@article{8ff37787102a49f7ae364be9f6398c70,
title = "TOI-132 b: A short-period planet in the Neptune desert transiting a v = 11.3 G-type star",
abstract = "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 TYC8003-1117-1 (TOI-132). TESS photometry shows transit-like dips at the level of ∼1400 ppm occurring every ∼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+0.84-0.85 ms-1, which, when combined with the stellar mass of 0.97 ± 0.06 M⊙, provides a planetary mass of 22.40+1.90-1.92 M⊕. Modelling the TESS light curve returns a planet radius of 3.42+0.13-0.14 R⊕, and therefore the planet bulk density is found to be 3.08+0.44-0.46 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+1.2-2.3 per cent. 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.",
keywords = "Planetary systems, Planets and satellites: fundamental parameters, Techniques: photometric, Techniques: radial velocities",
author = "D{\'i}az, {Mat{\'i}as R.} and Jenkins, {James S.} and Davide Gandolfi and Lopez, {Eric D.} and Soto, {Maritza G.} and P{\'i}a Cort{\'e}s-Zuleta and Berdi{\~n}as, {Zaira M.} and Stassun, {Keivan G.} and Collins, {Karen A.} and Vines, {Jos{\'e} I.} and Carl Ziegler and Malcom Fridlund and Jensen, {Eric L.N.} and Felipe Murgas and Alexandre Santerne and Wilson, {Paul A.} and Massimiliano Esposito and Hatzes, {Artie P.} and Johnson, {Marshall C.} and Lam, {Kristine W.F.} and Livingston, {John H.} and {Van Eylen}, Vincent and Norio Narita and Cesar Brice{\~n}o and Collins, {Kevin I.} and Szil{\'a}rd Csizmadia and Michael Fausnaugh and Tianjun Gan and Garc{\'i}a, {Rafael A.} and Iska Georgieva and Ana Glidden and Luc{\'i}a Gonz{\'a}lez-Cuesta and Jenkins, {Jon M.} and Latham, {David W.} and Law, {Nicholas M.} and Mann, {Andrew W.} and Savita Mathur and Ismael Mireles and Robert Morris and Enric Pall{\'e} and Persson, {Carina M.} and George Ricker and Stephen Rinehart and Rose, {Mark E.} and Sara Seager and Smith, {Jeffrey C.} and Tan, {Thiam Guan} and Andrei Tokovinin and Andrew Vanderburg and Roland Vanderspek and Winn, {Joshua N.} and Yahalomi, {Daniel A.}",
note = "Funding Information: MRD acknowledges support of CONICYT-PFCHA/Doctorado Nacional-21140646 and Proyecto Basal AFB-170002. JSJ is supported by FONDECYT grant 1161218 and partial support from CATA-Basal (PB06, CONICYT). ZMB acknowledges funds from CONICYT-FONDECYT/Chile Postdoctorado 3180405. JIV acknowledges support of CONICYT- PFCHA/Doctorado Nacional-21191829, Chile. ME acknowledges the support of the DFG priority program SPP 1992 'Exploring the Diversity of Extrasolar Planets' (HA 3279/12-1). KWFL, SzCs acknowledge support by DFG grant RA 714/14-1 within the DFG Schwerpunkt SPP 1992, 'Exploring the Diversity of Extrasolar Planets'. LGC acknowledges support from the MINECO FPI-SO doctoral research project SEV-2015-0548-17-2 and predoctoral contract BES-2017-082610. SM acknowledges support from the Spanish Ministry under the Ramon y Cajal fellowship number RYC-2015-17697. NN acknowledges support by JSPS KAKENHI grant JP18H01265 and JP18H05439, and JST PRESTO grant JPMJPR1775. AS acknowledges financial support from the French Programme National de Plan{\'e}tologie (PNP, INSU). Funding for the TESS mission is provided by NASA's Science Mission directorate. We acknowledge the use of TESS Alert data, from pipelines at the TESS Science Office and at the TESS SPOC. Resources supporting this work were provided by the NASA High-End Computing Program through the NASA Advanced Supercomputing Division at Ames Research Center for the production of the SPOC data products. This research has used the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This work uses observations from the LCOGT network. Funding Information: MRD acknowledges support of CONICYT-PFCHA/Doctorado Nacional-21140646 and Proyecto Basal AFB-170002. JSJ is supported by FONDECYT grant 1161218 and partial support from CATA-Basal (PB06, CONICYT). ZMB acknowledges funds from CONICYT-FONDECYT/Chile Postdoctorado 3180405. JIV acknowledges support of CONICYT-PFCHA/Doctorado Nacional-21191829, Chile. ME acknowledges the support of the DFG priority program SPP 1992 {\textquoteleft}Exploring the Diversity of Extrasolar Planets{\textquoteright} (HA 3279/12-1). KWFL, SzCs acknowledge support by DFG grant RA 714/14-1 within the DFG Schwerpunkt SPP 1992, {\textquoteleft}Exploring the Diversity of Extrasolar Planets{\textquoteright}. LGC acknowledges support from the MINECO FPI-SO doctoral research project SEV- 2015-0548-17-2 and predoctoral contract BES-2017-082610. SM acknowledges support from the Spanish Ministry under the Ramon y Cajal fellowship number RYC-2015-17697. NN acknowledges support by JSPS KAKENHI grant JP18H01265 and JP18H05439, and JST PRESTO grant JPMJPR1775. AS acknowledges financial support from the French Programme National de Plan{\'e}tologie (PNP, INSU). Funding for the TESS mission is provided by NASA{\textquoteright}s Science Mission directorate. We acknowledge the use of TESS Alert data, from pipelines at the TESS Science Office and at the TESS SPOC. Resources supporting this work were provided by the NASA High-End Computing Program through the NASA Advanced Supercomputing Division at Ames Research Center for the production of the SPOC data products. This research has used the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This work uses observations from the LCOGT network. Publisher Copyright: {\textcopyright} 2020 The Author(s).",
year = "2020",
month = mar,
day = "1",
doi = "10.1093/mnras/staa277",
language = "English (US)",
volume = "493",
pages = "973--985",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "1",
}