Astronomy and Astrophysics – Astrophysics
Scientific paper
Jan 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...293l...9g&link_type=abstract
Astronomy and Astrophysics 293L, L9-L12 (1995)
Astronomy and Astrophysics
Astrophysics
16
Binaries: Symbiotic, Stars: Ag Pegasi, Stars: Mass Loss, Novae
Scientific paper
The 313-220 line of water at 183 GHz has been observed from the ground at three different periods toward W49N, a key galactic source in the study of water masers. The line profiles consist of two strong velocity spikes superimposed on a broad plateau extending over a velocity range of about 400 km/s. The first spike corresponds to the "ambient" cloud component (AC) which is observed in many other molecular lines, whereas the second spke (termed HVC, for high-velocity component) is blueshifted by about 36 km/s with respect to the ambient emission, and does not have known counterparts in other tracers. Although probably of maser nature, the 183 GHz water line emission is spatially extended along the cloud, and it is more stable in time than the 22 and 325 GHz lines of water. We give plausible lower limits of the water column density and abundance. Furthermore, we report the discovery of a unusually fast CO outflow -- with velocities in excess of 150 km/s -- toward the center of W49N. A comparison of the H2O and CO data suggests taht the HVC feature arises in a dense layer of hot material which has been shock-compressed by the action of the outflows.
Bachiller Rafael
Cernicharo Jose
Fuente Asuncion
Gonzalez-Alfonso Eduardo
No associations
LandOfFree
183 GHz water emission in W 49N. does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with 183 GHz water emission in W 49N., we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and 183 GHz water emission in W 49N. will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1817731