The Radio Continuum, Far-Infrared Emission, And Dense Molecular Gas In Galaxies

TL;DR

This study reveals tight linear correlations between HCN line luminosity, radio continuum, and far-infrared emission in galaxies, highlighting HCN's effectiveness as a star formation tracer and the potential of radio luminosity as a FIR proxy.

Contribution

It demonstrates that FIR-RC and FIR-HCN correlations are the tightest and most linear, establishing RC as a practical FIR indicator and confirming HCN's superior role in tracing star-forming molecular gas.

Findings

FIR-RC and FIR-HCN correlations are the tightest and most linear.

RC luminosity can serve as a proxy for FIR in star formation rate estimation.

HCN correlates better with FIR than CO, emphasizing its role as a star formation tracer.

Abstract

A tight linear correlation is established between the HCN line luminosity and the radio continuum (RC) luminosity for a sample of 65 galaxies (from Gao & Solomon's HCN survey), including normal spiral galaxies and luminous and ultraluminous infrared galaxies (LIRGs/ULIRGs). After analyzing the various correlations among the global far-infrared (FIR), RC, CO, and HCN luminosities and their various ratios, we conclude that the FIR-RC and FIR-HCN correlations appear to be linear and are the tightest among all correlations. The combination of these two correlations could result in the tight RC-HCN correlation we observed. Meanwhile, the non-linear RC-CO correlation shows slightly larger scatter as compared with the RC-HCN correlation, and there is no correlation between ratios of either RC/HCN-CO/HCN or RC/FIR-CO/FIR. In comparison, a meaningful correlation is still observed between ratios of RC/CO-HCN/CO. Nevertheless, the correlation between RC/FIR and HCN/FIR also disappears, reflecting again the two tightest FIR-RC and FIR-HCN correlations as well as suggesting that FIR seems to be the bridge that connects HCN with RC. Interestingly, despite obvious HCN-RC and RC-CO correlations, multi-parameter fits hint that while both RC and HCN contribute significantly (with no contribution from CO) to FIR, yet RC is primarily determined from FIR with a very small contribution from CO and essentially no contribution from HCN. These analyses confirm independently the former conclusions that it is practical to use RC luminosity instead of FIR luminosity, at least globally, as an indicator of star formation rate in galaxies including LIRGs/ULIRGs, and HCN is a much better tracer of star-forming molecular gas and correlates with FIR much better than that of CO.