The TESS-Keck Survey. VII. A Superdense Sub-Neptune Orbiting TOI-1824
Article
Article Title | The TESS-Keck Survey. VII. A Superdense Sub-Neptune Orbiting TOI-1824 |
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ERA Journal ID | 1048 |
Article Category | Article |
Authors | Lange, Sarah, Akana Murphy, Joseph M., Batalha, Natalie M., Crossfield, Ian J. M., Dressing, Courtney D., Fulton, Benjamin, Howard, Andrew W., Huber, Daniel, Isaacson, Howard, Kane, Stephen R., Petigura, Erik A., Robertson, Paul, Weiss, Lauren M., Behmard, Aida, Beard, Corey, Blunt, Sarah, Brinkman, Casey L., Chontos, Ashley, Dai, Fei, Dalba, Paul A., Fetherolf, Tara, Giacalone, Steven, Hill, Michelle L., Holcomb, Rae, Lubin, Jack, MacDougall, Mason G., Mayo, Andrew W., Mocnik, Teo, Pidhorodetska, Daria, Polanski, Alex S., Rice, Malena, Rosenthal, Lee J., Rubenzahl, Ryan A., Scarsdale, Nicholas, Turtelboom, Emma V., Van Zandt, Judah, Ciardi, David R. and Boyle, Andrew W. |
Journal Title | The Astronomical Journal |
Journal Citation | 167 (6) |
Article Number | 282 |
Number of Pages | 21 |
Year | 2024 |
Publisher | IOP Publishing |
Place of Publication | United States |
ISSN | 0004-6256 |
1538-3881 | |
Digital Object Identifier (DOI) | https://doi.org/10.3847/1538-3881/ad34d9 |
Web Address (URL) | https://iopscience.iop.org/article/10.3847/1538-3881/ad34d9 |
Abstract | We confirm a massive sub-Neptune-sized planet on a P = 22.8 days orbit around the star TOI-1824 (Teff = 5200 K, V = 9.7 mag). TESS first identified TOI-1824 b (formerly TOI-1824.01) as an object of interest in 2020 April after two transits in Sector 22 were matched with a single transit in Sector 21. TOI-1824 was subsequently targeted for ground-based Doppler monitoring with Keck-HIRES and APF-Levy. Using a joint model of the TESS photometry, radial velocities, and Ca ii H and K emission measurements as an activity indicator, we find that TOI-1824 b is an unusually dense sub-Neptune. The planet has a radius Rp = 2.63 ± 0.15 R⊕ and mass Mp = 18.5 ± 3.2 M⊕, implying a bulk density of 5.6 ± 1.4 g cm−3. TOI-1824 b's mass and radius situate it near a small group of "superdense sub-Neptunes" (Rp ≲ 3 R⊕ and Mp ≳ 20 M⊕). While the formation mechanism of superdense sub-Neptunes is a mystery, one possible explanation is the constructive collision of primordial icy cores; such giant impacts would drive atmospheric escape and could help explain these planets' apparent lack of massive envelopes. We discuss TOI-1824 b in the context of these overdense planets, whose unique location in the exoplanet mass–radius plane make them a potentially valuable tracer of planet formation. |
Keywords | Radial velocity; Transit photometry; Exoplanets |
Contains Sensitive Content | Does not contain sensitive content |
ANZSRC Field of Research 2020 | 5101. Astronomical sciences |
Byline Affiliations | University of California Santa Cruz, United States |
University of Kansas, United States | |
University of California Berkeley, United States | |
NASA Exoplanet Science Institute, United States | |
California Institute of Technology (Caltech), United States | |
University of Hawaii, United States | |
University of Sydney | |
Centre for Astrophysics | |
University of California Riverside, United Sates | |
University of California Los Angeles, United States | |
University of California Irvine, United States | |
University of Notre Dame, United States | |
American Museum of Natural History, United States | |
Northwestern University, United States | |
Princeton University, United States | |
Division of Geological and Planetary Sciences, United States | |
California State University San Marcos, United States | |
Gemini Observatory, United States | |
NSF's National Optical Infrared Astronomy Research Laboratory (NOIRLab), United States | |
University of Kansas, United States | |
Yale University, United States |
https://research.usq.edu.au/item/z8512/the-tess-keck-survey-vii-a-superdense-sub-neptune-orbiting-toi-1824
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