Astron. Astrophys. 362, 1122-1126 (2000)

4. Conclusions

We have reported the first search for glycine in a solar type protostar. Our search was unsuccessful and provides an upper limit for the glycine column density of  cm^-2 in the cold envelope and consequently to the glycine abundance of . In the hot core, our upper limit on the glycine abundance is worse because of the beam dilution: . We discussed briefly that these observations already challenge a recently published model of glycine formation in the gas phase (Chakrabarti & Chakrabarti 2000). Deeper searches directed towards solar type-protostars may, however, still detect traces of glycine, as we have not yet reached the confusion limit, like in the case of massive protostars (Combes et al. 1996).

© European Southern Observatory (ESO) 2000

Online publication: October 30, 2000
helpdesk.link@springer.de