An ultrahot Neptune in the Neptune desert

James S. Jenkins; Matías R. Díaz; Nicolás T. Kurtovic; Néstor Espinoza; Jose I. Vines; Pablo A.Peña Rojas; Rafael Brahm; Pascal Torres; Pía Cortés-Zuleta; Maritza G. Soto; Eric D. Lopez; George W. King; Peter J. Wheatley; Joshua N. Winn; David R. Ciardi; George Ricker; Roland Vanderspek; David W. Latham; Sara Seager; Jon M. Jenkins; Charles A. Beichman; Allyson Bieryla; Christopher J. Burke; Jessie L. Christiansen; Christopher E. Henze; Todd C. Klaus; Sean McCauliff; Mayuko Mori; Norio Narita; Taku Nishiumi; Motohide Tamura; Jerome Pitogo de Leon; Samuel N. Quinn; Jesus Noel Villaseñor; Michael Vezie; Jack J. Lissauer; Karen A. Collins; Kevin I. Collins; Giovanni Isopi; Franco Mallia; Andrea Ercolino; Cristobal Petrovich; Andrés Jordán; Jack S. Acton; David J. Armstrong; Daniel Bayliss; François Bouchy; Claudia Belardi; Edward M. Bryant; Matthew R. Burleigh; Juan Cabrera; Sarah L. Casewell; Alexander Chaushev; Benjamin F. Cooke; Philipp Eigmüller; Anders Erikson; Emma Foxell; Boris T. Gänsicke; Samuel Gill; Edward Gillen; Maximilian N. Günther; Michael R. Goad; Matthew J. Hooton; James A.G. Jackman; Tom Louden; James McCormac; Maximiliano Moyano; Louise D. Nielsen; Don Pollacco; Didier Queloz; Heike Rauer; Liam Raynard; Alexis M.S. Smith; Rosanna H. Tilbrook; Ruth Titz-Weider; Oliver Turner; Stéphane Udry; Simon R. Walker; Christopher A. Watson; Richard G. West; Enric Palle; Carl Ziegler; Nicholas Law; Andrew W. Mann

doi:10.1038/s41550-020-1142-z

An ultrahot Neptune in the Neptune desert

James S. Jenkins, Matías R. Díaz, Nicolás T. Kurtovic, Néstor Espinoza, Jose I. Vines, Pablo A.Peña Rojas, Rafael Brahm, Pascal Torres, Pía Cortés-Zuleta, Maritza G. Soto, Eric D. Lopez, George W. King, Peter J. Wheatley, Joshua N. Winn, David R. Ciardi, George Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Jon M. JenkinsCharles A. Beichman, Allyson Bieryla, Christopher J. Burke, Jessie L. Christiansen, Christopher E. Henze, Todd C. Klaus, Sean McCauliff, Mayuko Mori, Norio Narita, Taku Nishiumi, Motohide Tamura, Jerome Pitogo de Leon, Samuel N. Quinn, Jesus Noel Villaseñor, Michael Vezie, Jack J. Lissauer, Karen A. Collins, Kevin I. Collins, Giovanni Isopi, Franco Mallia, Andrea Ercolino, Cristobal Petrovich, Andrés Jordán, Jack S. Acton, David J. Armstrong, Daniel Bayliss, François Bouchy, Claudia Belardi, Edward M. Bryant, Matthew R. Burleigh, Juan Cabrera, Sarah L. Casewell, Alexander Chaushev, Benjamin F. Cooke, Philipp Eigmüller, Anders Erikson, Emma Foxell, Boris T. Gänsicke, Samuel Gill, Edward Gillen, Maximilian N. Günther, Michael R. Goad, Matthew J. Hooton, James A.G. Jackman, Tom Louden, James McCormac, Maximiliano Moyano, Louise D. Nielsen, Don Pollacco, Didier Queloz, Heike Rauer, Liam Raynard, Alexis M.S. Smith, Rosanna H. Tilbrook, Ruth Titz-Weider, Oliver Turner, Stéphane Udry, Simon R. Walker, Christopher A. Watson, Richard G. West, Enric Palle, Carl Ziegler, Nicholas Law, Andrew W. Mann

Astrophysical Sciences

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28 Scopus citations

Abstract

About 1 out of 200 Sun-like stars has a planet with an orbital period shorter than one day: an ultrashort-period planet^1,2. All of the previously known ultrashort-period planets are either hot Jupiters, with sizes above 10 Earth radii (R_⊕), or apparently rocky planets smaller than 2 R_⊕. Such lack of planets of intermediate size (the ‘hot Neptune desert’) has been interpreted as the inability of low-mass planets to retain any hydrogen/helium (H/He) envelope in the face of strong stellar irradiation. Here we report the discovery of an ultrashort-period planet with a radius of 4.6 R_⊕ and a mass of 29 M_⊕, firmly in the hot Neptune desert. Data from the Transiting Exoplanet Survey Satellite³ revealed transits of the bright Sun-like star LTT 9779 every 0.79 days. The planet’s mean density is similar to that of Neptune, and according to thermal evolution models, it has a H/He-rich envelope constituting 9.0−2.9+2.7% of the total mass. With an equilibrium temperature around 2,000 K, it is unclear how this ‘ultrahot Neptune’ managed to retain such an envelope. Follow-up observations of the planet’s atmosphere to better understand its origin and physical nature will be facilitated by the star’s brightness (V_mag = 9.8).

Original language	English (US)
Pages (from-to)	1148-1157
Number of pages	10
Journal	Nature Astronomy
Volume	4
Issue number	12
DOIs	https://doi.org/10.1038/s41550-020-1142-z
State	Published - Dec 2020

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Astronomy and Astrophysics

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10.1038/s41550-020-1142-z

Cite this

Jenkins, J. S., Díaz, M. R., Kurtovic, N. T., Espinoza, N., Vines, J. I., Rojas, P. A. P., Brahm, R., Torres, P., Cortés-Zuleta, P., Soto, M. G., Lopez, E. D., King, G. W., Wheatley, P. J., Winn, J. N., Ciardi, D. R., Ricker, G., Vanderspek, R., Latham, D. W., Seager, S., ... Mann, A. W. (2020). An ultrahot Neptune in the Neptune desert. Nature Astronomy, 4(12), 1148-1157. https://doi.org/10.1038/s41550-020-1142-z

@article{08230b15b1104327a717e52719ad56dc,

title = "An ultrahot Neptune in the Neptune desert",

abstract = "About 1 out of 200 Sun-like stars has a planet with an orbital period shorter than one day: an ultrashort-period planet1,2. All of the previously known ultrashort-period planets are either hot Jupiters, with sizes above 10 Earth radii (R⊕), or apparently rocky planets smaller than 2 R⊕. Such lack of planets of intermediate size (the {\textquoteleft}hot Neptune desert{\textquoteright}) has been interpreted as the inability of low-mass planets to retain any hydrogen/helium (H/He) envelope in the face of strong stellar irradiation. Here we report the discovery of an ultrashort-period planet with a radius of 4.6 R⊕ and a mass of 29 M⊕, firmly in the hot Neptune desert. Data from the Transiting Exoplanet Survey Satellite3 revealed transits of the bright Sun-like star LTT 9779 every 0.79 days. The planet{\textquoteright}s mean density is similar to that of Neptune, and according to thermal evolution models, it has a H/He-rich envelope constituting 9.0−2.9+2.7% of the total mass. With an equilibrium temperature around 2,000 K, it is unclear how this {\textquoteleft}ultrahot Neptune{\textquoteright} managed to retain such an envelope. Follow-up observations of the planet{\textquoteright}s atmosphere to better understand its origin and physical nature will be facilitated by the star{\textquoteright}s brightness (Vmag = 9.8).",

author = "Jenkins, {James S.} and D{\'i}az, {Mat{\'i}as R.} and Kurtovic, {Nicol{\'a}s T.} and N{\'e}stor Espinoza and Vines, {Jose I.} and Rojas, {Pablo A.Pe{\~n}a} and Rafael Brahm and Pascal Torres and P{\'i}a Cort{\'e}s-Zuleta and Soto, {Maritza G.} and Lopez, {Eric D.} and King, {George W.} and Wheatley, {Peter J.} and Winn, {Joshua N.} and Ciardi, {David R.} and George Ricker and Roland Vanderspek and Latham, {David W.} and Sara Seager and Jenkins, {Jon M.} and Beichman, {Charles A.} and Allyson Bieryla and Burke, {Christopher J.} and Christiansen, {Jessie L.} and Henze, {Christopher E.} and Klaus, {Todd C.} and Sean McCauliff and Mayuko Mori and Norio Narita and Taku Nishiumi and Motohide Tamura and {de Leon}, {Jerome Pitogo} and Quinn, {Samuel N.} and Villase{\~n}or, {Jesus Noel} and Michael Vezie and Lissauer, {Jack J.} and Collins, {Karen A.} and Collins, {Kevin I.} and Giovanni Isopi and Franco Mallia and Andrea Ercolino and Cristobal Petrovich and Andr{\'e}s Jord{\'a}n and Acton, {Jack S.} and Armstrong, {David J.} and Daniel Bayliss and Fran{\c c}ois Bouchy and Claudia Belardi and Bryant, {Edward M.} and Burleigh, {Matthew R.} and Juan Cabrera and Casewell, {Sarah L.} and Alexander Chaushev and Cooke, {Benjamin F.} and Philipp Eigm{\"u}ller and Anders Erikson and Emma Foxell and G{\"a}nsicke, {Boris T.} and Samuel Gill and Edward Gillen and G{\"u}nther, {Maximilian N.} and Goad, {Michael R.} and Hooton, {Matthew J.} and Jackman, {James A.G.} and Tom Louden and James McCormac and Maximiliano Moyano and Nielsen, {Louise D.} and Don Pollacco and Didier Queloz and Heike Rauer and Liam Raynard and Smith, {Alexis M.S.} and Tilbrook, {Rosanna H.} and Ruth Titz-Weider and Oliver Turner and St{\'e}phane Udry and Walker, {Simon R.} and Watson, {Christopher A.} and West, {Richard G.} and Enric Palle and Carl Ziegler and Nicholas Law and Mann, {Andrew W.}",

note = "Funding Information: Funding for the TESS mission is provided by NASA{\textquoteright}s Science Mission directorate. We acknowledge the use of public TESS alert data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This research has made use of 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. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. J.S.J. and N.T. acknowledge support by FONDECYT grants 1161218 and 1201371, and partial support from CONICYT project Basal AFB-170002. M.R.D. is supported by CONICYT-PFCHA/Doctorado Nacional-21140646/Chile and Proyecto Basal AFB-170002. J.I.V. acknowledges support of CONICYT-PFCHA/Doctorado Nacional-21191829. This work was made possible owing to ESO Projects 0102.C-0525 (principal investigator, D{\'i}az) and 0102.C-0451 (principal investigator, Brahm). R.B. acknowledges support from FONDECYT Post-doctoral Fellowship Project 3180246. This work is partly supported by JSPS KAKENHI grant numbers JP18H01265 and JP18H05439, and JST PRESTO grant number JPMJPR1775. The IRSF project is a collaboration between Nagoya University and the South African Astronomical Observatory (SAAO) supported by the Grants-in-Aid for Scientific Research on Priority Areas (A) (numbers 10147207 and 10147214) and Optical and Near-Infrared Astronomy Inter-University Cooperation Program, from the Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan and the National Research Foundation (NRF) of South Africa. We thank A. Fukui, N. Kusakabe, K. Morihana, T. Nagata, T. Nagayama and the staff of SAAO for their kind support for IRSF SIRIUS observations and analyses. C.P. acknowledges support from the Gruber Foundation Fellowship and Jeffrey L. Bishop Fellowship. This research includes data collected under the NGTS project at the ESO La Silla Paranal Observatory. NGTS is funded by a consortium of institutes consisting of the University of Warwick, the University of Leicester, Queen{\textquoteright}s University Belfast, the University of Geneva, the Deutsches Zentrum f{\"u}r Luft-und Raumfahrt e.V. (DLR; under the {\textquoteleft}Gro{\ss}investition GI-NGTS{\textquoteright}), the University of Cambridge, together with the UK Science and Technology Facilities Council (STFC; project reference ST/M001962/1 and ST/S002642/1). P.J.W., D.B., B.T.G., S.G., T.L., D.P. and R.G.W. are supported by STFC consolidated grant ST/P000495/1. D.J.A. gratefully acknowledges support from the STFC via an Ernest Rutherford Fellowship (ST/R00384X/1). E.G. gratefully acknowledges support from the David and Claudia Harding Foundation in the form of a Winton Exoplanet Fellowship. M.J.H. acknowledges funding from the Northern Ireland Department for the Economy. M.T. is supported by JSPS KAKENHI (18H05442, 15H02063). A.J., R.B. and P.T. acknowledge support from FONDECYT project 1171208, and by the Ministry for the Economy, Development, and Tourism{\textquoteright}s Programa Iniciativa Cient{\'i}fica Milenio through grant IC 120009, awarded to the Millennium Institute of Astrophysics (MAS). P.E., A.C. and H.R. acknowledge the support of the DFG priority programme SPP 1992 {\textquoteleft}Exploring the Diversity of Extrasolar Planets{\textquoteright} (RA 714/13-1). We acknowledge the effort of A. Tokovinin in helping to perform the observations and reduction of the SOAR data. Publisher Copyright: {\textcopyright} 2020, The Author(s), under exclusive licence to Springer Nature Limited.",

year = "2020",

month = dec,

doi = "10.1038/s41550-020-1142-z",

language = "English (US)",

volume = "4",

pages = "1148--1157",

journal = "Nature Astronomy",

issn = "2397-3366",

publisher = "Nature Publishing Group",

number = "12",

}

Jenkins, JS, Díaz, MR, Kurtovic, NT, Espinoza, N, Vines, JI, Rojas, PAP, Brahm, R, Torres, P, Cortés-Zuleta, P, Soto, MG, Lopez, ED, King, GW, Wheatley, PJ, Winn, JN, Ciardi, DR, Ricker, G, Vanderspek, R, Latham, DW, Seager, S, Jenkins, JM, Beichman, CA, Bieryla, A, Burke, CJ, Christiansen, JL, Henze, CE, Klaus, TC, McCauliff, S, Mori, M, Narita, N, Nishiumi, T, Tamura, M, de Leon, JP, Quinn, SN, Villaseñor, JN, Vezie, M, Lissauer, JJ, Collins, KA, Collins, KI, Isopi, G, Mallia, F, Ercolino, A, Petrovich, C, Jordán, A, Acton, JS, Armstrong, DJ, Bayliss, D, Bouchy, F, Belardi, C, Bryant, EM, Burleigh, MR, Cabrera, J, Casewell, SL, Chaushev, A, Cooke, BF, Eigmüller, P, Erikson, A, Foxell, E, Gänsicke, BT, Gill, S, Gillen, E, Günther, MN, Goad, MR, Hooton, MJ, Jackman, JAG, Louden, T, McCormac, J, Moyano, M, Nielsen, LD, Pollacco, D, Queloz, D, Rauer, H, Raynard, L, Smith, AMS, Tilbrook, RH, Titz-Weider, R, Turner, O, Udry, S, Walker, SR, Watson, CA, West, RG, Palle, E, Ziegler, C, Law, N & Mann, AW 2020, 'An ultrahot Neptune in the Neptune desert', Nature Astronomy, vol. 4, no. 12, pp. 1148-1157. https://doi.org/10.1038/s41550-020-1142-z

TY - JOUR

T1 - An ultrahot Neptune in the Neptune desert

AU - Jenkins, James S.

AU - Díaz, Matías R.

AU - Kurtovic, Nicolás T.

AU - Espinoza, Néstor

AU - Vines, Jose I.

AU - Rojas, Pablo A.Peña

AU - Brahm, Rafael

AU - Torres, Pascal

AU - Cortés-Zuleta, Pía

AU - Soto, Maritza G.

AU - Lopez, Eric D.

AU - King, George W.

AU - Wheatley, Peter J.

AU - Winn, Joshua N.

AU - Ciardi, David R.

AU - Ricker, George

AU - Vanderspek, Roland

AU - Latham, David W.

AU - Seager, Sara

AU - Jenkins, Jon M.

AU - Beichman, Charles A.

AU - Bieryla, Allyson

AU - Burke, Christopher J.

AU - Christiansen, Jessie L.

AU - Henze, Christopher E.

AU - Klaus, Todd C.

AU - McCauliff, Sean

AU - Mori, Mayuko

AU - Narita, Norio

AU - Nishiumi, Taku

AU - Tamura, Motohide

AU - de Leon, Jerome Pitogo

AU - Quinn, Samuel N.

AU - Villaseñor, Jesus Noel

AU - Vezie, Michael

AU - Lissauer, Jack J.

AU - Collins, Karen A.

AU - Collins, Kevin I.

AU - Isopi, Giovanni

AU - Mallia, Franco

AU - Ercolino, Andrea

AU - Petrovich, Cristobal

AU - Jordán, Andrés

AU - Acton, Jack S.

AU - Armstrong, David J.

AU - Bayliss, Daniel

AU - Bouchy, François

AU - Belardi, Claudia

AU - Bryant, Edward M.

AU - Burleigh, Matthew R.

AU - Cabrera, Juan

AU - Casewell, Sarah L.

AU - Chaushev, Alexander

AU - Cooke, Benjamin F.

AU - Eigmüller, Philipp

AU - Erikson, Anders

AU - Foxell, Emma

AU - Gänsicke, Boris T.

AU - Gill, Samuel

AU - Gillen, Edward

AU - Günther, Maximilian N.

AU - Goad, Michael R.

AU - Hooton, Matthew J.

AU - Jackman, James A.G.

AU - Louden, Tom

AU - McCormac, James

AU - Moyano, Maximiliano

AU - Nielsen, Louise D.

AU - Pollacco, Don

AU - Queloz, Didier

AU - Rauer, Heike

AU - Raynard, Liam

AU - Smith, Alexis M.S.

AU - Tilbrook, Rosanna H.

AU - Titz-Weider, Ruth

AU - Turner, Oliver

AU - Udry, Stéphane

AU - Walker, Simon R.

AU - Watson, Christopher A.

AU - West, Richard G.

AU - Palle, Enric

AU - Ziegler, Carl

AU - Law, Nicholas

AU - Mann, Andrew W.

N1 - Funding Information: Funding for the TESS mission is provided by NASA’s Science Mission directorate. We acknowledge the use of public TESS alert data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This research has made use of 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. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. J.S.J. and N.T. acknowledge support by FONDECYT grants 1161218 and 1201371, and partial support from CONICYT project Basal AFB-170002. M.R.D. is supported by CONICYT-PFCHA/Doctorado Nacional-21140646/Chile and Proyecto Basal AFB-170002. J.I.V. acknowledges support of CONICYT-PFCHA/Doctorado Nacional-21191829. This work was made possible owing to ESO Projects 0102.C-0525 (principal investigator, Díaz) and 0102.C-0451 (principal investigator, Brahm). R.B. acknowledges support from FONDECYT Post-doctoral Fellowship Project 3180246. This work is partly supported by JSPS KAKENHI grant numbers JP18H01265 and JP18H05439, and JST PRESTO grant number JPMJPR1775. The IRSF project is a collaboration between Nagoya University and the South African Astronomical Observatory (SAAO) supported by the Grants-in-Aid for Scientific Research on Priority Areas (A) (numbers 10147207 and 10147214) and Optical and Near-Infrared Astronomy Inter-University Cooperation Program, from the Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan and the National Research Foundation (NRF) of South Africa. We thank A. Fukui, N. Kusakabe, K. Morihana, T. Nagata, T. Nagayama and the staff of SAAO for their kind support for IRSF SIRIUS observations and analyses. C.P. acknowledges support from the Gruber Foundation Fellowship and Jeffrey L. Bishop Fellowship. This research includes data collected under the NGTS project at the ESO La Silla Paranal Observatory. NGTS is funded by a consortium of institutes consisting of the University of Warwick, the University of Leicester, Queen’s University Belfast, the University of Geneva, the Deutsches Zentrum für Luft-und Raumfahrt e.V. (DLR; under the ‘Großinvestition GI-NGTS’), the University of Cambridge, together with the UK Science and Technology Facilities Council (STFC; project reference ST/M001962/1 and ST/S002642/1). P.J.W., D.B., B.T.G., S.G., T.L., D.P. and R.G.W. are supported by STFC consolidated grant ST/P000495/1. D.J.A. gratefully acknowledges support from the STFC via an Ernest Rutherford Fellowship (ST/R00384X/1). E.G. gratefully acknowledges support from the David and Claudia Harding Foundation in the form of a Winton Exoplanet Fellowship. M.J.H. acknowledges funding from the Northern Ireland Department for the Economy. M.T. is supported by JSPS KAKENHI (18H05442, 15H02063). A.J., R.B. and P.T. acknowledge support from FONDECYT project 1171208, and by the Ministry for the Economy, Development, and Tourism’s Programa Iniciativa Científica Milenio through grant IC 120009, awarded to the Millennium Institute of Astrophysics (MAS). P.E., A.C. and H.R. acknowledge the support of the DFG priority programme SPP 1992 ‘Exploring the Diversity of Extrasolar Planets’ (RA 714/13-1). We acknowledge the effort of A. Tokovinin in helping to perform the observations and reduction of the SOAR data. Publisher Copyright: © 2020, The Author(s), under exclusive licence to Springer Nature Limited.

PY - 2020/12

Y1 - 2020/12

N2 - About 1 out of 200 Sun-like stars has a planet with an orbital period shorter than one day: an ultrashort-period planet1,2. All of the previously known ultrashort-period planets are either hot Jupiters, with sizes above 10 Earth radii (R⊕), or apparently rocky planets smaller than 2 R⊕. Such lack of planets of intermediate size (the ‘hot Neptune desert’) has been interpreted as the inability of low-mass planets to retain any hydrogen/helium (H/He) envelope in the face of strong stellar irradiation. Here we report the discovery of an ultrashort-period planet with a radius of 4.6 R⊕ and a mass of 29 M⊕, firmly in the hot Neptune desert. Data from the Transiting Exoplanet Survey Satellite3 revealed transits of the bright Sun-like star LTT 9779 every 0.79 days. The planet’s mean density is similar to that of Neptune, and according to thermal evolution models, it has a H/He-rich envelope constituting 9.0−2.9+2.7% of the total mass. With an equilibrium temperature around 2,000 K, it is unclear how this ‘ultrahot Neptune’ managed to retain such an envelope. Follow-up observations of the planet’s atmosphere to better understand its origin and physical nature will be facilitated by the star’s brightness (Vmag = 9.8).

AB - About 1 out of 200 Sun-like stars has a planet with an orbital period shorter than one day: an ultrashort-period planet1,2. All of the previously known ultrashort-period planets are either hot Jupiters, with sizes above 10 Earth radii (R⊕), or apparently rocky planets smaller than 2 R⊕. Such lack of planets of intermediate size (the ‘hot Neptune desert’) has been interpreted as the inability of low-mass planets to retain any hydrogen/helium (H/He) envelope in the face of strong stellar irradiation. Here we report the discovery of an ultrashort-period planet with a radius of 4.6 R⊕ and a mass of 29 M⊕, firmly in the hot Neptune desert. Data from the Transiting Exoplanet Survey Satellite3 revealed transits of the bright Sun-like star LTT 9779 every 0.79 days. The planet’s mean density is similar to that of Neptune, and according to thermal evolution models, it has a H/He-rich envelope constituting 9.0−2.9+2.7% of the total mass. With an equilibrium temperature around 2,000 K, it is unclear how this ‘ultrahot Neptune’ managed to retain such an envelope. Follow-up observations of the planet’s atmosphere to better understand its origin and physical nature will be facilitated by the star’s brightness (Vmag = 9.8).

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U2 - 10.1038/s41550-020-1142-z

DO - 10.1038/s41550-020-1142-z

M3 - Article

AN - SCOPUS:85091611527

SN - 2397-3366

VL - 4

SP - 1148

EP - 1157

JO - Nature Astronomy

JF - Nature Astronomy

IS - 12

ER -

An ultrahot Neptune in the Neptune desert

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