Molecular Line Emission as a Tool for Galaxy Observations (LEGO)

I. HCN as a tracer of moderate gas densities in molecular clouds and galaxies

¹ Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
e-mail: jens.kauffmann@gmail.com
² Jet Propulsion Lab, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
³ Harvard–Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
⁴ Departamento de Astronomía, Universidad de Chile, Camino El Observatorio 1515, Las Condes, Santiago, Chile

Received: 7 May 2017
Accepted: 9 August 2017

Abstract

Trends observed in galaxies, such as the Gao & Solomon relation, suggest a linear relationship between the star formation rate and the mass of dense gas available for star formation. Validation of such trends requires the establishment of reliable methods to trace the dense gas in galaxies. One frequent assumption is that the HCN (J = 1–0) transition is unambiguously associated with gas at H₂ densities ≫ 10⁴ cm^-3. If so, the mass of gas at densities ≫ 10⁴ cm^-3 could be inferred from the luminosity of this emission line, L_{HCN (1–0)}. Here we use observations of the Orion A molecular cloud to show that the HCN (J = 1–0) line traces much lower densities ~ 10³ cm^-3 in cold sections of this molecular cloud, corresponding to visual extinctions A_V ≈ 6 mag. We also find that cold and dense gas in a cloud like Orion produces too little HCN emission to explain L_{HCN (1–0)} in star forming galaxies, suggesting that galaxies might contain a hitherto unknown source of HCN emission. In our sample of molecules observed at frequencies near 100 GHz (also including ¹²CO, ¹³CO, C¹⁸O, CN, and CCH), N₂H⁺ is the only species clearly associated with relatively dense gas.