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| Format: | Preprint |
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2026
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| Online Access: | https://arxiv.org/abs/2603.18395 |
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| _version_ | 1866908900389814272 |
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| author | Mihaylov, Deyan P. Eberhardt, Jan Trifonov, Trifon Brahm, Rafael Henning, Thomas Jordán, Andrés Stoeva, Denitza Jones, Matías I. Acuña-Aguirre, Lorena Stefanov, Stefan Pinto, M. Tala Hobson, Melissa J. Espinoza, Nestor Rojas, Felipe I. Schlecker, Martin Bozhilov, Vladimir Guillot, Tristan Triaud, Amaury H. M. J. Lissauer, Jack J. Korth, Judith Parviainen, Hannu Kreidberg, Laura Bendjoya, Philippe Suarez, Olga Ziegler, Carl Rowden, Pamela Rudat, Alexander Kostov, Veselin Winn, Joshua N. Jenkins, Jon M. Collins, Karen A. Watkins, Cristilyn N. Radford, Don J. Stockdale, Chris Gan, Tianjun |
| author_facet | Mihaylov, Deyan P. Eberhardt, Jan Trifonov, Trifon Brahm, Rafael Henning, Thomas Jordán, Andrés Stoeva, Denitza Jones, Matías I. Acuña-Aguirre, Lorena Stefanov, Stefan Pinto, M. Tala Hobson, Melissa J. Espinoza, Nestor Rojas, Felipe I. Schlecker, Martin Bozhilov, Vladimir Guillot, Tristan Triaud, Amaury H. M. J. Lissauer, Jack J. Korth, Judith Parviainen, Hannu Kreidberg, Laura Bendjoya, Philippe Suarez, Olga Ziegler, Carl Rowden, Pamela Rudat, Alexander Kostov, Veselin Winn, Joshua N. Jenkins, Jon M. Collins, Karen A. Watkins, Cristilyn N. Radford, Don J. Stockdale, Chris Gan, Tianjun |
| contents | TOI-1232 is a G-dwarf star with a mass of $1.06_{-0.06}^{+0.07} M_\odot$, a radius of $1.07\pm 0.05 R_\odot$, and slightly higher metallicity than solar of Fe/H = $0.18 \pm 0.05$. The star hosts a transiting warm Jovian-mass planet, TOI-1232 b, with an orbital period of $P_{b} = 14.256_{-0.001}^{+0.001}$ days, identified with data from multiple sectors of the $\textit{TESS}$ space telescope. The $\textit{TESS}$ light curve of TOI-1232 is complex, as it is contaminated by a background eclipsing binary with a period of $1.37$ days. The TOI-1232 b was firmly confirmed by ground-based transit follow-up campaigns from Las Cumbres, Hazelwood, Brierfield, and ASTEP observatories.Additionally, the $\textit{TESS}$ transits of TOI-1232 b exhibit strong transit timing variations (TTVs) with a super-period of $235.5 \pm 0.7$ days and a semi-amplitude of 27 minutes. Radial velocity (RV) follow-up with the FEROS spectrograph confirms the planetary nature of the transiting candidate, while a self-consistent $N$-body analysis of RVs and TTVs pinpoints the presence of a second outer Saturn-mass companion, TOI-1232 c with a period of $P_{c} = 30.356_{-0.012}^{+0.010}$ days. The TOI-1232 warm-giant system is particularly important due to the evidence of two massive planets that reside near the 2:1 commensurability but are not locked in a mean motion resonance (MMR). Thanks to $\textit{TESS}$, we have revealed a handful of these rare systems. Hence, TOI-1232 is an important addition to understanding the formation and dynamical evolution of such compact, massive, warm giant planets. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2603_18395 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | A Warm Massive Pair of Planets around TOI-1232 Revealed with Transit-timing Variations and Doppler Spectroscopy Mihaylov, Deyan P. Eberhardt, Jan Trifonov, Trifon Brahm, Rafael Henning, Thomas Jordán, Andrés Stoeva, Denitza Jones, Matías I. Acuña-Aguirre, Lorena Stefanov, Stefan Pinto, M. Tala Hobson, Melissa J. Espinoza, Nestor Rojas, Felipe I. Schlecker, Martin Bozhilov, Vladimir Guillot, Tristan Triaud, Amaury H. M. J. Lissauer, Jack J. Korth, Judith Parviainen, Hannu Kreidberg, Laura Bendjoya, Philippe Suarez, Olga Ziegler, Carl Rowden, Pamela Rudat, Alexander Kostov, Veselin Winn, Joshua N. Jenkins, Jon M. Collins, Karen A. Watkins, Cristilyn N. Radford, Don J. Stockdale, Chris Gan, Tianjun Earth and Planetary Astrophysics TOI-1232 is a G-dwarf star with a mass of $1.06_{-0.06}^{+0.07} M_\odot$, a radius of $1.07\pm 0.05 R_\odot$, and slightly higher metallicity than solar of Fe/H = $0.18 \pm 0.05$. The star hosts a transiting warm Jovian-mass planet, TOI-1232 b, with an orbital period of $P_{b} = 14.256_{-0.001}^{+0.001}$ days, identified with data from multiple sectors of the $\textit{TESS}$ space telescope. The $\textit{TESS}$ light curve of TOI-1232 is complex, as it is contaminated by a background eclipsing binary with a period of $1.37$ days. The TOI-1232 b was firmly confirmed by ground-based transit follow-up campaigns from Las Cumbres, Hazelwood, Brierfield, and ASTEP observatories.Additionally, the $\textit{TESS}$ transits of TOI-1232 b exhibit strong transit timing variations (TTVs) with a super-period of $235.5 \pm 0.7$ days and a semi-amplitude of 27 minutes. Radial velocity (RV) follow-up with the FEROS spectrograph confirms the planetary nature of the transiting candidate, while a self-consistent $N$-body analysis of RVs and TTVs pinpoints the presence of a second outer Saturn-mass companion, TOI-1232 c with a period of $P_{c} = 30.356_{-0.012}^{+0.010}$ days. The TOI-1232 warm-giant system is particularly important due to the evidence of two massive planets that reside near the 2:1 commensurability but are not locked in a mean motion resonance (MMR). Thanks to $\textit{TESS}$, we have revealed a handful of these rare systems. Hence, TOI-1232 is an important addition to understanding the formation and dynamical evolution of such compact, massive, warm giant planets. |
| title | A Warm Massive Pair of Planets around TOI-1232 Revealed with Transit-timing Variations and Doppler Spectroscopy |
| topic | Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2603.18395 |