Discovery of a giant and luminous Ly α+C? IV+He? II nebula at z = 3.326 with extreme emission line ratios ?

摘要

We present the discovery of HLock01-LAB, a luminous and large Ly α nebula at z ?=?3.326. Medium-band imaging and long-slit spectroscopic observations with the Gran Telescopio Canarias reveal extended emission in the Ly α 1215 ?, C? IV 1550 ?, and He? II 1640 ? lines over ～100 kpc, and a total luminosity L _(Ly α )?=?(6.4?±?0.1)×10~(44)erg s~(?1). HLock01-LAB presents an elongated morphology aligned with two faint radio sources contained within the central ～8 kpc of the nebula. The radio structures are consistent with faint radio jets or lobes of a central galaxy, whose spectrum shows nebular emission characteristic of a type-II active galactic nucleus (AGN). The continuum emission of the AGN at short wavelengths is however likely dominated by stellar emission of the host galaxy, for which we derive a stellar mass M _(*)???2.3?×?10~(11)? M _(⊙). Our kinematic analysis shows that the ionized gas is perturbed almost exclusively in the inner region between the radio structures, probably as a consequence of jet–gas interactions, whereas in the outer regions the ionized gas appears more quiescent. The detection of extended emission in C? IV and C III] indicates that the gas within the nebula is not primordial. Feedback may have enriched the halo at at least 50 kpc from the nuclear region. Using rest-frame UV emission-line diagnostics, we find that the gas in the nebula is likely heated by the AGN. Nevertheless, at the center of the nebula we find extreme emission line ratios of Ly α /C? IV ～60 and Ly α /He? II ～80, one of the highest values measured to date, and well above the standard values of photoionization models (Ly α /He? II ～30 for case B photoionization). Our data suggest that jet-induced shocks are likely responsible for the increase of the electron temperature and, thus, the observed Ly α enhancement in the center of the nebula. This scenario is further supported by the presence of radio structures and perturbed kinematics in this region. The large Ly α luminosity in HLock01-LAB is likely due to a combination of AGN photoionization and jet-induced shocks, highlighting the diversity of sources of energy powering Ly α nebulae. Future follow-up observations of HLock01-LAB will help to reveal the finer details of the excitation conditions of the gas induced by jets and to investigate the underlying cooling and feedback processes in this unique object.