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A super-Earth and two sub-Neptunes transiting the nearby and quiet M dwarf TOI-270

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Gunther_2019_NA_TOI_270_AAM.pdf (3.843Mb)
Date
29/07/2019
Author
Günther, Maximilian N.
Pozuelos, Francisco J.
Dittmann, Jason A.
Dragomir, Diana
Kane, Stephen R.
Daylan, Tansu
Feinstein, Adina D.
Huang, Chelsea X.
Morton, Timothy D.
Bonfanti, Andrea
Bouma, L. G.
Burt, Jennifer
Collins, Karen A.
Lissauer, Jack J.
Matthews, Elisabeth
Montet, Benjamin T.
Vanderburg, Andrew
Wang, Songhu
Winters, Jennifer G.
Ricker, George R.
Vanderspek, Roland K.
Latham, David W.
Seager, Sara
Winn, Joshua N.
Jenkins, Jon M.
Armstrong, James D.
Barkaoui, Khalid
Batalha, Natalie
Bean, Jacob L.
Caldwell, Douglas A.
Ciardi, David R.
Collins, Kevin I.
Crossfield, Ian
Fausnaugh, Michael
Furesz, Gabor
Gan, Tianjun
Gillon, Michaël
Guerrero, Natalia
Horne, Keith
Howell, Steve B.
Ireland, Michael
Isopi, Giovanni
Jehin, Emmanuël
Kielkopf, John F.
Lepine, Sebastien
Mallia, Franco
Matson, Rachel A.
Myers, Gordon
Palle, Enric
Quinn, Samuel N.
Relles, Howard M.
Rojas-Ayala, Bárbara
Schlieder, Joshua
Sefako, Ramotholo
Shporer, Avi
Suárez, Juan C.
Tan, Thiam-Guan
Ting, Eric B.
Twicken, Joseph D.
Waite, Ian A.
Keywords
QB Astronomy
3rd-DAS
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Abstract
One of the primary goals of exoplanetary science is to detect small, temperate planets passing (transiting) in front of bright and quiet host stars. This enables the characterization of planetary sizes, orbits, bulk compositions, atmospheres and formation histories. These studies are facilitated by small and cool M dwarf host stars. Here we report the Transiting Exoplanet Survey Satellite (TESS)1 discovery of three small planets transiting one of the nearest and brightest M dwarf hosts observed to date, TOI-270 (TIC 259377017, with K-magnitude 8.3, and 22.5 parsecs away from Earth). The M3V-type star is transited by the super-Earth-sized planet TOI-270 b (1.247+0.089−0.083 R⊕) and the sub-Neptune-sized planets TOI-270 c (2.42 ± 0.13 R⊕) and TOI-270 d (2.13 ± 0.12 R⊕). The planets orbit close to a mean-motion resonant chain, with periods (3.36 days, 5.66 days and 11.38 days, respectively) near ratios of small integers (5:3 and 2:1). TOI-270 is a prime target for future studies because (1) its near-resonance allows the detection of transit timing variations, enabling precise mass measurements and dynamical studies; (2) its brightness enables independent radial-velocity mass measurements; (3) the outer planets are ideal for atmospheric characterization via transmission spectroscopy; and (4) the quietness of the star enables future searches for habitable zone planets. Altogether, very few systems with small, temperate exoplanets are as suitable for such complementary and detailed characterization as TOI-270.
Citation
Günther , M N , Pozuelos , F J , Dittmann , J A , Dragomir , D , Kane , S R , Daylan , T , Feinstein , A D , Huang , C X , Morton , T D , Bonfanti , A , Bouma , L G , Burt , J , Collins , K A , Lissauer , J J , Matthews , E , Montet , B T , Vanderburg , A , Wang , S , Winters , J G , Ricker , G R , Vanderspek , R K , Latham , D W , Seager , S , Winn , J N , Jenkins , J M , Armstrong , J D , Barkaoui , K , Batalha , N , Bean , J L , Caldwell , D A , Ciardi , D R , Collins , K I , Crossfield , I , Fausnaugh , M , Furesz , G , Gan , T , Gillon , M , Guerrero , N , Horne , K , Howell , S B , Ireland , M , Isopi , G , Jehin , E , Kielkopf , J F , Lepine , S , Mallia , F , Matson , R A , Myers , G , Palle , E , Quinn , S N , Relles , H M , Rojas-Ayala , B , Schlieder , J , Sefako , R , Shporer , A , Suárez , J C , Tan , T-G , Ting , E B , Twicken , J D & Waite , I A 2019 , ' A super-Earth and two sub-Neptunes transiting the nearby and quiet M dwarf TOI-270 ' , Nature Astronomy . https://doi.org/10.1038/s41550-019-0845-5
Publication
Nature Astronomy
Status
Peer reviewed
DOI
https://doi.org/10.1038/s41550-019-0845-5
ISSN
2397-3366
Type
Journal article
Rights
Copyright © The Author(s), under exclusive licence to Springer Nature Limited 2019. This work has been made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.1038/s41550-019-0845-5
Description
K.H. acknowledges support from STFC grant ST/R000824/1.
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  • University of St Andrews Research
URL
https://arxiv.org/abs/1903.06107
URI
http://hdl.handle.net/10023/19356

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