TOI-2490b- The most eccentric brown dwarf transiting in the brown dwarf desert
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2024
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| author | Henderson, Beth A. Casewell, Sarah L. Jordán, Andrés Brahm, Rafael Henning, Thomas Gill, Samuel Mayorga, L. C. Ziegler, Carl Stassun, Keivan G. Goad, Michael R. Acton, Jack Alves, Douglas R. Anderson, David R. Apergis, Ioannis Armstrong, David J. Bayliss, Daniel Burleigh, Matthew R. Dragomir, Diana Gillen, Edward Günther, Maximilian N. Hedges, Christina Hesse, Katharine M. Hobson, Melissa J. Jenkins, James S. Jenkins, Jon M. Kendall, Alicia Lendl, Monika Lund, Michael B. McCormac, James Moyano, Maximiliano Osborn, Ares Pinto, Marcelo Tala Ramsay, Gavin Rapetti, David Saha, Suman Seager, Sara Trifonov, Trifon Udry, Stéphane Vines, Jose I. West, Richard G. Wheatley, Peter J. Winn, Joshua N. Zivave, Tafadzwa |
| author_facet | Henderson, Beth A. Casewell, Sarah L. Jordán, Andrés Brahm, Rafael Henning, Thomas Gill, Samuel Mayorga, L. C. Ziegler, Carl Stassun, Keivan G. Goad, Michael R. Acton, Jack Alves, Douglas R. Anderson, David R. Apergis, Ioannis Armstrong, David J. Bayliss, Daniel Burleigh, Matthew R. Dragomir, Diana Gillen, Edward Günther, Maximilian N. Hedges, Christina Hesse, Katharine M. Hobson, Melissa J. Jenkins, James S. Jenkins, Jon M. Kendall, Alicia Lendl, Monika Lund, Michael B. McCormac, James Moyano, Maximiliano Osborn, Ares Pinto, Marcelo Tala Ramsay, Gavin Rapetti, David Saha, Suman Seager, Sara Trifonov, Trifon Udry, Stéphane Vines, Jose I. West, Richard G. Wheatley, Peter J. Winn, Joshua N. Zivave, Tafadzwa |
| contents | We report the discovery of the most eccentric transiting brown dwarf in the brown dwarf desert, TOI02490b. The brown dwarf desert is the lack of brown dwarfs around main sequence stars within $\sim3$~AU and is thought to be caused by differences in formation mechanisms between a star and planet. To date, only $\sim40$ transiting brown dwarfs have been confirmed. \systemt is a $73.6\pm2.4$ \mjupnospace, $1.00\pm0.02$ \rjup brown dwarf orbiting a $1.004_{-0.022}^{+0.031}$ \msunnospace, $1.105_{-0.012}^{+0.012}$ \rsun sun-like star on a 60.33~d orbit with an eccentricity of $0.77989\pm0.00049$. The discovery was detected within \tess sectors 5 (30 minute cadence) and 32 (2 minute and 20 second cadence). It was then confirmed with 31 radial velocity measurements with \feros by the WINE collaboration and photometric observations with the Next Generation Transit Survey. Stellar modelling of the host star estimates an age of $\sim8$~Gyr, which is supported by estimations from kinematics likely placing the object within the thin disc. However, this is not consistent with model brown dwarf isochrones for the system age suggesting an inflated radius. Only one other transiting brown dwarf with an eccentricity higher than 0.6 is currently known in the brown dwarf desert. Demographic studies of brown dwarfs have suggested such high eccentricity is indicative of stellar formation mechanisms. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2408_04475 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | TOI-2490b- The most eccentric brown dwarf transiting in the brown dwarf desert Henderson, Beth A. Casewell, Sarah L. Jordán, Andrés Brahm, Rafael Henning, Thomas Gill, Samuel Mayorga, L. C. Ziegler, Carl Stassun, Keivan G. Goad, Michael R. Acton, Jack Alves, Douglas R. Anderson, David R. Apergis, Ioannis Armstrong, David J. Bayliss, Daniel Burleigh, Matthew R. Dragomir, Diana Gillen, Edward Günther, Maximilian N. Hedges, Christina Hesse, Katharine M. Hobson, Melissa J. Jenkins, James S. Jenkins, Jon M. Kendall, Alicia Lendl, Monika Lund, Michael B. McCormac, James Moyano, Maximiliano Osborn, Ares Pinto, Marcelo Tala Ramsay, Gavin Rapetti, David Saha, Suman Seager, Sara Trifonov, Trifon Udry, Stéphane Vines, Jose I. West, Richard G. Wheatley, Peter J. Winn, Joshua N. Zivave, Tafadzwa Earth and Planetary Astrophysics Solar and Stellar Astrophysics We report the discovery of the most eccentric transiting brown dwarf in the brown dwarf desert, TOI02490b. The brown dwarf desert is the lack of brown dwarfs around main sequence stars within $\sim3$~AU and is thought to be caused by differences in formation mechanisms between a star and planet. To date, only $\sim40$ transiting brown dwarfs have been confirmed. \systemt is a $73.6\pm2.4$ \mjupnospace, $1.00\pm0.02$ \rjup brown dwarf orbiting a $1.004_{-0.022}^{+0.031}$ \msunnospace, $1.105_{-0.012}^{+0.012}$ \rsun sun-like star on a 60.33~d orbit with an eccentricity of $0.77989\pm0.00049$. The discovery was detected within \tess sectors 5 (30 minute cadence) and 32 (2 minute and 20 second cadence). It was then confirmed with 31 radial velocity measurements with \feros by the WINE collaboration and photometric observations with the Next Generation Transit Survey. Stellar modelling of the host star estimates an age of $\sim8$~Gyr, which is supported by estimations from kinematics likely placing the object within the thin disc. However, this is not consistent with model brown dwarf isochrones for the system age suggesting an inflated radius. Only one other transiting brown dwarf with an eccentricity higher than 0.6 is currently known in the brown dwarf desert. Demographic studies of brown dwarfs have suggested such high eccentricity is indicative of stellar formation mechanisms. |
| title | TOI-2490b- The most eccentric brown dwarf transiting in the brown dwarf desert |
| topic | Earth and Planetary Astrophysics Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2408.04475 |