[8] A further detailed investigation of the spectroscopic properties of 4C +71.07 is presented by Raiteri et al. (in preparation), which researchers estimated a systemic redshift of z = 2.213 from the Balmer Hα and Hβ broad emission lines.

The quasar has a 5 GHz flux greater than 1 Jy,[4] and has both stationary and superluminally moving components in a bright one-sided jet emerging from its core.

The 1992 flare may also have been detected at millimeter and centimeter frequencies, but with a delay of 0.10.5 yr.[18] At soft X-ray energies (0.12 keV), the source underwent a flux decrease by a factor of 2 between March and November 1992, without any spectral change,[19] implying a high flux level close to the optical flaring period; the source was still dim when reobserved by the Advanced Satellite for Cosmology and Astrophysics in March 1995.

[21] A study done by Asada et al. (2010), shows researchers inferring a Faraday rotation measure gradient from multifrequency VLBI polarimetry, suggesting a helical magnetic field for the jet of 4C +71.07.

[23] Evidences in favor of a helical jet structure, were presented also by Perucho et al. (2012a) based on very long baseline interferometry data.

Not to mention, 4C +71.07 shows a prominent accretion disc bump peaking in the ultra-violet band, which makes this source an excellent candidate to investigate not only the jet emission but also the non thermal one.

[9] Researchers also calculated that the best-guess density value for the hydrogen column through the analysis of X-ray spectra, is N_H^best=6.3 × 10^{20} cm^{-2}, but found out that the light curves do not show persistent correlations among flux changes at different frequencies.

Integration of the thermal continuum traced by our big blue bump template allows them to estimate the disc bolometric luminosity, which is Ldisc = 2.45 x 1047 ergs −1 showing the Eddington ratio, high as 0.66.