191 research outputs found
GW190412: Observation of a Binary-Black-Hole Coalescence with Asymmetric Masses
We report the observation of gravitational waves from a binary-black-hole coalescence during the first two weeks of LIGOâs and Virgoâs third observing run. The signal was recorded on April 12, 2019 at 05â¶30â¶44 UTC with a network signal-to-noise ratio of 19. The binary is different from observations during the first two observing runs most notably due to its asymmetric masses: a âŒ30âM_â black hole merged with a âŒ8âM_â black hole companion. The more massive black hole rotated with a dimensionless spin magnitude between 0.22 and 0.60 (90% probability). Asymmetric systems are predicted to emit gravitational waves with stronger contributions from higher multipoles, and indeed we find strong evidence for gravitational radiation beyond the leading quadrupolar order in the observed signal. A suite of tests performed on GW190412 indicates consistency with Einsteinâs general theory of relativity. While the mass ratio of this system differs from all previous detections, we show that it is consistent with the population model of stellar binary black holes inferred from the first two observing runs
Properties and Astrophysical Implications of the 150 M_â Binary Black Hole Merger GW190521
The gravitational-wave signal GW190521 is consistent with a binary black hole (BBH) merger source at redshift 0.8 with unusually high component masses, 85âșÂČÂčâââ M_â and 66âșÂčâ·âââ M_â, compared to previously reported events, and shows mild evidence for spin-induced orbital precession. The primary falls in the mass gap predicted by (pulsational) pair-instability supernova theory, in the approximate range 65â120 M_â. The probability that at least one of the black holes in GW190521 is in that range is 99.0%. The final mass of the merger 142âșÂČâžâââ M_â) classifies it as an intermediate-mass black hole. Under the assumption of a quasi-circular BBH coalescence, we detail the physical properties of GW190521's source binary and its post-merger remnant, including component masses and spin vectors. Three different waveform models, as well as direct comparison to numerical solutions of general relativity, yield consistent estimates of these properties. Tests of strong-field general relativity targeting the merger-ringdown stages of the coalescence indicate consistency of the observed signal with theoretical predictions. We estimate the merger rate of similar systems to be 0.13_(-0.11)^(+0.30) Gpcâ»Âł yrâ»Âč. We discuss the astrophysical implications of GW190521 for stellar collapse and for the possible formation of black holes in the pair-instability mass gap through various channels: via (multiple) stellar coalescences, or via hierarchical mergers of lower-mass black holes in star clusters or in active galactic nuclei. We find it to be unlikely that GW190521 is a strongly lensed signal of a lower-mass black hole binary merger. We also discuss more exotic possible sources for GW190521, including a highly eccentric black hole binary, or a primordial black hole binary
GW190521 : a binary black hole merger with a total mass of 150 Mâ
On May 21, 2019 at 03:02:29 UTC Advanced LIGO and Advanced Virgo observed a short duration gravitational-wave signal, GW190521, with a three-detector network signal-to-noise ratio of 14.7, and an estimated false-alarm rate of 1 in 4900 yr using a search sensitive to generic transients. If GW190521 is from a quasicircular binary inspiral, then the detected signal is consistent with the merger of two black holes with masses of 85+21â14ââMâ and 66+17â18ââMâ (90% credible intervals). We infer that the primary black hole mass lies within the gap produced by (pulsational) pair-instability supernova processes, with only a 0.32% probability of being below 65ââMâ. We calculate the mass of the remnant to be 142+28â16ââMâ, which can be considered an intermediate mass black hole (IMBH). The luminosity distance of the source is 5.3+2.4â2.6ââGpc, corresponding to a redshift of 0.82+0.28â0.34. The inferred rate of mergers similar to GW190521 is 0.13+0.30â0.11ââGpcâ3âyrâ1
GW190425 : observation of a compact binary coalescence with total mass ~ 3.4 M o
On 2019 April 25, the LIGO Livingston detector observed a compact binary coalescence with signal-to-noise ratio 12.9. The Virgo detector was also taking data that did not contribute to detection due to a low signal-to-noise ratio, but were used for subsequent parameter estimation. The 90% credible intervals for the component masses range from to if we restrict the dimensionless component spin magnitudes to be smaller than 0.05). These mass parameters are consistent with the individual binary components being neutron stars. However, both the source-frame chirp mass and the total mass of this system are significantly larger than those of any other known binary neutron star (BNS) system. The possibility that one or both binary components of the system are black holes cannot be ruled out from gravitational-wave data. We discuss possible origins of the system based on its inconsistency with the known Galactic BNS population. Under the assumption that the signal was produced by a BNS coalescence, the local rate of neutron star mergers is updated to 250-2810
Search for Gravitational-wave Signals Associated with Gamma-Ray Bursts during the Second Observing Run of Advanced LIGO and Advanced Virgo
We present the results of targeted searches for gravitational-wave transients associated with gamma-ray bursts during the second observing run of Advanced LIGO and Advanced Virgo, which took place from 2016 November to 2017 August. We have analyzed 98 gamma-ray bursts using an unmodeled search method that searches for generic transient gravitational waves and 42 with a modeled search method that targets compact-binary mergers as progenitors of short gamma-ray bursts. Both methods clearly detect the previously reported binary merger signal GW170817, with p-values of <9.38 Ă 10â6 (modeled) and 3.1 Ă 10â4 (unmodeled). We do not find any significant evidence for gravitational-wave signals associated with the other gamma-ray bursts analyzed, and therefore we report lower bounds on the distance to each of these, assuming various source types and signal morphologies. Using our final modeled search results, short gamma-ray burst observations, and assuming binary neutron star progenitors, we place bounds on the rate of short gamma-ray bursts as a function of redshift for z †1. We estimate 0.07â1.80 joint detections with Fermi-GBM per year for the 2019â20 LIGO-Virgo observing run and 0.15â3.90 per year when current gravitational-wave detectors are operating at their design sensitivities
Search of the early O3 LIGO data for continuous gravitational waves from the Cassiopeia A and Vela Jr. supernova remnants
partially_open1412sĂŹWe present directed searches for continuous gravitational waves from the neutron stars in the Cassiopeia A (Cas A) and Vela Jr. supernova remnants. We carry out the searches in the LIGO detector data from the first six months of the third Advanced LIGO and Virgo observing run using the weave semicoherent method, which sums matched-filter detection-statistic values over many time segments spanning the observation period. No gravitational wave signal is detected in the search band of 20â976 Hz for assumed source ages greater than 300 years for Cas A and greater than 700 years for Vela Jr. Estimates from simulated continuous wave signals indicate we achieve the most sensitive results to date across the explored parameter space volume, probing to strain magnitudes as low as
âŒ6.3Ă10^â26 for Cas A and âŒ5.6Ă10^â26 for Vela Jr. at frequencies near 166 Hz at 95% efficiency.openAbbott, R.; Abbott, T.âD.; Acernese, F.; Ackley, K.; Adams, C.; Adhikari, N.; Adhikari, R.âX.; Adya, V.âB.; Affeldt, C.; Agarwal, D.; Agathos, M.; Agatsuma, K.; Aggarwal, N.; Aguiar, O.âD.; Aiello, L.; Ain, A.; Ajith, P.; Albanesi, S.; Allocca, A.; Altin, P.âA.; Amato, A.; Anand, C.; Anand, S.; Ananyeva, A.; Anderson, S.âB.; Anderson, W.âG.; Andrade, T.; Andres, N.; AndriÄ, T.; Angelova, S.âV.; Ansoldi, S.; Antelis, J.âM.; Antier, S.; Appert, S.; Arai, K.; Araya, M.âC.; Areeda, J.âS.; ArĂšne, M.; Arnaud, N.; Aronson, S.âM.; Arun, K.âG.; Asali, Y.; Ashton, G.; Assiduo, M.; Aston, S.âM.; Astone, P.; Aubin, F.; Austin, C.; Babak, S.; Badaracco, F.; Bader, M.âK.âM.; Badger, C.; Bae, S.; Baer, A.âM.; Bagnasco, S.; Bai, Y.; Baird, J.; Ball, M.; Ballardin, G.; Ballmer, S.âW.; Balsamo, A.; Baltus, G.; Banagiri, S.; Bankar, D.; Barayoga, J.âC.; Barbieri, C.; Barish, B.âC.; Barker, D.; Barneo, P.; Barone, F.; Barr, B.; Barsotti, L.; Barsuglia, M.; Barta, D.; Bartlett, J.; Barton, M.âA.; Bartos, I.; Bassiri, R.; Basti, A.; Bawaj, M.; Bayley, J.âC.; Baylor, A.âC.; Bazzan, M.; BĂ©csy, B.; Bedakihale, V.âM.; Bejger, M.; Belahcene, I.; Benedetto, V.; Beniwal, D.; Bennett, T.âF.; Bentley, J.âD.; BenYaala, M.; Bergamin, F.; Berger, B.âK.; Bernuzzi, S.; Bersanetti, D.; Bertolini, A.; Betzwieser, J.; Beveridge, D.; Bhandare, R.; Bhardwaj, U.; Bhattacharjee, D.; Bhaumik, S.; Bilenko, I.âA.; Billingsley, G.; Bini, S.; Birney, R.; Birnholtz, O.; Biscans, S.; Bischi, M.; Biscoveanu, S.; Bisht, A.; Biswas, B.; Bitossi, M.; Bizouard, M.-A.; Blackburn, J.âK.; Blair, C.âD.; Blair, D.âG.; Blair, R.âM.; Bobba, F.; Bode, N.; Boer, M.; Bogaert, G.; Boldrini, M.; Bonavena, L.âD.; Bondu, F.; Bonilla, E.; Bonnand, R.; Booker, P.; Boom, B.âA.; Bork, R.; Boschi, V.; Bose, N.; Bose, S.; Bossilkov, V.; Boudart, V.; Bouffanais, Y.; Bozzi, A.; Bradaschia, C.; Brady, P.âR.; Bramley, A.; Branch, A.; Branchesi, M.; Brau, J.âE.; Breschi, M.; Briant, T.; Briggs, J.âH.; Brillet, A.; Brinkmann, M.; Brockill, P.; Brooks, A.âF.; Brooks, J.; Brown, D.âD.; Brunett, S.; Bruno, G.; Bruntz, R.; Bryant, J.; Bulik, T.; Bulten, H.âJ.; Buonanno, A.; Buscicchio, R.; Buskulic, D.; Buy, C.; Byer, R.âL.; Cadonati, L.; Cagnoli, G.; Cahillane, C.; Bustillo, J. 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Chalathadka; Champion, E.; Chan, C.-H.; Chan, C.; Chan, C.âL.; Chan, K.; Chandra, K.; Chanial, P.; Chao, S.; Charlton, P.; Chase, E.âA.; Chassande-Mottin, E.; Chatterjee, C.; Chatterjee, Debarati; Chatterjee, Deep; Chaturvedi, M.; Chaty, S.; Chen, H.âY.; Chen, J.; Chen, X.; Chen, Y.; Chen, Z.; Cheng, H.; Cheong, C.âK.; Cheung, H.âY.; Chia, H.âY.; Chiadini, F.; Chiarini, G.; Chierici, R.; Chincarini, A.; Chiofalo, M.âL.; Chiummo, A.; Cho, G.; Cho, H.âS.; Choudhary, R.âK.; Choudhary, S.; Christensen, N.; Chu, Q.; Chua, S.; Chung, K.âW.; Ciani, G.; Ciecielag, P.; CieĆlar, M.; Cifaldi, M.; Ciobanu, A.âA.; Ciolfi, R.; Cipriano, F.; Cirone, A.; Clara, F.; Clark, E.âN.; Clark, J.âA.; Clarke, L.; Clearwater, P.; Clesse, S.; Cleva, F.; Coccia, E.; Codazzo, E.; Cohadon, P.-F.; Cohen, D.âE.; Cohen, L.; Colleoni, M.; Collette, C.âG.; Colombo, A.; Colpi, M.; Compton, C.âM.; Constancio, M.; Conti, L.; Cooper, S.âJ.; Corban, P.; Corbitt, T.âR.; Cordero-CarriĂłn, I.; Corezzi, S.; Corley, K.âR.; Cornish, N.; Corre, D.; Corsi, A.; Cortese, S.; Costa, C.âA.; Cotesta, R.; Coughlin, M.âW.; Coulon, J.-P.; Countryman, S.âT.; Cousins, B.; Couvares, P.; Coward, D.âM.; Cowart, M.âJ.; Coyne, D.âC.; Coyne, R.; Creighton, J.âD.âE.; Creighton, T.âD.; Criswell, A.âW.; Croquette, M.; Crowder, S.âG.; Cudell, J.âR.; Cullen, T.âJ.; Cumming, A.; Cummings, R.; Cunningham, L.; Cuoco, E.; CuryĆo, M.; Dabadie, P.; Canton, T. Dal; DallâOsso, S.; DĂĄlya, G.; Dana, A.; DaneshgaranBajastani, L.âM.; DâAngelo, B.; Danilishin, S.; DâAntonio, S.; Danzmann, K.; Darsow-Fromm, C.; Dasgupta, A.; Datrier, L.âE.âH.; Datta, S.; Dattilo, V.; Dave, I.; Davier, M.; Davies, G.âS.; Davis, D.; Davis, M.âC.; Daw, E.âJ.; Dean, R.; DeBra, D.; Deenadayalan, M.; Degallaix, J.; De Laurentis, M.; DelĂ©glise, S.; Del Favero, V.; De Lillo, F.; De Lillo, N.; Del Pozzo, W.; DeMarchi, L.âM.; De Matteis, F.; DâEmilio, V.; Demos, N.; Dent, T.; Depasse, A.; De Pietri, R.; De Rosa, R.; De Rossi, C.; DeSalvo, R.; De Simone, R.; Dhurandhar, S.; DĂaz, M.âC.; Diaz-Ortiz, M.; Didio, N.âA.; Dietrich, T.; Di Fiore, L.; Di Fronzo, C.; Di Giorgio, C.; Di Giovanni, F.; Di Giovanni, M.; Di Girolamo, T.; Di Lieto, A.; Ding, B.; Di Pace, S.; Di Palma, I.; Di Renzo, F.; Divakarla, A.âK.; Dmitriev, A.; Doctor, Z.; DâOnofrio, L.; Donovan, F.; Dooley, K.âL.; Doravari, S.; Dorrington, I.; Drago, M.; Driggers, J.âC.; Drori, Y.; Ducoin, J.-G.; Dupej, P.; Durante, O.; DâUrso, D.; Duverne, P.-A.; Dwyer, S.âE.; Eassa, C.; Easter, P.âJ.; Ebersold, M.; Eckhardt, T.; Eddolls, G.; Edelman, B.; Edo, T.âB.; Edy, O.; Effler, A.; Eichholz, J.; Eikenberry, S.âS.; Eisenmann, M.; Eisenstein, R.âA.; Ejlli, A.; Engelby, E.; Errico, L.; Essick, R.âC.; EstellĂ©s, H.; Estevez, D.; Etienne, Z.; Etzel, T.; Evans, M.; Evans, T.âM.; Ewing, B.âE.; Fafone, V.; Fair, H.; Fairhurst, S.; Farah, A.âM.; Farinon, S.; Farr, B.; Farr, W.âM.; Farrow, N.âW.; Fauchon-Jones, E.âJ.; Favaro, G.; Favata, M.; Fays, M.; Fazio, M.; Feicht, J.; Fejer, M.âM.; Fenyvesi, E.; Ferguson, D.âL.; Fernandez-Galiana, A.; Ferrante, I.; Ferreira, T.âA.; Fidecaro, F.; Figura, P.; Fiori, I.; Fishbach, M.; Fisher, R.âP.; Fittipaldi, R.; Fiumara, V.; Flaminio, R.; Floden, E.; Fong, H.; Font, J.âA.; Fornal, B.; Forsyth, P.âW.âF.; Franke, A.; Frasca, S.; Frasconi, F.; Frederick, C.; Freed, J.âP.; Frei, Z.; Freise, A.; Frey, R.; Fritschel, P.; Frolov, V.âV.; FronzĂ©, G.âG.; Fulda, P.; Fyffe, M.; Gabbard, H.âA.; Gadre, B.âU.; Gair, J.âR.; Gais, J.; Galaudage, S.; Gamba, R.; Ganapathy, D.; Ganguly, A.; Gaonkar, S.âG.; Garaventa, B.; GarcĂa-NĂșñez, C.; GarcĂa-QuirĂłs, C.; Garufi, F.; Gateley, B.; Gaudio, S.; Gayathri, V.; Gemme, G.; Gennai, A.; George, J.; Gerberding, O.; Gergely, L.; Gewecke, P.; Ghonge, S.; Ghosh, Abhirup; Ghosh, Archisman; Ghosh, Shaon; Ghosh, Shrobana; Giacomazzo, B.; Giacoppo, L.; Giaime, J.âA.; Giardina, K.âD.; Gibson, D.âR.; Gier, C.; Giesler, M.; Giri, P.; Gissi, F.; Glanzer, J.; Gleckl, A.âE.; Godwin, P.; Goetz, E.; Goetz, R.; Gohlke, N.; Goncharov, B.; GonzĂĄlez, G.; Gopakumar, A.; Gosselin, M.; Gouaty, R.; Gould, D.âW.; Grace, B.; Grado, A.; Granata, M.; Granata, V.; Grant, A.; Gras, S.; Grassia, P.; Gray, C.; Gray, R.; Greco, G.; Green, A.âC.; Green, R.; Gretarsson, A.âM.; Gretarsson, E.âM.; Griffith, D.; Griffiths, W.; Griggs, H.âL.; Grignani, G.; Grimaldi, A.; Grimm, S.âJ.; Grote, H.; Grunewald, S.; Gruning, P.; Guerra, D.; Guidi, Gianluca; Guimaraes, A.âR.; GuixĂ©, G.; Gulati, H.âK.; Guo, H.-K.; Guo, Y.; Gupta, Anchal; Gupta, Anuradha; Gupta, P.; Gustafson, E.âK.; Gustafson, R.; Guzman, F.; Haegel, L.; Halim, O.; Hall, E.âD.; Hamilton, E.âZ.; Hammond, G.; Haney, M.; Hanks, J.; Hanna, C.; Hannam, M.âD.; Hannuksela, O.; Hansen, H.; Hansen, T.âJ.; Hanson, J.; Harder, T.; Hardwick, T.; Haris, K.; Harms, J.; Harry, G.âM.; Harry, I.âW.; Hartwig, D.; Haskell, B.; Hasskew, R.âK.; Haster, C.-J.; Haughian, K.; Hayes, F.âJ.; Healy, J.; Heidmann, A.; Heidt, A.; Heintze, M.âC.; Heinze, J.; Heinzel, J.; Heitmann, H.; Hellman, F.; Hello, P.; Helmling-Cornell, A.âF.; Hemming, G.; Hendry, M.; Heng, I.âS.; Hennes, E.; Hennig, J.; Hennig, M.âH.; Hernandez, A.âG.; Vivanco, F. Hernandez; Heurs, M.; Hild, S.; Hill, P.; Hines, A.âS.; Hochheim, S.; Hofman, D.; Hohmann, J.âN.; Holcomb, D.âG.; Holland, N.âA.; Hollows, I.âJ.; Holmes, Z.âJ.; Holt, K.; Holz, D.âE.; Hopkins, P.; Hough, J.; Hourihane, S.; Howell, E.âJ.; Hoy, C.âG.; Hoyland, D.; Hreibi, A.; Hsu, Y.; Huang, Y.; HĂŒbner, M.âT.; Huddart, A.âD.; Hughey, B.; Hui, V.; Husa, S.; Huttner, S.âH.; Huxford, R.; Huynh-Dinh, T.; Idzkowski, B.; Iess, A.; Ingram, C.; Isi, M.; Isleif, K.; Iyer, B.âR.; JaberianHamedan, V.; Jacqmin, T.; Jadhav, S.âJ.; Jadhav, S.âP.; James, A.âL.; Jan, A.âZ.; Jani, K.; Janquart, J.; Janssens, K.; Janthalur, N.âN.; Jaranowski, P.; Jariwala, D.; Jaume, R.; Jenkins, A.âC.; Jenner, K.; Jeunon, M.; Jia, W.; Johns, G.âR.; Jones, A.âW.; Jones, D.âI.; Jones, J.âD.; Jones, P.; Jones, R.; Jonker, R.âJ.âG.; Ju, L.; Junker, J.; Juste, V.; Kalaghatgi, C.âV.; Kalogera, V.; Kamai, B.; Kandhasamy, S.; Kang, G.; Kanner, J.âB.; Kao, Y.; Kapadia, S.âJ.; Kapasi, D.âP.; Karat, S.; Karathanasis, C.; Karki, S.; Kashyap, R.; Kasprzack, M.; Kastaun, W.; Katsanevas, S.; Katsavounidis, E.; Katzman, W.; Kaur, T.; Kawabe, K.; KĂ©fĂ©lian, F.; Keitel, D.; Key, J.âS.; Khadka, S.; Khalili, F.âY.; Khan, S.; Khazanov, E.âA.; Khetan, N.; Khursheed, M.; Kijbunchoo, N.; Kim, C.; Kim, J.âC.; Kim, K.; Kim, W.âS.; Kim, Y.-M.; Kimball, C.; Kinley-Hanlon, M.; Kirchhoff, R.; Kissel, J.âS.; Kleybolte, L.; Klimenko, S.; Knee, A.âM.; Knowles, T.âD.; Knyazev, E.; Koch, P.; Koekoek, G.; Koley, S.; Kolitsidou, P.; Kolstein, M.; Komori, K.; Kondrashov, V.; Kontos, A.; Koper, N.; Korobko, M.; Kovalam, M.; Kozak, D.âB.; Kringel, V.; Krishnendu, N.âV.; KrĂłlak, A.; Kuehn, G.; Kuei, F.; Kuijer, P.; Kumar, A.; Kumar, P.; Kumar, Rahul; Kumar, Rakesh; Kuns, K.; Kuwahara, S.; Lagabbe, P.; Laghi, D.; Lalande, E.; Lam, T.âL.; Lamberts, A.; Landry, M.; Lane, B.âB.; Lang, R.âN.; Lange, J.; Lantz, B.; La Rosa, I.; Lartaux-Vollard, A.; Lasky, P.âD.; Laxen, M.; Lazzarini, A.; Lazzaro, C.; Leaci, P.; Leavey, S.; Lecoeuche, Y.âK.; Lee, H.âM.; Lee, H.âW.; Lee, J.; Lee, K.; Lehmann, J.; LemaĂźtre, A.; Leroy, N.; Letendre, N.; Levesque, C.; Levin, Y.; Leviton, J.âN.; Leyde, K.; Li, A.âK.âY.; Li, B.; Li, J.; Li, T.âG.âF.; Li, X.; Linde, F.; Linker, S.âD.; Linley, J.âN.; Littenberg, T.âB.; Liu, J.; Liu, K.; Liu, X.; Llamas, F.; Llorens-Monteagudo, M.; Lo, R.âK.âL.; Lockwood, A.; London, L.âT.; Longo, A.; Lopez, D.; Portilla, M. 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Model-based cross-correlation search for gravitational waves from the low-mass X-ray binary Scorpius X-1 in LIGO O3 data
Open data from the third observing run of LIGO, Virgo, KAGRA and GEO
The global network of gravitational-wave observatories now includes five
detectors, namely LIGO Hanford, LIGO Livingston, Virgo, KAGRA, and GEO 600.
These detectors collected data during their third observing run, O3, composed
of three phases: O3a starting in April of 2019 and lasting six months, O3b
starting in November of 2019 and lasting five months, and O3GK starting in
April of 2020 and lasting 2 weeks. In this paper we describe these data and
various other science products that can be freely accessed through the
Gravitational Wave Open Science Center at https://gwosc.org. The main dataset,
consisting of the gravitational-wave strain time series that contains the
astrophysical signals, is released together with supporting data useful for
their analysis and documentation, tutorials, as well as analysis software
packages.Comment: 27 pages, 3 figure
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