2014A&A...562A.131S

The IC 1396 A globule, located to the west of the young cluster Tr 37, is known to host many very young stars and protostars, and is also assumed to be a site of triggered star formation. Our aim is to test the triggering mechanisms and sequences leading to star formation in Tr 37 and similar regions. We mapped IC 1396 A with Herschel/PACS at 70 and 160µm. The maps reveal the structure of the most embedded parts of the star-forming site in great detail. The Herschel/PACS maps trace the very embedded protostellar objects and the structure of the cloud. PACS data reveal a previously unknown Class 0 object, labeled IC 1396 A-PACS-1, located behind the ionization front. IC 1396 A-PACS-1 is not detectable with Spitzer, but shows marginal X-ray emission. The data also allow the study of three of the Class I intermediate-mass objects within the cloud. We derived approximate cloud temperatures to study the effect and potential interactions between the protostars and the cloud. The Class 0 object is associated with the densest and coldest part of IC 1396 A. Heating in the cloud is dominated by the winds and radiation of the O6.5 star HD 206267 and, to a lesser extent, by the effects of the Herbig Ae star V 390 Cep. The surroundings of the Class I and Class II objects embedded in the cloud also appear warmer than the sourceless areas, although most of the low-mass objects cannot be individually extracted owing to distance and beam dilution. The observations suggest that at least two episodes of star formation have occurred in IC 1396 A. One would have been the origin of the known, ∼1Myr-old Class I and II objects in the cloud, and a new wave of star formation would have produced the Class 0 source at the tip of the bright-rimmed cloud. From its location and properties, IC 1396 A-PACS-1 is consistent with having been triggered via radiative driven implosion (RDI) induced by HD 206267. The mechanisms behind the formation of the more evolved population of Class I/II/III objects in the cloud are uncertain. Heating of most of the remaining cloud by Class I/Class II objects and by HD 206267 itself may preclude further star formation in the region.