Giada Arney

Goddard Space Flight Center

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Shawn Domagal‐Goldman

Goddard Space Flight Center

106

Victoria Meadows

University of Washington

Edward W. Schwieterman

University of Washington

R. Kopparapu

Goddard Space Flight Center

Stephen R. Kane

University of California, Riverside

Tyler D. Robinson

University of Arizona

Aki Roberge

Goddard Space Flight Center

N. R. Izenberg

Johns Hopkins University Applied Physics Laboratory

Avi M. Mandell

Goddard Space Flight Center

Thomas Fauchez

Goddard Space Flight Center

Cooperative Institutions

Goddard Space Flight Center

282

Jet Propulsion Laboratory

255

California Institute of Technology

249

Planetary Science Institute

205

Max Planck Society

152

Ames Research Center

143

University of Arizona

124

Centre National de la Recherche Scientifique

102

University of Washington

Johns Hopkins University Applied Physics Laboratory

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Deep Atmosphere of Venus Probe as a Mission Priority for the Upcoming Decade

Bulletin of the AAS (2021)

J. B. Garvin Giada Arney S. K. Atreya Stephanie Getty M. S. Gilmore

This is a white paper submitted to the Planetary Science and Astrobiology Decadal Survey. The deep atmosphere of Venus is largely unexplored and yet may harbor clues to the evolutionary pathways for a major silicate planet with implications across the solar system and beyond. In situ data is needed to resolve significant open questions related to the evolution and present-state of Venus, including questions of Venus' possibly early habitability and current volcanic outgassing. Deep atmosphere probe-based in situ missions carrying analytical suites of instruments are now implementable in the upcoming decade (before 2030), and will both reveal answers to fundamental questions on Venus and help connect Venus to exoplanet analogs to be observed in the JWST era of astrophysics.

Habitability

Atmosphere of Venus

Outgassing

10.3847/25c2cfeb.a4985366

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A Second Earth-Sized Planet in the Habitable Zone of the M Dwarf, TOI-700

arXiv (Cornell University) (2023)

Emily A. Gilbert Andrew Vanderburg Joseph E. Rodriguez Benjamin J. Hord Matthew S. Clement

We report the discovery of TOI-700 e, a 0.95 R$_\oplus$ planet residing in the Optimistic Habitable Zone (HZ) of its host star. This discovery was enabled by multiple years of monitoring from NASA's Transiting Exoplanet Survey Satellite (TESS) mission. The host star, TOI-700 (TIC 150428135), is a nearby (31.1 pc), inactive, M2.5 dwarf ($V_{mag} = 13.15$). TOI-700 is already known to host three planets, including the small, HZ planet, TOI-700 d. The new planet has an orbital period of 27.8 days and, based on its radius (0.95 R$_\oplus$), it is likely rocky. TOI-700 was observed for 21 sectors over Years 1 and 3 of the TESS mission, including 10 sectors at 20-second cadence in Year 3. Using this full set of TESS data and additional follow-up observations, we identify, validate, and characterize TOI-700 e. This discovery adds another world to the short list of small, HZ planets transiting nearby and bright host stars. Such systems, where the stars are bright enough that follow-up observations are possible to constrain planet masses and atmospheres using current and future facilities, are incredibly valuable. The presence of multiple small, HZ planets makes this system even more enticing for follow-up observations.

Kepler-69c

10.48550/arxiv.2301.03617

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Sensitive Probing of Exoplanetary Oxygen via Mid Infrared Collisional Absorption

American Astronomical Society Meeting Abstracts #235 (2020)

Thomas Fauchez Gerónimo Villanueva Edward W. Schwieterman Martin Turbet Giada Arney

The collision-induced fundamental vibration–rotation band at 6.4 μm is the strongest absorption feature from O2 in the infrared1–3, yet it has not been previously incorporated into exoplanet spectral analyses for several reasons. Either collision-induced absorptions (CIAs) were not included or incomplete/obsolete CIA databases were used. Also, the current version of HITRAN does not include CIAs at 6.4 μm with other collision partners (O2–X). We include O2–X CIA features in our transmission spectroscopy simulations by parameterizing the 6.4-μm O2–N2 CIA based on ref. 3 and the O2–CO2 CIA based on ref. 4. Here we report that the O2–X CIA may be the most detectable O2 feature for transit observations. For a potential TRAPPIST-1 e analogue system within 5 pc of the Sun, it could be the only O2 signature detectable with the James Webb Space Telescope (JWST) (using MIRI LRS (Mid-Infrared Instrument low-resolution spectrometer)) for a modern Earth-like cloudy atmosphere with biological quantities of O2. Also, we show that the 6.4-μm O2–X CIA would be prominent for O2-rich desiccated atmospheres5 and could be detectable with JWST in just a few transits. For systems beyond 5 pc, this feature could therefore be a powerful discriminator of uninhabited planets with non-biological ‘false-positive’ O2 in their atmospheres, as they would only be detectable at these higher O2 pressures. Spectroscopic simulations of exoplanetary atmospheres show that our best chance to detect molecular oxygen lies in the 6.4-μm band of collision-induced absorptions. The first detections could be possible with the James Webb Space Telescope.

HITRAN

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Exoplanetary Atmospheric Retrieval via Bayesian Machine Learning

AAS/Division for Extreme Solar Systems Abstracts (2019)

Michael D. Himes Adam D. Cobb Frank Soboczenski Simone Zorzan Molly D. O’Beirne

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Retrievals Applied to a Decision Tree Framework Can Characterize Earthlike Exoplanet Analogs

The Planetary Science Journal (2024)

Amber V. Young Jaime Crouse Giada Arney Shawn Domagal‐Goldman Tyler D. Robinson

Abstract Exoplanet characterization missions planned for the future will soon enable searches for life beyond our solar system. Critical to the search will be the development of life detection strategies that can search for biosignatures while maintaining observational efficiency. In this work, we adopted a newly developed biosignature decision tree strategy for remote characterization of Earthlike exoplanets. The decision tree offers a step-by-step roadmap for detecting exoplanet biosignatures and excluding false positives, based on Earth’s biosphere and its evolution over time. We followed the pathways for characterizing a modern-Earth-like planet and an Archean-Earth-like planet and evaluated the observational trades associated with coronagraph bandpass combinations of designs consistent with the Habitable Worlds Observatory precursor studies. With retrieval analyses of each bandpass (or combination), we demonstrate the utility of the decision tree and evaluate the uncertainty on a suite of biosignature chemical species and habitability indicators (i.e., the gas abundances of H 2 O, O 2 , O 3 , CH 4 , and CO 2 ). Notably for modern Earth, less than an order of magnitude spread in the 1 σ uncertainties was achieved for the abundances of H 2 O and O 2 , planetary surface pressure, and atmospheric temperature, with three strategically placed bandpasses (two in the visible and one in the near-infrared). For the Archean, CH 4 and H 2 O were detectable in the visible with a single bandpass.

Coronagraph

Planetary habitability

10.3847/psj/ad09b1

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Citations (4)

Exploring Habitable-Zone Earths In Synchronous Rotation Around Cool Stars with General Circulation Models and Simulated Spectra

American Astronomical Society Meeting Abstracts #235 (2020)

G. Engelmann-Suissa Avi M. Mandell R. Kopparapu Eric Wolf G. L. Villanueva

Tidal locking

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