Open Access
Erratum
This article is an erratum for:
[https://doi.org/10.1051/0004-6361/202346365]


Issue
A&A
Volume 683, March 2024
Article Number C4
Number of page(s) 3
Section Letters to the Editor
DOI https://doi.org/10.1051/0004-6361/202346365e
Published online 13 March 2024

We identified an error in our opacity calculations for Quaoar’s rings in the original paper.

We used the Cuzzi (1985) calculations to obtain the ring opacity, accounting for both the Fresnel diffraction caused by the ring and the Airy diffraction caused by individual particles. These calculations show that the actual ring optical depth is half the apparent optical depth observed during Earth-based stellar occultations, as detailed in the correct equations of our Appendix E. However, this correction was applied twice in our fitting code, resulting in optical depths underestimated by a factor of two in the text and Table E.1.

The corrected values of optical depths are listed in Table 1 below, with the associated corrections on equivalent widths and equivalent depths. This does not change the main conclusion of the original paper, but using the incorrect normal optical depths presented previously would result in underestimated values of the particle filling factor and thus collision rate. Also, when ring photometry becomes available, it would underestimate the particle albedo.

Table 1.

Revised physical parameters of rings Q1R and Q2R.

Moreover, we mentioned an optical depth peaking at τN ∼ 0.4 for the dense part of ring Q1R. Previously, this value was obtained from the equivalent optical depth and the full width at half maximum (FWHM) of the fitted Lorentzian. Here we used the exact peak value to calculate the normal opacities, pN, and optical depths, τN, for the Q1R dense region.

References

  1. Cuzzi, J. N. 1985, Icarus, 63, 312 [NASA ADS] [CrossRef] [Google Scholar]

© The Authors 2024

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All Tables

Table 1.

Revised physical parameters of rings Q1R and Q2R.

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