Publisher Correction: A planet within the debris disk around the pre-main-sequence star AU Microscopii

Plavchan, Peter; Barclay, Thomas; Gagné, Jonathan; Cale, Bryson; Matzko, William; Dragomir, Diana; Quinn, S. N.; Feliz, Dax L.; Stassun, Keivan G.; Crossfield, Ian J. M.; Berardo, David; Latham, David W.; Tieu, Ben; Anglada‐Escudé, G.; Ricker, G.; Vanderspek, R.; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Rinehart, Stephen A.; Krishnamurthy, Akshata; Dynes, Scott; Doty, J.; Adams, Fred C.; Afanasev, Dennis; Beichman, C. A.; Bottom, Michael; Bowler, Brendan P.; Brinkworth, Carolyn; Brown, Carolyn J.; Cancino, Andrew; Ciardi, David R.; Clampin, Mark; Clark, Jake T.; Collins, Karen A.; Davison, C.; Foreman-Mackey, Daniel; Furlan, Elise; Gaidos, Eric; Geneser, Claire; Giddens, Frank; Gilbert, Emily A.; Hall, Ryan; Hellier, C.; Henry, Todd J.; Horner, Jonathan; Howard, Andrew W.; Huang, Chelsea X.; Huber, J.; Kane, Stephen R.; Kenworthy, Matthew A.; Kielkopf, John F.; Kipping, David; Klenke, Chris; Kruse, Ethan; Latouf, Natasha; Lowrance, P.; Mennesson, Bertrand; Mengel, M. W.; Mills, Sean M.; Morton, Tim; Narita, Norio; Newton, Elisabeth R.; Nishimoto, America; Okumura, Jack; Πάλλη, Ε.; Pepper, Joshua; Quintana, Elisa V.; Roberge, Aki; Roccatagliata, V.; Schlieder, Joshua E.; Tanner, Angelle; Teske, Johanna; Tinney, C. G.; Vanderburg, Andrew; Braun, Kaspar von; Walp, Bernie; Wang, Jason; Wang, Sharon Xuesong; Weigand, Denise; White, R. J.; Wittenmyer, Robert A.; Wright, D. E.; Youngblood, Allison; Zhang, Hui; Zilberman, P.

doi:10.1038/s41586-020-2516-1

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“…The discovery of a young multiplanet system can be especially valuable for improving our understanding of exoplanet formation and evolution, both the demographics of the exoplanet architectures, and the atmospheric evolution as a function of stellar age, orbital period, and host star spectral type (Marchwinski et al 2015;Fulton et al 2017;Newton et al 2019;Hirano et al 2020;Carolan et al 2020;Benatti et al 2021;Alvarado-Gomez et al 2022;Cohen et al 2022;Feinstein et al 2022a;Flagg et al 2022;Ilin & Poppenhaeger 2022;Klein et al 2022). We know that the orbital properties of planets change over time as shown by the existence of hot Jupiters; we also see evidence for orbital distance dependent mass loss via photoevaporation, which may be responsible for producing the planetradius gap and may impact our understanding of the occurrence rate of terrestrial planets at larger orbital separations (Pascucci et al 2019;Mann et al 2020;Plavchan et al 2020;Klein et al 2021). Therefore, we would benefit from examining the orbital architecture and atmospheric properties of multiplanetary systems over a wide range of evolutionary phases.…”

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confidence: 96%

TOI 560: Two Transiting Planets Orbiting a K Dwarf Validated with iSHELL, PFS, and HIRES RVs

Mufti

Plavchan

Isaacson

et al. 2022

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We validate the presence of a two-planet system orbiting the 0.15–1.4 Gyr K4 dwarf TOI 560 (HD 73583). The system consists of an inner moderately eccentric transiting mini-Neptune (TOI 560 b, P = 6.3980661 − 0.0000097 + 0.0000095 days, e = 0.294 − 0.062 + 0.13 , M = 0.94 − 0.23 + 0.31 M Nep ) initially discovered in the Sector 8 Transiting Exoplanet Survey Satellite (TESS) mission observations, and a transiting mini-Neptune (TOI 560 c, P = 18.8805 − 0.0011 + 0.0024 days, M = 1.32 − 0.32 + 0.29 M Nep ) discovered in the Sector 34 observations, in a rare near-1:3 orbital resonance. We utilize photometric data from TESS Spitzer, and ground-based follow-up observations to confirm the ephemerides and period of the transiting planets, vet false-positive scenarios, and detect the photoeccentric effect for TOI 560 b. We obtain follow-up spectroscopy and corresponding precise radial velocities (RVs) with the iSHELL spectrograph at the NASA Infrared Telescope Facility and the HIRES Spectrograph at Keck Observatory to validate the planetary nature of these signals, which we combine with published Planet Finder Spectrograph RVs from the Magellan Observatory. We detect the masses of both planets at >3σ significance. We apply a Gaussian process (GP) model to the TESS light curves to place priors on a chromatic RV GP model to constrain the stellar activity of the TOI 560 host star, and confirm a strong wavelength dependence for the stellar activity demonstrating the ability of near-IR RVs to mitigate stellar activity for young K dwarfs. TOI 560 is a nearby moderately young multiplanet system with two planets suitable for atmospheric characterization with the James Webb Space Telescope and other upcoming missions. In particular, it will undergo six transit pairs separated by <6 hr before 2027 June.

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