4C +29.30

The nucleus of 4C +29.30 is found to be active. It is specially classified as a Fanaroff-Riley Class I (FR-I)^[4] radio galaxy producing an optical radio jet,^[5] although it shows characteristics of a Fanaroff-Riley Class II.^[4] 4C +29.30 shows existence of weak extended emission, which has an angular size of ~520 arcsec (639 kpc) embedded within the galaxy with a compact edge-brightened double-lobed source of 29 arcsecs (36 kpc).^[6] 4C +29.30 has been catalogued as an infrared point source by IRAS, WISE and the Two Micron All Sky Survey (2MASS).^[7]

The galaxy shows a complex X-ray morphology which shows the main features of a nucleus, a jet, hotspots and lobes which was detected during the snapshot 8 ks Chandra Observation by Gambil et al. (2003).^[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.^[9] Furthermore, it shows an early-type morphology, which has a moderate radio luminosity of ~10 ergs 1, presenting signatures of jet reactivation.^[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.^[7]

A 4.3 kpc x 6.2 kpc extended emission in ionized gas can be found in 4C +29.30, displaying structures that resembles rotated disks, spiral arms and bars^[12] resembling a spiral galaxy of type Sc.^[1] The galaxy also displays a dust lane passing through its central region similar to Centaurus A.^[10] According to Jamrozy et al. (2007),^[6] a low-surface brightness, radio emission extending to ~600 kpc has been detected and studied, which its structure is characterized by a steep radio spectrum. The age of the small-scale radio structure embedded within the extended radio emission, is estimated to be ≲ 100 Myr, with the inner double knots of a spectral age of ≲ 33 Myr^[13] being resolved to two separate nuclear knots of spectral ages of ~15 yr and ~70 yr.

Between January 12 and March 15, 2016, 4C +29.30 was observed by the Integral Field Unit (IFU) of the Gemini Multi-object Spectrograph, mounted on a Gemini North Telescope. A 'One-slit' model is used, with a rectangular view of ≈ 3.5 arcsec × 5.0 arcsec which corresponds to 4.3 x 6.2 kpc² at the 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.^[10]

For the spectral with wavelength coverage in range of ʎ4500-7300 and centered at ʎ5900, this were obtained through the use of B600+_G5307 grating and IFU-R mask. 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. The spectral dithering was also performed with a maximum separation of 102.5 Å  between exposures. 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.^[10]