The host galaxy and optical light curve of the gamma-ray burst GRB 980703

We present deep HST/STIS and ground-based photometry of the host galaxy of the gamma-ray burst GRB 980703 taken 17, 551, 710, and 716 days after the b urst. We find that the host is a blue, slightly over-luminous galaxy with V -gal = 23.00 +/-0.10, (V - R)(gal) = 0.43 +/-0.13, and a centre that is app roximate to0.2 mag bluer than the outer regions of the galaxy. The galaxy h as a star-formation rate of 8-13 M-circle dot yr(-1), assuming no extinctio n in the host. We find that the galaxy is best fit by a Sersic R-1/n profil e with n approximate to 1.0 and a half-light radius of 0." 13 (= 0:72h(100) (-1) proper kpc.) This corresponds to an exponential disk with a scale radi us of 0." 22 (= 1.21h(100)(-1) proper kpc). Subtracting a fit with elliptic al isophotes leaves large residuals, which suggests that the host galaxy ha s a somewhat irregular morphology, but we are unable to connect the locatio n of GRB 980703 with any special features in the host. The host galaxy appe ars to be a typical example of a compact star forming galaxy similar to tho se found in the Hubble Deep Field North. The R-band light curve of the opti cal afterglow associated with this gamma-ray burst is consistent with a sin gle power-law decay having a slope of alpha = 1.37 +/-0.14. Due to the brig ht underlying host galaxy the late time properties of the light-curve are v ery poorly constrained. The decay of the optical light curve is consistent with a contribution from an underlying type Ic supernova like SN1998bw, or a dust echo, but such contributions cannot be securely established.