J/A+A/625/A152ivo://CDS.VizieR/J/A+A/625/A152doi:10.26093/cds/vizier.36250152CDSBarbieri C.Salafia O.S.Perego A.Colpi M.Ghirlanda G.2019-07-24T12:14:01Z2019-05-30T07:33:34ZCDS support team

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

cds-question@unistra.frastronomical-modelsblack-holesphotometryIn the new era of gravitational wave (GW) and multi-messenger astrophysics, the detection of a GW signal from the coalescence of a black hole - neutron star (BHNS) binary remains a highly anticipated discovery. This kind of system is expected to be within reach of the second generation of ground-based detectors. In this context, we develop a series of versatile semi-analytical models to predict the properties of all the electromagnetic (EM) counterparts of BHNS mergers.We include the nuclear-decay-powered kilonova emission, its radio remnant, the prompt emission from the jet and the related afterglow. The properties of these counterparts depend upon those of the outflows that result from the partial disruption of the NS during the merger and from the accretion disc around the remnant, which are necessary ingredients for transient EM emission to accompany the GW signal. We therefore define ways to relate the properties of these outflows to those of the progenitor binary, establishing a link between the binary parameters and the counterpart properties. From the resulting model, we anticipate the variety of light curves that can emerge after a BHNS coalescence, from the radio up to gamma-rays. These light curves feature universal traits which are the imprint of the dynamics of the emitting outflows, but at the same time they show a clear dependence on the BH mass and spin, though with a high degree of degeneracy. The latter can be deduced by joint GW - EM analysis. In this paper, we perform a proof-of-concept multi-messenger parameter estimation of a BHNS merger with an associated kilonova, to test how the information from the EM counterpart can complement that from the GW signal. Our results indicate that the observation and modeling of the kilonova can help to break the degeneracies in the GW parameter space, leading to better constraints on, e.g., the BH spin.2019A&A...625A.152Bhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/625/A152CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/625/A152https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/625/A152http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/625/A152https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/625/A152https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/625/A152http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/625/A152GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tap9.260793613549584e-20 3.0267355711601367e-19defaultJ/A+A/625/A152/panelaPanel a: Kilonova (KN) lightcurves varying the black hole massrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTime[0.1/50] Timedtime.agedoublemaga1Kilonova (KN) lightcurve magnitude (M_BH_=5.3M_{sun}_, Wavelength=657nm) (AB)magphot.mag;meta.modelledfloatmaga2Kilonova (KN) lightcurve magnitude (M_BH_=6.8M_{sun}_, Wavelength=657nm)magphot.mag;meta.modelledfloatmaga3Kilonova (KN) lightcurve magnitude (M_BH_=8.3M_{sun}_, Wavelength=657nm) (AB)magphot.mag;meta.modelledfloatmaga4Kilonova (KN) lightcurve magnitude (M_BH_=9.8M_{sun}_, Wavelength=657nm) (AB)magphot.mag;meta.modelledfloatmaga5Kilonova (KN) lightcurve magnitude (M_BH_=11.2M_{sun}_, Wavelength=657nm) (AB)magphot.mag;meta.modelledfloatmaga6Kilonova (KN) lightcurve magnitude (M_BH_=5.3M_{sun}_, Wavelength=2143nm) (AB)magphot.mag;meta.modelledfloatmaga7Kilonova (KN) lightcurve magnitude (M_BH_=6.8M_{sun}_, Wavelength=2143nm) (AB)magphot.mag;meta.modelledfloatmaga8Kilonova (KN) lightcurve magnitude (M_BH_=8.3M_{sun}_, Wavelength=2143nm) (AB)magphot.mag;meta.modelledfloatmaga9Kilonova (KN) lightcurve magnitude (M_BH_=9.8M_{sun}_, Wavelength=2143nm) (AB)magphot.mag;meta.modelledfloatmaga10Kilonova (KN) lightcurve magnitude (M_BH_=11.2M_{sun}_, Wavelength=2143nm) (AB)magphot.mag;meta.modelledfloatJ/A+A/625/A152/panelbPanel b: Kilonova (KN) lightcurves varying the black hole spinrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTime[0.1/50] Timedtime.agedoublemagb1Kilonova (KN) lightcurve magnitude (X_BH_=0.4, Wavelength=657nm) (AB) (G1)magphot.mag;meta.modelledfloatmagb2Kilonova (KN) lightcurve magnitude (X_BH_=0.5, Wavelength=657nm) (AB) (G1)magphot.mag;meta.modelledfloatmagb3Kilonova (KN) lightcurve magnitude (X_BH_=0.6, Wavelength=657nm) (AB) (G1)magphot.mag;meta.modelledfloatmagb4Kilonova (KN) lightcurve magnitude (X_BH_=0.7, Wavelength=657nm) (AB) (G1)magphot.mag;meta.modelledfloatmagb5Kilonova (KN) lightcurve magnitude (X_BH_=0.9, Wavelength=657nm) (AB) (G1)magphot.mag;meta.modelledfloatmagb6Kilonova (KN) lightcurve magnitude (X_BH_=0.4, Wavelength=2143nm) (AB) (G1)magphot.mag;meta.modelledfloatmagb7Kilonova (KN) lightcurve magnitude (X_BH_=0.5, Wavelength=2143nm) (AB) (G1)magphot.mag;meta.modelledfloatmagb8Kilonova (KN) lightcurve magnitude (X_BH_=0.6, Wavelength=2143nm) (AB) (G1)magphot.mag;meta.modelledfloatmagb9Kilonova (KN) lightcurve magnitude (X_BH_=0.7, Wavelength=2143nm) (AB) (G1)magphot.mag;meta.modelledfloatmagb10Kilonova (KN) lightcurve magnitude (X_BH_=0.9, Wavelength=2143nm) (AB) (G1)magphot.mag;meta.modelledfloatJ/A+A/625/A152/panelcPanel c: GRB Afterglow lightcurves at 657nm varying the black hole mass and viewing anglerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTime[1/10000] Timedtime.agedoubleFluxc1GRB Afterglow lightcurve flux (M_BH_=5.3M_{sun}_, Viewing angle=0deg)mJyphot.flux;meta.modelleddoubleFluxc2GRB Afterglow lightcurve flux (M_BH_=6.8M_{sun}_, Viewing angle=0deg)mJyphot.flux;meta.modelleddoubleFluxc3GRB Afterglow lightcurve flux (M_BH_=8.3M_{sun}_, Viewing angle=0deg)mJyphot.flux;meta.modelleddoubleFluxc4GRB Afterglow lightcurve flux (M_BH_=9.8M_{sun}_, Viewing angle=0deg)mJyphot.flux;meta.modelleddoubleFluxc5GRB Afterglow lightcurve flux (M_BH_=11.2M_{sun}_, Viewing angle=0deg)mJyphot.flux;meta.modelleddoubleFluxc6GRB Afterglow lightcurve flux (M_BH_=5.3M_{sun}_, Viewing angle=30deg)mJyphot.flux;meta.modelleddoubleFluxc7GRB Afterglow lightcurve flux (M_BH_=6.8M_{sun}_, Viewing angle=30deg)mJyphot.flux;meta.modelleddoubleFluxc8GRB Afterglow lightcurve flux (M_BH_=8.3M_{sun}_, Viewing angle=30deg)mJyphot.flux;meta.modelleddoubleFluxc9GRB Afterglow lightcurve flux (M_BH_=9.8M_{sun}_, Viewing angle=30deg)mJyphot.flux;meta.modelleddoubleFluxc10GRB Afterglow lightcurve flux (M_BH_=11.2M_{sun}_, Viewing angle=30deg)mJyphot.flux;meta.modelleddoubleFluxc11GRB Afterglow lightcurve flux (M_BH_=5.3M_{sun}_, Viewing angle=60deg)mJyphot.flux;meta.modelleddoubleFluxc12GRB Afterglow lightcurve flux (M_BH_=6.8M_{sun}_, Viewing angle=60deg)mJyphot.flux;meta.modelleddoubleFluxc13GRB Afterglow lightcurve flux (M_BH_=8.3M_{sun}_, Viewing angle=60deg)mJyphot.flux;meta.modelleddoubleFluxc14GRB Afterglow lightcurve flux (M_BH_=9.8M_{sun}_, Viewing angle=60deg)mJyphot.flux;meta.modelleddoubleFluxc15GRB Afterglow lightcurve flux (M_BH_=11.2M_{sun}_, Viewing angle=60deg)mJyphot.flux;meta.modelleddoubleJ/A+A/625/A152/paneldPanel d: GRB Afterglow lightcurves at 657nm varying the black hole spin and viewing anglerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTime[1/10000] Timedtime.agedoubleFluxd1[0] GRB Afterglow lightcurve flux (X_BH_=0.4, Viewing angle=0deg) (G1)mJyphot.flux;meta.modelledintFluxd2GRB Afterglow lightcurve flux (X_BH_=0.5, Viewing angle=0deg) (G1)mJyphot.flux;meta.modelleddoubleFluxd3GRB Afterglow lightcurve flux (X_BH_=0.6, Viewing angle=0deg) (G1)mJyphot.flux;meta.modelleddoubleFluxd4GRB Afterglow lightcurve flux (X_BH_=0.7, Viewing angle=0deg) (G1)mJyphot.flux;meta.modelleddoubleFluxd5GRB Afterglow lightcurve flux (X_BH_=0.9, Viewing angle=0deg) (G1)mJyphot.flux;meta.modelleddoubleFluxd6[0] GRB Afterglow lightcurve flux (X_BH_=0.4, Viewing angle=30deg) (G1)mJyphot.flux;meta.modelledintFluxd7GRB Afterglow lightcurve flux (X_BH_=0.5, Viewing angle=30deg) (G1)mJyphot.flux;meta.modelleddoubleFluxd8GRB Afterglow lightcurve flux (X_BH_=0.6, Viewing angle=30deg) (G1)mJyphot.flux;meta.modelleddoubleFluxd9GRB Afterglow lightcurve flux (X_BH_=0.7, Viewing angle=30deg) (G1)mJyphot.flux;meta.modelleddoubleFluxd10GRB Afterglow lightcurve flux (X_BH_=0.9, Viewing angle=30deg) (G1)mJyphot.flux;meta.modelleddoubleFluxd11[0] GRB Afterglow lightcurve flux (X_BH_=0.4, Viewing angle=60deg) (G1)mJyphot.flux;meta.modelledintFluxd12GRB Afterglow lightcurve flux (X_BH_=0.5, Viewing angle=60deg) (G1)mJyphot.flux;meta.modelleddoubleFluxd13GRB Afterglow lightcurve flux (X_BH_=0.6, Viewing angle=60deg) (G1)mJyphot.flux;meta.modelleddoubleFluxd14GRB Afterglow lightcurve flux (X_BH_=0.7, Viewing angle=60deg) (G1)mJyphot.flux;meta.modelleddoubleFluxd15GRB Afterglow lightcurve flux (X_BH_=0.9, Viewing angle=60deg) (G1)mJyphot.flux;meta.modelleddoubleJ/A+A/625/A152/panelePanel e: GRB Afterglow lightcurves at 1keV varying the black hole mass and viewing anglerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTime[1/10000] Timedtime.agedoubleFluxe1GRB Afterglow lightcurve flux (M_BH_=5.3M_{sun}_, Viewing angle=0deg)mJyphot.flux;meta.modelleddoubleFluxe2GRB Afterglow lightcurve flux (M_BH_=6.8M_{sun}_, Viewing angle=0deg)mJyphot.flux;meta.modelleddoubleFluxe3GRB Afterglow lightcurve flux (M_BH_=8.3M_{sun}_, Viewing angle=0deg)mJyphot.flux;meta.modelleddoubleFluxe4GRB Afterglow lightcurve flux (M_BH_=9.8M_{sun}_, Viewing angle=0deg)mJyphot.flux;meta.modelleddoubleFluxe5GRB Afterglow lightcurve flux (M_BH_=11.2M_{sun}_, Viewing angle=0deg)mJyphot.flux;meta.modelleddoubleFluxe6GRB Afterglow lightcurve flux (M_BH_=5.3M_{sun}_, Viewing angle=30deg)mJyphot.flux;meta.modelleddoubleFluxe7GRB Afterglow lightcurve flux (M_BH_=6.8M_{sun}_, Viewing angle=30deg)mJyphot.flux;meta.modelleddoubleFluxe8GRB Afterglow lightcurve flux (M_BH_=8.3M_{sun}_, Viewing angle=30deg)mJyphot.flux;meta.modelleddoubleFluxe9GRB Afterglow lightcurve flux (M_BH_=9.8M_{sun}_, Viewing angle=30deg)mJyphot.flux;meta.modelleddoubleFluxe10GRB Afterglow lightcurve flux (M_BH_=11.2M_{sun}_, Viewing angle=30deg)mJyphot.flux;meta.modelleddoubleFluxe11GRB Afterglow lightcurve flux (M_BH_=5.3M_{sun}_, Viewing angle=60deg)mJyphot.flux;meta.modelleddoubleFluxe12GRB Afterglow lightcurve flux (M_BH_=6.8M_{sun}_, Viewing angle=60deg)mJyphot.flux;meta.modelleddoubleFluxe13GRB Afterglow lightcurve flux (M_BH_=8.3M_{sun}_, Viewing angle=60deg)mJyphot.flux;meta.modelleddoubleFluxe14GRB Afterglow lightcurve flux (M_BH_=9.8M_{sun}_, Viewing angle=60deg)mJyphot.flux;meta.modelleddoubleFluxe15GRB Afterglow lightcurve fluxmJyphot.flux;meta.modelleddoubleJ/A+A/625/A152/panelfPanel f: GRB Afterglow lightcurves at 1keV varying the black hole spin and viewing anglerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTime[1/10000] Timedtime.agedoubleFluxf1[0] GRB Afterglow lightcurve flux (X_BH_=0.4, Viewing angle=0deg) (G1)mJyphot.flux;meta.modelledintFluxf2GRB Afterglow lightcurve flux (X_BH_=0.5, Viewing angle=0deg) (G1)mJyphot.flux;meta.modelleddoubleFluxf3GRB Afterglow lightcurve flux (X_BH_=0.6, Viewing angle=0deg) (G1)mJyphot.flux;meta.modelleddoubleFluxf4GRB Afterglow lightcurve flux (X_BH_=0.7, Viewing angle=0deg) (G1)mJyphot.flux;meta.modelleddoubleFluxf5GRB Afterglow lightcurve flux (X_BH_=0.9, Viewing angle=0deg) (G1)mJyphot.flux;meta.modelleddoubleFluxf6[0] GRB Afterglow lightcurve flux (X_BH_=0.4, Viewing angle=30deg) (G1)mJyphot.flux;meta.modelledintFluxf7GRB Afterglow lightcurve flux (X_BH_=0.5, Viewing angle=30deg) (G1)mJyphot.flux;meta.modelleddoubleFluxf8GRB Afterglow lightcurve flux (X_BH_=0.6, Viewing angle=30deg) (G1)mJyphot.flux;meta.modelleddoubleFluxf9GRB Afterglow lightcurve flux (X_BH_=0.7, Viewing angle=30deg) (G1)mJyphot.flux;meta.modelleddoubleFluxf10GRB Afterglow lightcurve flux (X_BH_=0.9, Viewing angle=30deg) (G1)mJyphot.flux;meta.modelleddoubleFluxf11[0] GRB Afterglow lightcurve flux (X_BH_=0.4, Viewing angle=60deg) (G1)mJyphot.flux;meta.modelledintFluxf12GRB Afterglow lightcurve flux (X_BH_=0.5, Viewing angle=60deg) (G1)mJyphot.flux;meta.modelleddoubleFluxf13GRB Afterglow lightcurve flux (X_BH_=0.6, Viewing angle=60deg) (G1)mJyphot.flux;meta.modelleddoubleFluxf14GRB Afterglow lightcurve flux (X_BH_=0.7, Viewing angle=60deg) (G1)mJyphot.flux;meta.modelleddoubleFluxf15GRB Afterglow lightcurve flux (X_BH_=0.9, Viewing angle=60deg) (G1)mJyphot.flux;meta.modelleddoubleJ/A+A/625/A152/panelgPanel g: KNR and GRB Afterglow lightcurves at 1.4GHz varying the black hole mass and viewing anglerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTime[1/10000] Timedtime.agedoubleFluxg1GRB Afterglow lightcurve flux (M_BH_=5.3M_{sun}_, Viewing angle=0deg)mJyphot.flux;meta.modelleddoubleFluxg2GRB Afterglow lightcurve flux (M_BH_=6.8M_{sun}_, Viewing angle=0deg)mJyphot.flux;meta.modelleddoubleFluxg3GRB Afterglow lightcurve flux (M_BH_=8.3M_{sun}_, Viewing angle=0deg)mJyphot.flux;meta.modelleddoubleFluxg4GRB Afterglow lightcurve flux (M_BH_=9.8M_{sun}_, Viewing angle=0deg)mJyphot.flux;meta.modelleddoubleFluxg5GRB Afterglow lightcurve flux (M_BH_=11.2M_{sun}_, Viewing angle=0deg)mJyphot.flux;meta.modelleddoubleFluxg6GRB Afterglow lightcurve flux (M_BH_=5.3M_{sun}_, Viewing angle=30deg)mJyphot.flux;meta.modelleddoubleFluxg7GRB Afterglow lightcurve flux (M_BH_=6.8M_{sun}_, Viewing angle=30deg)mJyphot.flux;meta.modelleddoubleFluxg8GRB Afterglow lightcurve flux (M_BH_=8.3M_{sun}_, Viewing angle=30deg)mJyphot.flux;meta.modelleddoubleFluxg9GRB Afterglow lightcurve flux (M_BH_=9.8M_{sun}_, Viewing angle=30deg)mJyphot.flux;meta.modelleddoubleFluxg10GRB Afterglow lightcurve flux (M_BH_=11.2M_{sun}_, Viewing angle=30deg)mJyphot.flux;meta.modelleddoubleFluxg11GRB Afterglow lightcurve flux (M_BH_=5.3M_{sun}_, Viewing angle=60deg)mJyphot.flux;meta.modelleddoubleFluxg12GRB Afterglow lightcurve flux (M_BH_=6.8M_{sun}_, Viewing angle=60deg)mJyphot.flux;meta.modelleddoubleFluxg13GRB Afterglow lightcurve flux (M_BH_=8.3M_{sun}_, Viewing angle=60deg)mJyphot.flux;meta.modelleddoubleFluxg14GRB Afterglow lightcurve flux (M_BH_=9.8M_{sun}_, Viewing angle=60deg)mJyphot.flux;meta.modelleddoubleFluxg15GRB Afterglow lightcurve flux (M_BH_=11.2M_{sun}_, Viewing angle=60deg)mJyphot.flux;meta.modelleddoubleFluxg16Kilonova radio remnant (KNR) lightcurve flux (M_BH_=5.3M_{sun}_)mJyphot.flux;meta.modelleddoubleFluxg17Kilonova radio remnant (KNR) lightcurve flux (M_BH_=6.8M_{sun}_)mJyphot.flux;meta.modelleddoubleFluxg18Kilonova radio remnant (KNR) lightcurve flux (M_BH_=8.3M_{sun}_)mJyphot.flux;meta.modelleddoubleFluxg19Kilonova radio remnant (KNR) lightcurve flux (M_BH_=9.8M_{sun}_)mJyphot.flux;meta.modelleddoubleFluxg20Kilonova radio remnant (KNR) lightcurve flux (M_BH_=11.2M_{sun}_)mJyphot.flux;meta.modelleddoubleJ/A+A/625/A152/panelhPanel h: KNR and GRB Afterglow lightcurves at 1.4GHz varying the black hole spin and viewing angleFluxh17Kilonova radio remnant (KNR) lightcurve flux (X_BH_=0.5) (G1)mJyphot.flux;meta.modelleddoublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTime[1/10000] Timedtime.agedoubleFluxh1[0] GRB Afterglow lightcurve flux (X_BH_=0.4, Viewing angle=0deg) (G1)mJyphot.flux;meta.modelledintFluxh2GRB Afterglow lightcurve flux (X_BH_=0.5, Viewing angle=0deg) (G1)mJyphot.flux;meta.modelleddoubleFluxh3GRB Afterglow lightcurve flux (X_BH_=0.6, Viewing angle=0deg) (G1)mJyphot.flux;meta.modelleddoubleFluxh4GRB Afterglow lightcurve flux (X_BH_=0.7, Viewing angle=0deg) (G1)mJyphot.flux;meta.modelleddoubleFluxh5GRB Afterglow lightcurve flux (X_BH_=0.9, Viewing angle=0deg) (G1)mJyphot.flux;meta.modelleddoubleFluxh6[0] GRB Afterglow lightcurve flux (X_BH_=0.4, Viewing angle=30deg) (G1)mJyphot.flux;meta.modelledintFluxh7GRB Afterglow lightcurve flux (X_BH_=0.5, Viewing angle=30deg) (G1)mJyphot.flux;meta.modelleddoubleFluxh8GRB Afterglow lightcurve flux (X_BH_=0.6, Viewing angle=30deg) (G1)mJyphot.flux;meta.modelleddoubleFluxh9GRB Afterglow lightcurve flux (X_BH_=0.7, Viewing angle=30deg) (G1)mJyphot.flux;meta.modelleddoubleFluxh10GRB Afterglow lightcurve flux (X_BH_=0.9, Viewing angle=30deg) (G1)mJyphot.flux;meta.modelleddoubleFluxh11[0] GRB Afterglow lightcurve flux (X_BH_=0.4, Viewing angle=60deg) (G1)mJyphot.flux;meta.modelledintFluxh12GRB Afterglow lightcurve flux (X_BH_=0.5, Viewing angle=60deg) (G1)mJyphot.flux;meta.modelleddoubleFluxh13GRB Afterglow lightcurve flux (X_BH_=0.6, Viewing angle=60deg) (G1)mJyphot.flux;meta.modelleddoubleFluxh14GRB Afterglow lightcurve flux (X_BH_=0.7, Viewing angle=60deg) (G1)mJyphot.flux;meta.modelleddoubleFluxh15GRB Afterglow lightcurve flux (X_BH_=0.9, Viewing angle=60deg) (G1)mJyphot.flux;meta.modelleddoubleFluxh16Kilonova radio remnant (KNR) lightcurve flux (X_BH_=0.4) (G1)mJyphot.flux;meta.modelleddoubleFluxh18Kilonova radio remnant (KNR) lightcurve flux (X_BH_=0.6) (G1)mJyphot.flux;meta.modelleddoubleFluxh19Kilonova radio remnant (KNR) lightcurve flux (X_BH_=0.7) (G1)mJyphot.flux;meta.modelleddoubleFluxh20Kilonova radio remnant (KNR) lightcurve flux (X_BH_=0.9) (G1)mJyphot.flux;meta.modelleddouble