2024A&A...686L..18S

Query : 2024A&A...686L..18S

2024A&A...686L..18S - Astronomy and Astrophysics, volume 686L18 (2024/6-1)

HIP 41378 observed by CHEOPS: Where is planet d?

SULIS S., BORSATO L., GROUFFAL S., OSBORN H.P., SANTERNE A., BRANDEKER A., GUNTHER M.N., HEITZMANN A., LENDL M., FRIDLUND M., GANDOLFI D., ALIBERT Y., ALONSO R., BARCZY T., BARRADO NAVASCUES D., BARROS S.C.C., BAUMJOHANN W., BECK T., BENZ W., BERGOMI M., BILLOT N., BONFANTI A., BROEG C., COLLIER CAMERON A., CORRAL VAN DAMME C., CORREIA A.C.M., CSIZMADIA S., CUBILLOS P.E., DAVIES M.B., DELEUIL M., DELINE A., DELREZ L., DEMANGEON O.D.S., DEMORY B.-O., DEREKAS A., EDWARDS B., EHRENREICH D., ERIKSON A., FORTIER A., FOSSATI L., GAZEAS K., GILLON M., GUDEL M., HELLING C., HOYER S., ISAAK K.G., KISS L.L., KORTH J., LAM K.W.F., LASKAR J., LECAVELIER DES ETANGS A., MAGRIN D., MAXTED P.F.L., MORDASINI C., 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., RIBAS I., SANTOS N.C., SCANDARIATO G., SEGRANSAN D., SIMON A.E., SMITH A.M.S., SOUSA S.G., STALPORT M., STEINBERGER M., SZABO G.M., TUSON A., UDRY S., ULMER-MOLL S., VAN GROOTEL V., VENTURINI J., VILLAVER E., WALTON N.A., WILSON T.G., WOLTER D. and ZINGALES T.

Abstract (from CDS):

HIP 41378 d is a long-period planet that has only been observed to transit twice, three years apart, with K2. According to stability considerations and a partial detection of the Rossiter-McLaughlin effect, Pd = 278.36 d has been determined to be the most likely orbital period. We targeted HIP 41378 d with CHEOPS at the predicted transit timing based on Pd = 278.36 d, but the observations show no transit. We find that large (> 22.4 h) transit timing variations (TTVs) could explain this non-detection during the CHEOPS observation window. We also investigated the possibility of an incorrect orbital solution, which would have major implications for our knowledge of this system. If Pd ≠ 278.36 d, the periods that minimize the eccentricity would be 101.22 d and 371.14 d. The shortest orbital period will be tested by TESS, which will observe HIP 41378 in Sector 88 starting in January 2025. Our study shows the importance of a mission like CHEOPS, which today is the only mission able to make long observations (i.e., from space) to track the ephemeris of long-period planets possibly affected by large TTVs.

Abstract Copyright: © The Authors 2024

Journal keyword(s): planets and satellites: individual: HIP 41378

VizieR on-line data: <Available at CDS (J/A+A/686/L18): dataset.dat>

Simbad objects: 8

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Number of rows : 8
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 HD 12572c Pl 02 03 37.0252967640 +21 16 51.112623468           ~ 6 0
2 HD 15906b Pl? 02 33 05.2824651120 -10 21 06.411381228           ~ 5 0
3 TOI-5678b Pl 03 09 32.2118130648 -34 11 53.149633152           ~ 10 0
4 HD 22946d Pl 03 39 16.7617744728 -42 45 45.185938812           ~ 9 0
5 BD+10 1799 Em* 08 26 27.8490900672 +10 04 49.334175156   9.42 8.92     F6 76 0
6 BD+10 1799d Pl 08 26 27.8490900672 +10 04 49.334175156           ~ 27 0
7 CD-43 6219c Pl 10 23 29.2522978464 -43 50 05.841369096           ~ 3 0
8 BD+40 2790c Pl 14 29 34.2426073536 +39 47 25.543283496           ~ 22 0

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