# APEX Millimeter Observations of Methanol Emission Toward High-Mass Star-Forming Cores

## TL;DR

This study uses APEX telescope observations at 247 GHz to analyze methanol emission in sixteen high-mass star-forming regions, revealing temperature, density, and chemical differences across evolutionary stages, and exploring potential maser activity.

## Contribution

First detailed methanol line survey across diverse high-mass star-forming cores, estimating physical parameters and examining maser emission potential.

## Key findings

- Hot cores show rich methanol spectra, warm cores do not.
- Methanol rotational temperatures range from 104 to 168 K.
- Virial masses are significantly higher than gas masses.

## Abstract

We present 247-GHz molecular line observations of methanol (CH$_3$OH) toward sixteen massive star-forming regions, using the APEX telescope with an angular resolution of $25''$. The sample covers a range of evolutionary states, including warm molecular cores, hot molecular cores, and ultracompact HII regions. The hot cores, all of which include UC HII regions, show rich molecular line spectra, although the strength of different species and transitions varies from source to source. In contrast, the warm cores do not show significant molecular line emission. Multiple methanol transitions are detected toward nine of the hot cores; eight of these had enough transitions to use the rotation diagram method to estimate rotational temperatures and column densities. The temperatures lie in the range 104$-$168 K and column densities from $3\times10^{16}$ to $7\times10^{18}$ cm$^{-2}$. Using the average methanol line parameters, we estimate virial masses, which fall in the range from 145 to 720 M$_\odot$ and proved to be significantly higher than the measured gas masses. We discuss possible scenarios to explain the chemical differences between hot cores and warm molecular cores. One of the observed methanol lines, $4_{2}-5_{1}A^{+}$ at 247.228 GHz, is predicted to show class II maser emission, similar in intensity to previously reported $J_0-J_{-1}E$ masers at 157 GHz. We did not find any clear evidence for maser emission among the observed sources; however, a weak maser in this line may exist in G345.01+1.79.