We present an analysis of the emission line property and the broad band spectral energy distribution of the ultra-luminous infrared Type II quasar Q132+058 .
The optical and ultraviolet emission lines show four distinct components : a LINER-like component at the systematic velocity , a heavily reddened HII-like component blueshifted by about 400km s ^ { -1 } , and two broad components blueshifted by about 400km s ^ { -1 } and 1900km s ^ { -1 } , respectively .
The emission line ratios suggest that broad components are produced in dense and \alpha -enriched outflows with a metalicity of 3-5Z _ { \odot } and a density of n _ { H } \sim 10 ^ { 7 } ~ { } cm ^ { -3 } .
The optical–UV continuum is dominated by stellar light and can be modeled with a young ( < 1 Myr ) plus an intermediate age ( 0.5-0.8Gyr ) stellar populations .
The near to mid-infrared light is dominated by hot and warm dust heated by the hidden quasar .
We derive a star formation rate ( SFR ) of 300-500 M _ { \odot } yr ^ { -1 } from the UV spectrum and far-infrared luminosity , which is two orders of magnitude larger than that indicated by reddening uncorrected [ OII ] luminosity .