[8] Its nucleus is found to have absorbed (N H ~= 3.95+0.27 -0.33 × 1023 cm-2) and an unabsorbed luminosity of L 2-10 keV ~= (5.08 ± 0.52) × 1043 erg s-1, showing a characteristic of a Seyfert Type 2.

[10] 4C +29.30 is particularly a subject of interest since there has been multiple episodes of activity revealed from morphology and by spectral properties of radio emission over broad range of scales.

It was first studied by van Breugel et al. (1986)[11] who found optical line emitting gas to ~20 arcsec north of nucleus, and adjacent to the radio jet along a position angle PA = 24°.

There is evidence of the radio jet interacting with dense extranuclear gas,[10] suggesting the recent activity in 4C +29.30 after merging with a gas-rich disk galaxy.

At least 15 exposures of 1140s were obtained, slightly shifted and dithered up to 0.8 arcsec for both axes, to correct detector effects after the combination of frames.

The spectral resolution is found to be R~3600 at ~ʎ3700 (~83 km1), derived from the full width half-maximum (FWHM) of the CuAr emission lines.

These data reduction were performed through using IRAF packages[14] provided by the Gemini Observatory, with the procedure consisting of sky and bias subtraction, flat-fielding, trimming, wavelength and relative flux calibration, building of the datacubes, final alignment and average combination with an average sigma clipping into the final datacube, which has a spatial binning of 0.1 x 0.1 arcsec 2.

A pool of hot gas is around the black hole, in which some of the material will be consumed and the magnetized whirlpool triggers more output in return to the radio jet.