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We study the Gamma Ray Burst (GRB) environment and intervening absorbers byanalyzing the optical absorption features produced by gas surrounding the GRBor along its line of sight. We analyzed high resolution spectroscopicobservations (R=40000, S/N=3 - 6) of the optical afterglow of GRB080330, takenwith UVES at the VLT ~ 1.5 hours after the GRB trigger. The spectrumillustrates the complexity of the ISM of the GRB host galaxy at z = 1.51 whichhas at least four components in the main absorption system. We detect strongFeII, SiII, and NiII excited absorption lines associated with the bluemostcomponent only. In addition to the host galaxy, at least two more absorberslying along the line of sight to the afterglow have been detected in theredshift range 0.8 < z < 1.1, each exhibiting MgII absorption. For the bluemostcomponent in the host galaxy, we derive information about its distance from thesite of the GRB explosion. We do so by assuming that the excited absorptionlines are produced by indirect UV pumping, and compare the data with a timedependent photo-excitation code. The distance of this component is found to be280+40-50 pc, which is lower than found for other GRBs (1 - 6 kpc). We identifytwo additional MgII absorbers, one of them with a rest frame equivalent widthlarger than 1A. The distance between the GRB and the absorber measured in thispaper confirms that the power of the GRB radiation can influence the conditionsof the interstellar medium up to a distance of at least several hundred pc. Forthe intervening absorbers, we confirm the trend that on average one strongintervening system is found per afterglow, as has been noted in studiesexhibiting an excess of strong MgII absorbers along GRB sightlines compared toquasars.

UVES/VLT high resolution absorption spectroscopy of the GRB080330 afterglow: a study of the GRB host galaxy and intervening absorbers