2022A&A...664A.156O

Query : 2022A&A...664A.156O

2022A&A...664A.156O - Astronomy and Astrophysics, volume 664A, 156-156 (2022/8-1)

Uncovering the true periods of the young sub-Neptunes orbiting TOI-2076.

OSBORN H.P., BONFANTI A., GANDOLFI D., HEDGES C., LELEU A., FORTIER A., FUTYAN D., GUTERMANN P., MAXTED P.F.L., BORSATO L., COLLINS K.A., GOMES DA SILVA J., GOMEZ MAQUEO CHEW Y., HOOTON M.J., LENDL M., PARVIAINEN H., SALMON S., SCHANCHE N., SERRANO L.M., SOUSA S.G., TUSON A., ULMER-MOLL S., VAN GROOTEL V., WELLS R.D., WILSON T.G., ALIBERT Y., ALONSO R., ANGLADA G., ASQUIER J., BARRADO Y NAVASCUES D., BAUMJOHANN W., BECK T., BENZ W., BIONDI F., BONFILS X., BOUCHY F., BRANDEKER A., BROEG C., BARCZY T., BARROS S.C.C., CABRERA J., CHARNOZ S., COLLIER CAMERON A., CSIZMADIA S., DAVIES M.B., DELEUIL M., DELREZ L., DEMORY B.-O., EHRENREICH D., ERIKSON A., FOSSATI L., FRIDLUND M., GILLON M., GOMEZ-MUNOZ M.A., GUDEL M., HENG K., HOYER S., ISAAK K.G., KISS L., LASKAR J., LECAVELIER DES ETANGS A., LOVIS C., MAGRIN D., MALAVOLTA L., McCORMAC J., NASCIMBENI V., OLOFSSON G., OTTENSAMER R., PAGANO I., PALLE E., PETER G., PIAZZA D., PIOTTO G., POLLACCO D., QUELOZ D., RAGAZZONI R., RANDO N., RAUER H., REIMERS C., RIBAS I., DEMANGEON O.D.S., SMITH A.M.S., SABIN L., SANTOS N., SCANDARIATO G., SCHROFFENEGGER U., SCHWARZ R.P., SHPORER A., SIMON A.E., STELLER M., SZABO G.M., SEGRANSAN D., THOMAS N., UDRY S., WALTER I. and WALTON N.

Abstract (from CDS):


Context. TOI-2076 is a transiting three-planet system of sub-Neptunes orbiting a bright (G = 8.9 mag), young (340 ± 80 Myr) K-type star. Although a validated planetary system, the orbits of the two outer planets were unconstrained as only two non-consecutive transits were seen in TESS photometry. This left 11 and 7 possible period aliases for each.
Aims. To reveal the true orbits of these two long-period planets, precise photometry targeted on the highest-probability period aliases is required. Long-term monitoring of transits in multi-planet systems can also help constrain planetary masses through TTV measurements.
Methods. We used the MonoTools package to determine which aliases to follow, and then performed space-based and ground-based photometric follow-up of TOI-2076 c and d with CHEOPS, SAINT-EX, and LCO telescopes.
Results. CHEOPS observations revealed a clear detection for TOI-2076 c at P=21.02538–0.00074+0.00084d, and allowed us to rule out three of the most likely period aliases for TOI-2076 d. Ground-based photometry further enabled us to rule out remaining aliases and confirm the P = 35.12537 ± 0.00067 d alias. These observations also improved the radius precision of all three sub-Neptunes to 2.518 ± 0.036, 3.497 ± 0.043, and 3.232 ± 0.063 R⊕. Our observations also revealed a clear anti-correlated TTV signal between planets b and c likely caused by their proximity to the 2:1 resonance, while planets c and d appear close to a 5:3 period commensurability, although model degeneracy meant we were unable to retrieve robust TTV masses. Their inflated radii, likely due to extended H-He atmospheres, combined with low insolation makes all three planets excellent candidates for future comparative transmission spectroscopy with JWST.

Abstract Copyright: © ESO 2022

Journal keyword(s): planets and satellites: detection - stars: individual: TOI-2076 - techniques: photometric

VizieR on-line data: <Available at CDS (J/A+A/664/A156): cheops_0.dat cheops_1.dat cheops_2.dat cheops_3.dat g_lco.dat r_lco.dat i_lco.dat z_lco.dat r_sex.dat z_mcd.dat>

Simbad objects: 13

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Number of rows : 13
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024 		#notes
1 TOI-178g Pl 00 29 12.3029193648 -30 27 13.466857032           ~ 10 0
2 HD 63433 BY* 07 49 55.0606576176 +27 21 47.457467316   7.59 6.91     G5V 157 0
3 BD+10 1799f Pl 08 26 27.8490900672 +10 04 49.334175156           ~ 29 0
4 BD+10 1799 * 08 26 27.8490900672 +10 04 49.334175156   9.42 8.92     F6 50 0
5 HD 108236f Pl 12 26 17.8919204184 -51 21 46.215656244           ~ 4 0
6 TOI-2257b Pl 12 58 57.6816623624 +77 39 41.689782344           ~ 8 0
7 BD+39 2643 PM* 13 25 07.9957316160 +38 55 20.944920864   11.131 10.257 9.736   K3V 33 0
8 BD+40 2790c Pl 14 29 34.2426073536 +39 47 25.543283496           ~ 11 0
9 BD+40 2790b Pl 14 29 34.2426073536 +39 47 25.543283496           ~ 24 0
10 BD+40 2790d Pl 14 29 34.2426073536 +39 47 25.543283496           ~ 8 0
11 BD+40 2790 PM* 14 29 34.2426073536 +39 47 25.543283496   10.03 9.14     K0 21 0
12 Kepler-36 Er* 19 25 00.0428079600 +49 13 54.630900876   12.795 12.174 12.094   F2 219 1
13 HD 197481 BY* 20 45 09.5324974119 -31 20 27.237889841   10.05 8.627 9.078 6.593 M1VeBa1 1153 0

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