J/A+A/642/A85ivo://CDS.VizieR/J/A+A/642/A85doi:10.26093/cds/vizier.36420085CDSde Gasperin F.Brunetti G.Bruggen M.van Weeren R.Williams W.L.,Botteon A.Cuciti V.Dijkema T.J.Edler H.Iacobelli M.Kang H.,Offringa A.Orru E.Pizzo R.Rafferty D.Rottgering H.Shimwell T.2021-01-04T08:31:55Z2020-10-09T08:57:48ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frgalaxy-clustersradio-sourcesinterferometryUltra-low frequency observations (<100MHz) are particularly challenging because they are usually performed in a low signal-to-noise ratio regime due to the high sky temperature and because of ionospheric disturbances whose effects are inversely proportional to the observing frequency. Nonetheless, these observations are crucial for studying the emission from low-energy populations of cosmic rays. We aim to obtain the first thermal-noise limited (~1.5mJy/beam) deep continuum radio map using the Low Frequency Array's Low Band Antenna (LOFAR LBA) system. Our demonstration observation targeted the galaxy cluster RX J0603.3+4214 (known as the Toothbrush cluster). We used the resulting ultra-low frequency (39-78MHz) image to study cosmic-ray acceleration and evolution in the post shock region considering the presence of a radio halo. We describe the data reduction we used to calibrate LOFAR LBA observations. The resulting image was combined with observations at higher frequencies (LOFAR 150MHz and VLA 1500MHz) to extract spectral information.Results.We obtained the first thermal-noise limited image from an observation carried out with the LOFAR LBA system using allDutch stations at a central frequency of 58MHz. With eight hours of data, we reached an rms noise of 1.3mJy/beam at a resolution of 18"x11". The procedure we developed is an important step towards routine high-fidelity imaging with the LOFAR LBA. Theanalysis of the radio spectra shows that the radio relic extends to distances of 800kpc downstream from the shock front, larger than what is allowed by electron cooling time. Furthermore, the shock wave started accelerating electrons already at a projected distance of <300kpc from the crossing point of the two clusters. These results may be explained by electrons being re-accelerated down stream by background turbulence, possibly combined with projection effects with respect to the radio halo.2020A&A...642A..85Dhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/642/A85CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/642/A85https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/642/A85http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/642/A85https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/642/A85https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/642/A85http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/642/A85GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/642/A85/list (List of fits images)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/642/A85/list?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/642/A85/list?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/642/A85/list?GETtext/xml+votable180.050000true90.923742.252770.0055555555555555566/6827https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/642/A85?format=asciiRadiodefaultJ/A+A/642/A85/listList of fits imagesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRAJ2000Right Ascension of center (J2000)degpos.eq.ra;meta.mainDEJ2000Declination of center (J2000)degpos.eq.dec;meta.mainNxNumber of pixels along X-axismeta.numberintNyNumber of pixels along Y-axismeta.numberintObs.dateObservation datestime.epoch;obsnullableFreqObserved frequencyMHzem.freqfloatsizeSize of FITS fileKibytephys.size;meta.fitsintFileNameName of FITS file, in subdirectory fitsmeta.id;meta.fitscharTitleTitle of the FITS filemeta.title;meta.fitschar