TITLE: GCN CIRCULAR NUMBER: 13257 SUBJECT: GRB 120422A: VLT/X-shooter spectroscopy of the GRB counterpart DATE: 12/04/23 09:13:23 GMT FROM: Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst S. Schulze (Univ. Iceland), A. J. Levan (Univ. Warwick), D. Malesani (DARK/NBI), J. P. U. Fynbo (DARK/NBI), N. R. Tanvir (Univ. Leicester), B. Milvang-Jensen (DARK/NBI), A. de Ugarte Postigo (IAA/CSIC and DARK/NBI), V. D'Elia (ASI/ASDC and INAF/OAR), J. Sollerman (OKC, Stockholm), J. Hjorth (DARK/NBI), report on behalf of the X-shooter GRB GTO collaboration: We observed the optical counterpart of GRB 120422A (Troja et al., GCN 13243; Cucchiara et al., GCN 13245) with the ESO VLT equipped with the X-shooter spectrograph. Observations started on 2012 April 22.99 UT (16.5 hr after the GRB), for a total exposure time of 80 min in each of the UVB, VIS, and NIR arms, covering the wavelength range 3000-25000 AA. The slit was aligned so to cover both the galaxy at z = 0.28 present in the SDSS (Cucchiara et al., GCN 13245; Tanvir et al., GCN 13251) and the GRB optical counterpart (Cucchiara et al., GCN 13245). We detect a plethora of nebular emission lines from the candidate host galaxy, including [O II], [O III], Balmer lines up to Hzeta, [N II], [S II], at a common redshift z = 0.283, thus confirming the results of Tanvir et al. (GCN 13251). The trace of the GRB counterpart is rather blue (see also Nardini et al., GCN 13256), and we detect Mg II at z = 0.283 in absorption. No further absorption features are visible. We also note that the spatial extent of the brightest emission lines from the SDSS galaxy encompasses the position of the GRB counterpart, indicating nebular emission at z = 0.283 at the GRB position. While a chance superposition cannot be excluded, we note that the lack of absorption features at z > 0.283 would require a very tenuous environment at the GRB location. Furthermore, the UVOT detection in all the UV filters (Kuin & Troja, GCN 13248) implies a low redshift z <~ 1.3. Last, we note that the UVOT photometry at t ~ 5 ks after the burst reveals a very blue spectrum, which is not typical of GRB afterglows, but is reminiscent of the very blue early emission of GRB 060218 (Campana et al. 2006, Nature, 442, 1008). We thus conclude that the GRB is also likely at z = 0.283. Using the gamma-ray fluence reported by Barthelmy et al. (GCN 13246), at z = 0.283 the isotropic-equivalent energy release of GRB 120422A is ~4.4*10^49 erg, which is typical of local GRBs, often associated with supernovae. We encourage photometric and spectroscopic follow-up to detect the emergence of a supernova, or lack thereof. We acknowledge the excellent support of the ESO observing staff in Paranal, in particular Henri Boffin and Giovanni Carraro. We thank Nino Cucchiara for providing us with a finding chart from the Gemini observation (GCN 13245).