of the $TACTIC$ telescope and in Section 3 we present details of observation and data analysis. In Section 4 we present the MWL data analysis of the source from radio to HE. In Section 5 we discuss the results and the conclusions are presented in Section 6.

TACTIC Telescope
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The $TACTIC$ $\gamma$–ray telescope is located at Mount Abu (1300 m asl, $24.6^{\circ}$N, $72.7^{\circ}$E), India [@Tact07]. The telescope is equipped with a F/1-type tessellated light collector of approximately 9.5 $m^{2}$ area consisting of 34 front-face aluminium coated, spherical glass mirror facets of 60 cm diameter. The point-spread function has a full width at half maxima (FWHM) of 0.185$^{\circ}$ ($\equiv$12.5mm) and D$_{90}$ $\sim$0.34$^{\circ}$ ($\equiv$22.8mm). Here, D$_{90}$ is defined as the diameter of a circle, concentric with the centroid of the image, within which 90$\%$ of reflected rays lie. The telescope deploys a 349-pixel imaging camera, with a uniform pixel resolution of $0.31^{\circ}$ and a $5.9^{\circ}\times5.9^{\circ}$ field-of-view, to record atmospheric Cherenkov events produced by an incoming cosmic-ray particle or a $\gamma$-ray photon. Data used in this work have been collected with inner 225 pixels where the innermost 121 pixels (11 $\times$ 11 matrix) are used for generating the event trigger. The trigger 