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. 2019 Jun 21;10:2751. doi: 10.1038/s41467-019-10708-w

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© The Author(s) 2019

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. 4 — Estimated electron density N_e0 of the JDP locations using the propagation model. This profile is the upper bound ionospheric density because the JDP L–O mode waves should transect Jupiter’s ionosphere and plasma irregularities from the lightning stroke to Juno. The transparent regions correspond to vertical projections of Juno when the Waves LFR-Hi observations were made. The observational locations of radio occultation measurements are depicted as triangles for Voyager 2²⁰ and crosses for Galileo²¹. The Jovian image was provided by NASA/JPL-Caltech/SSI/SwRI/MSSS/ASI/INAF/JIRAM/Björn Jónsson (http://www.planetary.org/multimedia/space-images/jupiter/merged-cassini-and-juno.html)