• DOI:10.1051/0004-6361/201527319
• Corpus ID: 54988209

Opacity broadening and interpretation of suprathermal CO linewidths: Macroscopic Turbulence and Tangled Molecular Clouds

@article{Hacar2016OpacityBA,
  title={Opacity broadening and interpretation of suprathermal CO linewidths: Macroscopic Turbulence and Tangled Molecular Clouds},
  author={{\'A}lvaro Hacar and Jo{\~a}o Alves and Andreas Burkert and Paul. F. Goldsmith},
  journal={arXiv: Astrophysics of Galaxies},
  year={2016}
}

• Á. Hacar, J. Alves, +1 author P. Goldsmith
• Published 28 March 2016
• Physics
• arXiv: Astrophysics of Galaxies

(Abridged) Many of the observed CO line profiles exhibit broad linewidths that greatly exceed the thermal broadening expected within molecular clouds. These suprathermal CO linewidths are assumed to be originated from the presence of unresolved supersonic motions inside clouds. Typically overlooked in the literature, in this paper we aim to quantify the impact of the opacity broadening effects on the current interpretation of the CO suprathermal line profiles. Without any additional contributions to the gas velocity field, a large fraction of the apparently supersonic (${\cal M}\sim$2-3) linewidths measured in both $^{12}$CO and $^{13}$CO (J=1-0) lines can be explained by the saturation of their corresponding sonic-like, optically-thin C$^{18}$O counterparts assuming standard isotopic fractionation. Combined with the presence of multiple components detected in our C$^{18}$O spectra, these opacity effects seem to be also responsible of the highly supersonic linewidths (${\cal M}>$8-10) detected in the broadest $^{12}$CO and $^{13}$CO spectra in Taurus. Our results demonstrate that most of the suprathermal $^{12}$CO and $^{13}$CO linewidths could be primarily created by a combination of opacity broadening effects and multiple gas velocity components blended in these saturated emission lines. Once corrected by their corresponding optical depth, each of these gas components present transonic intrinsic linewidths consistently traced by the three CO isotopologues within a factor of 2. Highly correlated and velocity-coherent at large scales, the largest and highly supersonic velocity differences inside clouds are generated by the relative motions between individual gas components. This highly discretized structure of the molecular gas traced in CO suggest that the gas dynamics inside molecular clouds could be better described by the properties of a fully-resolved macroscopic turbulence.