Solar disk observations of the AR. Upper part: simultaneous snapshots of the source region in EUVI-A (top row) and EUVI-B (bottom row) 284 Å channel images. (a) AR loops exhibiting a “sigmoidal”-like pre-eruptive morphology. The approximate eruptive volume and CME footpoints are also shown. (b) Arrows pointing in the direction of ribbon expansion during the eruption, indicating the likely orientation of the erupted MFR. (c) Our estimate for the shape of the MFR axis, represented by the dashed line, compared to the overall shape of the PEAs. The full movie of the event is available online. Lower part: (d) and (e) Evolution of the AR in magnetograms as observed by SDO/HMI, where positive (negative) polarity is indicated in white (black). The images are taken from JHelioviewer using the latitudinal projection and Carrington coordinates. As the AR is located near the far-side central meridian from Earth’s perspective, the magnetograms correspond to the times before the CME (d), when the AR was located close to the west limb, and after the CME (e), when the AR was located close to the east limb. The NOAA AR numbers are given on the legend. (f) EUVI-A 195 Å image, where the PEA orientation is indicated with the dashed white curve and the coronal loops overlaying the pre-eruptive flux rope are indicated with the dashed yellow curve (details given in the main text). The wavelet enhanced EUVI-A and EUVI-B images are obtained after processing the original data with the technique described in Stenborg et al. (2008) and are available at http://solar.jhuapl.edu/Data-Products/EUVI-Wavelets.php.