Optical spectra of 3CR radio galaxies

Hine, R. G.; Longair, M. S.

doi:10.1093/mnras/188.1.111

Cited by 244 publications

(220 citation statements)

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“…In contrast, FRII host galaxies are usually found in smaller groups (Zirbel 1997). Related to this, Hine & Longair (1979) found that radio galaxies in clusters (typically FRIs) tended to show only absorption lines or weak [O II] emission in their optical spectra, whereas most radio galaxies with strong emission lines were not members of clusters. This is not surprising given the known star formation-density (Lewis et al 2002) and morphologydensity (Dressler 1980) relations.…”

Section: Introductionmentioning

confidence: 98%

Galaxy And Mass Assembly (GAMA): the environments of high- and low-excitation radio galaxies

Ching

Croom

Sadler

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We study the environments of low-and high-excitation radio galaxies (LERGs and HERGs respectively) in the redshift range 0.01 < z < 0.4, using a sample of 399 radio galaxies and environmental measurements from the Galaxy And Mass Assembly (GAMA) survey. In our analysis we use the fifth nearest neighbour density (Σ 5 ) and the GAMA galaxy groups catalogue (G3Cv6) and construct control samples of galaxies matched in stellar mass and colour to the radio-detected sample.We find that LERGs and HERGs exist in different environments and that this difference is dependent on radio luminosity. High-luminosity LERGs (L NVSS 10 24 W Hz −1 ) lie in much denser environments than a matched radio-quiet control sample (about three times as dense, as measured by Σ 5 ), and are more likely to be members of galaxy groups (82 +5 −7 percent of LERGs are in GAMA groups, compared to 58 +3 −3 percent of the control sample). In contrast, the environments of the HERGs and lower luminosity LERGs are indistinguishable from that of a matched control sample. Our results imply that high-luminosity LERGs lie in more massive haloes than non-radio galaxies of similar stellar mass and colour, in agreement with earlier studies (Wake et al. 2008;Donoso et al. 2010). When we control for the preference of LERGs to be found in groups, both high-and low-luminosity LERGs are found in higher-mass haloes (∼ 0.2 dex; at least 97 percent significant) than the non-radio control sample.

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Section: Introductionmentioning

confidence: 98%

Galaxy And Mass Assembly (GAMA): the environments of high- and low-excitation radio galaxies

Ching

Croom

Sadler

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…Kristian, Sandage, andWestphal 1974, 1978;Laing et al 1978;Riley, Longair, and Gunn 1980;Gunn et al 1981) even at very faint optical magnitudes. These faint, presumably distant 3CR sources all have very high radio luminosities, and this property correlates with the long-known propensity of the central optical galaxy to show strong (nuclear) emission lines (Smith, Spinrad, and Smith 1976;Hine and Longair 1979;Wilkinson, Hine, and Sargent 1981).…”

Section: Introduction Observational Philosophy Data Presentationmentioning

confidence: 61%

Redshifts and spectroscopy of very distant radio galaxies with strong emission lines

Spinrad¹

1982

PASP

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The optical spectra of six newly observed 3CR radio galaxies, mostly with redshifts near unity, are unique with enormously strong [O II] emission. The observed equivalent widths of A 0 3727 range from 100 Á to about 2000 Á, and the luminosity in this single line exceeds 10 10 L© in the extreme case of 3C 368 (z = 1.13).The coarse line ratios and linewidths of [Oïl], [NeIII], [Ne v], and the occasional presence of MgII suggest a shock-excitation model for the gas in 3C 368, 3C 184, 3C 175.1, and possibly 3C 34. 3C 356 and 3C 280 have moderately strong [Nev] and may require a uv power-law continuum. A rough inverse-correlation exists between the emission lines velocity width and relative strengths of the high-ionization [Nev] and the strong low-ionization [Oil] lines. The energetics of a shock-origin for the low-ionization lines may be difficult unless a large reservoir of neutral gas is available.The shape of the thermal continuum of 3C 280 has been measured-this galaxy consists of old stars with a spectral distribution consistent with Bruzual models which have a last epoch of star formation ceasing at 2 > 4.We note that these very luminous radio galaxies are the ones which experience rapid evolution needed to explain the radio source counts. They are about 300 times more abundant (per unit co-moving volume) at 2 ~ 1.0 than locally (z ~ 0.1). Perhaps this rapid evolutionary turnoff at the present epoch represents some efficient utilization and later unavailability of an external fuel source, much more commonly available to gE galaxies a half-Hubble-time ago.

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“…The FRII-quasar sources are galaxies with class 'A' spectra (Hine & Longair, 1979), having strong, high-excitation emission lines in their optical/UV spectra. The FRII-BL Lac sources are galaxies with class 'B' spectra (Hine & Longair, 1979), having only weak, if any, high-excitation lines in their spectra. The second part of the scheme posits that FRI radio galaxies are the parent population of the remainder of the BL Lac type objects.…”

Section: Radio Source Evolutionmentioning

confidence: 99%

Radio Source Evolution Derived from Low Frequency Surveys

Jackson

Wall

2002

Symp. - Int. Astron. Union

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Abstract. We find simple parametric models to describe the space density evolution of radio-loud AGN, treating FRI and FRII radio galaxies separately as the two parent populations in our dual-population unified scheme. In this we use low frequency radio data (v < 500 MHz), where radio samples are unbiased by Doppler beaming. Incorporated into this latest analysis is a new determination of the local radio luminosity function at 1.4 GHz from galaxies common to both the 2dFGRS and NVSS surveys.

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Optical spectra of 3CR radio galaxies

Cited by 244 publications

References 0 publications

Galaxy And Mass Assembly (GAMA): the environments of high- and low-excitation radio galaxies

Galaxy And Mass Assembly (GAMA): the environments of high- and low-excitation radio galaxies

Redshifts and spectroscopy of very distant radio galaxies with strong emission lines

Radio Source Evolution Derived from Low Frequency Surveys

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