| Download | - View final version: A near-infrared survey of candidate Haumea family members (PDF, 623 KiB)
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| DOI | Resolve DOI: https://doi.org/10.3847/1538-3881/ad864e |
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| Author | Search for: Proudfoot, Benjamin C. N.ORCID identifier: https://orcid.org/0000-0002-1788-870X; Search for: Fernández-Valenzuela, EstelaORCID identifier: https://orcid.org/0000-0003-2132-7769; Search for: Stansberry, John A.ORCID identifier: https://orcid.org/0000-0003-2434-5225; Search for: Kiss, CsabaORCID identifier: https://orcid.org/0000-0002-8722-6875; Search for: Ragozzine, DarinORCID identifier: https://orcid.org/0000-0003-1080-9770; Search for: Fraser, Wesley C.1ORCID identifier: https://orcid.org/0000-0001-6680-6558; Search for: Pike, Rosemary E.ORCID identifier: https://orcid.org/0000-0003-4797-5262; Search for: Pinilla-Alonso, NoemiORCID identifier: https://orcid.org/0000-0002-2770-7896 |
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| Affiliation | - National Research Council Canada. Herzberg Astronomy and Astrophysics
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| Funder | Search for: National Research, Development and Innovation Office; Search for: Space Telescope Science Institute |
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| Format | Text, Article |
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| Subject | trans-Neptunian objects; HST photometry; dynamical evolution |
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| Abstract | The Haumea family is the only known dynamical family in the trans-Neptunian region. To date, 10 family members have been unambiguously identified using near-infrared (NIR) spectral or photometric data in combination with their strong dynamical proximity and the rest of the family. In this work, we build off previous empirically constructed models of the family to identify 39 candidate family members and follow up on eight of them using the Hubble Space Telescope (HST) to measure their visible and NIR colors. Six of the candidates have strong water-ice absorption features—consistent with family membership. Based on these initial findings, our sample of 39 candidate family members should contain about 20 more water-rich objects. Combining the HST visible and NIR photometry with past results, we find no evidence for significant color heterogeneity within the family. Of the six new family members, two have Δv ∼ 300 m s⁻¹, well outside of the traditionally defined velocity dispersion limit of ∼150 m s⁻¹. As evidence suggests they are not affected by any of Neptune's resonances, we propose that these family members are the result of dynamical sculpting by Neptune during its outward migration. Further searches for far-flung family members will be able to further explore this hypothesis. |
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| Publication date | 2024-11-18 |
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| Publisher | American Astronomical Society |
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| Licence | |
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| In | |
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| Language | English |
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| Peer reviewed | Yes |
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| Export citation | Export as RIS |
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| Report a correction | Report a correction (opens in a new tab) |
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| Record identifier | 0d29292c-4fd4-4af1-9226-1392cb246ec4 |
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| Record created | 2025-02-12 |
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| Record modified | 2025-02-12 |
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