B2 0648+27: A radio galaxy in a major merger

Morganti, Raffaella; Oosterloo, Tom; Capetti, A.; Ruiter, H. R. de; Fanti, R.; Parma, P.; Tadhunter, C. N.; Wills, K. A.

doi:10.1051/0004-6361:20021806

Cited by 17 publications

(22 citation statements)

References 38 publications

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“…5, top left panel) confirm the structure as a double, with flux densities of 19 and 14 mJy in the northern and southern components, respectively, in agreement with the data from Morganti et al (2003). However, both components are resolved at 22 GHz (see top right panel in Fig.…”

Section: +27supporting

confidence: 82%

“…We expect that the external lobe regions are much older, confirming that this source is confined, and is expected to remain compact similar to NGC 4278 ) despite its relatively higher total radio power and larger size. The connection between the small size of the radio emission and the presence of a major merger in this galaxy about 10 9 years ago, with the presence of a large amount of H in this galaxy (Morganti et al 2003), is remarkable.…”

Section: +27mentioning

confidence: 90%

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Low-power compact radio galaxies at high angular resolution

Giroletti

Giovannini

Taylor

2007

Proceedings of 8th European VLBI Network Symposium — PoS(8thEVN)

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Abstract. We present sub-arcsecond resolution multi-frequency (8 and 22 GHz) VLA images of five low power compact (LPC) radio sources, and phase referenced VLBA images at 1.6 GHz of their nuclear regions. At the VLA resolution we resolve the structure and identify component positions and flux densities. The phase referenced VLBA data at 1.6 GHz reveals flat-spectrum, compact cores (down to a few milliJansky) in four of the five sources. The absolute astrometry provided by the phase referencing allows us to identify the center of activity on the VLA images. Moreover, these data reveal rich structures, including two-sided jets and secondary components. On the basis of the arcsecond scale structures and of the nuclear properties, we rule out the presence of strong relativistic effects in our LPCs, which must be intrinsically small (deprojected linear sizes < ∼ 10 kpc). Fits of continuous injection models reveal break frequencies in the GHz domain, and ages in the range 10 5 − 10 7 yrs. In LPCs, the outermost edge may be advancing more slowly than in more powerful sources or could even be stationary; some LPCs might also have ceased their activity. In general, the properties of LPCs can be related to a number of reasons, including, but not limited to: youth, frustration, low kinematic power jets, and short-lived activity in the radio.

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Section: +27supporting

confidence: 82%

Section: +27mentioning

confidence: 90%

Low-power compact radio galaxies at high angular resolution

Giroletti

Giovannini

Taylor

2007

Proceedings of 8th European VLBI Network Symposium — PoS(8thEVN)

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“…It was resolved into a double source extended about 1 with VLA observations at 8.4 GHz (Giroletti et al 2005b). Morganti et al (2003) detected a large amount of H I. The two radio lobes do not show any evidence of a jet-like structure or hot spots.…”

Section: B2 0648+27mentioning

confidence: 85%

Compact sources in the Bologna Complete Sample: high-resolution VLA observations and optical data

Liuzzo

Buttiglione

Giovannini

et al. 2013

A&A

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Context. Among radio galaxies, compact sources are a class of objects that are not yet well understood, and most of them cannot be included in classical populations of compact radio sources (flat-spectrum or compact steep-spectrum sources). Aims. Our main goal is to analyze the radio and optical properties of a sample of compact sources and compare them with Faranoff-Riley I and II extended radio galaxies. Methods. We selected in the Bologna Complete Sample a subsample of compact sources, naming it the C BCS sample. We collected new and literature subarcsecond resolution multi-frequency VLA images and optical data. We compared total and nuclear radio power with optical emission line measurements. Results. The [OIII] luminosity − 408 MHz total power relation found in high-and low-excitation galaxies as well as in young (CSS) sources holds also for the C BCSs. However, C BCSs present higher [OIII] luminosity than expected at a given total radio power, and they show the same correlation as core radio galaxies, but with a higher radio power. Conclusions. The C BCSs appear to be the high-power tail of core radio galaxies. For most of the C BCSs, the morphology seems to be strongly dependent on the presence of dense environments (e.g., cluster or HI-rich galaxies) and on a young age or restarted radio activity.

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“…Fanti et al 1987;Parma et al 1987;De Ruiter et al 1990;Morganti et al 1997). However, a complete broad band imaging survey of the B2 sample was carried out by Gonzalez-Serrano et al (1993) and Gonzalez-Serrano & Carballo (2000), while narrow band Hα images were obtained by Morganti et al (1992).…”

Section: The Datamentioning

confidence: 99%

Are radio galaxies and quiescent galaxies different? Results from the analysis of HST brightness profiles

Ruiter

Parma

Capetti

et al. 2005

A&A

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Abstract. We present a study of the optical brightness profiles of early type galaxies, using a number of samples of radio galaxies and optically selected elliptical galaxies. For the radio galaxy samples -B2 of Fanaroff-Riley type I and 3C of Fanaroff-Riley type II -we determined a number of parameters that describe a "Nuker-law" profile, which were compared with those already known for the optically selected objects. We find that radio active galaxies are always of the "core" type (i.e. an inner Nuker law slope γ < 0.3). However, there are core-type galaxies which harbor no significant radio source and which are indistinguishable from the radio active galaxies. We do not find any radio detected galaxy with a power law profile (γ > 0.5). This difference is not due to any effect with absolute magnitude, since in a region of overlap in magnitude the dichotomy between radio active and radio quiescent galaxies remains. We speculate that core-type objects represent the galaxies that have been, are, or may become, radio active at some stage in their lives; active and non-active core-type galaxies are therefore identical in all respects except their eventual radio-activity: on HST scales we do not find any relationship between boxiness and radio-activity. There is a fundamental plane, defined by the parameters of the core (break radius r b and break brightness µ b ), which is seen in the strong correlation between r b and µ b . The break radius is also linearly proportional to the optical Luminosity in the I band. Moreover, for the few galaxies with an independently measured black hole mass, the break radius turns out to be tightly correlated with M BH . The black hole mass correlates even better with the combination of fundamental plane parameters r b and µ b , which represents the central velocity dispersion.

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B2 0648+27: A radio galaxy in a major merger

Cited by 17 publications

References 38 publications

Low-power compact radio galaxies at high angular resolution

Low-power compact radio galaxies at high angular resolution

Compact sources in the Bologna Complete Sample: high-resolution VLA observations and optical data

Are radio galaxies and quiescent galaxies different? Results from the analysis of HST brightness profiles

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