ASASSN-24fw: Candidate circumplanetary disk occultation of a main-sequence star
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arXiv
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| Natura: | Preprint |
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2025
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| author | Zakamska, Nadia L. Pallathadka, Gautham Adamane Bizyaev, Dmitry Merc, Jaroslav Owen, James E. Reggiani, Henrique Schlaufman, Kevin C. Bąkowska, Karolina Bednarz, Sławomir Bernacki, Krzysztof Gurgul, Agnieszka Hall, Kirsten R. Hambsch, Franz-Josef Joachimczyk, Barbara Kotysz, Krzysztof Kurowski, Sebastian Liakos, Alexios Mikołajczyk, Przemysław J. Pakštienė, Erika Pojmański, Grzegorz Popowicz, Adam Reichart, Daniel E. Wyrzykowski, Łukasz Zdanavičius, Justas Żejmo, Michał Zieliński, Paweł Zola, Staszek |
| author_facet | Zakamska, Nadia L. Pallathadka, Gautham Adamane Bizyaev, Dmitry Merc, Jaroslav Owen, James E. Reggiani, Henrique Schlaufman, Kevin C. Bąkowska, Karolina Bednarz, Sławomir Bernacki, Krzysztof Gurgul, Agnieszka Hall, Kirsten R. Hambsch, Franz-Josef Joachimczyk, Barbara Kotysz, Krzysztof Kurowski, Sebastian Liakos, Alexios Mikołajczyk, Przemysław J. Pakštienė, Erika Pojmański, Grzegorz Popowicz, Adam Reichart, Daniel E. Wyrzykowski, Łukasz Zdanavičius, Justas Żejmo, Michał Zieliński, Paweł Zola, Staszek |
| contents | Dusty disks around planetary and substellar companions in outer reaches of exo-planetary systems can be detected as long-lasting occultations, provided the observer is close to the secondary's orbital plane. Here we report optical spectroscopy with KOSMOS (APO), MagE (Magellan) and GHOST (Gemini-S) of ASASSN-24fw (Gaia 07:05:18.97+06:12:19.4), a 4-magnitude dimming event of a main-sequence star which lasted 8.5 months. We discover multiple low-ionization metal emission lines with velocity dispersion $\lesssim 10$ km/s blue-shifted by 27 km/s with respect to the star, as well as kinematically complex Na D absorption. If associated with the occulter, these detections suggest that the occulter is gas-rich. Further, we detect blue-shifted and broad ($\sim 200$ km/s) H$α$ line, which likely originates in the inner circumstellar disk. We confirm the previously reported occultations in 1981 and 1937 seen in historic data, yielding a semi-major axis of the occulter's orbital motion around the star of 14 AU. If the occulter is a circumsecondary disk filling 30-100% of the Hill radius, we estimate the minimum mass of the secondary to be a few Jupiter masses and a disk mass of 1% of the mass of the Moon. Given the age of the star ($>2$ Gyr), the disk is unlikely to be a survivor of the planet formation stage and may be a result of a planetary collision. If Na D absorption and/or metal emission lines originate in the disk, the observations presented here are the first discovery of a circumsecondary disk wind or rotation. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2507_05367 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | ASASSN-24fw: Candidate circumplanetary disk occultation of a main-sequence star Zakamska, Nadia L. Pallathadka, Gautham Adamane Bizyaev, Dmitry Merc, Jaroslav Owen, James E. Reggiani, Henrique Schlaufman, Kevin C. Bąkowska, Karolina Bednarz, Sławomir Bernacki, Krzysztof Gurgul, Agnieszka Hall, Kirsten R. Hambsch, Franz-Josef Joachimczyk, Barbara Kotysz, Krzysztof Kurowski, Sebastian Liakos, Alexios Mikołajczyk, Przemysław J. Pakštienė, Erika Pojmański, Grzegorz Popowicz, Adam Reichart, Daniel E. Wyrzykowski, Łukasz Zdanavičius, Justas Żejmo, Michał Zieliński, Paweł Zola, Staszek Earth and Planetary Astrophysics Solar and Stellar Astrophysics Dusty disks around planetary and substellar companions in outer reaches of exo-planetary systems can be detected as long-lasting occultations, provided the observer is close to the secondary's orbital plane. Here we report optical spectroscopy with KOSMOS (APO), MagE (Magellan) and GHOST (Gemini-S) of ASASSN-24fw (Gaia 07:05:18.97+06:12:19.4), a 4-magnitude dimming event of a main-sequence star which lasted 8.5 months. We discover multiple low-ionization metal emission lines with velocity dispersion $\lesssim 10$ km/s blue-shifted by 27 km/s with respect to the star, as well as kinematically complex Na D absorption. If associated with the occulter, these detections suggest that the occulter is gas-rich. Further, we detect blue-shifted and broad ($\sim 200$ km/s) H$α$ line, which likely originates in the inner circumstellar disk. We confirm the previously reported occultations in 1981 and 1937 seen in historic data, yielding a semi-major axis of the occulter's orbital motion around the star of 14 AU. If the occulter is a circumsecondary disk filling 30-100% of the Hill radius, we estimate the minimum mass of the secondary to be a few Jupiter masses and a disk mass of 1% of the mass of the Moon. Given the age of the star ($>2$ Gyr), the disk is unlikely to be a survivor of the planet formation stage and may be a result of a planetary collision. If Na D absorption and/or metal emission lines originate in the disk, the observations presented here are the first discovery of a circumsecondary disk wind or rotation. |
| title | ASASSN-24fw: Candidate circumplanetary disk occultation of a main-sequence star |
| topic | Earth and Planetary Astrophysics Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2507.05367 |