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000453899 0247_ $$2ISSN$$a1432-0746
000453899 0247_ $$2arXiv$$aarXiv:2002.10431
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000453899 088__ $$2arXiv$$aarXiv:2002.10431
000453899 1001_ $$0F.De.Gasperin.1$$ade Gasperin, F.$$b0
000453899 245__ $$aCassiopeia A, Cygnus A, Taurus A, and Virgo A at ultra-low radio frequencies
000453899 260__ $$aLes Ulis$$bEDP Sciences$$c2020
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000453899 500__ $$a© ESO 2020   7 pages, 2 figures, accepted A&A, online data on A&A website
000453899 520__ $$aContext. The four persistent radio sources in the northern sky with the highest flux density at metre wavelengths are Cassiopeia A, Cygnus A, Taurus A, and Virgo A; collectively they are called the A-team. Their flux densities at ultra-low frequencies (< 100 MHz) can reach several thousands of janskys, and they often contaminate observations of the low-frequency sky by interfering with image processing. Furthermore, these sources are foreground objects for all-sky observations hampering the study of faint signals, such as the cosmological 21 cm line from the epoch of reionisation.Aims. We aim to produce robust models for the surface brightness emission as a function of frequency for the A-team sources at ultra-low frequencies. These models are needed for the calibration and imaging of wide-area surveys of the sky with low-frequency interferometers. This requires obtaining images at an angular resolution better than 15″ with a high dynamic range and good image fidelity.Methods. We observed the A-team with the Low Frequency Array (LOFAR) at frequencies between 30 MHz and 77 MHz using the Low Band Antenna system. We reduced the datasets and obtained an image for each A-team source.Results. The paper presents the best models to date for the sources Cassiopeia A, Cygnus A, Taurus A, and Virgo A between 30 MHz and 77 MHz. We were able to obtain the aimed resolution and dynamic range in all cases. Owing to its compactness and complexity, observations with the long baselines of the International LOFAR Telescope will be required to improve the source model for Cygnus A further.
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000453899 650_7 $$2autogen$$aradio continuum: general
000453899 650_7 $$2autogen$$atechniques: interferometric
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000453899 7001_ $$0J.S.Vink.1$$aVink, J.$$b1
000453899 7001_ $$0J.P.McKean.1$$aMcKean, J. P.$$b2
000453899 7001_ $$0A.Asgekar.1$$aAsgekar, A.$$b3
000453899 7001_ $$0M.J.Bentum.1$$aBentum, M. J.$$b4
000453899 7001_ $$0R.Blaauw.1$$aBlaauw, R.$$b5
000453899 7001_ $$0A.Bonafede.1$$aBonafede, A.$$b6
000453899 7001_ $$0M.Brueggen.1$$aBruggen, M.$$b7
000453899 7001_ $$0F.Breitling.1$$aBreitling, F.$$b8
000453899 7001_ $$0W.N.Brouw.1$$aBrouw, W. N.$$b9
000453899 7001_ $$0H.Butcher.1$$aButcher, H. R.$$b10
000453899 7001_ $$0B.Ciardi.1$$aCiardi, B.$$b11
000453899 7001_ $$0V.Cuciti.1$$aCuciti, V.$$b12
000453899 7001_ $$0M.de.Vos.1$$ade Vos, M.$$b13
000453899 7001_ $$0S.Duscha.1$$aDuscha, S.$$b14
000453899 7001_ $$0J.Eisloffel.1$$aEisloffel, J.$$b15
000453899 7001_ $$0D.Engels.1$$aEngels, D.$$b16
000453899 7001_ $$0R.A.Fallows.1$$aFallows, R. A.$$b17$$eCorresponding author
000453899 7001_ $$0T.M.O.Franzen.2$$aFranzen, T. M. O.$$b18
000453899 7001_ $$0M.A.Garrett.1$$aGarrett, M. A.$$b19
000453899 7001_ $$0A.W.Gunst.1$$aGunst, A. W.$$b20
000453899 7001_ $$0J.R.Horandel.1$$aHorandel, J.$$b21
000453899 7001_ $$0G.Heald.1$$aHeald, G.$$b22
000453899 7001_ $$0L.V.E.Koopmans.3$$aKoopmans, L. V. E.$$b23
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000453899 7001_ $$aOrrú, E.$$b32
000453899 7001_ $$0H.Paas.1$$aPaas, H.$$b33
000453899 7001_ $$0M.Pandey.Pommier.1$$aPandey-Pommier, M.$$b34
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000453899 7001_ $$aReich, W.$$b36
000453899 7001_ $$0A.Rowlinson.1$$aRowlinson, A.$$b37
000453899 7001_ $$0D.J.Schwarz.2$$aSchwarz, D. J.$$b38
000453899 7001_ $$0A.Shulevski.1$$aShulevski, A.$$b39
000453899 7001_ $$aSmirnov, O.$$b40
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000453899 7001_ $$0M.Tagger.1$$aTagger, M.$$b42
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000453899 7001_ $$0A.van.Ardenne.1$$avan Ardenne, A.$$b44
000453899 7001_ $$0A.J.Van.Der.Horst.4$$avan der Horst, A. J.$$b45
000453899 7001_ $$0M.P.V.Haarlem.1$$avan Haarlem, M. P.$$b46
000453899 7001_ $$0R.J.van.Weeren.1$$avan Weeren, R. J.$$b47
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