The Molonglo Reference Catalog/1 Jansky Radio Source Survey. I. Radio Galaxy Identifications

McCarthy, Patrick J.; Kapahi, V. K.; Breugel, Wil van; Persson, S. E.; Athreya, R.; Subrahmanya, C. R.

doi:10.1086/192353

Cited by 91 publications

(85 citation statements)

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“…As the median spectral index for the 446 MRC galaxies resulted to be α 1400 408 = −0.85 ± 0.01, a 'canonical' spectral index bias α 1400 408 < −1 has been chosen to select this newly defined MRC USS sample. McCarthy et al (1996) reported a 96% identification fraction of the MRC radio sources down to the r = 25 magnitude. To date, r-band magnitudes are available for 334 of these 446 MRC galaxies and redshift information is available for 225 of these 334 galaxies (McCarthy et al 1996, Kapahi et al 1998 and references therein).…”

Section: The Mrc/1jy Sample -Radio and Optical Datamentioning

confidence: 97%

“…Actually, the only available low-frequency sample, free of selection biases and with a reasonably complete radio/optical dataset is the MRC/1Jy sample selected by McCarthy et al(1996) from the Molonglo Reference Catalogue (Large et al 1981). In the following it will be shown that, despite a substantial redshift incompleteness toward the faintest magnitudes, this sample can provide a dataset five times larger than the B2/1Jy sample, well suited for statistical studies.…”

Section: The Mrc/1jy Sample -Radio and Optical Datamentioning

confidence: 99%

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On the efficiency of the Ultra Steep Spectrum technique in finding high-z radiogalaxies

Pedani

2003

New Astronomy

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Section: The Mrc/1jy Sample -Radio and Optical Datamentioning

confidence: 97%

Section: The Mrc/1jy Sample -Radio and Optical Datamentioning

confidence: 99%

On the efficiency of the Ultra Steep Spectrum technique in finding high-z radiogalaxies

Pedani

2003

New Astronomy

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“…With the present 23.2 GHz observations we detect total intensity and polarised emission only from component "c". Here we have used a redshift of 1.41 ± 0.05 (McCarthy et al 1996) for estimating the rest-frame RM. 0116+319 (4C 31.04) -This source was observed by van Breugel et al (1984) at 15 GHz with the VLA.…”

Section: Comments On Individual Sourcesmentioning

confidence: 99%

Radio polarimetry of compact steep spectrum sources at sub-arcsecond resolution

Mantovani

Rossetti

Junor

et al. 2013

A&A

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Aims. We report new Very Large Array (VLA) polarimetric observations of compact steep-spectrum (CSS) sources at 8.4, 15, and 23 GHz. Methods. Using multi-frequency VLA observations we have derived sub-arcsecond resolution images of the total intensity, polarisation, and rotation measure (RM) distributions.Results. We present multi-frequency VLA polarisation observations of CSS sources. About half of the sources are point-like even at the resolution of ∼0.1 × 0.1 arcsec. The remaining sources have double or triple structure. Low values for the percentage of polarised emission in CSS sources is confirmed. On the average, quasars are more polarised than galaxies. A wide range of RM values have been measured. There are clear indications of very large RMs up to ≈5585 rad m −2 . CSS galaxies are characterized by RM values that are larger than CSS quasars. The majority of the objects show very large values of RM. Conclusions. The available data on sub-arcsecond-scale rest-frame RM estimates for CSS sources show that these have a wide range of values extending up to ∼36 000 rad m −2 . RM estimates indicate an overall density of the magneto-ionic medium larger than classical radio sources.

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“…To examine the relation between our observed spectral index and redshift in a consistent way, we determined the spectral indices for those spectroscopically identiÐed radio galaxies from the complete 3CR (Spinrad et al 1985) and MRC (McCarthy et al 1996) samples. We used spectral indices determined from the same radio surveys as in our USS sample (see Paper I for a discussion on our sample FIG.…”

Section: Redshift Distribution Of Uss Sourcesmentioning

confidence: 99%

Spectroscopy of Ultra–steep-Spectrum Radio Sources

Breuck

Breugel

Röttgering

et al. 2001

The Astronomical Journal

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112

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We present optical spectroscopy of 62 objects selected from several samples of ultraÈsteep-spectrum radio sources. Forty-six of these are from our primary catalog, consisting of 669 sources with radio spectral indices a \ [1.30 this Ðrst spectroscopic subsample was selected on the basis of their faint (S l P la) ; optical and near-IR identiÐcations. Most are identiÐed as narrow-lined radio galaxies with redshifts ranging from z \ 0.25 to z \ 5.19. Ten objects are at z [ 3, nearly doubling the number of such sources known to date. Four of the USS radio sources are identiÐed with quasars, of which at least three have very red spectral energy distributions. The source TN J0936[2242 is identiÐed with an extremely red object (ERO, R[K [ 5) ; both it and a close companion are at z \ 1.479. The spectrum of the ERO closely resembles that of previously discovered radio galaxies at z D 1.5. Five sources show continuum emission, but fail to show any clear emission or absorption features, despite integrations of D1 hr with the Keck telescope. We suggest that these objects could be (1) radio galaxies with faint emission lines in the "" redshift desert ÏÏ at (2) radio galaxies with an obscured active galactic nucleus, which 1.5 [ z [ 2.3, are dominated by a stellar continuum observed with an insufficient signal-to-noise ratio, or (3) pulsars. Three radio sources identiÐed with faint objects in the K-band images remain undetected in 50È90 minute spectroscopic integrations with the Keck telescope, and are possible z [ 7 candidates.

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The Molonglo Reference Catalog/1 Jansky Radio Source Survey. I. Radio Galaxy Identifications

Cited by 91 publications

References 0 publications

On the efficiency of the Ultra Steep Spectrum technique in finding high-z radiogalaxies

On the efficiency of the Ultra Steep Spectrum technique in finding high-z radiogalaxies

Radio polarimetry of compact steep spectrum sources at sub-arcsecond resolution

Spectroscopy of Ultra–steep-Spectrum Radio Sources

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