Auxiliary Material for Paper 2011GL050253 Auroral evidence of Io's control over the magnetosphere of Jupiter B. Bonfond, D. Grodent, and J.-C. Gerard Laboratoire de Physique Atmospherique et Planetaire, Universite de Liege, Liege, Belgium T. Stallard Department of Physics and Astronomy, University of Leicester, Leicester, UK J. T. Clarke Center for Space Physics, Boston University, Boston, Massachusetts, USA M. Yoneda Planetary Plasma and Atmospheric Research Center, Graduate School of Science, Tohoku University, Sendai, Japan A. Radioti and J. Gustin Laboratoire de Physique Atmospherique et Planetaire, Universite de Liege, Liege, Belgium Bonfond, B., D. Grodent, J.-C. Gerard, T. Stallard, J. T. Clarke, M. Yoneda, A. Radioti, and J. Gustin (2012), Auroral evidence of Io's control over the magnetosphere of Jupiter, Geophys. Res. Lett., 39, L01105, doi:10.1029/2011GL050253. Introduction This auxiliary material contains six animations. 1. 2011gl050253-ms01.gif Animation S1. Engulfing of the Ganymede auroral footprint in the main auroral oval of Jupiter. Polar projection of the northern hemisphere aurora on February 27th and on May 21st 2007. The observing geometry was very similar, with CMLs of 155.3 deg and 159.7 deg respectively and a Ganymede S3 longitude of 246.6 deg and 247.0 deg respectively. Nevertheless, the Ganymede footprint is outside the main emission in the first image and inside it in the second case, suggesting that the corotation breakdown boundary has moved inside the Ganymede orbit (15 Rj). Additionally, the Ganymede footprint location moved 0.5 deg equatorwards implying an increased stretching of the magnetic field lines. The white line is the reference oval from February 2007. 2. 2011gl050253-ms02.gif Animation S2. Expansion of the northern main oval. Averaged polar projections of the northern hemisphere aurora for the Spring 2005, Spring 2006, February 2007, March 2007, May 2007 and June 2007 periods. We can clearly see the main oval expending in May-June 2007. The white line is the reference oval from February 2007. 3. 2011gl050253-ms03.gif Animation S3. Expansion of the southern main oval. Averaged polar projections of the southern hemisphere aurora for the February 2007, March 2007, April 2007, May 2007 and June 2007 periods. We can clearly see the main oval expending in May-June 2007. The white line is the reference oval from February 2007. 4. 2011gl050253-ms04.gif Animation S4. Injection blob in the IR and the UV. This animation shows two images sets acquired less than 2 hours apart in the IR domain with the IRTF in the southern hemisphere on the bottom side and in the UV domain with the Hubble Space Telescope in the northern hemisphere on the top side. On each side, the white line underlines the large auroral blob which is tracked from one hemisphere to the other. 5. 2011gl050253-ms05.gif Animation S5. Io footprint in the northern hemisphere. Typical sequence of images of the northern aurora on Jupiter. The Io footprint is clearly visible. 6. 2011gl050253-ms06.gif Animation S6. Disappearance of the Io footprint in the northern hemisphere. While Io's S3 longitude is nearly the same as in the previous animation, the Io footprint only becomes visible at the end of the sequence, while it would be expected to lie at the border of the unusually equatorward patch of diffuse emission. This disappearance of the Io fooprint is unique within more than 10 years of high-resolution/high sensibility HST images and is probably due to a disrupted interaction between Io and the depleted flux tubes connected to the patch.