Bulges and Disklike Components in the Host Galaxies of Low‐Redshift 3CR Sources: A Near‐Infrared View of Their Radial Brightness Profiles

Donzelli, C. J.; Chiaberge, M.; Macchetto, F.; Madrid, Juan P.; Capetti, A.; Marchesini, Danilo

doi:10.1086/520758

Cited by 35 publications

(74 citation statements)

References 46 publications

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“…since it provides the most complete coverage (∼85%) for the 3CR sample by using measurements from the 2MASS (Skrutskie et al 2006) or, when this is not available, from HST images (Donzelli et al 2007). For the BLO we also corrected the host luminosity for the contribution of their bright IR nuclei, measured by Baldi et al (2009).…”

Section: Comparison With Previous Studiesmentioning

confidence: 99%

An optical spectroscopic survey of the 3CR sample of radio galaxies withz$\mathsf{<}$ 0.3

Buttiglione¹,

Capetti

Celotti³

et al. 2010

A&A

260

390

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In a previous paper we presented a homogeneous and 92% complete optical spectral dataset of the 3CR radio sources with redshift <0.3. Here we use the emission line measurements to explore the spectroscopic properties of the sample. The 3CR sources show a bimodal distribution of excitation index, a new spectroscopic indicator that measures the relative intensity of low and high excitation lines. This unveils the presence of two main sub-populations of radio-loud AGN to which we refer to, following previous studies, as high and low excitation galaxies (HEG and LEG, respectively). In addition to the two main classes, we find one source with a spectrum typical of star forming galaxies, and 3 objects of extremely low level of excitation. All broad-line objects are HEG from the point of view of their narrow emission line ratios and all HEG are FR II radio-galaxies with log L 178 [erg s −1 ] > ∼ 32.8. Conversely LEG cover the whole range of radio power encompassed by this 3CR subsample (30.7 < ∼ log L 178 < ∼ 35.4) and they are of both FR I and FR II type. The brightest LEG are all FR II. HEG and LEG obey to two (quasi) linear correlations between the optical line and extended radio luminosities, with HEG being brighter than LEG in the [O III] line by a factor of ∼10. HEG and LEG are offset also in a plane that compares the black hole mass and the ionizing nuclear luminosity. However, although HEG are associated with higher nuclear luminosities, we find LEG among the brightest radio sources of the sample and with a clear FR II morphology, indistinguishable from those seen in HEG. This suggests that LEG are not simply objects with a lower level of accretion. We speculate that the differences between LEG and HEG are related to a different mode of accretion: LEG are powered by hot gas, while HEG require the presence of cold accreting material. The high temperature of the accreting gas in LEG accounts for the lack of "cold" structures (i.e. molecular torus and broad line region), for the reduced radiative output of the accretion disk, and for the lower gas excitation.

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Section: Comparison With Previous Studiesmentioning

confidence: 99%

An optical spectroscopic survey of the 3CR sample of radio galaxies withz$\mathsf{<}$ 0.3

Buttiglione¹,

Capetti

Celotti³

et al. 2010

A&A

260

390

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show abstract

“…Many radio MOHEGs (Table 3 and Figures 1-4) appear to have a galactic stellar disk (Donzelli et al 2007), dust disk, or dust lanes (De Koff et al 2000). Stellar or dust disks may indicate a past gas-rich merger, which would help to explain the presence of large quantities of H 2 .…”

Section: Host Galaxies and Environsmentioning

confidence: 99%

Jet-Powered Molecular Hydrogen Emission From Radio Galaxies

Ogle

Boulanger

Guillard

et al. 2010

ApJ

154

342

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H 2 pure-rotational emission lines are detected from warm (100-1500 K) molecular gas in 17/55 (31% of) radio galaxies at redshift z < 0.22 observed with the Spitzer IR Spectrograph. The summed H 2 0-038 -2 × 10 42 erg s −1 , yielding warm H 2 masses up to 2 × 10 10 M . These radio galaxies, of both FR radio morphological types, help to firmly establish the new class of radio-selected molecular hydrogen emission galaxies (radio MOHEGs). MOHEGs have extremely large H 2 to 7.7 μm polycyclic aromatic hydrocarbon (PAH) emission ratios: L(H 2 )/L(PAH7.7) = 0.04-4, up to a factor 300 greater than the median value for normal star-forming galaxies. In spite of large H 2 masses, MOHEGs appear to be inefficient at forming stars, perhaps because the molecular gas is kinematically unsettled and turbulent. Low-luminosity mid-IR continuum emission together with low-ionization emission line spectra indicates low-luminosity active galactic nuclei (AGNs) in all but three radio MOHEGs. The AGN X-ray emission measured with Chandra is not luminous enough to power the H 2 emission from MOHEGs. Nearly all radio MOHEGs belong to clusters or close pairs, including four cool-core clusters (Perseus, Hydra, A2052, and A2199). We suggest that the H 2 in radio MOHEGs is delivered in galaxy collisions or cooling flows, then heated by radio-jet feedback in the form of kinetic energy dissipation by shocks or cosmic rays.

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“…We also test model galaxies at various distances. More specifically, we produce images of elliptical galaxies following a De Vaucouleur's law, with an effective radius of 4.6 kpc, the value measured by Donzelli et al (2007) for 3C radio-galaxies. The model is then convolved with a gaussian with FWHM of 1.…”

Section: Measurement Of the Optical Position Anglementioning

confidence: 99%

Origin of X-shaped radio-sources: further insights from the properties of their host galaxies

Gillone

Capetti

Rossi

2016

A&A

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We analyze the properties of a sample of X-shaped radio-sources (XRSs). These objects show, in addition to the main lobes, a pair of wings that produce their peculiar radio morphology. We obtain our sample by selecting from the initial list of Cheung (2007( , AJ, 133, 2097) the 53 galaxies with the better defined wings and with available SDSS images. We identify the host galaxies and measure their optical position angle, obtaining a positive result in 22 cases. The orientation of the secondary radio structures shows a strong connection with the optical axis, with all (but one) wing forming an angle larger than 40 • with the host major axis. The probability that this is compatible with a uniform distribution is P = 0.9 × 10 −4 . For all but three sources of the sample, spectroscopic or photometric redshifts are avaliable. The radio luminosity distribution of XRSs has a high power cut-off at L ∼ 10 34 erg s −1 Hz −1 at 1.4 GHz. Spectra are available from the SDSS for 28 XRSs. We modeled them to extract information on their emission lines and stellar population properties. The sample is formed by approximately the same number of high and low excitation galaxies (HEGs and LEGs); this classification is essential for a proper comparison with non-winged radio-galaxies. XRSs follow the same relations between radio and line luminosity defined by radio-galaxies in the 3C sample. While in HEGs a young stellar population is often present, this is not detected in the 13 LEGs, which is, again, in agreement with the properties of non-XRSs. The lack of young stars in LEGs supports the idea that they have not experienced a recent gas-rich merger. The connection between the optical axis and the wing orientation, as well as the stellar population and emission-line properties, provide further support for a hydro-dynamic origin of the radio-wings (for example, associated with the expansion of the radio cocoon in an asymmetric external medium) rather than with a change of orientation of the jet axis. In this framework, the high luminosity limit of XRSs can be interpreted as being due to high power jets being less affected by the properties of the surrounding medium.

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Bulges and Disklike Components in the Host Galaxies of Low‐Redshift 3CR Sources: A Near‐Infrared View of Their Radial Brightness Profiles

Cited by 35 publications

References 46 publications

An optical spectroscopic survey of the 3CR sample of radio galaxies withz$\mathsf{<}$ 0.3

An optical spectroscopic survey of the 3CR sample of radio galaxies withz$\mathsf{<}$ 0.3

Jet-Powered Molecular Hydrogen Emission From Radio Galaxies

Origin of X-shaped radio-sources: further insights from the properties of their host galaxies

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