# CO multi-line observations of HH 80-81: a two-component molecular outflow associated with the largest protostellar jet in our Galaxy

## TL;DR

This study presents multi-line CO observations revealing a two-component molecular outflow associated with the largest known protostellar jet, providing insights into high-mass star formation and outflow evolution.

## Contribution

It identifies a two-component outflow structure in HH 80-81 and analyzes its properties, linking jet and outflow dynamics in massive star formation.

## Key findings

- Detection of a collimated and a wide-angle outflow component.
- Outflow temperature around 88 K indicating shock heating.
- Mass of outflow dominated by the wide-angle component.

## Abstract

Stretching a length reaching 10 pc projected in the plane of sky, the radio jet associated with Herbig-Haro objects 80 and 81 (HH 80-81) is known as the largest and best collimated protostellar jet in our Galaxy. The nature of the molecular outflow associated with this extraordinary jet remains an unsolved question which is of great interests to our understanding of the relationship between jets and outflows in high-mass star formation. Here we present Atacama Pathfinder EXperiment CO(6-5) and (7-6), James Clerk Maxwell Telescope CO(3-2), Caltech Submillimeter Observatory CO(2-1), and Submillimeter Array CO and $^{13}$CO(2-1) mapping observations of the outflow. We report on the detection of a two-component outflow consisting of a collimated component along the jet path and a wide-angle component with an opening angle of about $30^{\circ}$. The gas velocity structure suggests that each of the two components traces part of a primary wind. From LVG calculations of the CO lines, the outflowing gas has a temperature around 88 K, indicating that the gas is being heated by shocks. Based on the CO(6-5) data, the outflow mass is estimated to be a few $M_{\odot}$, which is dominated by the wide-angle component. A comparison between the HH 80-81 outflow and other well shaped massive outflows suggests that the opening angle of massive outflows continues to increase over time. Therefore, the mass loss process in the formation of early-B stars seems to be similar to that in low-mass star formation, except that a jet component would disappear as the central source evolves to an ultracompact HII region.