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. 2021 Oct 5;12:5837. doi: 10.1038/s41467-021-26071-8

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© The Author(s) 2021

Open Access This article is licensed under a Creative Commons Attribution 4.0 International License, which permits use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons license, and indicate if changes were made. The images or other third party material in this article are included in the article’s Creative Commons license, unless indicated otherwise in a credit line to the material. If material is not included in the article’s Creative Commons license and your intended use is not permitted by statutory regulation or exceeds the permitted use, you will need to obtain permission directly from the copyright holder. To view a copy of this license, visit http://creativecommons.org/licenses/by/4.0/.

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Fig. 7 — Spectral comparison of the north polar region (solid blue line) with the possible parent bodies, (142) Polana, (163) Erigone, and (495) Eulalia, the B-type near-Earth asteroid (3200) Phaethon and (101955) Bennu. Spectra are normalized at 0.55 µm and offset by 0.3. Reflectance spectra of (142) Polana, (163) Erigone, (495) Eulalia, (3200) Phaethon, and (101955) Bennu were obtained by refs. ^25,68,69, and ref. ³², respectively. Gray hatches for (142) Polana, (163) Erigone, and (495) Eulalia indicate 80% of the distribution of slope among their family members^29,70. Gray hatch for Phaethon indicates spectral variation over one rotation³¹.