NEID Reveals That the Young Warm Neptune TOI-2076 b Has a Low Obliquity

Frazier, Robert C.; Stefánsson, Guðmundur; Mahadevan, Suvrath; Yee, Samuel W.; Cañas, Caleb I.; Winn, Joshua N.; Luhn, Jacob K.; Dai, Fei; Doyle, Lauren; Cegla, H. M.; Kanodia, Shubham; Robertson, Paul; Wisniewski, John P.; Bender, Chad F.; Dong, Jiayin; Gupta, Arvind F.; Halverson, Samuel; Hawley, Suzanne L.; Hebb, Leslie; Holcomb, Rae; Kowalski, Adam F.; Libby-Roberts, Jessica E.; Lin, Andrea S. J.; McElwain, Michael; Ninan, Joe P.; Petrovich, Cristóbal; Roy, Arpita; Schwab, Christian; Terrien, Ryan C.; Wright, Jason T.

doi:10.3847/2041-8213/acba18

Cited by 8 publications

(2 citation statements)

References 74 publications

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“…Interestingly, the few warm Neptunes that have their obliquities constrained around cool stars are observed to show a bifurcation of obliquities (see, e.g., Albrecht et al 2022;Stefànsson et al 2022) from well aligned (e.g., K2-25b; Stefansson et al 2020b) to close to polar (e.g., HAT-P-11b; Winn et al 2009;GJ 436b, Bourrier et al 2018;WASP-107b Rubenzahl et al 2021;GJ 3470b Stefànsson et al 2022). Further, there is a rising sample of compact multiplanet systems that tend to be well aligned (e.g., Albrecht et al 2022;Frazier et al 2023).…”

Section: Prospects For Rossiter-mclaughlin Observationsmentioning

confidence: 99%

TOI-2015 b: A Warm Neptune with Transit Timing Variations Orbiting an Active Mid-type M Dwarf

Jones,

Stefánsson,

Masuda

et al. 2024

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We report the discovery of a close-in (P orb = 3.349 days) warm Neptune with clear transit timing variations (TTVs) orbiting the nearby (d = 47.3 pc) active M4 star, TOI-2015. We characterize the planet's properties using Transiting Exoplanet Survey Satellite (TESS) photometry, precise near-infrared radial velocities (RVs) with the Habitable-zone Planet Finder Spectrograph, ground-based photometry, and high-contrast imaging. A joint photometry and RV fit yields a radius R p = 3.37 − 0.20 + 0.15 R ⊕ , mass m p = 16.4 − 4.1 + 4.1 M ⊕ , and density ρ p = 2.32 − 0.37 + 0.38 g cm − 3 for TOI-2015 b, suggesting a likely volatile-rich planet. The young, active host star has a rotation period of P rot = 8.7 ± 0.9 days and associated rotation-based age estimate of 1.1 ± 0.1 Gyr. Though no other transiting planets are seen in the TESS data, the system shows clear TTVs of super-period P sup ≈ 430 days and amplitude ∼100 minutes. After considering multiple likely period-ratio models, we show an outer planet candidate near a 2:1 resonance can explain the observed TTVs while offering a dynamically stable solution. However, other possible two-planet solutions—including 3:2 and 4:3 resonances—cannot be conclusively excluded without further observations. Assuming a 2:1 resonance in the joint TTV-RV modeling suggests a mass of m b = 13.3 − 4.5 + 4.7 M ⊕ for TOI-2015 b and m c = 6.8 − 2.3 + 3.5 M ⊕ for the outer candidate. Additional transit and RV observations will be beneficial to explicitly identify the resonance and further characterize the properties of the system.

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Section: Prospects For Rossiter-mclaughlin Observationsmentioning

confidence: 99%

TOI-2015 b: A Warm Neptune with Transit Timing Variations Orbiting an Active Mid-type M Dwarf

Jones,

Stefánsson,

Masuda

et al. 2024

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“…Both TOI-3984 A and TOI-5293 A have a measured rotation period (see Section 3.4), which allows for constraints on the 3D obliquity, ψ (e.g., Stefánsson et al 2022;Frazier et al 2023). A measurement of ψ for exoplanets across all spectral types has revealed that these planets do not span the full range of ψ but tend to be either polar or well aligned, which may be a remnant of formation and not due to tidal evolution (Albrecht et al 2021;Spalding & Winn 2022).…”

Section: Stellar Obliquitymentioning

confidence: 99%

TOI-3984 A b and TOI-5293 A b: Two Temperate Gas Giants Transiting Mid-M Dwarfs in Wide Binary Systems

Cañas

Kanodia

Libby-Roberts

et al. 2023

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We confirm the planetary nature of two gas giants discovered by TESS to transit M dwarfs with stellar companions at wide separations. TOI-3984 A (J = 11.93) is an M4 dwarf hosting a short-period (4.353326 ± 0.000005 days) gas giant (M p = 0.14 ± 0.03 M J and R p = 0.71 ± 0.02 R J) with a wide-separation white dwarf companion. TOI-5293 A (J = 12.47) is an M3 dwarf hosting a short-period (2.930289 ± 0.000004 days) gas giant (M p = 0.54 ± 0.07 M J and R p = 1.06 ± 0.04 R J) with a wide-separation M dwarf companion. We characterize both systems using a combination of ground- and space-based photometry, speckle imaging, and high-precision radial velocities from the Habitable-zone Planet Finder and NEID spectrographs. TOI-3984 A b (T eq = 563 ± 15 K and TSM = 138 − 27 + 29 ) and TOI-5293 A b ( T eq = 675 − 30 + 42 K and TSM = 92 ± 14) are two of the coolest gas giants among the population of hot Jupiter–sized gas planets orbiting M dwarfs and are favorable targets for atmospheric characterization of temperate gas giants and 3D obliquity measurements to probe system architecture and migration scenarios.

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Orbital obliquity of the young planet TOI-5398 b and the evolutionary history of the system

Mantovan,

Malavolta,

Locci

et al. 2024

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Multi-planet systems exhibit remarkable architectural diversity. However, short-period giant planets are typically isolated. Compact systems like TOI-5398, with an outer close-orbit giant and an inner small-size planet, are rare among systems containing short-period giants. TOI-5398’s unusual architecture coupled with its young age (650 pm 150 Myr) make it a promising system for measuring the original obliquity between the orbital axis of the giant and the stellar spin axis in order to gain insight into its formation and orbital migration. We collected in-transit (plus suitable off-transit) observations of TOI-5398 b with HARPS-N at TNG on March 25, 2023, obtaining high-precision radial velocity time series that allowed us to measure the Rossiter-McLaughlin (RM) effect. By modelling the RM effect, we obtained a sky-projected obliquity of $ $ deg for TOI-5398 b, consistent with the planet being aligned. With knowledge of the stellar rotation period, we estimated the true 3D obliquity, finding $ deg. Based on theoretical considerations, the orientation we measure is unaffected by tidal effects, offering a direct diagnostic for understanding the formation path of this planetary system. The orbital characteristics of TOI-5398, with its compact architecture, eccentricity consistent with circular orbits, and hints of orbital alignment, appear more compatible with the disc-driven migration scenario. TOI-5398, with its relative youth (compared with similar compact systems) and exceptional suitability for transmission spectroscopy studies, presents an outstanding opportunity to establish a benchmark for exploring the disc-driven migration model.

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NEID Reveals That the Young Warm Neptune TOI-2076 b Has a Low Obliquity

Cited by 8 publications

References 74 publications

TOI-2015 b: A Warm Neptune with Transit Timing Variations Orbiting an Active Mid-type M Dwarf

TOI-2015 b: A Warm Neptune with Transit Timing Variations Orbiting an Active Mid-type M Dwarf

TOI-3984 A b and TOI-5293 A b: Two Temperate Gas Giants Transiting Mid-M Dwarfs in Wide Binary Systems

Orbital obliquity of the young planet TOI-5398 b and the evolutionary history of the system

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