We present new, wide, and deep images in the AzTEC/ASTE 1.1 mm continuum and the 12 CO (J = 1–0) emission toward the northern part of the Orion-A GMC. We have found evidence for interactions between molecular clouds and the external forces that may trigger star formation. Two types of possible triggers were revealed: (1) Collisions of the diffuse gas on the cloud surface, particularly at the eastern side of the OMC-2/3 region, and (2) Irradiation of UV on the pre-existing filaments and dense molecular cloud cores. Our wide-field and high-sensitivity imaging has provided the first comprehensive view of the potential sites of triggered star formation in the Orion-A GMC.

A new high-resolution infrared spectrometer using an optical parametric oscillator working at 5 μm as radiaton source has been assembled in the Cologne laboratory and is now operated routinely. As one of the first projects, we have reobserved the ν3 vibrational fundamental (asymmetric C-C stretching mode) of Si2C3 located at 1968.2 cm-1.

We present the initial results of a spectral line survey of L1157 B1 with the Nobeyama 45 m telescope. So far, we have covered the frequencey range of 13.7 GHz (82.0–94.5 GHz and 96.3–97.5 GHz), and have detected 22 species including CH3CHO, HCOOH, HCOOCH3, HNCO, NH2CHO, CH3CN, and CCS. We have also detected the line of CH2DOH. These results demonstrate rich chemistry in this shocked region, which would mainly originate from evaporation of ice mantles by means of shocks.

Herschel-HIFI observations of high-J lines (up toJu = 10) of 12CO, 13CO andC18O are presented toward three deeply embedded low-mass protostars in NGC1333. The observations show several energetic components including shocked and quiescentgas. Radiative transfer models are used to quantify the C18O envelope abundancewhich require a jump in the abundance at an evaporation temperature,Tev ~ 25 K, providing new direct evidence of a COice evaporation zone around protostars. The abundance in the outermost part of theenvelope, X0, is within the canonical value of2 × 10-4; however the inner abundance, Xin, isfound around a factor of 3–5 lower than X0.