ALMA Resolves the Nuclear Disks of Arp 220

Abstract

We present 90 mas (37 pc) resolution ALMA imaging of Arp 220 in the CO (1-0) line and continuum at $\lambda =2.6$ mm. The internal gas distribution and kinematics of both galactic nuclei are well-resolved for the first time. In the West nucleus, the major gas and dust emission extends out to 0.2\arcsec radius (74 pc); the central resolution element shows a strong peak in the dust emission but a factor 3 dip in the CO line emission. In this nucleus, the dust is apparently optically thick (${\tau }_{2.6mm}\sim 1$) at $\lambda =2.6$ mm with a dust brightness temperature $\sim 147$ K. The column of ISM at this nucleus is ${\mathrm{N}}_{H2}\ge 2\times 10^{26}$ cm${}^{-2}$, corresponding to $\sim$900 gr cm${}^{-2}$. The East nucleus is more elongated with radial extent 0.3\arcsec or $\sim 111$ pc. The derived kinematics of the nuclear disks provide a good fit to the line profiles, yielding the emissivity distributions, the rotation curves and velocity dispersions. In the West nucleus, there is evidence of a central Keplerian component requiring a central mass of $8\times 10^8$ \msun. The intrinsic widths of the emission lines are $\Delta \mathrm{v}(\mathrm{FWHM})$ = 250 (West) and 120 (East) \kms. Given the very short dissipation timescales for turbulence ($\lesssim 10^5$ yrs), we suggest that the line widths may be due to semi-coherent motions within the nuclear disks. The symmetry of the nuclear disk structures is impressive -- implying the merger timescale is significantly longer than the rotation period of the disks.

arXiv commentApJ in press

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