[3] Using a new generation of infrared spectrograph, it made it possible to begin systematic studies of the dominant ionization mechanisms in these galaxies via their rest frame optical emission-line spectra.
In particular, using the new K-Band[8] on the University of Hawaii 2.2 m telescope on Mauna Kea, provides the unique capability of simultaneous coverage of the 1.02.4 m wavelength band at typical spectral resolution / 700, while the infrared spectrograph (CGS4) on the 3.8 m United Kingdom Infrared Telescope (UKIRT) on Mauna Kea can provide coverage of either the full J-, H-, or K-band near-infrared windows at a spectral resolution of / 860.
The Ly, CIV and HeII emission lines in 4C +48.48 shows a striking morphology, which they extend several arcseconds towards the north-east section, in close alignment with the radio source.
[10] The properties above, suggests 4C +48.48 is embedded inside a large ionized gas nebula where Lyα emission is extended across ~100 kpc or more.
[10] From another research, which using deep spectroscopy of the ultraviolet (UV) line and continuum emission obtained from KECK II and the Very Large Telescope, they were able to investigate the nature of jet-gas interactions in 4C +48.48.