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Architecture of TOI-561 planetary system

Fuente: arXiv

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Main Authors:	Piotto, G., Zingales, T., Borsato, L., Egger, J. A., Correia, A. C. M., Simon, A. E., Florén, H. G., Sousa, S. G., Maxted, P. F. L., Nardiello, D., Malavolta, L., Wilson, T. G., Alibert, Y., Adibekyan, V., Bonfanti, A., Luque, R., Santos, N. C., Hooton, M. J., Fossati, L., Smith, A. M. S., Salmon, S., Lacedelli, G., Alonso, R., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Beck, T., Benz, W., Billot, N., Brandeker, A., Broeg, C., Buder, M., Cameron, A. Collier, Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Deline, A., Demangeon, O. D. S., Demory, B. O., Derekas, A., Edwards, B., Ehrenreich, D., Erikson, A., Fortier, A., Fridlund, M., Gandolfi, D., Gazeas, K., Gillon, M., Güdel, M., Günther, M. N., Heitzmann, A., Helling, Ch., Isaak, K. G., Kiss, L. L., Korth, J., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Lendl, M., Leonardi, P., Magrin, D., Mantovan, G., Mordasini, C., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Ratti, F., Rauer, H., Ribas, I., Scandariato, G., Ségransan, D., Sicilia, D., Stalport, M., Sulis, S., Szabó, Gy. M., Udry, S., Ulmer-Moll, S., Van Grootel, V., Venturini, J., Villaver, E., Walton, N. A., Winn, J. N., Wolf, S.
Format:	Preprint
Published:	2024
Subjects:	Earth and Planetary Astrophysics
Online Access:	Acceder al recurso
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author	Piotto, G. Zingales, T. Borsato, L. Egger, J. A. Correia, A. C. M. Simon, A. E. Florén, H. G. Sousa, S. G. Maxted, P. F. L. Nardiello, D. Malavolta, L. Wilson, T. G. Alibert, Y. Adibekyan, V. Bonfanti, A. Luque, R. Santos, N. C. Hooton, M. J. Fossati, L. Smith, A. M. S. Salmon, S. Lacedelli, G. Alonso, R. Bárczy, T. Navascues, D. Barrado Barros, S. C. C. Baumjohann, W. Beck, T. Benz, W. Billot, N. Brandeker, A. Broeg, C. Buder, M. Cameron, A. Collier Csizmadia, Sz. Cubillos, P. E. Davies, M. B. Deleuil, M. Deline, A. Demangeon, O. D. S. Demory, B. O. Derekas, A. Edwards, B. Ehrenreich, D. Erikson, A. Fortier, A. Fridlund, M. Gandolfi, D. Gazeas, K. Gillon, M. Güdel, M. Günther, M. N. Heitzmann, A. Helling, Ch. Isaak, K. G. Kiss, L. L. Korth, J. Lam, K. W. F. Laskar, J. Etangs, A. Lecavelier des Lendl, M. Leonardi, P. Magrin, D. Mantovan, G. Mordasini, C. Nascimbeni, V. Olofsson, G. Ottensamer, R. Pagano, I. Pallé, E. Peter, G. Ottensamer, R. Pollacco, D. Queloz, D. Ragazzoni, R. Rando, N. Ratti, F. Rauer, H. Ribas, I. Scandariato, G. Ségransan, D. Sicilia, D. Stalport, M. Sulis, S. Szabó, Gy. M. Udry, S. Ulmer-Moll, S. Van Grootel, V. Venturini, J. Villaver, E. Walton, N. A. Winn, J. N. Wolf, S.
author_facet	Piotto, G. Zingales, T. Borsato, L. Egger, J. A. Correia, A. C. M. Simon, A. E. Florén, H. G. Sousa, S. G. Maxted, P. F. L. Nardiello, D. Malavolta, L. Wilson, T. G. Alibert, Y. Adibekyan, V. Bonfanti, A. Luque, R. Santos, N. C. Hooton, M. J. Fossati, L. Smith, A. M. S. Salmon, S. Lacedelli, G. Alonso, R. Bárczy, T. Navascues, D. Barrado Barros, S. C. C. Baumjohann, W. Beck, T. Benz, W. Billot, N. Brandeker, A. Broeg, C. Buder, M. Cameron, A. Collier Csizmadia, Sz. Cubillos, P. E. Davies, M. B. Deleuil, M. Deline, A. Demangeon, O. D. S. Demory, B. O. Derekas, A. Edwards, B. Ehrenreich, D. Erikson, A. Fortier, A. Fridlund, M. Gandolfi, D. Gazeas, K. Gillon, M. Güdel, M. Günther, M. N. Heitzmann, A. Helling, Ch. Isaak, K. G. Kiss, L. L. Korth, J. Lam, K. W. F. Laskar, J. Etangs, A. Lecavelier des Lendl, M. Leonardi, P. Magrin, D. Mantovan, G. Mordasini, C. Nascimbeni, V. Olofsson, G. Ottensamer, R. Pagano, I. Pallé, E. Peter, G. Ottensamer, R. Pollacco, D. Queloz, D. Ragazzoni, R. Rando, N. Ratti, F. Rauer, H. Ribas, I. Scandariato, G. Ségransan, D. Sicilia, D. Stalport, M. Sulis, S. Szabó, Gy. M. Udry, S. Ulmer-Moll, S. Van Grootel, V. Venturini, J. Villaver, E. Walton, N. A. Winn, J. N. Wolf, S.
contents	We present new observations from CHEOPS and TESS to clarify the architecture of the planetary system hosted by the old Galactic thick disk star TOI-561. Our global analysis, which also includes previously published photometric and radial velocity data, incontrovertibly proves that TOI-561 is hosting at least four transiting planets with periods of 0.44 days (TOI-561 b), 10.8 days (TOI-561 c), 25.7 days (TOI-561 d), and 77.1 days (TOI-561 e) and a fifth non-transiting candidate, TOI-561f with a period of 433 days. The precise characterisation of TOI-561's orbital architecture is interesting since old and metal-poor thick disk stars are less likely to host ultra-short period Super-Earths like TOI-561 b. The new period of planet -e is consistent with the value obtained using radial velocity alone and is now known to be $77.14399\pm0.00025$ days, thanks to the new CHEOPS and TESS transits. The new data allowed us to improve its radius ($R_p = 2.517 \pm 0.045 R_{\oplus}$ from 5$\%$ to 2$\%$ precision) and mass ($M_p = 12.4 \pm 1.4 M_{\oplus}$) estimates, implying a density of $ρ_p = 0.778 \pm 0.097 ρ_{\oplus}$. Thanks to recent TESS observations and the focused CHEOPS visit of the transit of TOI-561 e, a good candidate for exomoon searches, the planet's period is finally constrained, allowing us to predict transit times through 2030 with 20-minute accuracy. We present an updated version of the internal structure of the four transiting planets. We finally performed a detailed stability analysis, which confirmed the long-term stability of the outer planet TOI-561 f.
format	Preprint
id	arxiv_https___arxiv_org_abs_2410_18169
institution	arXiv
publishDate	2024
record_format	arxiv
spellingShingle	Architecture of TOI-561 planetary system Piotto, G. Zingales, T. Borsato, L. Egger, J. A. Correia, A. C. M. Simon, A. E. Florén, H. G. Sousa, S. G. Maxted, P. F. L. Nardiello, D. Malavolta, L. Wilson, T. G. Alibert, Y. Adibekyan, V. Bonfanti, A. Luque, R. Santos, N. C. Hooton, M. J. Fossati, L. Smith, A. M. S. Salmon, S. Lacedelli, G. Alonso, R. Bárczy, T. Navascues, D. Barrado Barros, S. C. C. Baumjohann, W. Beck, T. Benz, W. Billot, N. Brandeker, A. Broeg, C. Buder, M. Cameron, A. Collier Csizmadia, Sz. Cubillos, P. E. Davies, M. B. Deleuil, M. Deline, A. Demangeon, O. D. S. Demory, B. O. Derekas, A. Edwards, B. Ehrenreich, D. Erikson, A. Fortier, A. Fridlund, M. Gandolfi, D. Gazeas, K. Gillon, M. Güdel, M. Günther, M. N. Heitzmann, A. Helling, Ch. Isaak, K. G. Kiss, L. L. Korth, J. Lam, K. W. F. Laskar, J. Etangs, A. Lecavelier des Lendl, M. Leonardi, P. Magrin, D. Mantovan, G. Mordasini, C. Nascimbeni, V. Olofsson, G. Ottensamer, R. Pagano, I. Pallé, E. Peter, G. Ottensamer, R. Pollacco, D. Queloz, D. Ragazzoni, R. Rando, N. Ratti, F. Rauer, H. Ribas, I. Scandariato, G. Ségransan, D. Sicilia, D. Stalport, M. Sulis, S. Szabó, Gy. M. Udry, S. Ulmer-Moll, S. Van Grootel, V. Venturini, J. Villaver, E. Walton, N. A. Winn, J. N. Wolf, S. Earth and Planetary Astrophysics We present new observations from CHEOPS and TESS to clarify the architecture of the planetary system hosted by the old Galactic thick disk star TOI-561. Our global analysis, which also includes previously published photometric and radial velocity data, incontrovertibly proves that TOI-561 is hosting at least four transiting planets with periods of 0.44 days (TOI-561 b), 10.8 days (TOI-561 c), 25.7 days (TOI-561 d), and 77.1 days (TOI-561 e) and a fifth non-transiting candidate, TOI-561f with a period of 433 days. The precise characterisation of TOI-561's orbital architecture is interesting since old and metal-poor thick disk stars are less likely to host ultra-short period Super-Earths like TOI-561 b. The new period of planet -e is consistent with the value obtained using radial velocity alone and is now known to be $77.14399\pm0.00025$ days, thanks to the new CHEOPS and TESS transits. The new data allowed us to improve its radius ($R_p = 2.517 \pm 0.045 R_{\oplus}$ from 5$\%$ to 2$\%$ precision) and mass ($M_p = 12.4 \pm 1.4 M_{\oplus}$) estimates, implying a density of $ρ_p = 0.778 \pm 0.097 ρ_{\oplus}$. Thanks to recent TESS observations and the focused CHEOPS visit of the transit of TOI-561 e, a good candidate for exomoon searches, the planet's period is finally constrained, allowing us to predict transit times through 2030 with 20-minute accuracy. We present an updated version of the internal structure of the four transiting planets. We finally performed a detailed stability analysis, which confirmed the long-term stability of the outer planet TOI-561 f.
title	Architecture of TOI-561 planetary system
topic	Earth and Planetary Astrophysics
url	https://arxiv.org/abs/2410.18169