2022A&A...657A..45S


Query : 2022A&A...657A..45S

2022A&A...657A..45S - Astronomy and Astrophysics, volume 657A, 45-45 (2022/1-1)

TOI-2257 b: A highly eccentric long-period sub-Neptune transiting a nearby M dwarf.

SCHANCHE N., POZUELOS F.J., GUNTHER M.N., WELLS R.D., BURGASSER A.J., CHINCHILLA P., DELREZ L., DUCROT E., GARCIA L.J., GOMEZ MAQUEO CHEW Y., JOFRE E., RACKHAM B.V., SEBASTIAN D., STASSUN K.G., STERN D., TIMMERMANS M., BARKAOUI K., BELINSKI A., BENKHALDOUN Z., BENZ W., BIERYLA A., BOUCHY F., BURDANOV A., CHARBONNEAU D., CHRISTIANSEN J.L., COLLINS K.A., DEMORY B.-O., DEVORA-PAJARES M., DE WIT J., DRAGOMIR D., DRANSFIELD G., FURLAN E., GHACHOUI M., GILLON M., GNILKA C., GOMEZ-MUNOZ M.A., GUERRERO N., HARRIS M., HENG K., HENZE C.E., HESSE K., HOWELL S.B., JEHIN E., JENKINS J., JENSEN E.L.N., KUNIMOTO M., LATHAM D.W., LESTER K., McLEOD K.K., MIRELES I., MURRAY C.A., NIRAULA P., PEDERSEN P.P., QUELOZ D., QUINTANA E.V., RICKER G., RUDAT A., SABIN L., SAFONOV B., SCHROFFENEGGER U., SCOTT N., SEAGER S., STRAKHOV I., TRIAUD A.H.M.J., VANDERSPEK R., VEZIE M. and WINN J.

Abstract (from CDS):


Context. Thanks to the relative ease of finding and characterizing small planets around M-dwarf stars, these objects have become cornerstones in the field of exoplanet studies. The current paucity of planets in long-period orbits around M dwarfs makes such objects particularly compelling as they provide clues about the formation and evolution of these systems.
Aims. In this study we present the discovery of TOI-2257 b (TIC 198485881), a long-period (35 d) sub-Neptune orbiting an M3 star at 57.8 pc. Its transit depth is about 0.4%, large enough to be detected with medium-size, ground-based telescopes. The long transit duration suggests the planet is in a highly eccentric orbit (e ∼ 0.5), which would make it the most eccentric planet known to be transiting an M-dwarf star.
Methods. We combined TESS and ground-based data obtained with the 1.0-meter SAINT-EX, 0.60-meter TRAPPIST-North, and 1.2-meter FLWO telescopes to find a planetary size of 2.2 R and an orbital period of 35.19 days. In addition, we make use of archival data, high-resolution imaging, and vetting packages to support our planetary interpretation.
Results. With its long period and high eccentricity, TOI-2257 b falls into a novel slice of parameter space. Despite the planet's low equilibrium temperature (∼256 K), its host star's small size (R* = 0.311 ±0.015) and relative infrared brightness (Kmag = 10.7) make it a suitable candidate for atmospheric exploration via transmission spectroscopy.

Abstract Copyright: © ESO 2022

Journal keyword(s): planets and satellites: detection - stars: individual: TOI-2257 - stars: individual: TIC 198485881 - techniques: photometric

Simbad objects: 9

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Number of rows : 9
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 TOI-700d Pl 06 28 23.2287828000 -65 34 45.521569925           ~ 28 0
2 L 98-59 PM* 08 18 07.6214406393 -68 18 46.805365587   13.22 11.685 11.294   M3V 60 0
3 Ross 1003b Pl 11 41 44.6360191016 +42 45 07.104818145           ~ 22 1
4 TOI-2257b Pl? 12 58 57.6814372241 +77 39 41.689594968           ~ 4 0
5 UCAC4 839-012174 * 12 58 57.6814372241 +77 39 41.689594968   16.648 15.211 14.793   M3 1 0
6 Gaia DR2 1716345832871506560 * 12 59 01.2647240325 +77 39 53.423539229           ~ 1 0
7 HZ 44 HS* 13 23 35.2629445608 +36 07 59.544140304 10.186 11.42 11.65 12.00 11.995 sdBN0VIIHe28 402 0
8 Kepler-1652b Pl 19 37 27.832944 +49 54 54.21708           ~ 30 0
9 * 51 Peg b Pl 22 57 27.9804167474 +20 46 07.782240714           ~ 620 1

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2023.01.31-08:36:24

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