TOI-880 is an Aligned, Coplanar, Multi-planet System
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| Main Authors: | , , , , , , , , , , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2025
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| author | Zhang, Elina Y. Teng, Huan-Yu Dai, Fei Howard, Andrew W. Halverson, Samuel P. Isaacson, Howard Rubenzahl, Ryan A. Wang, Xian-Yu Wang, Songhu Fulton, Benjamin J. Nielsen, Louise D. Lubin, Jack Giacalone, Steven Handley, Luke B. Petigura, Erik A. Turtelboom, Emma V. Polanski, Alex S. Gibson, Steve R. Rider, Kodi Roy, Arpita Baker, Ashley Edelstein, Jerry Smith, Christopher L. Walawender, Josh Winn, Joshua N. |
| author_facet | Zhang, Elina Y. Teng, Huan-Yu Dai, Fei Howard, Andrew W. Halverson, Samuel P. Isaacson, Howard Rubenzahl, Ryan A. Wang, Xian-Yu Wang, Songhu Fulton, Benjamin J. Nielsen, Louise D. Lubin, Jack Giacalone, Steven Handley, Luke B. Petigura, Erik A. Turtelboom, Emma V. Polanski, Alex S. Gibson, Steve R. Rider, Kodi Roy, Arpita Baker, Ashley Edelstein, Jerry Smith, Christopher L. Walawender, Josh Winn, Joshua N. |
| contents | Although many cases of stellar spin-orbit misalignment are known, it is usually unclear whether a single planet's orbit was tilted or if the entire protoplanetary disk was misaligned. Measuring stellar obliquities in multi-transiting planetary systems helps to distinguish these possibilities. Here, we present a measurement of the sky-projected spin-orbit angle for TOI-880 c (TOI-880.01), a member of a system of three transiting planets, using the Keck Planet Finder (KPF). We found that the host star is a K-type star ($T_{\rm eff}=5050 \pm 100$ K). Planet b (TOI-880.02) has a radius of $2.19\pm0.11\mathrm{R_{\oplus}}$ and an orbital period of $2.6$ days; planet c (TOI-880.01) is a Neptune-sized planet with $4.95\pm0.20\mathrm{R_{\oplus}}$ on a $6.4$-day orbit; and planet d (TOI-880.03) has a radius of $3.40_{-0.21}^{+0.22}\mathrm{R_{\oplus}}$ and a period of $14.3$ days. By modeling the Rossiter-McLaughlin (RM) effect, we found the sky-projected obliquity to be $|λ_c| = 7.4_{-7.2}^{+6.8}$$^{\circ}$, consistent with a prograde, well-aligned orbit. The lack of detectable rotational modulation of the flux of the host star and a low $\rm v\sin{i_\star}$ (1.6~km/s) imply slow rotation and correspondingly slow nodal precession of the planetary orbits and the expectation that the system will remain in this coplanar configuration. TOI-880 joins a growing sample of well-aligned, coplanar, multi-transiting systems. Additionally, TOI-880 c is a promising target for JWST follow-up, with a transmission spectroscopy metric (TSM) of $\sim 170$. We could not detect clear signs of atmospheric erosion in the H$α$ line from TOI-880 c, as photoevaporation might have diminished for this mature planet. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2507_16194 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | TOI-880 is an Aligned, Coplanar, Multi-planet System Zhang, Elina Y. Teng, Huan-Yu Dai, Fei Howard, Andrew W. Halverson, Samuel P. Isaacson, Howard Rubenzahl, Ryan A. Wang, Xian-Yu Wang, Songhu Fulton, Benjamin J. Nielsen, Louise D. Lubin, Jack Giacalone, Steven Handley, Luke B. Petigura, Erik A. Turtelboom, Emma V. Polanski, Alex S. Gibson, Steve R. Rider, Kodi Roy, Arpita Baker, Ashley Edelstein, Jerry Smith, Christopher L. Walawender, Josh Winn, Joshua N. Earth and Planetary Astrophysics Although many cases of stellar spin-orbit misalignment are known, it is usually unclear whether a single planet's orbit was tilted or if the entire protoplanetary disk was misaligned. Measuring stellar obliquities in multi-transiting planetary systems helps to distinguish these possibilities. Here, we present a measurement of the sky-projected spin-orbit angle for TOI-880 c (TOI-880.01), a member of a system of three transiting planets, using the Keck Planet Finder (KPF). We found that the host star is a K-type star ($T_{\rm eff}=5050 \pm 100$ K). Planet b (TOI-880.02) has a radius of $2.19\pm0.11\mathrm{R_{\oplus}}$ and an orbital period of $2.6$ days; planet c (TOI-880.01) is a Neptune-sized planet with $4.95\pm0.20\mathrm{R_{\oplus}}$ on a $6.4$-day orbit; and planet d (TOI-880.03) has a radius of $3.40_{-0.21}^{+0.22}\mathrm{R_{\oplus}}$ and a period of $14.3$ days. By modeling the Rossiter-McLaughlin (RM) effect, we found the sky-projected obliquity to be $|λ_c| = 7.4_{-7.2}^{+6.8}$$^{\circ}$, consistent with a prograde, well-aligned orbit. The lack of detectable rotational modulation of the flux of the host star and a low $\rm v\sin{i_\star}$ (1.6~km/s) imply slow rotation and correspondingly slow nodal precession of the planetary orbits and the expectation that the system will remain in this coplanar configuration. TOI-880 joins a growing sample of well-aligned, coplanar, multi-transiting systems. Additionally, TOI-880 c is a promising target for JWST follow-up, with a transmission spectroscopy metric (TSM) of $\sim 170$. We could not detect clear signs of atmospheric erosion in the H$α$ line from TOI-880 c, as photoevaporation might have diminished for this mature planet. |
| title | TOI-880 is an Aligned, Coplanar, Multi-planet System |
| topic | Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2507.16194 |