other query modes : |
Identifier query |
Coordinate query |
Criteria query |
Reference query |
Basic query |
Script submission |
TAP |
Output options |
Object types |
Help |
2011MNRAS.411.2293J - Mon. Not. R. Astron. Soc., 411, 2293-2310 (2011/March-2)
Spectral imaging of the Sagittarius B2 region in multiple 7-mm molecular lines.
JONES P.A., BURTON M.G., TOTHILL N.F.H. and CUNNINGHAM M.R.
Abstract (from CDS):
There are significant differences between the distributions of different molecules, in part due to spatial differences in chemical abundance across the complex. For example, HNCO and HOCO+ are found preferentially in the north cloud, and CH2 NH near Sgr B2 (N). Some of the differences between lines are due to excitation differences, as shown by the 36.17- and 44.07-GHz lines of CH3OH, which have maser emission, compared to the 48.37-GHz line of CH3OH. Other major differences in integrated molecular line distribution are due to absorption of the 7-mm free-free continuum emission (spatially traced by the radio recombination line emission) by cool intervening molecular material, causing a central dip in the molecular line distributions.
These line distribution similarities and differences have been statistically described by Principal Component Analysis and interpreted in terms of simple Sgr B2 physical components of the cooler, lower density envelope, and dense, hot cores Sgr B2 (N), (M) and (S).
Abstract Copyright: 2010 The Authors Monthly Notices of the Royal Astronomical Society2010 RAS
Journal keyword(s): ISM: individual objects: Sagittarius B2 - ISM: kinematics and dynamics - ISM: molecules - radio lines: ISM
Simbad objects: 7
To bookmark this query, right click on this link: simbad:2011MNRAS.411.2293J and select 'bookmark this link' or equivalent in the popup menu