2021A&A...650A.145C

Query : 2021A&A...650A.145C

2021A&A...650A.145C - Astronomy and Astrophysics, volume 650A145-145 (2021/6-1)

TOI-269 b: an eccentric sub-Neptune transiting a M2 dwarf revisited with ExTrA.

COINTEPAS M., ALMENARA J.M., BONFILS X., BOUCHY F., ASTUDILLO-DEFRU N., MURGAS F., OTEGI J.F., WYTTENBACH A., ANDERSON D.R., ARTIGAU E., CANTO MARTINS B.L., CHARBONNEAU D., COLLINS K.A., COLLINS K.I., CORREIA J.-J., CURABA S., DELBOULBE A., DELFOSSE X., DIAZ R.F., DORN C., DOYON R., FEAUTRIER P., FIGUEIRA P., FORVEILLE T., GAISNE G., GAN T., GLUCK L., HELLED R., HELLIER C., JOCOU L., KERN P., LAFRASSE S., LAW N., LEAO I.C., LOVIS C., MAGNARD Y., MANN A.W., MAUREL D., DE MEDEIROS J.R., MELO C., MOULIN T., PEPE F., RABOU P., ROCHAT S., RODRIGUEZ D.R., ROUX A., SANTOS N.C., SEGRANSAN D., STADLER E., TING E.B., TWICKEN J.D., UDRY S., WAALKES W.C., WEST R.G., WUNSCHE A., ZIEGLER C., RICKER G., VANDERSPEK R., LATHAM D.W., SEAGER S., WINN J. and JENKINS J.M.

Abstract (from CDS):

We present the confirmation of a new sub-Neptune close to the transition between super-Earths and sub-Neptunes transiting the M2 dwarf TOI-269 (TIC 220 479 565, V=14.4mag, J=10.9mag, R*=0.40R☉, M*=0.39M☉, d=57pc). The exoplanet candidate has been identified in multiple TESS sectors, and validated with high-precision spectroscopy from HARPS and ground-based photometric follow-up from ExTrA and LCO-CTIO. We determined mass, radius, and bulk density of the exoplanet by jointly modeling both photometry and radial velocities with juliet. The transiting exoplanet has an orbital period of P=3.6977104±0.0000037 days, a radius of 2.77±0.12R⊕, and a mass of 8.8±1.4M⊕. Since TOI-269 b lies among the best targets of its category for atmospheric characterization, it would be interesting to probe the atmosphere of this exoplanet with transmission spectroscopy in order to compare it to other sub-Neptunes. With an eccentricity e=0.425–0.086+0.082, TOI-269 b has one of the highest eccentricities of the exoplanets with periods less than 10 days. The star being likely a few Gyr old, this system does not appear to be dynamically young. We surmise TOI-269 b may have acquired its high eccentricity as it migrated inward through planet-planet interactions.

Abstract Copyright: © M. Cointepas et al. 2021

Journal keyword(s): planets and satellites: detection - stars: low-mass - techniques: photometric - techniques: radial velocities

VizieR on-line data: <Available at CDS (J/A+A/650/A145): table1.dat table2.dat table3.dat>

Simbad objects: 12

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Number of rows : 12
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 NAME L 231-32c Pl 04 33 39.7200127728 -51 57 22.435373160           ~ 45 0
2 CD-54 1007 * 05 02 25.7403865272 -53 59 39.799878648   11.67 10.23     ~ 1 0
3 TOI-269b Pl 05 03 23.0610114456 -54 10 37.924879404           ~ 25 0
4 TOI-269 PM* 05 03 23.0610114456 -54 10 37.924879404   15.969 14.410 13.920   M2 20 0
5 NAME LP 424-4b Pl 07 59 05.8395356736 +15 23 29.236065000           ~ 387 1
6 NAME L 678-39b Pl 09 36 01.6372169407 -21 39 38.877606712           ~ 86 0
7 NAME G 162-44b Pl 10 18 35.1372361341 -11 43 00.243355403           ~ 44 0
8 G 162-44 PM* 10 18 35.1372361341 -11 43 00.243355403   14.68 13.14 12.84   M4.0 98 0
9 K2-18b Pl 11 30 14.5177445592 +07 35 18.255348492           ~ 303 0
10 Ross 905b Pl 11 42 11.0933350978 +26 42 23.650782778           ~ 913 1
11 NAME G 139-21b Pl 17 15 18.9339850845 +04 57 50.066612336           ~ 845 1
12 BD+47 2936b Pl 19 50 50.2472976936 +48 04 51.101390496           ~ 493 1

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