  Based on the two epochs EVN archive data from OH line observations of IIZw
096, we confirm that the high-resolution OH emission in this source mainly
comes from two spots (OH1 and OH2) of comp D1 of this merging system. We found
no significant variations in the OH line emission. The OH 1665 MHz line
emission is detected at about 6 $\sigma$ level in the OH1 region by combining
two epoch EVN observations. We found that the comp D1 shows the brightest CO,
HCO+ line emission, as well as multi-band radio continuum emission. The
environment around D1 shows no clear velocity structure associated with
circular motions, making it different from most other OHMs in the literature,
which might have been caused by an effect during the merger stage. Meanwhile,
we found that the CO emission shows three velocity structures around D1,
including the central broad FWHM region, the double peak region where the CO
line profile shows two separated peaks, and the region of the high-velocity
clouds where the CO line peaks at a high velocity ($\sim$ 11000 \kms). \HI in
absorption also show high-velocity clouds around the D1 region, which might be
due to inflows caused by the merging of two or more galaxy components. Based on
the high-resolution K-band VLA and L-band VLBA observations of the radio
continuum emission, we derived the brightness temperature in the range $10^{5}$
K to $10^{6}$ K, which is consistent with other starburst dominant OHM sources
in the literature. The multi-band VLA observations show that the radio
continuum emission of comp D might also have contributions from free-free
emission, besides synchrotron emission. As a concenquence, these results
support a starburst origin for the OHMs, without the presence of an AGN.

Astrophysics of Galaxies