ALMA Sub-arcsec-resolution 183 GHz H2O and Dense Molecular Line Observations of Nearby Ultraluminous Infrared Galaxies

Abstract

We present the results of ALMA $\sim$2 mm, $\lesssim$1${}^{\prime \prime }$-resolution observations of ten (ultra)luminous infrared galaxies ([U]LIRGs; infrared luminosity $\gtrsim$ 10${}^{11.7}$L${}_{\odot }$) at $z<$ 0.15, targeting dense ($>$10${}^4$ cm${}^{-3}$) molecular (HCN, HCO${}^{+}$, and HNC J=2-1) and 183 GHz H${}_2$O 3${}_{1,3}$-2${}_{2,0}$ emission lines. Higher HCN to HCO${}^{+}$ J=2-1 flux ratios are observed in some, but not all, AGN-important ULIRGs than in starburst-classified sources. We detect 183 GHz H${}_2$O emission in almost all AGN-important ULIRGs, and elevated H${}_2$O emission is found in two sources with elevated HCN J=2-1 emission, relative to HCO${}^{+}$ J=2-1. Except one ULIRG (the Superantennae), the H${}_2$O emission largely comes from the entire nuclear regions ($\sim$1 kpc), rather than AGN-origin megamaser at the very center ($<<$1 kpc). Nuclear ($\sim$1 kpc) dense molecular gas mass derived from HCO${}^{+}$ J=2-1 luminosity is $\gtrsim$a few $\times$ 10${}^8$M${}_{\odot }$, and its depletion time is estimated to be $\gtrsim$10${}^6$ yr in all sources. Vibrationally excited J=2-1 emission lines of HCN and HNC are detected in a few (U)LIRGs, but those of HCO${}^{+}$ are not. It is suggested that in mid-infrared-radiation-exposed innermost regions around energy sources, HCO${}^{+}$ and HNC are substantially less abundant than HCN. In our ALMA $\sim$2 mm data of ten (U)LIRGs, two continuum sources are serendipitously detected within $\sim$10${}^{\prime \prime }$, which are likely to be an infrared luminous dusty galaxy at $z>$ 1 and a blazar.

arXiv comment50 pages, 16 Figures. ApJ accepted

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