We present the detailed optical to far-infrared observations of SST J1604+4304 , an ULIRG at z = 1.135 .
Analyzing the stellar absorption lines , namely , the CaII H & K and Balmer H lines in the optical spectrum , we derive the upper limits of an age for the stellar population .
Given this constraint , the minimum \chi ^ { 2 } method is used to fit the stellar population models to the observed SED from 0.44 to 5.8µm .
We find the following properties .
The stellar population has an age 40 - 200 Myr with a metallicity 2.5 Z _ { \sun } .
The starlight is reddened by E ( B - V ) = 0.8 .
The reddening is caused by the foreground dust screen , indicating that dust is depleted in the starburst site and the starburst site is surrounded by a dust shell .
The infrared ( 8-1000µm ) luminosity is L _ { ir } = 1.78 \pm 0.63 \times 10 ^ { 12 } L _ { \sun } .
This is two times greater than that expected from the observed starlight , suggesting either that 1/2 of the starburst site is completely obscured at UV-optical wavelengths , or that 1/2 of L _ { ir } comes from AGN emission .
The inferred dust mass is 2.0 \pm 1.0 \times 10 ^ { 8 } M _ { \sun } .
This is sufficient to form a shell surrounding the galaxy with an optical depth E ( B - V ) = 0.8 .
From our best stellar population model - an instantaneous starburst with an age 40 Myr , we infer the rate of 19 supernovae ( SNe ) per year .
Simply analytical models imply that 2.5 Z _ { \sun } in stars was reached when the gas mass reduced to 30 % of the galaxy mass .
The gas metallcity is 4.8 Z _ { \sun } at this point .
The gas-to-dust mass ratio is then 120 \pm 73 .
The inferred dust production rate is 0.24 \pm 0.12 M _ { \sun } per SN .
If 1/2 of L _ { ir } comes from AGN emission , the rate is 0.48 \pm 0.24 M _ { \sun } per SN .
We discuss the evolutionary link of SST J1604+4304 to other galaxy populations in terms of the stellar masses and the galactic winds , including optically selected low-luminosity Lyman \alpha -emitters and submillimeter selected high-luminosity galaxies .