OH as an Alternate Tracer for Molecular Gas: Excitation Temperatures of the OH 18-cm Main Lines in W5

TL;DR

This study measures excitation temperatures of OH 18-cm lines in the W5 star-forming region, revealing differences between the main lines and demonstrating a method for more precise temperature estimation using continuum background variations.

Contribution

The paper introduces a continuum background method for measuring OH excitation temperatures, providing more accurate results than traditional methods and confirming temperature differences between the main lines.

Findings

$T^{65}_{ex} = 6.0 \,\pm\, 0.5$ K

$T^{67}_{ex} = 5.1 \,\pm\, 0.2$ K

The excitation temperature difference is approximately 0.9 K

Abstract

We present excitation temperatures $T_{ex}$ for the OH 18-cm main lines at 1665 and 1667 MHz measured directly in front of the W5 star-forming region, using observations from the Green Bank Telescope and the Very Large Array. We find unequivocally that $T_{ex}$ at 1665 MHz is greater than $T_{ex}$ at 1667 MHz. Our method exploits variations in the continuum emission from W5, and the fact that the continuum brightness temperatures $T_C$ in this nebula are close to the excitation temperatures of the OH lines in the foreground gas. The result is that an OH line can appear in emission in one location and in absorption in a neighboring location, and the value of $T_C$ where the profiles switch from emission to absorption indicates $T_{ex}$. Absolute measurements of $T_{ex}$ for the main lines were subject to greater uncertainty because of unknown effects of geometry of the OH features. We also employed the traditional "expected profile" method for comparison with our "continuum background" method, and found that the continuum background method provided more precise results, and was the one to definitively show the $T_{ex}$ difference. Our best estimate values are: $T^{65}_{ex} = 6.0 \pm 0.5$ K, $T^{67}_{ex} = 5.1 \pm 0.2$ K, and $T^{65}_{ex} - T^{67}_{ex} = 0.9 \pm 0.5$ K. The $T_{ex}$ values we have measured for the ISM in front of W5 are similar to those found in the quiescent ISM, indicating that proximity to massive star-forming regions does not generally result in widespread anomalous excitation of OH emission.