2022AJ....164...97M

Query : 2022AJ....164...97M

2022AJ....164...97M - Astron. J., 164, 97 (2022/September-0)

The TESS-Keck Survey. XIII. An Eccentric Hot Neptune with a Similar-mass Outer Companion around TOI-1272.

MacDOUGALL M.G., PETIGURA E.A., FETHEROLF T., BEARD C., LUBIN J., ANGELO I., BATALHA N.M., BEHMARD A., BLUNT S., BRINKMAN C., CHONTOS A., CROSSFIELD I.J.M., DAI F., DALBA P.A., DRESSING C., FULTON B., GIACALONE S., HILL M.L., HOWARD A.W., HUBER D., ISAACSON H., KANE S.R., KOSIAREK M., MAYO A., MOCNIK T., MURPHY J.M.A., PIDHORODETSKA D., POLANSKI A., RICE M., ROBERTSON P., ROSENTHAL L.J., ROY A., RUBENZAHL R.A., SCARSDALE N., TURTELBOOM E.V., TYLER D., VAN ZANDT J., WEISS L.M., ESPARZA-BORGES E., FUKUI A., ISOGAI K., KAWAUCHI K., MORI M., MURGAS F., NARITA N., NISHIUMI T., PALLE E., PARVIAINEN H., WATANABE N., JENKINS J.M., LATHAM D.W., RICKER G.R., SEAGER S., VANDERSPEK R.K., WINN J.N., BIERYLA A., CALDWELL D.A., DRAGOMIR D., FAUSNAUGH M.M., MIRELES I. and RODRIGUEZ D.R.

Abstract (from CDS):

We report the discovery of an eccentric hot Neptune and a non-transiting outer planet around TOI-1272. We identified the eccentricity of the inner planet, with an orbital period of 3.3 days and Rp,b = 4.1 ± 0.2 R⊕, based on a mismatch between the observed transit duration and the expected duration for a circular orbit. Using ground-based radial velocity (RV) measurements from the HIRES instrument at the Keck Observatory, we measured the mass of TOI-1272b to be Mp,b = 25 ± 2 M⊕. We also confirmed a high eccentricity of eb = 0.34 ± 0.06, placing TOI-1272b among the most eccentric well-characterized sub-Jovians. We used these RV measurements to also identify a non-transiting outer companion on an 8.7 day orbit with a similar mass of Mp,c sin i = 27 ± 3 M⊕ and ec ≲ 0.35. Dynamically stable planet-planet interactions have likely allowed TOI-1272b to avoid tidal eccentricity decay despite the short circularization timescale expected for a close-in eccentric Neptune. TOI-1272b also maintains an envelope mass fraction of fenv ≈ 11% despite its high equilibrium temperature, implying that it may currently be undergoing photoevaporation. This planet joins a small population of short-period Neptune-like planets within the “Hot Neptune Desert” with a poorly understood formation pathway.

Abstract Copyright: © 2022. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Exoplanets - Eccentricity - Hot Neptunes

VizieR on-line data: <Available at CDS (J/AJ/164/97): table1.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 TOI-849b Pl 01 54 51.7040408544 -29 25 18.468394788           ~ 59 0
2 TOI-269b Pl 05 03 23.0610114456 -54 10 37.924879404           ~ 25 0
3 NAME LP 424-4b Pl 07 59 05.8395356736 +15 23 29.236065000           ~ 387 1
4 Ross 905b Pl 11 42 11.0933350978 +26 42 23.650782778           ~ 913 1
5 TOI-1272 MS* 13 16 47.1902624798 +49 51 39.739099624   12.846 11.878 11.618   K1 15 0
6 TOI-1272b Pl 13 16 47.1902624798 +49 51 39.739099624           ~ 11 0
7 TOI-1272c Pl 13 16 47.1902624798 +49 51 39.739099624           ~ 3 0
8 Kepler-1656b Pl 18 57 53.3246033136 +39 54 42.531984144           ~ 52 0
9 Kepler-411b Pl 19 10 25.3469947368 +49 31 23.712634632           ~ 59 0
10 BD+73 878b Pl 19 44 58.6385661360 +74 03 45.855506952           ~ 16 0
11 BD+47 2936b Pl 19 50 50.2472976936 +48 04 51.101390496           ~ 493 1
12 CD-44 14956b Pl 22 33 35.8684307688 -43 26 11.916565332           ~ 22 0

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