1 millimeter continuum observations of quasars

Ennis, D. J.; Neugebauer, G.; Werner, M. W.

doi:10.1086/160441

Cited by 40 publications

(8 citation statements)

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“…There was no evidence for IR through mm variability in 3C273 (14,15) and we referred to the spectrum of Fig 4a as the 'quiescent' state. During 1983 we observed a major flare in the IR through ran emission (15) and subsequent monitoring showed the spectral development of this flare (Fig 4b). The IR flux increased by a factor of four, the submm flux trebled, increased and then evolved to lower frequencies at approximately constant flux density.…”

Section: The Programme Of Observationsmentioning

confidence: 92%

Multifrequency Observations of Blazars

Robson¹,

Gear²,

Brown³

1987

Symp. - Int. Astron. Union

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This paper reports the results of a programme of multifrequency observations of a sample of Blazars concentrating particularly on the millimetre through infrared region. Our observations have demonstrated the need for a new model to explain the spectral behaviour of a major flare in 3C273. This also provides a good description of the variability exhibited by Blazars. We have also shown that the radio through mid-IR synchrotron spectrum of 3C273 is a separate component from the optical/IR.

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Section: The Programme Of Observationsmentioning

confidence: 92%

Multifrequency Observations of Blazars

Robson¹,

Gear²,

Brown³

1987

Symp. - Int. Astron. Union

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“…( 2) Absorption from the intervening plasma local to quasars and synchrotron self-absorption could also be important reasons (Strittmatter et al 1980;Condon et al 1980). However, radio searches at the lower band where the opacity is expected to be small do not show any significant change on the RLs to RQs ratio (Ennis et al 1982;Robson et al 1985). ( 3) Geometry effect could also be an important issue of RLs, if we consider the radio emission may be relativistically beamed for the small fraction of quasars with the jet point towards us (Urry et al 1995;Fan et al 2004;Fan et al 2014;Xiao et al 2015;Pei et al 2016).…”

Section: The Radio Dichotomymentioning

confidence: 99%

“…However, radio searches at the lower band where the opacity is expected to be small do not show any significant change on the RLs to RQs ratio (Ennis et al 1982;Robson et al 1985). ( 3) Geometry effect could also be an important issue of RLs, if we consider the radio emission may be relativistically beamed for the small fraction of quasars with the jet point towards us (Urry et al 1995;Fan et al 2004;Fan et al 2014;Xiao et al 2015;Pei et al 2016). The relativistic beaming models have enjoyed the popularity of interpreting the apparent superluminal motions (Kellermann et al 2004;Xiao et al 2019).…”

Section: The Radio Dichotomymentioning

confidence: 99%

The radio dichotomy of active galactic nuclei

Xiao,

Zhu,

et al. 2022

Preprint

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The question of radio dichotomy in the active galactic nuclei (AGNs) is still in debate even it has been proposed for more than forty years. In order to solve the old riddle, we collect a sample of AGNs with optical B band and radio 6cm wavelength data to analyze the radio loudness logR.Our results indicate a separation of logR = 1.37 ± 0.02 between radio-loud (RL) AGNs and radio-quiet (RQ) AGNs, suggest the existence of an RL/RQ dichotomy. For the first time, we suggest combining radio luminosity and radio loudness as a double-criterion to divide AGNs into RLs and RQs to avoid misclassification problems that may happen in the single-criterion scenario, we propose the double-criterion dividing line logL 6cm = −2.7logR + 44.3 by using a machine learning method.In addition, the key point of the RL/RQ dichotomy is the origin of radio emission for the two classes, we suggest the radio emission from RLs and RQs share the same origin, e.g. jets

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“…The near-infrared points were obtained at the Palomar Observatory. The radio points for 3C 48 are from Kellermann, Pauliny-Toth, and Williams (1969), while the millimeter limit is from Ennis, Neugebauer, and Werner (1982) and the visual observations are from Neugebauer et al (1979). kpc from the central source of 3C 48 (Sandage and Miller 1966;Wampler et al 1975).…”

Section: Origin Of Infrared Luminositymentioning

confidence: 99%

“…The measurements of 3C 345, including the IRAS and near-infrared points, were obtained in the 1983 April-May time period (Bregman et al 1985). For 1351 +640, the millimeter limit is from Ennis et al (1982), the radio point is from Condon et al (1981), and the visual observations are from Neugebauer et al (1979).…”

Section: • • Logc Rest Frequency Chzjmentioning

confidence: 99%

A new luminosity component in 3C 48

Neugebauer

Soifer

Miley

1985

ApJ

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The infrared emission from the quasar 3C 48 has a luminosity L z 5 x 10 12 L 0 and dominates the power outpu~ of the quasar system. It is shown that the infrared emission, unlike that of most radio-loud quasars, is ~ost likely not an extension of the radio emission of the quasar. It is argued that the infrared emission in 3C 48 is probably thermal radiation arising in a highly luminous galaxy surrounding the quasar.

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1 millimeter continuum observations of quasars

Cited by 40 publications

References 0 publications

Multifrequency Observations of Blazars

Multifrequency Observations of Blazars

The radio dichotomy of active galactic nuclei

A new luminosity component in 3C 48

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