Flux densities of radio galaxies at 8000 MHz.

Stull, M. A.

doi:10.1086/111073

Cited by 10 publications

(5 citation statements)

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“…At radio wavelengths the data were collected from NED, which gives reference to the following papers: Pilkington and Scott (1965); Pauliny-Toth et al (1966); Gower et al (1967); Aslanian et al (1968); Kellermann et al (1969); Colla et al (1970); Stull (1971); Colla et al (1972); Kellermann and Pauliny-Toth (1973); Fanti et al (1974); Laing and Peacock (1980); Kuehr et al (1981); Large et al (1981); Geldzahler and Kuhr (1983); Ficarra et al (1985); Baldwin et al (1985); Hales et al (1988Hales et al ( , 1990; Becker et al (1991); Gregory and Condon (1991); Hales et al (1991); Becker et al (1995); Waldram et al (1996); Wiren et al (1992); Hales et al (1993); Gear et al (1994); Hales et al (1995); Griffith et al (1995); Klein et al (1996); Rengelink et al (1997)…”

Section: Radio Wavelengthsmentioning

confidence: 99%

STAR FORMATION IN 3CR RADIO GALAXIES AND QUASARS AT z < 1*

Westhues¹,

Haas²,

Barthel³

et al. 2016

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Using the Herschel Space Observatory we have observed a representative sample of 87 powerful 3CR sources at redshift z < 1. The far-infrared (FIR, 70-500 µm) photometry is combined with mid-infrared (MIR) photometry from the Wide-Field Infrared Survey Explorer (WISE) and catalogued data to analyse the complete spectral energy distributions (SEDs) of each object from optical to radio wavelength. To disentangle the contributions of different components, the SEDs are fitted with a set of templates to derive the luminosities of host galaxy starlight, dust torus emission powered by active galactic nuclei (AGN) and cool dust heated by stars. The level of emission from relativistic jets is also estimated, in order to isolate the thermal host galaxy contribution. The new data are in line with the orientation-based unification of highexcitation radio-loud AGN, in that the dust torus becomes optically thin longwards of 30 µm. The low excitation radio galaxies and the MIR weak sources represent MIR-and FIR-faint AGN population different from the high-excitation MIR-bright objects; it remains an open question whether they are at a later evolutionary state or an intrinsically different population. The derived luminosities for host starlight and dust heated by star formation are converted to stellar masses and star formation rates (SFR). The host-normalized SFR of the bulk of the 3CR sources is low when compared to other galaxy populations at the same epoch. Estimates of the dust mass yield a 1-100 times lower dust/stellar mass ratio than for the Milky Way, indicating that these 3CR hosts have very low levels of interstellar matter explaining the low level of star formation. Less than 10% of the 3CR sources show levels of star formation above those of the main sequence of star forming galaxies.

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Section: Radio Wavelengthsmentioning

confidence: 99%

STAR FORMATION IN 3CR RADIO GALAXIES AND QUASARS AT z < 1*

Westhues¹,

Haas²,

Barthel³

et al. 2016

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“…These mostly reflect classifications in LRL, supplemented by references quoted in H97, or from the spectrophotometry of Laing and co-workers (L94: Laing, private communication) for sources in LRL. The non-LRL sources have been classified from the following literature: 3C 15, 3C 105, 3C 403, Tadhunter et al(1993);3C 111, Sargent (1977) Stull (1971), as these sources were all seriously undersampled by the VLA observations. These numbers are to be treated with caution.…”

Section: Modelling: Future Workmentioning

confidence: 99%

“…References in parentheses are to papers used to classify the jets of objects that were not included in the analysis. 3C 136.1, 3C 192, 3C 227, 3C 327 and 3C 445 are taken from the single-dish measurements of Stull (1971), as these sources were all seriously undersampled by the VLA observations. These numbers are to be treated with caution.…”

Section: Modelling: Future Workmentioning

confidence: 99%

FRII radio galaxies with z < 0.3 - I. Properties of jets, cores and hotspots

Hardcastle

Alexander²,

Pooley³

et al. 1998

Monthly Notices of the Royal Astronomical Society

139

120

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In previous papers we have discussed high-resolution observations of a large sample of powerful radio galaxies with z < 0.3. Jets are detected in up to 80 per cent of the sample, and radio cores in nearly all the objects; in addition, we are able to resolve the hotspots in most sources. In this paper we present measurements of the radio properties of these components.The prominences of the jets detected do not appear to be a function of radio luminosity, providing the clearest evidence yet that the reported low detection rate of jets in radio galaxies has been an artefact of low-sensitivity observations. We find a positive correlation between the total source length and core prominence in the narrow-line radio galaxies. We have found evidence for a relationship between hotspot size and total source size, but few other significant relationships between hotspot properties and those of the jets or lobes. We compare our measurements with those of Bridle et al., based on observations of a sample of quasars, and argue that the results are consistent with a modification of the unified model in which the broad-line radio galaxies are the low-luminosity counterparts of quasars, although the situation is complicated by contamination with low-excitation radio galaxies which appear to have radio properties different from the high-excitation objects. We discuss the classes of empirical model that can be fitted to the data set.

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“…The luminosity at 1 GHz is 3.9 • 10 34 erg/Hz/s. Cygnus A, for example, has a flux of 214 Jy at 8 GHz (Stull, 1971), as two of our model cocoons if they are placed at the luminosity distance of 265 Mpc, similar to that of Cygnus A for H 0 = 65 km/s/Mpc and q 0 = 0.5 (Owen et al, 1997, for the redshift). The synchrotron and SSC central surface brightness of our radio cocoons are shown in Fig.…”

Section: Cygnus A-like Radio Galaxiesmentioning

confidence: 60%

Synchrotron self-Comptonized emission of low energy cosmic ray electrons in the Universe

Enßlin

Sunyaev

2002

A&A

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Abstract. Most of the Universe's populations of low energy cosmic ray electrons in the energy range of 1-100 MeV still manage to elude detection by our instruments, since their synchrotron emission is at too low frequencies. We investigate a mechanism which can lead to observable emission of such electron populations: synchrotronself Comptonization (SSC). The inverse Compton (IC) scattering can shift otherwise unobservable low-frequency 10 kHz-10 MHz photons into observable radio, infrared (IR) or even more energetic wave-bands. The resulting emission should be polarized. We also consider IC scattering of the cosmic microwave background (CMB) and the cosmic radio background (CRB). Electron spectral aging due to synchrotron, IC and adiabatic losses or gains influences the resulting spectrum. The predicted radiation spectrum is a strong function of the history of the source, of the low energy spectrum of relativistic electrons, and of redshift. It has typically two maxima, and a decrement in between at CMB frequencies. Detection will provide a sensitive probe of the environment of radio galaxies. We demonstrate that the fossil remnants of powerful radio galaxies are promising detection candidates, especially when they are embedded in a dense intra-cluster medium (ICM). GHz peaked sources (GPS) have very low SSC luminosities, which may, however, extend into the X-ray or even the gamma ray regime. Clusters of galaxies with relativistic electron populations may be another detectable sources. Fossil radio plasma released by our own Galaxy could be revealed by its large angular scale SSC flux. We discuss the expected detectability of these sources with new and upcoming instruments such as LOFAR, GMRT, EVLA, ATA, ALMA, PLANCK, and HERSCHEL.

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Flux densities of radio galaxies at 8000 MHz.

Cited by 10 publications

References 0 publications

STAR FORMATION IN 3CR RADIO GALAXIES AND QUASARS AT z < 1*

STAR FORMATION IN 3CR RADIO GALAXIES AND QUASARS AT z < 1*

FRII radio galaxies with z < 0.3 - I. Properties of jets, cores and hotspots

Synchrotron self-Comptonized emission of low energy cosmic ray electrons in the Universe

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