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Summary
| Description |
Fig. 1: Detection of Q1R, Q2R, and the main body in the Gemini (z’) light curve. The normalized flux is plotted in black vs. time (UTC), while the best-fitting models are over plotted in red. The shallow events caused by Q1R (ingress) and Q2R (ingress & egress) are fitted by a square model. A Lorentzian function fits the dense part of Q1R at egress; see Sect. 3. The spikes observed during the disappearance and the re-appearance of the star behind Quaoar stem from the diffraction by the sharp opaque limb of the body. Note: there is a variation in the flux close to -110 and 290 seconds, caused by sudden variations in the seeing, and they can be neglected. More detailed views of Q1R and Q2R obtained at other telescopes are displayed in Figs. 2, D.1, E.1, and E.2. |
| Date | |
| Source | https://arxiv.org/abs/2304.09237 |
| Author | C. L. Pereira et al., posted on arXiv |
| Permission (Reusing this file) |
This paper and its contents (including this image) are licensed under CC-BY-4.0 International as noted under the download options of the arXiv abstract: https://arxiv.org/abs/2304.09237 |
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| Date/Time | Thumbnail | Dimensions | User | Comment | |
|---|---|---|---|---|---|
| current | 03:26, 22 April 2023 | | 3,496 × 1,400 (395 KB) | Nrco0e | Uploaded a work by C. L. Pereira et al., posted on arXiv from https://arxiv.org/abs/2304.09237 with UploadWizard |
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