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-2032319691
----- Attempting Submission 1 (Mon Feb 16 21:24:48 GMT 2026) -----
----- Attempting Submission 2 (Tue Feb 24 00:20:44 GMT 2026) -----
----- Attempting Submission 3 (Mon Mar 23 23:48:21 GMT 2026) -----
----- Attempting Submission 4 (Tue Mar 24 19:10:07 GMT 2026) -----
----- Attempting Submission 5 (Fri Apr 17 20:50:53 GMT 2026) -----
----- Attempting Submission 6 (Fri May 08 22:00:55 GMT 2026) -----
STELa: Survey of Transiting Exoplanets in Lyman-alpha
Atmospheric escape is a key process that sculpts the exoplanetary population, especially for planets smaller than Neptune. Transit observations in the Lyman-alpha line allow for direct studies of atmospheric escape, but progress is reaching the limit of what is possible with small programs targeting one or two new planets at a time. To advance atmospheric escape studies into a new statistical regime, we propose the Survey of Transiting Exoplanets in Lyman-alpha (STELa), a Multi-Cycle Treasury program aimed at efficiently probing atmospheric escape across the entire exoplanetary population using a proven reconnaissance-detection-characterization strategy. STELa's statistical sample will map the role of mass loss throughout the population of known exoplanets, investigate the nature of "transitional" worlds such as those in near radius valley, and probe the physical mechanism driving the atmospheric erosion of sub-Neptunes. A wide array of treasury science will be possible with the STELa dataset, including a new 3D map of the local interstellar medium, the first survey of stellar wind strengths within the astropause, an atlas of host star XUV spectra in the mass-rotation plane, and investigations of exosphere-thermosphere-lower atmosphere connections through synergies with He 10830 and JWST observations. Implementing a broad Lyman-alpha transit survey now is essential to enable the scientific leap from ``stamp collecting'' to population science within the limited remaining life of the only observatory capable of these observations.
Stage 2 (Cycle 33) observations will observe the Lya transits of target planets using two visit sets of 2 + 5 exposures. The first visit will establish the pre-transit baseline clear of any early ingress. Following an SAA passage, the second visit will measure transit absorption.
Because Stage 1 (Cycle 32) of the STELa program is ongoing, targets will be added periodically to this program throughout Cycle 33 based on a selection process that relies on Stage 1 observations. Each new batch of targets receives a new program number.
The second visit in a set may be offset from mid-optical-transit when this is predicted to increase the detectability of a transit signal based on a grid of simulations where a cometary tail is pushed by the stellar wind:
GJ 143 b 0
HD 207897 b 2
HD 42813 b 0
HD 95338 b 0
K2-136 c 0
TOI-1434 1 0
TOI-2134 b 0
TOI-2134 c 0
TOI-2134 c 9
TOI-2285 b 0
TOI-2443 b 0
TOI-260 b 0
TOI-431 d 0
WASP-107 b 3
STIS G140M observations will be used in most cases, with the aperture chosen for optimal transit SNR based on the target's known Lya emission and the planet's predicted absorption, accounting for instrumental and stellar sources of variability, including slit breathing at the RMS values given in Bohil & Hartig 1998. COS G130M might be used in some cases where the target flux is sufficiently high that using COS is not expected to significantly degrade Lya SNR, thereby enabling simultaneous measurement of the planetary transit in metal lines. STIS E140M may be used in some instances for detector safety. The program will use long slit apertures for E140M to facilitate Lya airglow subtraction. For this batch, the optimal configurations are
GJ 143 b 52x0.2 g140m
HD 207897 b 52x0.2 g140m
HD 42813 b 52x0.2 g140m
HD 95338 b 52x0.2 g140m
K2-136 c 52x0.2 g140m
TOI-1434 1 52x0.1 g140m
TOI-2134 b 52x0.2 g140m
TOI-2134 c 52x0.1 g140m
TOI-2285 b 52x0.2 g140m
TOI-2443 b 52x0.5 g140m
TOI-260 b 52x0.2 g140m
TOI-431 d 52x0.5 g140m
WASP-107 b 52x0.2 g140m
R. O. Parke Loyd has extensive experience in planning, reducing, and analyzing HST FUV observations, with nine first-author papers published using such data since 2014. He was a key contributor to the discovery of the Lyman-alpha transit of GJ 436 b (Kulow et al. 2014) and later led work placing constraints on its C II and Si III transits. He recently led the discovery of a Lyman-alpha transit from the ~2 Rearth planets in the TOI-776 system. He has PIed 4 HST observing programs, including Lyman-alpha transit programs and was a key contributor in the creation of the treasury-scale MUSCLES and HAZMAT datasets (e.g. Loyd et al. 2016, 2018a, 2018b).
Dr. Shreyas Vissapragada is an expert in observations of atmospheric escape, especially using the metastable helium 10830 triplet in which he has observed over a dozen planets (and used these observations to benchmark planetary outflow models). Recently he is using HST to push towards Lyman-alpha constraints on the Earth-sized exoplanet GJ 12b (GO-17600).
Drs. James Owen, Ruth Murray-Clay, and Hilke Schlichting are leaders in the field of exoplanetary atmospheric scape and sub-Neptune evolution (e.g., Owen and Alvarez, 2016; Murray-Clay et al., 2009; Gupta and Schlichting 2019). Dr. Owen was one of the founders of the XUV evaporation theory and Dr. Schilchting of core-powered mass loss. Dr. Owen's student Ethan Schreyer developed the outflow model that will be used in this work. Dr. Akash Gupta and Dr. James Rogers are expert in population modeling under the influence of atmospheric escape due to core-powered mass loss and photoevaporation (Gupta and Schlichting 2019, Rogers et al. 2023). Dr. Murray-Clay and her students are experts in outflow modeling, having developed both 3D and 1D outflow models (e.g., McCann et al. 2019).
Dr. Allison Youngblood is the PI of multiple HST programs to study exoplanets and their host stars in the UV, including a large ~200 orbit survey of the UV emission from JWST Cycle 1 transiting exoplanet host stars (GO-16701) and a Lyman alpha transit of the sub-Neptune TOI-1231b.
Dr. Evgenya Shkolnik has been studying exoplanets and the stellar activity of their host stars, including star- planet interactions, for over 20 years, ranging from systems around Sun-like stars down to the lowest mass M dwarfs, including extensive studies of the Sun-as-a-star. She is also the PI or Co-I of several HST programs, including those studying the UV evolution of K and M stars.
David Ardila is an expert in UV instrumentation and observations. He serves as lead instrument scientist on the Star-Planet Activity Research CubeSat and has served leadership roles in UV mission concepts like UV-SCOPE.
Drs. Sarah Peacock and Travis Barman are experts in modeling stellar and giant planet atmospheres. A modified PHOENIX model they have developed can be used to predict the EUV emission of a low-mass star by matching the model-simulated FUV emission to observations (Peacock et al. 2019). 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. Girish Duvvuri is an expert in the XUV reconstructions using a DEM method scalable to large numbers of datasets (Duvvuri et al. 2021). He is PI of an archival HST program to reconstruct XUV spectra for a broad sample of targets with existing FUV spectra (AR-17054).
Mercedes Lopez-Morales is an expert in the study of exoplanet atmospheres via transmission spectroscopy. She has led HST and ground-based transmission spectroscopy surveys, namely The HST PanCET program, GO: 14767, PIs: Sing & Lopez-Morales and The Arizona-CfA-Catolica-Carnegie Exoplanet Spectroscopy Survey, ACCESS, PIs: Lopez-Morales, Apai, Jordan.
Exoplanets and Exoplanet Formation
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EXTRA-SOLAR PLANETARY SYSTEM
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J2000
G=7.69, NUV=16.38
STAR
K V-IV
EXTRA-SOLAR PLANETARY SYSTEM
Predicted Lya flux before ISM absorption 1.9e-13;FUV used for buffer time estimate 24.89;deemed INACTIVE on the basis fuv no more than 3x brighter than median for field stars of similar Teff < 5500;stellar mass 0.82;stellar Teff 5106.00;GALEX fuv mag > 21.52;Rossby number estimate of 3.39 based on measured 37.0 d rotation period;cataloged age of 5 Gyr
J2000
G=8.14, NUV=15.34
STAR
K V-IV
EXTRA-SOLAR PLANETARY SYSTEM
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J2000
G=8.39
STAR
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STAR
G V-IV
EXTRA-SOLAR PLANETARY SYSTEM
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J2000
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STAR
K V-IV
EXTRA-SOLAR PLANETARY SYSTEM
Predicted Lya flux before ISM absorption 1.7e-13;FUV used for buffer time estimate 25.60;deemed INACTIVE on the basis fuv no more than 3x brighter than median for field stars of similar Teff < 5500;stellar mass 0.74;stellar Teff 4580.00;GALEX fuv mag > 21.26;Rossby number estimate of 4.58 based on measured 45.8 d rotation period;cataloged age of 4 Gyr
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STAR
M V-IV
EXTRA-SOLAR PLANETARY SYSTEM
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J2000
G=12.422335624694824, NUV=22.76286966325075
STAR
K V-IV
EXTRA-SOLAR PLANETARY SYSTEM
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J2000
G=9.04, NUV=18.44
STAR
M V-IV
EXTRA-SOLAR PLANETARY SYSTEM
J2000
G=9.316665649414062
STAR
K V-IV
EXTRA-SOLAR PLANETARY SYSTEM
J2000
G=8.798720359802246
STAR
EXTRA-SOLAR PLANETARY SYSTEM
K V-IV
This 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.
J2000
STAR
K V-IV
EXTRA-SOLAR PLANETARY SYSTEM
Predicted Lya flux before ISM absorption 1.2e-13;FUV used for buffer time estimate 22.53;deemed INACTIVE on the basis fuv no more than 3x brighter than median for field stars of similar Teff < 5500;stellar mass 0.66;stellar Teff 4195.00;GALEX fuv mag = 22.53;Rossby number unknown due to no cataloged rotation period;no cataloged age
J2000
G=10.17, NUV=19.00, FUV=22.53
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:al-overhead-at-end 0
:internal-dur-at-end 622
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2868
:pcs-gap 0
)
true
2
0
Timing link suitability includes constraints ([28 After 27 by 0.2 to 1.0 days])
The scheduling data was generated by CASM 34.0.
CASM was run in Phase II mode.
/private/var/folders/6l/1fvgkb5d08b8tf7zpvnzkd7c0000gn/T/OPVisit2571871328009117138.xml
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