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We present multi-wavelength observations of a typical long duration GRB120326A at $z=1.798$, including rapid observations using a submillimeter array(SMA), and a comprehensive monitoring in X-ray and optical. The SMA observationprovided the fastest detection to date among seven submillimeter afterglows at230 GHz. The prompt spectral analysis, using Swift and Suzaku yielded aspectral peak energy of $E^{\rm src}_{\rm peak}=107.8^{+15.3}_{-15.3}$ keV andequivalent isotropic energy of $E_{\rm iso}$ as $3.18^{+0.40}_{-0.32}\times10^{52}$ erg. The temporal evolution and spectral properties in the opticalwere consistent with the standard forward shock synchrotron with jetcollimation ($6^{\circ}.69\pm0^{\circ}.16$). The forward shock modeling using a2D relativistic hydrodynamic jet simulation also determined the reasonableburst explosion and the synchrotron radiation parameters for the opticalafterglow. The X-ray light curve showed no apparent jet break and the temporaldecay index relation between the X-ray and optical ($\alpha{\rmo}-\alpha_{X}=-1.45\pm0.10$) indicated different radiation processes in theX-ray and optical. Introducing synchrotron self-inverse Compton radiation fromreverse shock is a possible solution, and the detection and the slow decay ofthe afterglow in submillimeter supports that this is a plausible idea. Theobserved temporal evolution and spectral properties as well as forward shockmodeling parameters, enabled to determine reasonable functions to describe theafterglow properties. Because half of events share similar properties in theX-ray and optical to the current event, GRB120326A will be a benchmarks withfurther rapid follow-ups, using submillimeter instruments such as SMA and ALMA.

Synchrotron Self-inverse Compton Radiation From Reverse-shock on GRB120326A