As a stellar X-ray source DG Tau shows two rather unusual features: A resolved X-ray jet [2] and an X-ray spectrum best described by two thermal components with different absorbing column densities, a so called “two-absorber X-ray (TAX)” morphology [1, 2]. In an effort to understand the properties of the central X-ray source in DG Tau a detailed position analysis was carried out. Our work is based on the archival Chandra data of DG Tau (90 ks in total) described in detail in [2]. We use the same energy ranges for the soft (0.3–1.1 keV) and the hard spectral component (1.7–7.0 keV) as in [2]. The excellent angular resolution of the Chandra telescope allows to measure relative positions with an accuracy of ~0.1 arcsec. We tentatively identify the hard, strongly absorbed, X-ray component with coronal emission of DG Tau. The TAX property of the spectrum suppresses the mutual contamination of the components almost completely. If the soft component is emitted not from the star itself but rather from – say – a shocked wind, one might find a position difference between the soft and the hard X-ray components.