2017A&A...604A..74S

Context. Recent studies with, for example, Spitzer and Herschel have suggested that star formation in dense molecular gas may be governed by essentially the same "law" in Galactic clouds and external galaxies. This conclusion remains controversial, however, in large part because different tracers have been used to probe the mass of dense molecular gas in Galactic and extragalactic studies.
Aims. We aimed to calibrate the HCN and HCO⁺ lines commonly used as dense gas tracers in extragalactic studies and to test the possible universality of the star-formation efficiency in dense gas (≥10⁴cm^–3), SFE_dense.
Methods. We conducted wide-field mapping of the Aquila, Ophiuchus, and Orion B clouds at ∼0.04pc resolution in the J=1-0 transition of HCN, HCO⁺, and their isotopomers. For each cloud, we derived a reference estimate of the dense gas mass M_Herschel^AV>8, as well as the strength of the local far-ultraviolet (FUV) radiation field, using Herschel Gould Belt survey data products, and estimated the star-formation rate from direct counting of the number of Spitzer young stellar objects.
Results. The H¹³CO⁺(1-0) and H¹³CN(1-0) lines were observed to be good tracers of the dense star-forming filaments detected with Herschel. Comparing the luminosities L_HCN and L_HCO+^_ measured in the HCN and HCO⁺ lines with the reference masses M_Herschel^AV>8, the empirical conversion factors α_{Herschel–HCN} (=M_Herschel^AV>8/L_HCN) and α_{Herschel–HCO+} (=M_Herschel^AV>8/L_HCO+^_) were found to be significantly anti-correlated with the local FUV strength. In agreement with a recent independent study of Orion B by Pety et al., the HCN and HCO⁺ lines were found to trace gas down to A_V≥2. As a result, published extragalactic HCN studies must be tracing all of the moderate density gas down to n_H2≤10³cm^–3. Estimating the contribution of this moderate density gas from the typical column density probability distribution functions in nearby clouds, we obtained the following G₀-dependent HCN conversion factor for external galaxies: α_{Herschel–HCN}^fit'=64xG₀^–0.34. Re-estimating the dense gas masses in external galaxies with α_{Herschel–HCN}^fit'(G₀), we found that SFE_dense is remarkably constant, with a scatter of less than 1.5 orders of magnitude around 4.5x10^–8yr^–1, over eight orders of magnitude in dense gas mass.
Conclusions. Our results confirm that SFE_dense of galaxies is quasi-universal on a wide range of scales from ∼1-10pc to >10kpc. Based on the tight link between star formation and filamentary structure found in Herschel studies of nearby clouds, we argue that SFE_dense is primarily set by the "microphysics" of core and star formation along filaments.