Volume 578, June 2015
|Number of page(s)||12|
|Published online||27 May 2015|
J0010+1058 This Seyfert 1 galaxy has a σ of the Hβ broad component ~2300 km s-1 and showed several flaring episodes and superluminal motion in VLBI observations that can be explained with the presence of a relativistic jet (Brunthaler et al. 2000, 2005). Taylor et al. (1996) found that an exponential disk fits the near-IR (NIR) surface brightness of the source, while Surace et al. 2001 found a single tidal arm with high star formation extended 22 kpc to the north. J0150−0725 This is a Seyfert 2 galaxy with a possible S0 host (McKernan et al. 2010). It has a strong radio emission but is unresolved on VLA scale (Thean et al. 2000). It has a flat FIR-to-radio spectrum, indicative of a strong nonthermal component (Heisler & Vader 1995). J0316+4119 This is a Seyfert 2 radio galaxy in a lenticular host (Paturel et al. 2003). It was detected at very high energy, as reported in Neronov et al. (2010) and also in Kadler et al. (2012). It seems to be a low-luminosity FR I galaxy with an angle between the jet axis and the line of sight of θ ≲ 38°. J0407+0342 This is a Seyfert 2 galaxy. According to Inskip et al. (2010), the host galaxy has both a bulge and a disk component, with the first being the brighter of the two. In radio the source has a typical FR II morphology, with a weak core and bright hot spots (Cohen et al. 1999). Its spectrum, retrieved in the NED archive and derived from the Low Resolution Spectrograph at TNG, has a spectral resolution of 20 Å, therefore the [OIII] line was not resolved. J0433+0521 This is a Seyfert 1 galaxy with a low Hβ broad component, ~1500 km s-1. It has a confirmed FR I morphology, with jets whose total extent exceeds 760 kpc (Walker et al. 1987). There is an optical jet in the same apparent direction as the radio jet (Barway et al. 2003). The host galaxy was analyzed by Inskip et al. (2010), and they found that it is better reproduced with a disk+bulge model, plus a nuclear point source that contributes 33% to the total flux. J0552−0727 This is a Seyfert 2 galaxy, hosted in an SAB0 according to the RC3 catalog. HST imaging spectroscopy of the source revealed a jet-like region of [OIII] emission extended for 1′′ (Mulchaey et al. 1994). It has a radio source consisting of a compact core with a flat spectrum and symmetric jets (Mundell et al. 2000). J0725+2957 This is a Seyfert 2 galaxy with strong absorption lines in the optical spectrum. It is associated with a disk galaxy, particularly an S0, the only source in the B2 sample of this kind. The radio emission originates in two symmetric jets that form an angle of ~45° with the Galactic disk (Capetti et al. 2000). J1140+1743 This is a Seyfert 2 galaxy hosted in an S0 with a large-scale dust lane (Noel-Storr et al. 2003). Its spectrum is extremely red, with weak emission lines. We cannot exclude that the AGN is in its last phase before reaching a quiescent state (Hota et al. 2012). The source has symmetric jets, and it appears to be forming a disk. J1252+5634 This is an Seyfert 1.5 galaxy hosted in a spiral galaxy with large tidal arms. It is a compact steep-spectrum object with a triple
structure (O’Dea 1998) that shows emission-line gas aligned with the radio source (Hamilton et al. 2002). The gas structure forms a double shell-like morphology, with one lobe brighter and better defined than the other (Axon et al. 2000). J1312+3515 This is a Seyfert 1 galaxy with a Hβ broad component σ ~ 2530 km s-1, and it is hosted in a spiral galaxy (Hamilton et al. 2002). It was classified by Kellermann et al. (1989) as a flat-spectrum radio-intermediate QSO because of a relatively low radio-loudness, in agreement with our result. J1324+3622 This is a Seyfert 2 galaxy with weak emission lines and a red spectrum. It is hosted by a S0 galaxy with a strong nuclear dust lane. Its radio morphology is that of a FR I radio galaxy with twin jets resolved on VLA scales (Noel-Storr et al. 2003). J1352+3126 This is a Seyfert 2 galaxy whose optical spectrum increases toward longer wavelengths. It is a postmerger object, with the merged object being consistent with a late-type spiral galaxy. The radio source is also known as 3C 293, and it exhibits a one-sided jet. The latter shows emissions in optical, near-IR, and UV and has a FR II structure (Floyd et al. 2006). J1409−0302 Also known as Speca, this is an AGN, possibly a Seyfert 2 galaxy, hosted by a spiral galaxy that shows signs of recent episodes of star formation. The radio source has three pairs of lobes, probably produced by an intermittent radio jet activity from the AGN (Hota et al. 2011). J1413−0312 Based to its optical spectrum, this source would be classified as a Seyfert 2 galaxy, with no broad component in the permitted lines and no sign of FeII. Nevertheless, on the basis of its IR spectrum, Nagar et al. (2002) classified it as a NLS1, and we included it in the S-NLS1s sample. Since its Hβ line shows no sign of a broad component, we determined its physical properties using the technique for type 2 AGN. Our results show that the source has a bolometric luminosity lower than the other NLS1s, and as a consequence a lower Eddington ratio. Its BH mass is not significantly different from the others. This discrepancy can be due to the strong absorption that affects the optical spectra of this object, which might lead to an underestimation of the bolometric luminosity. When this parameter is estimated from a different spectral range, its value appears to be higher (Soldi et al. 2011). J1449+6316 This is a Seyfert 2 galaxy. Its host has a disturbed morphology, and shows isophotal twists and two spiral arms, with a thin dust lane that crosses the nuclear region. The radio source has an FR I morphology with double-sided jets (Jackson et al. 2003). J1550+1120 This is a Seyfert 1.5 galaxy, with a strongly asymmetric Hβ profile because of a strongly redshifted broad component. The host galaxy appears to have large tidal arms and a surface brightness profile well represented with an exponential profile (Hamilton et al. 2002). It also has jets, whose outer lobes show multiple bright spots (Rector et al. 1995). J1704+6044 This is a Seyfert 1.5 galaxy with a very large Hβ broad component. The host galaxy is a spiral that contains a ring that surrounds an off-center bulge (Hamilton et al. 2002). The radio source is very steep and lobe-dominated; the two lobes are asymmetric, and one of them appears to be stopped by a dense environment (Goodlet et al. 2004).
© ESO, 2015
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