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HIP 41378 observed by CHEOPS: Where is planet d?

Fuente: arXiv

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Main Authors:	Sulis, S., Borsato, L., Grouffal, S., Osborn, H. P., Santerne, A., Brandeker, A., Günther, M. N., Heitzmann, A., Lendl, M., Fridlund, M., Gandolfi, D., Alibert, Y., Alonso, R., Bárczy, T., Navascues, D. Barrado, Barros, S. C., Baumjohann, W., Beck, T., Benz, W., Bergomi, M., Billot, N., Bonfanti, A., Broeg, C., Cameron, A. Collier, van Damme, C. Corral, Correia, A. C. M., Csizmadia, Sz., 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., Güdel, M., Helling, Ch., Hoyer, S., Isaak, K. G., Kiss, L., Korth, J., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Magrin, D., Maxted, P. F. L., Mordasini, C., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piazza, D., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Santos, N. C., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Sousa, S. G., Stalport, M., Steinberger, M., Szabó, M. Gy., Tuson, A., Udry, S., Ulmer-Moll, S., Van Grootel, V., Venturini, J., Villaver, E., Walton, N. A., Wilson, T. G., Wolter, D., Zingales, T.
Format:	Preprint
Published:	2024
Subjects:	Earth and Planetary Astrophysics
Online Access:	Acceder al recurso
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_version_	1866909231037284352
author	Sulis, S. Borsato, L. Grouffal, S. Osborn, H. P. Santerne, A. Brandeker, A. Günther, M. N. Heitzmann, A. Lendl, M. Fridlund, M. Gandolfi, D. Alibert, Y. Alonso, R. Bárczy, T. Navascues, D. Barrado Barros, S. C. Baumjohann, W. Beck, T. Benz, W. Bergomi, M. Billot, N. Bonfanti, A. Broeg, C. Cameron, A. Collier van Damme, C. Corral Correia, A. C. M. Csizmadia, Sz. 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. Güdel, M. Helling, Ch. Hoyer, S. Isaak, K. G. Kiss, L. Korth, J. Lam, K. W. F. Laskar, J. Etangs, A. Lecavelier des Magrin, D. Maxted, P. F. L. Mordasini, C. Nascimbeni, V. Olofsson, G. Ottensamer, R. Pagano, I. Pallé, E. Peter, G. Piazza, D. Piotto, G. Pollacco, D. Queloz, D. Ragazzoni, R. Rando, N. Rauer, H. Ribas, I. Santos, N. C. Scandariato, G. Ségransan, D. Simon, A. E. Smith, A. M. S. Sousa, S. G. Stalport, M. Steinberger, M. Szabó, M. Gy. Tuson, A. Udry, S. Ulmer-Moll, S. Van Grootel, V. Venturini, J. Villaver, E. Walton, N. A. Wilson, T. G. Wolter, D. Zingales, T.
author_facet	Sulis, S. Borsato, L. Grouffal, S. Osborn, H. P. Santerne, A. Brandeker, A. Günther, M. N. Heitzmann, A. Lendl, M. Fridlund, M. Gandolfi, D. Alibert, Y. Alonso, R. Bárczy, T. Navascues, D. Barrado Barros, S. C. Baumjohann, W. Beck, T. Benz, W. Bergomi, M. Billot, N. Bonfanti, A. Broeg, C. Cameron, A. Collier van Damme, C. Corral Correia, A. C. M. Csizmadia, Sz. 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. Güdel, M. Helling, Ch. Hoyer, S. Isaak, K. G. Kiss, L. Korth, J. Lam, K. W. F. Laskar, J. Etangs, A. Lecavelier des Magrin, D. Maxted, P. F. L. Mordasini, C. Nascimbeni, V. Olofsson, G. Ottensamer, R. Pagano, I. Pallé, E. Peter, G. Piazza, D. Piotto, G. Pollacco, D. Queloz, D. Ragazzoni, R. Rando, N. Rauer, H. Ribas, I. Santos, N. C. Scandariato, G. Ségransan, D. Simon, A. E. Smith, A. M. S. Sousa, S. G. Stalport, M. Steinberger, M. Szabó, M. Gy. Tuson, A. Udry, S. Ulmer-Moll, S. Van Grootel, V. Venturini, J. Villaver, E. Walton, N. A. Wilson, T. G. Wolter, D. Zingales, T.
contents	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, $P_\mathrm{d} = 278.36$ 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 $P_\mathrm{d}= 278.36$ d, but the observations show no transit. We find that large ($>22.4$ hours) 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 $P_\mathrm{d} \neq 278.36$ 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.
format	Preprint
id	arxiv_https___arxiv_org_abs_2405_20077
institution	arXiv
publishDate	2024
record_format	arxiv
spellingShingle	HIP 41378 observed by CHEOPS: Where is planet d? Sulis, S. Borsato, L. Grouffal, S. Osborn, H. P. Santerne, A. Brandeker, A. Günther, M. N. Heitzmann, A. Lendl, M. Fridlund, M. Gandolfi, D. Alibert, Y. Alonso, R. Bárczy, T. Navascues, D. Barrado Barros, S. C. Baumjohann, W. Beck, T. Benz, W. Bergomi, M. Billot, N. Bonfanti, A. Broeg, C. Cameron, A. Collier van Damme, C. Corral Correia, A. C. M. Csizmadia, Sz. 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. Güdel, M. Helling, Ch. Hoyer, S. Isaak, K. G. Kiss, L. Korth, J. Lam, K. W. F. Laskar, J. Etangs, A. Lecavelier des Magrin, D. Maxted, P. F. L. Mordasini, C. Nascimbeni, V. Olofsson, G. Ottensamer, R. Pagano, I. Pallé, E. Peter, G. Piazza, D. Piotto, G. Pollacco, D. Queloz, D. Ragazzoni, R. Rando, N. Rauer, H. Ribas, I. Santos, N. C. Scandariato, G. Ségransan, D. Simon, A. E. Smith, A. M. S. Sousa, S. G. Stalport, M. Steinberger, M. Szabó, M. Gy. Tuson, A. Udry, S. Ulmer-Moll, S. Van Grootel, V. Venturini, J. Villaver, E. Walton, N. A. Wilson, T. G. Wolter, D. Zingales, T. Earth and Planetary Astrophysics 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, $P_\mathrm{d} = 278.36$ 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 $P_\mathrm{d}= 278.36$ d, but the observations show no transit. We find that large ($>22.4$ hours) 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 $P_\mathrm{d} \neq 278.36$ 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.
title	HIP 41378 observed by CHEOPS: Where is planet d?
topic	Earth and Planetary Astrophysics
url	https://arxiv.org/abs/2405.20077