TESS Reveals a Short-period Sub-Neptune Sibling (HD 86226c) to a Known Long-period Giant Planet

• Published in: arXiv.org 2020-07
• Main Authors: Teske, Johanna, Díaz, Matías R, Luque, Rafael, Teo Močnik, Seidel, Julia V, Jon Fernández Otegi, Fabo Feng, Jenkins, James S, Pallè, Enric, Ségransan, Damien, Udry, Stèphane, Collins, Karen A, Eastman, Jason D, Ricker, George R, Vanderspek, Roland, Latham, David W, Seager, Sara, Winn, Joshua N, Jenkins, Jon M, Anderson, David R, Barclay, Thomas, Bouchy, François, Burt, Jennifer A, Butler, R Paul, Caldwell, Douglas A, Collins, Kevin I, Crane, Jeffrey D, Dorn, Caroline, Flowers, Erin, Haldemann, Jonas, Helled, Ravit, Hellier, Coel, Jensen, Eric L N, Kane, Stephen R, Law, Nicholas, Lissauer, Jack J, Mann, Andrew W, Marmier, Maxime, Nielsen, Louise Dyregaard, Rose, Mark E, Shectman, Stephen A, Shporer, Avi, Torres, Guillermo, Wang, Sharon X, Wolfgang, Angie, Wong, Ian, Ziegler, Carl
• Format: Article
• Language: English
• Subjects: Extrasolar planets; Gas giant planets; Jupiter; Planet detection; Radial velocity; Transit
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.2007.13927

The Transiting Exoplanet Survey Satellite mission was designed to find transiting planets around bright, nearby stars. Here we present the detection and mass measurement of a small, short-period (\(\approx\,4\)\,days) transiting planet around the bright (\(V=7.9\)), solar-type star HD 86226 (TOI-652, TIC 22221375), previously known to host a long-period (\(\sim\)1600 days) giant planet. HD 86226c (TOI-652.01) has a radius of \(2.16\pm0.08\) \(R_{\oplus}\) and a mass of 7.25\(^{+1.19}_{-1.12}\) \(M_{\oplus}\) based on archival and new radial velocity data. We also update the parameters of the longer-period, not-known-to-transit planet, and find it to be less eccentric and less massive than previously reported. The density of the transiting planet is \(3.97\) g cm\(^{-3}\), which is low enough to suggest that the planet has at least a small volatile envelope, but the mass fractions of rock, iron, and water are not well-constrained. Given the host star brightness, planet period, and location of the planet near both the ``radius gap'' and the ``hot Neptune desert'', HD 86226c is an interesting candidate for transmission spectroscopy to further refine its composition.