The OH Megamaser Emission in Arp\,220: the rest of the story

TL;DR

This study re-observed and imaged the OH megamaser emission in Arp220, revealing detailed structures around the nuclei, supporting a foreground maser amplification scenario driven by star formation and FIR radiation.

Contribution

It provides high-resolution imaging and analysis of OH megamaser emission in Arp220, confirming the distribution and kinematics of maser and star-forming regions around the nuclei.

Findings

Extended emission structures confirmed around both nuclei.

Foreground molecular material dominates the OH emission.

Systemic velocities and velocity offsets of nuclei determined.

Abstract

The OH Megamaser emission in the merging galaxy Arp220 has been re-observed with the Multi-Element Radio Linked Interferometer Network (MERLIN) and the European VLBI Network (EVN). Imaging results of the OH line emission at the two nuclei are found to be consistent with earlier observations and confirm additional extended emission structures surrounding the nuclei. Detailed information about the distributed emission components around the two nuclei has been obtained using a concatenated MERLIN and EVN database with intermediate (40 mas) spatial resolution. Continuum imaging shows a relatively compact West nucleus and a more extended East nucleus in addition to an extended continuum ridge stretching below and beyond the two nuclei. Spectral line imaging show extended emission regions at both nuclei together with compact components and additional weaker components north and south of the West nucleus. Spectral line analysis indicates that the dominant OH line emission originates in foreground molecular material that is part of a large-scale molecular structure that engulfs the whole nuclear region. Compact OH components are representative of star formation regions within the two nearly edge-on nuclei and define the systemic velocities of East and West as 5425 km/s and 5360 km/s. The foreground material at East and West has a 100 km/s lower velocity at 5314 and 5254 km/s. These emission results confirm a maser amplification scenario where the background continuum and the line emission of the star formation regions are amplified by foreground masering material that is excited by the FIR radiation field originating in the two nuclear regions.