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

Gilbert, Emily A.; Vanderburg, Andrew; Rodriguez, Joseph E.; Sefako, Ramotholo; Clement, Matthew S.; Barclay, Thomas; Quintana, Elisa V.; Schlieder, Joshua E.; Kane, Stephen R.; Jenkins, Jon M.; Twicken, Joseph D.; Kunimoto, Michelle; Vanderspek, R.; Arney, Giada; Charbonneau, David; Günther, Maximilian N.; Huang, Chelsea X.; Isopi, Giovanni; Kostov, Veselin B.; Kristiansen, Martti H.; Latham, David W.; Mallia, F.; Mamajek, Eric E.; Mireles, Ismael; Quinn, Samuel N.; Ricker, G.; Schulte, Jack; Winn, Joshua N.; Suissa, Gabrielle; Winn, Joshua N.; Youngblood, Allison; Zapparata, Aldo

doi:10.3847/2041-8213/acb599

Cited by 13 publications

(7 citation statements)

References 85 publications

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“…The period of 272 days makes this planet the second longest-period confirmed planet identified in the TESS data to date (with the longest being TOI 4600c, Mireles et al 2023), and only one of five confirmed TESS planets with orbital periods longer than 100 days (Dalba et al 2022;Heitzmann et al 2023). Furthermore, the long orbital period and incident flux of ∼1.6 F ⊕ places it in the habitable zone of its host star, making it only the fourth habitable zone planet identified in the TESS data to date, following TOI 700 d (Gilbert et al 2020;Rodriguez et al 2020), TOI 700 e (Gilbert et al 2023), and TOI 715 b (Dransfield et al 2024).…”

Section: Introductionmentioning

confidence: 86%

Planet Hunters TESS. V. A Planetary System Around a Binary Star, Including a Mini-Neptune in the Habitable Zone

Eisner,

Grunblatt,

Barragán

et al. 2024

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We report on the discovery and validation of a transiting long-period mini-Neptune orbiting a bright (V = 9.0 mag) G dwarf (TOI 4633; R = 1.05 R ⊙, M = 1.10 M ⊙). The planet was identified in data from the Transiting Exoplanet Survey Satellite by citizen scientists taking part in the Planet Hunters TESS project. Modelling of the transit events yields an orbital period of 271.9445 ± 0.0040 days and radius of 3.2 ± 0.20 R ⊕. The Earth-like orbital period and an incident flux of 1.56 − 0.16 + 0.20 F ⊕ places it in the optimistic habitable zone around the star. Doppler spectroscopy of the system allowed us to place an upper mass limit on the transiting planet and revealed a non-transiting planet candidate in the system with a period of 34.15 ± 0.15 days. Furthermore, the combination of archival data dating back to 1905 with new high angular resolution imaging revealed a stellar companion orbiting the primary star with an orbital period of around 230 yr and an eccentricity of about 0.9. The long period of the transiting planet, combined with the high eccentricity and close approach of the companion star makes this a valuable system for testing the formation and stability of planets in binary systems.

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Section: Introductionmentioning

confidence: 86%

Planet Hunters TESS. V. A Planetary System Around a Binary Star, Including a Mini-Neptune in the Habitable Zone

Eisner,

Grunblatt,

Barragán

et al. 2024

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“…TOI-700 is an M2.5 dwarf star that hosts three planets discovered by TESS, with four planets (Kirkpatrick et al 1991;Gilbert et al 2020Gilbert et al , 2023Rodriguez et al 2020). Two of these planets, TOI-700 d and TOI-700 e, are Earth-sized planets in the habitable zone of the star (Gilbert et al 2020(Gilbert et al , 2023Rodriguez et al 2020). The SMs (S s , S c ) for this system are (103.0, 16.0).…”

Section: Appendix a A Simplified Expression Of Mass Concentration For...mentioning

confidence: 99%

Predicting the Dominant Formation Mechanism of Multiplanetary Systems

Shariat,

Hasegawa,

Hansen

et al. 2024

ApJL

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Most, if not all, Sun-like stars host one or more planets, making multiplanetary systems commonplace in our Galaxy. We utilize hundreds of multiplanet simulations to explore the origin of such systems, focusing on their orbital architecture. The first set of simulations assumes in situ assembly of planetary embryos, while the second explores planetary migration. After applying observational biases to the simulations, we compare them to 250+ observed multiplanetary systems, including 13 systems with planets in the habitable zone. For all of the systems, we calculate two of the so-called statistical measures: the mass concentration (S c ) and orbital spacing (S s ). After analytic and empirical analyses, we find that the measures are related to first order with a power law: S c ∼ S s β . The in situ systems exhibit steeper power-law relations relative to the migration systems. We show that different formation scenarios cover different regions in the S s –S c diagram with some overlap. Furthermore, we discover that observed systems with S s < 30 are likely dominated by the migration scenario, while those with S s ≥ 30 are likely dominated by the in situ scenario. We apply these criteria to determine that a majority (62%) of observed multiplanetary systems formed via migration, whereas most systems with currently observed habitable planets formed via in situ assembly. This work provides methods of leveraging the statistical measures (S s and S c ) to disentangle the formation history of observed multiplanetary systems based on their present-day architectures.

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“…In Table 5, we compare the TSM values between the TOI-2095 planets and other VZ planets that have equilibrium temperatures less than 400 K (TRAPPIST-1 d, TRAPPIST-1 c, TOI-237 b, and TOI-700 e; Gillon et al (2016), Waalkes et al (2021), Gilbert et al (2023)). Although six confirmed VZ planets with R p < 1.5R ⊕ have higher TSM values, the TOI-2095 planets offer observational advantages.…”

Section: Prospects For Atmospheric Characterizationmentioning

confidence: 99%

Two Warm Super-Earths Transiting the Nearby M Dwarf TOI-2095

Quintana,

Gilbert,

Barclay

et al. 2023

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We report the detection and validation of two planets orbiting TOI-2095 (TIC 235678745). The host star is a 3700 K M1V dwarf with a high proper motion. The star lies at a distance of 42 pc in a sparsely populated portion of the sky and is bright in the infrared (K = 9). With data from 24 sectors of observation during Cycles 2 and 4 of the Transiting Exoplanet Survey Satellite, TOI-2095 exhibits two sets of transits associated with super-Earth-sized planets. The planets have orbital periods of 17.7 days and 28.2 days and radii of 1.30 R ⊕ and 1.39 R ⊕, respectively. Archival data, preliminary follow-up observations, and vetting analyses support the planetary interpretation of the detected transit signals. The pair of planets have estimated equilibrium temperatures of approximately 400 K, with stellar insolations of 3.23 and 1.73 S ⊕, placing them in the Venus zone. The planets also lie in a radius regime signaling the transition between rock-dominated and volatile-rich compositions. They are thus prime targets for follow-up mass measurements to better understand the properties of warm, transition-radius planets. The relatively long orbital periods of these two planets provide crucial data that can help shed light on the processes that shape the composition of small planets orbiting M dwarfs.

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

Cited by 13 publications

References 85 publications

Planet Hunters TESS. V. A Planetary System Around a Binary Star, Including a Mini-Neptune in the Habitable Zone

Planet Hunters TESS. V. A Planetary System Around a Binary Star, Including a Mini-Neptune in the Habitable Zone

Predicting the Dominant Formation Mechanism of Multiplanetary Systems

Two Warm Super-Earths Transiting the Nearby M Dwarf TOI-2095

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