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We attempt to achieve a better understanding of the gas distribution andvelocity field around the deeply embedded Class 0 protostar SMM 3 in the OrionB9 star-forming region. Using the APEX 12-m telescope, we mapped the lineemission from the J=2-1 rotational transition of two CO isotopologues, 13CO andC18O, over a 4' x 4' region around Orion B9/SMM 3. Both the 13CO and C18O linesexhibit two well separated velocity components at about 1.3 and 8.7 km/s. Theemission of both CO isotopologues is more widely distributed than thesubmillimetre dust continuum emission as probed by LABOCA. The LABOCA870-micron peak position of SMM 3 is devoid of strong CO isotopologue emission,which is consistent with our earlier detection of strong CO depletion in thesource. No signatures of a large-scale outflow were found towards SMM 3. The13CO and C18O emission seen at ~1.3 km/s is concentrated into a singleclump-like feature at the eastern part of the map. The peak H2 column densitytowards a C18O maximum of the low-velocity component is estimated to be ~10^22cm-2. A velocity gradient was found across both the 13CO and C18O maps.Interestingly, SMM 3 lies on the border of this velocity gradient. The 13CO andC18O emission at ~1.3 km/s is likely to originate from the "low-velocity part"of Orion B. Our analysis suggests that it contains high density gas, whichconforms to our earlier detection of deuterated species at similarly low radialvelocities. The sharp velocity gradient in the region might represent a shockfront resulting from the feedback from the nearby expanding HII region NGC2024. The formation of SMM 3, and possibly of the other members of Orion B9,might have been triggered by this feedback.

13CO and C18O J=2-1 mapping of the environment of the Class 0 protostellar core SMM 3 in Orion B9