Deeply Buried Nuclei in the Infrared-luminous Galaxies NGC 4418 and Arp 220. I. ALMA Observations at λ = 1.4-0.4 mm and Continuum Analysis

Abstract

We observed with Atacama Large Millimeter/submillimeter Array three deeply buried nuclei in two galaxies, NGC 4418 and Arp 220, at ~0.″2 resolution over a total bandwidth of 67 GHz in f _rest = 215-697 GHz. Here we (1) introduce our program, (2) describe our data reduction method for wide-band, high-resolution imaging spectroscopy, (3) analyze in visibilities the compact nuclei with line forests, (4) develop a continuum-based estimation method of dust opacity and gas column density in heavily obscured nuclei, which uses the buried galactic nuclei (BGN) model and is sensitive to $\mathrm{log}({N}_{{{\rm{H}}}_{2}}/{\mathrm{cm}}^{-2})$ log(NH2/cm-2) ~ 25-26 at λ ~ 1 mm, and (5) present the continuum data and diagnosis of our targets. The three continuum nuclei have major-axis FWHMs of ~0.″1-0.″3 (20-140 pc) aligned to their rotating nuclear disks of molecular gas. However, each nucleus is described better with two or three concentric components than with a single Gaussian. The innermost cores have sizes of 0.″05-0.″10 (8-40 pc), peak brightness temperatures of ~100-500 K at 350 GHz, and more fractional flux at lower frequencies. The intermediate components correspond to the nuclear disks. They have axial ratios of ≈0.5 and hence inclinations ≳60°. The outermost elements include the bipolar outflow from Arp 220W. We estimate 1 mm dust opacity of τ _{d,1 mm} ≈ 2.2, 1.2, and ≲0.4, respectively, for NGC 4418, Arp 220W, and Arp 220E. The first two correspond to $\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})\sim 26$ log(NH/cm-2)~26 for conventional dust-opacity laws, and hence the nuclei are highly Compton thick.