Outflow In NGC Research Articles

Shocked molecular hydrogen in the bipolar outflow NGC 2071

Maps of the emission from the v = 1-0 S(1) line of molecular hydrogen in the bipolar outflow of NGC 2071 are presented. The line emission is shown to peak at six positions distributed irregularly along two lobes which are parallel to, but offset about 20 arcsec from, the lobes of the high-velocity CO-line emission. The energetics and composition of the high-velocity gas support a model in which the driving agent is a bipolar atomic wind which arises from the vicinity of the central IR sources and shocks the surrounding molecular cloud, evacuating a cavity within it.

High-resolution mapping of molecular outflows in NGC 2071, W49, and NGC 7538

On presente des cartes de haute resolution (7'') du gaz moleculaire et de l'emission continue dans les noyaux de NGC 2071, W 49 et NGC 7538. Les masses du gaz de haute vitesse, detecte par l'interferometre, sont respectivement de 0,2; 138 et 12 M ○. . L'emission continue a 2,7 mm a ete detectee dans toutes les sources

Energetic activity in a star-forming molecular cloud core - A disk constrained bipolar outflow in NGC 2071

The discovery of an extended, high-velocity molecular outflow associated with the infrared sources in NGC 2071 is reported. High-velocity CO emission from this star-forming molecular cloud core can be traced over a region 4' in diameter and detected over a velocity range of 70 km s/sup -1/. The flow is bipolar; the blueshifted CO emission is displaced to the northeast, while the redshifted emission is displaced to the southwest. Observations in the 98 GHz transition of CS reveal a ridge of dense gas oriented orthogonal to the high-velocity flow axis. A systematic velocity gradient seen in the CS line core suggests that the ridge is a dense, rotating disk centered on the IR source. The disk may be responsible for collimating a spherically symmetric wind originating near the IR source into the bipolar flow observed in the high-velocity CO line wings. The high-velocity CO line wings are modeled as beam diluted emission from clumps or filaments with /sup 12/ CO optical depths close to unity and a small filling factor. The clumps may be either objects ejected from the vicinity of the central infrared source or shocked gas at the front where a higher velocity but invisible flow encounters ambientmore » cloud material.« less