheres and is co-lead of the High-Energy subgroup of the Target Stars HWO working group. Modified PHOENIX models she has developed can be used to predict the EUV emission of main sequence stars by matching the model-simulated FUV emission to observations (Peacock et al. 2019a, 2019b, 2020, 2022). Dr. Peacock is also the PI of an HST program that obtained Lyman alpha observations of 6 M and K type stars with exceptionally large radial velocities that Doppler shift their Lyman alpha emission away from contaminating sources to reveal the intrinsic profiles.
Dr. Allison Youngblood is the PI of multiple HST programs to study the UV emission from late-type stars, including a large survey of the UV emission from JWST Cycle 1 transiting exoplanet host stars (GO-16701) and a study of high-RV stars at high spectral resolution (GO-15190). She is a member of the MUSCLES and Mega-MUSCLES teams, and has experience modeling emission and absorption lines throughout the UV.
Dr. Keighley Rockcliffe is a research scientist at NASA/GSFC. She has expertise in reducing and analyzing HST/STIS observations, with particular emphasis on Lyman alpha observations. She will contribute to the data analysis and publication efforts accompanying this program.
Dr. Breanna Binder is an Associate Professor of Physics and Astronomy at the California State Polytechnic University in Pomona (Cal Poly Pomona). Her research interests are broadly related to high energy (Xray and UV) stellar astrophysics, including coronal Xray emission from Sun-like and potential exoplanet host stars and evolved massive binary stars.
Dr. Edward Schwieterman is an astrobiologist at the University of California, Riverside (UCR). He is an expert in simulating the climate, chemistry, and spectral observables of terrestrial planet atmospheres, with a particular focus on planetary habitability and potential exoplanet biosignatures.
Dr. Margaret Turnbull is an Astrobiologist at the SETI Institute in Mountain View, California. Her expertise is in characterizing nearby stellar systems for habitable exoplanet detection, and in modeling climate outcomes and detectable biosignatures for exo-Earths.
Dr. Katherine Garcia-Sage has extensive experience in modeling of the atmosphere-ionosphere-magnetosphere system at Earth, Solar System planets, and exoplanets, with a specialty in ionospheric escape. She is a developer of the Polar Wind Outflow Model (PWOM). She has served as the thermosphere-ionosphere-magnetosphere expert at the Community Coordinated Modeling Center (CCMC) where, among other responsibilities, she managed instances of several global physics-based models of the ionosphere-thermosphere region and its coupling to geospace and space weather processes. She is deputy project scientist of the Geospace Dynamics Constellation (GDC) mission to characterize and understand Earth's ionosphere-thermosphere region and its response to space weather.
Dr. Stephen Kane is a Professor of Planetary Astrophysics at the University of California, Riverside (UCR), with interests in exoplanet detection and characterization, planetary habitability, orbital dynamics, and studying Venus as an exoplanet analog.
Dr. Alison Farrish is a postdoctoral research scientist at NASA Goddard Space Flight Center contracted via George Mason University. Her research interests include solar and stellar magnetic field modeling, with a focus on characterization of the space weather environments of exoplanet systems, including validation against observed stellar magnetic activity relationships.
Dr. 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. He is also PI of a Astrophysics Decadal Survey Precursor Science grant assessing the UV and X-ray data available for HWO target stars and is co-lead of the High-Energy subgroup of the Target Stars HWO working group.Stellar Physics and Stellar Types6falsetruefalsefalsefalsefalsefalseSUPPORTEDSTARF0-F2This 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.J2000J2000STARF3-F9This 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.J2000J2000STARG V-IVThis 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.J2000J2000STARG V-IVThis 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.J2000J2000STARG V-IVThis 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.J2000J2000STARG V-IVThis 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.J2000J2000STARG V-IVThis 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.J2000J2000STARK V-IVThis 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.J2000J2000STARK V-IVThis 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.J2000J2000STARK V-IVThis object was generated by the targetselector and retrieved from the SIMBAD database.
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