The Excitation of HCN and HCO+ in the Galactic Center Circumnuclear Disk

• Published in: arXiv.org
• Main Authors: Mills, Elisabeth A C, Güsten, Rolf, Requena Torres, Miguel A, Morris, Mark R
• Format: Paper Journal Article
• Language: English
• Published: Ithaca Cornell University Library, arXiv.org 24.10.2013
• Subjects: Dust; Emission; Excitation; Galaxies; Physics - Astrophysics of Galaxies; Radiative transfer
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.1309.7412

We present new observations of HCN and HCO+in the circumnuclear disk (CND) of the Galaxy, obtained with the APEX telescope. We have mapped emission in rotational lines of HCN J = 3-2, 4-3, and 8-7, as well as HCO+ J = 3-2, 4-3, and 9-8. We also present spectra of H13CN and H13CO+ toward four positions in the CND. Using the intensities of all of these lines, we present an excitation analysis for each molecule using the non-LTE radiative transfer code RADEX. The HCN line intensities toward the northern emission peak of the CND yield log densities (cm^-3) of 5.6 +0.6/-0.6, consistent with those measured with HCO+, as well as with densities recently reported for this region from an excitation analysis of highly-excited lines of CO. These densities are too low for the gas to be tidally stable. The HCN line intensities toward the CND's southern emission peak yield log densities of 6.5 +0.5/-0.7, higher than densities determined for this part of the CND with CO (although the densities measured with HCO+, log [n] = 5.6 +0.2/-0.2, are more consistent with the CO-derived densities). We investigate whether the higher densities we infer from HCN are affected by mid-infrared radiative excitation of this molecule through its 14 micron rovibrational transitions. We find that radiative excitation is important for at least one clump in the CND, where we additionally detect the J = 4-3, v2=1 vibrationally-excited transition of HCN, which is excited by dust temperatures of > 125-150 K. If this hot dust is present elsewhere in the CND, it could lower our inferred densities, potentially bringing the HCN-derived densities for the Southern part of the CND into agreement with those measured using HCO+ and CO. Additional sensitive, high-resolution submillimeter observations, as well as mid-infrared observations, would be useful to assess the importance of the radiative excitation of HCN in this environment.