J/A+A/586/A92ivo://CDS.VizieR/J/A+A/586/A92doi:10.26093/cds/vizier.35860092CDSPilia M.Hessels J.W.T.Stappers B.W.Kondratiev V.I.Kramer M.,van Leeuwen J.Weltevrede P.Lyne A.G.Zagkouris K.Hassall T.E.,Bilous A.V.Breton R.P.Falcke H.Griessmeier J.-M.Keane E.,Karastergiou A.Kuniyoshi M.Noutsos A.Oslowski S.Serylak M.,Sobey C.Ter Veen S.Alexov A.Anderson J.Asgekar A.Avruch I.M.,Bell M.E.Bentum M.J.Bernardi G.Birzan L.Bonafede A.Breitling F.,Broderick J.W.Brueggen M.Ciardi B.Corbel S.De Geus E.De Jong A.,Deller A.Duscha S.Eisloeffel J.Fallows R.A.Fender R.Ferrari C.,Frieswijk W.Garrett M.A.Gunst A.W.Hamaker J.P.Heald G.,Horneffer A.Jonker P.Juette E.Kuper G.Maat P.Mann G.Markoff S.,McFadden R.McKay-Bukowski D.Miller-Jones J.C.A.Nelles A.Paas H.,Pandey-Pommier M.Pietka M.Pizzo R.Polatidis A.G.Reich W.,Roettgering H.Rowlinson A.Schwarz D.Smirnov O.Steinmetz M.,Stewart A.Swinbank J.D.Tagger M.Tang Y.Tasse C.Thoudam S.,Toribio M.C.van der Horst A.J.Vermeulen R.Vocks C.van Weeren R.J.,Wijers R.A.M.J.Wijnands R.Wijnholds S.J.Wucknitz O.Zarka P.2019-02-27T13:41:54Z2016-06-09T08:55:36ZCDS support team

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

cds-question@unistra.frpulsarsradio-sourcesLOFAR offers the unique capability of observing pulsars across the 10-240MHz frequency range with a fractional bandwidth of roughly 50%. This spectral range is well suited for studying the frequency evolution of pulse profile morphology caused by both intrinsic and extrinsic effects such as changing emission altitude in the pulsar magnetosphere or scatter broadening by the interstellar medium, respectively. The magnitude of most of these effects increases rapidly towards low frequencies. LOFAR can thus address a number of open questions about the nature of radio pulsar emission and its propagation through the interstellar medium. We present the average pulse profiles of 100 pulsars observed in the two LOFAR frequency bands: high band (120-167MHz, 100 profiles) and low band (15-62MHz, 26 profiles). We compare them with Westerbork Synthesis Radio Telescope (WSRT) and Lovell Telescope observations at higher frequencies (350 and 1400MHz) to study the profile evolution. The profiles were aligned in absolute phase by folding with a new set of timing solutions from the Lovell Telescope, which we present along with precise dispersion measures obtained with LOFAR. We find that the profile evolution with decreasing radio frequency does not follow a specific trend; depending on the geometry of the pulsar, new components can enter into or be hidden from view. Nonetheless, in general our observations confirm the widening of pulsar profiles at low frequencies, as expected from radius-to-frequency mapping or birefringence theories.2016A&A...586A..92Phttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/586/A92CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/586/A92https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/586/A92http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/586/A92https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/586/A92https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/586/A92http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/586/A92GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapRadiodefaultJ/A+A/586/A92/tableb3Peak ratiosrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintFlag[pn] p for previously studied cases and and n for newmeta.code.errorcharPSRPSR Namemeta.id;meta.maincharn_PSRIP indicates pulsars with an interpulsemeta.notecharBand1[LBA]instr.bandpasscharP1LBA? LBA-band amplitude of the most prominent peak normalised to the amplitude of the main peak of the profiletime.periodfloatnullableP2LBA? LBA-band amplitude of the second most prominent peak normalised to the amplitude of the main peak of the profiletime.periodfloatnullablephi1LBA? LBA-band spin phase of the most prominent peakstat.fit.paramfloatnullablephi2LBA? LBA-band spin phase of the second most prominent peakstat.fit.paramfloatnullableP2/P1LBA? LBA-band P2/P1 ratiotime.periodfloatnullableBand2[HBA]instr.bandpasscharP1HBA? HBA-band amplitude of the most prominent peak normalised to the amplitude of the main peak of the profiletime.periodfloatnullableP2HBA? HBA-band amplitude of the second most prominent peak normalised to the amplitude of the main peak of the profiletime.periodfloatnullablephi1HBA? HBA-band spin phase of the most prominent peakstat.fit.paramfloatnullablephi2HBA? HBA-band spin phase of the second most prominent peakstat.fit.paramfloatnullableP2/P1HBA? HBA-band P2/P1 ratiotime.periodfloatnullableBand3[P]instr.bandpasscharP1P? P-band amplitude of the most prominent peak normalised to the amplitude of the main peak of the profiletime.periodfloatnullableP2P? P-band amplitude of the second most prominent peak normalised to the amplitude of the main peak of the profiletime.periodfloatnullablephi1P? P-band spin phase of the most prominent peakstat.fit.paramfloatnullablephi2P? P-band spin phase of the second most prominent peakstat.fit.paramfloatnullableP2/P1P? P-band P2/P1 ratiotime.periodfloatnullableBand4[L]instr.bandpasscharP1L? L-band amplitude of the most prominent peak normalised to the amplitude of the main peak of the profiletime.periodfloatnullableP2L? L-band amplitude of the second most prominent peak normalised to the amplitude of the main peak of the profiletime.periodfloatnullablephi1L? L-band spin phase of the most prominent peakstat.fit.paramfloatnullablephi2L? L-band spin phase of the second most prominent peakstat.fit.paramfloatnullableP2/P1L? L-band P2/P1 ratiotime.periodfloatnullableJ/A+A/586/A92/tableb1List of the 100 pulsars and their rotational and derived parametersrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintPSRPSR Name (BHHMM+DD or JHHMM+DDMM)meta.id;meta.maincharPSpin periodstime.periodfloatdP/dtPeriod derivatives/stime.perioddoubleEpochReference epoch of the rotational ephemeris that was used to fold the data (MJD)dmeta.ref;time.epoch;phys.mol.rotationintEpochL? Lofar LBA observation epoch (MJD)dtime.epoch;obsintnullableEpochHLofar HBA observation epoch (MJD)dtime.epochintDMephDispersion measure used to dedisperse the observations at higher frequenciespc.cm**-3phys.dispMeasuredoublee_DMephrms uncertainty on DMephpc.cm**-3stat.errorfloatr_DMephReference for DMeph (1)meta.ref;pos.frameintDMHBABest dispersion measure obtained from the fit of the HBA LOFAR observationspc.cm**-3phys.dispMeasuredoublel_e_DMHBALimit flag on DMHBAmeta.code.errorchare_DMHBArms uncertainty on DMHBApc.cm**-3stat.errorfloatlogtauPulsar spin-down agelog(yr)time.agefloatlogBMagnetic field strengthlog(G)phys.atmol.collStrength;obs.fieldfloatlogdE/dtSpin-down luminosity as derived from the rotational parameterslog(1e-07W)phys.luminosity;em.radiofloatObs1Note on observationmeta.id;obscharn_Obs1[bcd] Note for Obs1 (2)meta.notecharObs2Note on observationmeta.id;obscharn_Obs2[bcd] Note for Obs2 (2)meta.notecharSimbadSimbad column added by the CDSmeta.ref.urlcharJ/A+A/586/A92/tableb2Width of the full profile and duty cycleBand3[P]instr.bandpasscharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintPSRPSR Namemeta.id;meta.maincharn_PSRIP indicates pulsars with an interpulsemeta.notechard50? Spectral index {delta} of the evolution of W50 with observing frequency (1)spect.indexfloatnullablee_d50? rms uncertainty on d50stat.errorfloatnullabled10? Spectral index {delta} of the evolution of W10 with observing frequency (1)spect.indexfloatnullablee_d10? rms uncertainty on d10stat.errorfloatnullableBand1[LBA]instr.bandpasscharW50LBA? LBA-band full width at half maximum, W50degspect.line.widthfloatnullablee_W50LBA? rms uncertainty on W50LBAdegstat.errorfloatnullableW10LBA? LBA-band width of the full profile, W10degspect.line.widthfloatnullablee_W10LBA? rms uncertainty on W10LBAdegstat.errorfloatnullableW10/PLBA? LBA-band duty cycle of the pulse, W10/P, indicated as percent age of the total profile%spect.line.widthfloatnullablee_W10/PLBA? rms uncertainty on W10/PLBA%stat.errorfloatnullableSatLBA[s] s for saturated (2)meta.codecharBand2[HBA]instr.bandpasscharW50HBA? HBA-band full width at half maximum, W50degspect.line.widthfloatnullablee_W50HBA? rms uncertainty on W50HBAdegstat.errorfloatnullableW10HBA? HBA-band width of the full profile, W10degspect.line.widthfloatnullablee_W10HBA? rms uncertainty on W10HBAdegstat.errorfloatnullableW10/PHBA? HBA-band duty cycle of the pulse, W10/P, indicated as percent age of the total profile%spect.line.widthfloatnullablee_W10/PHBA? rms uncertainty on W10/PHBA%stat.errorfloatnullableSatHBA[s] s for saturated (2)meta.codecharW50P? P-band full width at half maximum, W50degspect.line.widthfloatnullablee_W50P? rms uncertainty on W50Pdegstat.errorfloatnullableW10P? P-band width of the full profile, W10degspect.line.widthfloatnullablee_W10P? rms uncertainty on W10Pdegstat.errorfloatnullableW10/PP? P-band duty cycle of the pulse, W10/P, indicated as percent age of the total profile%spect.line.widthfloatnullablee_W10/PP? rms uncertainty on W10/PP%stat.errorfloatnullableBand4[L]instr.bandpasscharW50L? L-band full width at half maximum, W50degspect.line.widthfloatnullablee_W50L? rms uncertainty on W50Ldegstat.errorfloatnullableW10L? L-band width of the full profile, W10degspect.line.widthfloatnullablee_W10L? rms uncertainty on W10Ldegstat.errorfloatnullableW10/PL? L-band duty cycle of the pulse, W10/P, indicated as percent age of the total profile%spect.line.widthfloatnullablee_W10/PL? rms uncertainty on W10/PL%stat.errorfloatnullable