J/A+A/693/A279ivo://CDS.VizieR/J/A+A/693/A279doi:10.26093/cds/vizier.36930279CDSPastor-Marazuela I.van Leeuwen J.Bilous A.Connor L.Maan Y.,Oostrum L.Petroff E.Vohl D.HessK.-M.Orru E.Sclocco A.Wang Y.2025-03-03T20:01:28Z2025-01-23T08:36:53ZCDS support team

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

cds-question@unistra.frradio-sourcesneutron-starsgalaxy-classification-systemsredshiftedUnderstanding the origin of energetic fast radio bursts (FRBs) has become the main science driver of recent dedicated FRB surveys powered by real-time instrumentation. Between July 2019 and February 2022, we carried out ALERT, an FRB survey at 1370MHz using the Apertif Radio Transient System (ARTS) installed at the Westerbork Synthesis Radio Telescope (WSRT). Here we report the detection of 18 new FRBs. We studied the properties of the entire 24-burst sample that were detected during the survey. For five bursts, we identified host galaxy candidates within their error regions with >50% probability association. We observed an average linear polarisation fraction of ~43% and an average circular polarisation fraction consistent with 0%. One-third of the FRBs display multiple components. These burst structures and the polarisation fractions are strikingly similar to those observed in young energetic pulsars and magnetars. The Apertif FRBs next reveal a population of highly scattered bursts. Given the observing frequency and time resolution, the scattering of most FRBs is likely to have been produced in the immediate circumburst environment. Furthermore, two FRBs show evidence of high rotation measure values, which could reach |RM|>10^3^rad/m^2^ in the source reference frames. This corroborates that some source environments are dominated by magneto-ionic effects. Together, the scattering and rotation measures that ALERT has found prove that a large fraction of FRBs are embedded in complex media such as star-forming regions or supernova remnants. Through the discovery of FRB20200719A, the third most dispersed FRB so far, we further show that one-off FRBs emit at frequencies in excess of 6GHz, the highest known to date. We compare this to the radio-bright high-frequency emission seen in magnetars. Finally, we determine an FRB all-sky rate of 459^+208^_-155_sky^-1^day^-1^ above a fluence limit of 4.1Jy.ms, and a fluence cumulative distribution with a power-law index gamma=-1.23+/-0.06+/-0.2, which is roughly consistent with the Euclidean Universe predictions. Through the high resolution in time, frequency, polarisation, and localisation that ALERT featured, we were able to determine the morphological complexity, polarisation, local scattering and magnetic environment, and high-frequency luminosity of FRBs. We find all of these parameters strongly resemble those seen in young, energetic, highly magnetised neutron stars.2025A&A...693A.279Phttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/693/A279CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/693/A279https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/693/A279http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/693/A279https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/693/A279https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/693/A279http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/693/A279GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/693/A279/frbs (Apertif fast radio burst properties)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/693/A279/frbs?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/693/A279/frbs?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/693/A279/frbs?GETtext/xml+votable180.050000true24.83208332.0586940.0055555555555555566/618 2156 2159 2241 3639 8032 8034-8035 8040 9283 10734 10838 12609 12611 14973-14975 15598 15905 15910 15940 16316 19435https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/693/A279?format=asciiOpticalRadiodefaultJ/A+A/693/A279/frbsApertif fast radio burst propertiesS/NSignal-to-noise ratiostat.snrintNNumber of burst subcomponentsmeta.numberintFluxBurst peak fluxJyphot.flux.density;em.radio.750-1500MHzfloate_FluxBurst peak flux errorJystat.error;phot.fluxfloatFluenceBurst fluenceJy.msphot.fluence;em.gamma.hardfloate_FluenceBurst fluence errorJy.msstat.error;phot.fluencefloatWidthBurst temporal widthmstime.intervalfloate_WidthBurst temporal width errormsstat.error;spect.line.widthfloattausc? Scattering timescale, {tau}_sc_mstime.scalefloatnullablee_tausc? Scattering timescale errormsstat.errorfloatnullablescbw? Scintillation bandwidth, {Delta}{nu}_sc_MHzem.freqfloatnullablee_scbw? Scintillation bandwidth errorMHzstat.errorfloatnullableFpeakBurst peak frequency (1)MHzphot.flux.density;em.radio.750-1500MHzinte_Fpeak? Burst peak frequency errorMHzstat.errorintnullableBWBurst bandwidth (2)MHzem.freqchare_BW? Burst bandwidth errorMHzstat.errorintnullableaLocalisation ellipse semi-major axis (3)arcsecphys.angSize;srcintbLocalisation ellipse semi-minor axis (3)arcsecphys.angSize.sminAxisfloatthetaBurst localisation ellipse angle (3)degpos.posAngfloatlocareaBurst localisation areaarcmin**2phys.areafloatCBBurst detection compound beamstat.fit.paramintSBBurst detection synthesised beamstat.fit.paramintDMNE2001Galactic DM contribution from NE2001 modelpc.cm**-3phys.dispMeasureintDMhaloGalactic halo DM contribution from Yamasaki & Totani (2020ApJ...888..105Y) modelpc.cm**-3phys.dispMeasureintzMedian redshift expected from the Macquart relation for the FRB excess DMsrc.redshiftfloatb_zRedshift 2.5% lower limit expected from the Macquart relation for the FRB excess DMsrc.redshift;stat.minfloatB_zRedshift 97.5% upper limit from the Macquart relation for the FRB excess DMsrc.redshift;stat.maxfloatSI? Spectral index Gamma of bursts with power-law spectrumspect.indexfloatnullablee_SI? Spectral index errorstat.errorfloatnullablealpha? Scattering index of scattered burstsspect.index;em.line.Halphafloatnullablee_alpha? Scattering index errorstat.error;pos.eq.rafloatnullableFrestExpected rest frame frequency at Macquart median redshift, nu_0_GHzem.freqfloatisoeExpected isotropic energy at Macquart median redshift1e-07Jphys.energyfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTNSSource id from transient name server (FRBYYYYMMDDA)meta.id;meta.maincharRAJ2000Right Ascension J2000pos.eq.ra;meta.mainDEJ2000Declination J2000pos.eq.dec;meta.mainMJDBarycentric modified Julian date of FRBdtime.epochdoubleDMDispersion measure of FRBpc.cm**-3phys.dispMeasure;instr.dispersionfloate_DMDispersion measure errorpc.cm**-3stat.errorfloat