Central molecular zones in galaxies: multitransition survey of dense gas tracers HCN, HNC, and HCO+

TL;DR

This study presents a comprehensive multitransition survey of dense gas tracers HCN, HNC, and HCO+ in 46 galaxies, revealing complex relationships between molecular line emissions, galaxy properties, and star formation indicators.

Contribution

It provides the first extensive multitransition database for HCN, HNC, and HCO+ in galaxies, analyzing their line ratios and physical conditions to better understand dense gas and star formation.

Findings

Line ratios do not correlate well with luminosities or other line ratios.

HCN and HCO+ trace similar gas, but HCO+ is depressed in active nuclei.

Most molecular gas has low temperature, density, and optical depth.

Abstract

New HCN, HNC, and HCO+ measurements of 46 normal galaxies in transitions up to J=4-3 are included in a multitransition database covering HCN and HCO+ (130 galaxies) and HNC (94 galaxies). The near-linear luminosity relations are dominated by distance effects and do not reflect galaxy physical properties. Individual galaxies show significant dispersion in both their luminosity and line ratio. Line ratios do not correlate well with either luminosities or other line ratios. Only the normalized J-transition ladders of HCN and HCO+ and the J=1-0 12CO/13CO isotopologue ratio are positively correlated with CO and far infrared (FIR) luminosity. The HCN and HCO+ molecules have very similar intensities and trace the same gas. In galaxies dominated by an active nucleus, HCO+ intensities are depressed relative to HCN intensities. Only a small fraction of the CO emission is directly associated with gas emitting in HCN and HCO, yet a significant fraction of even that gas appears to be translucent molecular gas. In the observed galaxy centers, the HCN/CO line intensity ratio is not a proxy for the dense gas fraction. Likewise, the FIR/HCN and FIR/CO ratios are not proxies for the star formation efficiency. The observed molecular line emission is fully consistent with UV-photon heating boosted by significant mechanical heating. The molecular gas sampled by HCN and HCO+ has low kinetic temperatures T(kin)=10-50 K, low densities n(H)=10^4-10^5 cm^(-3), and low optical depths in the ground-state lines. Most of the gas sampled by CO has densities lower by one to two orders of magnitude. For a mechanical heating fraction of 0.5, a modest energy input of only G=300 Go is required. A proper understanding of star formation requires a more appropriate determination of the gas mass than provided by the intensities of individual HCN or CO transitions.