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We present the results of the observations of a coronal mass ejection (CME),which occurred on May 13, 2009. The most important feature of theseobservations is that the CME was observed from the very early stage (the solarsurface) up to a distance of 15 solar radii ($R_\odot$). Below 2 $R_\odot$, weused the data from the TESIS EUV telescopes obtained in the Fe 171 A and He 304A lines, and above 2 $R_\odot$, we used the observations of the LASCO C2 and C3coronagraphs. The CME was formed at a distance of 0.2-0.5 $R_\odot$from theSun's surface as a U-shaped structure, which was observed both in the 171 Aimages and in white-light. Observations in the He 304 A line showed that theCME was associated with an erupting prominence, which was located not above-aspredicts the standard model-but in the lowest part of the U-shaped structureclose to the magnetic X-point. The prominence location can be explained withthe CME breakout model. Estimates showed that CME mass increased with time. TheCME trajectory was curved-its helio-latitude decreased with time. The CMEstarted at latitude of 50$^{\circ}$ and reached the ecliptic plane at distancesof 2.5 $R_\odot$. The CME kinematics can be divided into three phases: initialacceleration, main acceleration, and propagation with constant velocity. Afterthe CME onset GOES registered a sub-A-class flare.

Initiation and early evolution of the Coronal Mass Ejection on May 13, 2009 from EUV and white-light observations