  We present a multiwavelength study of the OH megamaser galaxy (OHMG)
IRAS17526+3253, based on new Gemini Multi-Object Spectrograph Integral Field
Unit (GMOS/IFU) observations, Hubble Space Telescope F814W and H$\alpha$+[N{\sc
ii}] images, and archival 2MASS and 1.49GHz VLA data. The HST images clearly
reveal a mid-to-advanced stage major merger whose northwestern and southeastern
nuclei have a projected separation of $\sim$8.5kpc. Our HST/H$\alpha$+[N{\sc
ii}] image shows regions of ongoing star-formation across the envelope on
$\sim$10kpc scales, which are aligned with radio features, supporting the
interpretation that the radio emission originates from star-forming regions.
The measured H$\alpha$ luminosities imply that the unobscured star-formation
rate is $\sim$10-30\,M$_{\odot}$yr$^{-1}$. The GMOS/IFU data reveal two
structures in northwestern separated by 850\,pc and by a discontinuity in the
velocity field of $\sim$~200~km~s$^{-1}$. We associate the blue-shifted and
red-shifted components with, respectively, the distorted disk of northwestern
and tidal debris, possibly a tail originating in southeastern. Star-formation
is the main ionization source in both components, which have SFRs of
$\sim$2.6-7.9\,M$_{\odot}$yr$^{-1}$ and $\sim$1.5-4.5\,M$_{\odot}$yr$^{-1}$,
respectively. Fainter line emission bordering these main components is
consistent with shock ionization at a velocity $\sim$200~km~s$^{-1}$ and may be
the result of an interaction between the tidal tail and the northwestern
galaxy's disk. IRAS17526+3253 is one of only a few systems known to host both
luminous OH and H$_{2}$O masers. The velocities of the OH and H$_{2}$O maser
lines suggest that they are associated with the northwestern and southeastern
galaxies, respectively.
