Discovery of a Debris Disk Around TWA 20
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arXiv
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2025
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| author | Palatnick, Skyler Millar-Blanchaer, Maxwell A. Zhang, Jingwen Lawson, Kellen Lewis, Briley L. Crotts, Katie A. Carter, Aarynn L. Biller, Beth Girard, Julien H. Marino, Sebastian Bendahan-West, Raphael Strampelli, Giovanni M. James, Andrew D. Stephenson, Klaus Subbotina Ferrer-Chavez, Rodrigo Booth, Mark Sutlieff, Ben J. Sanghi, Aniket Fontanive, Clemence Rickman, Emily Rebollido, Isabel Hoch, Kielan Balmer, William O. |
| author_facet | Palatnick, Skyler Millar-Blanchaer, Maxwell A. Zhang, Jingwen Lawson, Kellen Lewis, Briley L. Crotts, Katie A. Carter, Aarynn L. Biller, Beth Girard, Julien H. Marino, Sebastian Bendahan-West, Raphael Strampelli, Giovanni M. James, Andrew D. Stephenson, Klaus Subbotina Ferrer-Chavez, Rodrigo Booth, Mark Sutlieff, Ben J. Sanghi, Aniket Fontanive, Clemence Rickman, Emily Rebollido, Isabel Hoch, Kielan Balmer, William O. |
| contents | We report the discovery of a debris disk surrounding the M3 star, TWA 20, revealed by JWST coronagraphic observations using the Near-infrared Camera (NIRCam). With reference-star differential imaging (RDI), we resolve the disk in scattered light in the F200W filter at a high signal-to-noise ratio and in the F444W filter at a low signal-to-noise ratio. The disk morphology and orientation are characterized via a forward modeling approach, where we determine a radius of 64.7-6.5+6.2 AU and an inclination of 70.1-3.3+2.5 deg. Utilizing our forward model, we improve the fidelity of the debris disk image using model-constrained RDI (MCRDI). The newly discovered disk is one of only 6 disks detected in scattered light that orbit M dwarf stars; it is the third largest of the 6 resolved M dwarf disks and orbits the third faintest host star. The detection of this disk exemplifies the sensitivity of JWST to debris disks around low-luminosity host stars, which have historically been difficult to detect because these disks are cool and dim. We identify a nebulous structure that cannot be explained by an axisymmetric disk. A search for companions in the TWA 20 system yields no candidates. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2510_20216 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Discovery of a Debris Disk Around TWA 20 Palatnick, Skyler Millar-Blanchaer, Maxwell A. Zhang, Jingwen Lawson, Kellen Lewis, Briley L. Crotts, Katie A. Carter, Aarynn L. Biller, Beth Girard, Julien H. Marino, Sebastian Bendahan-West, Raphael Strampelli, Giovanni M. James, Andrew D. Stephenson, Klaus Subbotina Ferrer-Chavez, Rodrigo Booth, Mark Sutlieff, Ben J. Sanghi, Aniket Fontanive, Clemence Rickman, Emily Rebollido, Isabel Hoch, Kielan Balmer, William O. Earth and Planetary Astrophysics We report the discovery of a debris disk surrounding the M3 star, TWA 20, revealed by JWST coronagraphic observations using the Near-infrared Camera (NIRCam). With reference-star differential imaging (RDI), we resolve the disk in scattered light in the F200W filter at a high signal-to-noise ratio and in the F444W filter at a low signal-to-noise ratio. The disk morphology and orientation are characterized via a forward modeling approach, where we determine a radius of 64.7-6.5+6.2 AU and an inclination of 70.1-3.3+2.5 deg. Utilizing our forward model, we improve the fidelity of the debris disk image using model-constrained RDI (MCRDI). The newly discovered disk is one of only 6 disks detected in scattered light that orbit M dwarf stars; it is the third largest of the 6 resolved M dwarf disks and orbits the third faintest host star. The detection of this disk exemplifies the sensitivity of JWST to debris disks around low-luminosity host stars, which have historically been difficult to detect because these disks are cool and dim. We identify a nebulous structure that cannot be explained by an axisymmetric disk. A search for companions in the TWA 20 system yields no candidates. |
| title | Discovery of a Debris Disk Around TWA 20 |
| topic | Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2510.20216 |