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Context: We study the X-ray emission of the Galactic supernova remnant (SNR)CTB 109 (G109.1-1.0), which is well-known for its enigmatic half-shellmorphology both in radio and in X-rays and is associated with the anomalousX-ray pulsar (AXP) 1E2259+586. Aims: We want to understand the origin of theX-ray bright feature inside the SNR called the Lobe and the details of theinteraction of the SNR shock wave with the ambient interstellar medium (ISM).Methods: The Lobe and the northeastern part of the SNR were observed withChandra ACIS-I. We analysed the spectrum of the X-ray emission by dividing theentire observed emission into small regions. The X-ray emission is bestreproduced with one-component or two-component non-equilibrium ionisationmodels depending on the position. In the two-component model one emissioncomponent represents the shocked ISM and the other the shocked ejecta. Results:We detect enhanced element abundances, in particular for Si and Fe, in andaround the Lobe. There is one particular region next to the Lobe with a high Siabundance of 3.3 (2.6 - 4.0) times the solar value. This is the first,unequivocal detection of ejecta in CTB 109. Conclusions: The new Chandra dataconfirm that the Lobe was created by the interaction of the SNR shock and thesupernova ejecta with dense and inhomogeneous medium in the environment of SNRCTB 109. The newly calculated age of the SNR is t ~ 1.4 x 10^4 yr.

Chandra observation of the Galactic supernova remnant CTB 109 (G109.1-1.0)