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TOI-132 b: A short-period planet in the Neptune desert transiting a V=11.3 G-type star

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Title: TOI-132 b: A short-period planet in the Neptune desert transiting a V=11.3 G-type star
Authors: Diaz, Matias R., Jenkins, James S., Gandolfi, Davide, Lopez, Eric D., Soto, Maritza G., Cortes-Zuleta, Pia, Berdinas, Zaira M., Stassun, Keivan G., Collins, Karen A., Vines, Ziegler, Carl, Fridlund, Malcolm, 1952, Jensen, Eric L. N., Murgas, Felipe, Santerne, Alexandre, Wilson, Paul A., Esposito, Massimiliano, Hatzes, Artie P., Johnson, Marshall C., Lam, Kristine W. F., Livingston, John H., Van Eylen, Vincent, Narita, Norio, Briceno, Cesar, Collins, Csizmadia, Szilard, Fausnaugh, Michael, Gan, Tianjun, Garcia, Rafael A., Georgieva, Iskra, 1987, Glidden, Ana, Gonzalez-Cuesta, Lucia, Jenkins, Jon M., Latham, David W., Law, Nicholas M., Mann, Andrew W., Mathur, Savita, Mireles, Ismael, Morris, Robert, Palle, Enric, Persson, Carina, 1964, Ricker, George, Rinehart, Stephen, Rose, Mark E., Seager, Sara, Smith, Jeffrey C., Tan, Thiam-Guan, Tokovinin, Andrei, Vanderburg, Andrew, Vanderspek, Roland, Winn, Joshua N., Yahalomi, Daniel A.
Source: Monthly Notices of the Royal Astronomical Society. 493(1):973-985
Subject Terms: planets and satellites: fundamental parameters, techniques: radial velocities, techniques: photometric, planetary systems
Description: The Neptune desert is a feature seen in the radius-period plane, whereby a notable dearth of short period, Neptune-like planets is found. Here, we report the Transiting Exoplanet Survey Satellite (TESS) discovery of a new short-period planet in the Neptune desert, orbiting the G-type dwarf TYC 8003-1117-1 (TOI-132). TESS photometry shows transit-like dips at the level of similar to 1400 ppm occurring every similar to 2.11 d. High-precision radial velocity follow-up with High Accuracy Radial Velocity Planet Searcher confirmed the planetary nature of the transit signal and provided a semi-amplitude radial velocity variation of 11.38(-0.85)(+0.84) m s(-1), which, when combined with the stellar mass of 0.97 +/- 0.06 M-circle dot, provides a planetary mass of 22.40(-1.92)(+1.90) M-circle plus. Modelling the TESS light curve returns a planet radius of 3.42(-0.14)(+0.13) R-circle plus , and therefore the planet bulk density is found to be 3.08(-0.46)(+0.44) g cm(-3). Planet structure models suggest that the bulk of the planet mass is in the form of a rocky core, with an atmospheric mass fraction of 4.3(-2.3)(+1.2) percent. TOI-132 b is a TESS Level 1 Science Requirement candidate, and therefore priority follow-up will allow the search for additional planets in the system, whilst helping to constrain low-mass planet formation and evolution models, particularly valuable for better understanding of the Neptune desert.
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  Data: The Neptune desert is a feature seen in the radius-period plane, whereby a notable dearth of short period, Neptune-like planets is found. Here, we report the Transiting Exoplanet Survey Satellite (TESS) discovery of a new short-period planet in the Neptune desert, orbiting the G-type dwarf TYC 8003-1117-1 (TOI-132). TESS photometry shows transit-like dips at the level of similar to 1400 ppm occurring every similar to 2.11 d. High-precision radial velocity follow-up with High Accuracy Radial Velocity Planet Searcher confirmed the planetary nature of the transit signal and provided a semi-amplitude radial velocity variation of 11.38(-0.85)(+0.84) m s(-1), which, when combined with the stellar mass of 0.97 +/- 0.06 M-circle dot, provides a planetary mass of 22.40(-1.92)(+1.90) M-circle plus. Modelling the TESS light curve returns a planet radius of 3.42(-0.14)(+0.13) R-circle plus , and therefore the planet bulk density is found to be 3.08(-0.46)(+0.44) g cm(-3). Planet structure models suggest that the bulk of the planet mass is in the form of a rocky core, with an atmospheric mass fraction of 4.3(-2.3)(+1.2) percent. TOI-132 b is a TESS Level 1 Science Requirement candidate, and therefore priority follow-up will allow the search for additional planets in the system, whilst helping to constrain low-mass planet formation and evolution models, particularly valuable for better understanding of the Neptune desert.
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