TITLE: GCN CIRCULAR NUMBER: 32291 SUBJECT: GRB 220627A: VLT MUSE redshift DATE: 22/06/29 13:06:24 GMT FROM: Daniele B Malesani at Radboud U L. Izzo (DARK/NBI), V. D'Elia (ASI/SSDC, INAF/OAR), A. de Ugarte Postigo (OCA), J. P. U. Fynbo (DAWN/NBI), D. A. Kann (IAA-CSIC), A. J. Levan (Radboud Univ.), D. B. Malesani (Radboud Univ. and DAWN/NBI), A. Saccardi (GEPI/Paris Obs.), C. C. Thoene (ASU-CAS), J. F. Agui Fernandez (IAA-CSIC), S. de Wet (UCT), P. J. Groot (Radboud Univ., UCT, SAAO), report on behalf of the Stargate consortium: We observed the candidate optical afterglow (de Wet et al., GCN 32289) of the Fermi GBM and LAT GRB 220627A (Roberts et al., GCN 32288; Di Lalla et al., GCN 32283) using the ESO VLT equipped with the MUSE integral-field spectrograph. Observations were carried out starting on 2022 June 29.06 UT (1.17 days after the trigger), and cover the wavelength range 4800-9300 AA. A broad trough is detected centered around 4960 AA, which we interpret as due to DLA HI absorption. A number of metal lines are also detected, which we identify as, among others, O I, O I*, Si II, Si II*, C II, C II*, Si IV, C IV, Al II, at a common redshift z = 3.084. We also note the presence of a (rich) intervening system at z = 2.665 (as identified by, e.g., S IV, Si II, C IV, Fe II, Al II). The redshift and luminosity of this object, together with its X-ray emission (Evans et al., GCN 32284), make it very likely to be the afterglow of GRB 220627A. Using the preliminary GBM fluence and spectral parameters (Roberts et al., GCN 32288), we derive an isotropic-equivalent quasi-bolometric gamma-ray energy of 3.6*10^54 erg (0.1 keV - 100 MeV rest frame). We thank the ESO staff at Paranal for carrying out or observations, in particular Jonathan Smoker, Camila Navarrete, Rodrigo Palominos, and Marco Berton.