An All-sky Catalogue of Strong Radio Sources at 408 MHz

Robertson, J. G.

doi:10.1071/ph730403

Cited by 40 publications

(15 citation statements)

References 2 publications

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“…Finally, we investigated polarization from Fornax A through RM synthesis. We found no evidence of polarized emission above three times the noise at any Faraday depth, indicating that the polarization fraction of the (Ellis & Hamilton 1966), 18 (Shain & Higgins 1954), 20 (Shain 1958), 85 (Mills, Slee & Hill 1960), 100 (Stanley & Slee 1950;Bolton, Stanley & Slee 1954), 400 (McGee, Slee & Stanley 1955, 408 (Robertson 1973), 600 (Piddington & Trent 1956), 843 (Jones & McAdam 1992) and 1415 MHz (Ekers et al 1983). The filled circle is from this work.…”

Section: Fornax Amentioning

confidence: 70%

A 189 MHz, 2400 deg²POLARIZATION SURVEY WITH THE MURCHISON WIDEFIELD ARRAY 32-ELEMENT PROTOTYPE

Bernardi

Greenhill

Mitchell

et al. 2013

ApJ

102

139

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We present a Stokes I, Q and U survey at 189 MHz with the Murchison Widefield Array 32element prototype covering 2400 square degrees. The survey has a 15.6 arcmin angular resolution and achieves a noise level of 15 mJy beam −1 . We demonstrate a novel interferometric data analysis that involves calibration of drift scan data, integration through the co-addition of warped snapshot images and deconvolution of the point spread function through forward modeling. We present a point source catalogue down to a flux limit of 4 Jy. We detect polarization from only one of the sources, PMN J0351-2744, at a level of 1.8 ± 0.4%, whereas the remaining sources have a polarization fraction below 2%. Compared to a reported average value of 7% at 1.4 GHz, the polarization fraction of compact sources significantly decreases at low frequencies. We find a wealth of diffuse polarized emission across a large area of the survey with a maximum peak of ∼13 K, primarily with positive rotation measure values smaller than +10 rad m −2 . The small values observed indicate that the emission is likely to have a local origin (closer than a few hundred parsecs). There is a large sky area at α ≥ 2 h 30 m where the diffuse polarized emission rms is fainter than 1 K. Within this area of low Galactic polarization we characterize the foreground properties in a cold sky patch at (α, δ) = (4 h , −27 • .6) in terms of three dimensional power spectra.

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Section: Fornax Amentioning

confidence: 70%

A 189 MHz, 2400 deg²POLARIZATION SURVEY WITH THE MURCHISON WIDEFIELD ARRAY 32-ELEMENT PROTOTYPE

Bernardi

Greenhill

Mitchell

et al. 2013

ApJ

102

139

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“…2). Their sample of 1009 sources was taken from several catalogs including 5C12 (Benn et al 1982), B2 (Grueff & Vigotti 1979), MC1 (Davies et al 1973), MC2 and MC3 (Large et al 1981), All-sky Survey (Robertson 1973). Kapahi & Kulkarni (1986), Kulkarni & Mantovani (1985, 1985 and Kulkarni et al (1990) claimed that the median spectral index is constant at α med ∼ −0.9 in the same flux density range from 1 Jy to ∼0.1 Jy.…”

Section: Introductionmentioning

confidence: 99%

New results on the spectral index–flux density relation from the WENSS/NVSS catalogs

Zhang

Reich

et al. 2003

A&A

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Abstract. We present new statistical results on the spectral index-flux density relation for large samples of radio sources using archival data of the most sensitive surveys, such as WENSS and NVSS. Instrumental selection effects and the completeness of the catalogs used in this study are discussed. Our main results are based on the spectral indices calculated for about 185 800 sources from the WENSS (327 MHz) and the NVSS (1.4 GHz) catalogs and are summarized as follows: (1) The median spectral index increases from α med ∼ −0.9 to α med ∼ −0.8 (S ν ∝ ν α ) for S 327 flux densities decreasing from 0.1 Jy down to 23 mJy. The median spectral indices nearly show no variation within the error bars in the flux density range above 100 mJy up to several Jy. The median spectral index slightly increases again for S 327 above several Jy. The new results confirm published models of the radio luminosity function (RLF) for sources with S 327 > 0.1 Jy and give constraints to the models for sources of 0.023 Jy < S 327 < 0.1 Jy, respectively. (2) A dependence of the fractions of ultra-steep-spectrum sources (USS, −1.5 ≤ α < −1.0), steep-spectrum sources (SSS, −1.0 ≤ α < −0.5) and flat-spectrum sources (FSS, −0.5 ≤ α ≤ 0.0) is partly responsible for the spectral flattening. Another contribution to the spectral flattening comes from the variation of α med of steep-spectrum sources (α < −0.5) themselves which increases with decreasing flux densities. (3) The spectral flattening for faint sources (down to S 327 ∼ 20 mJy) with steep spectra (α < −0.5) suggests that α med is correlated with luminosity rather than redshift according to the source evolution model of Condon (1984).

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“…There are 177 sidelobes resulting from 248 sources from the MRC and the strong source list of Robertson (1973). With notable exceptions, all sources responsible for sidelobes are less than 3 deg.…”

Section: (A) Mds2 Mapsmentioning

confidence: 99%

“…To ensure that all sidelobes are recognized, the MRC, the catalogue of strong sources by Robertson (1973) and the list of strong sources from Allen (1973, p. 271) have been searched for sources expected to produce observable sidelobes at the >30 mJy level. Such sources must be stronger than ~0.7 Jy as the first subsidiary maximum of the beam is ~4.87 0 of the response.…”

Section: (A) Mds2 Mapsmentioning

confidence: 99%

A Confusion Limited Radio Survey from the Molonglo Cross

White

1984

Publ. Astron. Soc. Aust.

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Several catalogues of radio sources at 408 MHz have been prepared from observations made with the Molonglo cross telescope. These include (in chronological order) ‘The Molonglo Radio Source Catalogue 1’, the MC1, by Davies et al. (1973), the MC2 and MC3 by Sutton et al. (1974), MC4 by Clarke et al. (1976), ‘The Molonglo Deep Sky Survey of Radio Sources’ by Robertson (1977a,b,d) and ‘The Molonglo Reference Catalogue of Radio Sources’ (MRC) by Large et al. (1981). The catalogues MC1-4 cover selected areas of sky to a flux density limit of ~0.2 Jy to 0.3 Jy. The MRC includes extragalactic radio sources between δ = +18° and δ = −85° and is essentially complete at S408 = 1.00 Jy with raany sources to ˜0.7 Jy. The Wyllie (1969a,b) scale of flux density is used throughout.

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An All-sky Catalogue of Strong Radio Sources at 408 MHz

Cited by 40 publications

References 2 publications

A 189 MHz, 2400 deg²POLARIZATION SURVEY WITH THE MURCHISON WIDEFIELD ARRAY 32-ELEMENT PROTOTYPE

A 189 MHz, 2400 deg²POLARIZATION SURVEY WITH THE MURCHISON WIDEFIELD ARRAY 32-ELEMENT PROTOTYPE

New results on the spectral index–flux density relation from the WENSS/NVSS catalogs

A Confusion Limited Radio Survey from the Molonglo Cross

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An All-sky Catalogue of Strong Radio Sources at 408 MHz

Cited by 40 publications

References 2 publications

A 189 MHz, 2400 deg2POLARIZATION SURVEY WITH THE MURCHISON WIDEFIELD ARRAY 32-ELEMENT PROTOTYPE

A 189 MHz, 2400 deg2POLARIZATION SURVEY WITH THE MURCHISON WIDEFIELD ARRAY 32-ELEMENT PROTOTYPE

New results on the spectral index–flux density relation from the WENSS/NVSS catalogs

A Confusion Limited Radio Survey from the Molonglo Cross

Contact Info

Product

Resources

About

A 189 MHz, 2400 deg²POLARIZATION SURVEY WITH THE MURCHISON WIDEFIELD ARRAY 32-ELEMENT PROTOTYPE

A 189 MHz, 2400 deg²POLARIZATION SURVEY WITH THE MURCHISON WIDEFIELD ARRAY 32-ELEMENT PROTOTYPE