213 research outputs found
Cerebral Palsy:Early Markers of Clinical Phenotype and Functional Outcome
The Prechtl General Movement Assessment (GMA) has become a cornerstone assessment in early identification of cerebral palsy (CP), particularly during the fidgety movement period at 3-5 months of age. Additionally, assessment of motor repertoire, such as antigravity movements and postural patterns, which form the Motor Optimality Score (MOS), may provide insight into an infant's later motor function. This study aimed to identify early specific markers for ambulation, gross motor function (using the Gross Motor Function Classification System, GMFCS), topography (unilateral, bilateral), and type (spastic, dyskinetic, ataxic, and hypotonic) of CP in a large worldwide cohort of 468 infants. We found that 95% of children with CP did not have fidgety movements, with 100% having non-optimal MOS. GMFCS level was strongly correlated to MOS. An MOS > 14 was most likely associated with GMFCS outcomes I or II, whereas GMFCS outcomes IV or V were hardly ever associated with an MOS > 8. A number of different movement patterns were associated with more severe functional impairment (GMFCS III-V), including atypical arching and persistent cramped-synchronized movements. Asymmetrical segmental movements were strongly associated with unilateral CP. Circular arm movements were associated with dyskinetic CP. This study demonstrated that use of the MOS contributes to understanding later CP prognosis, including early markers for type and severity
Replication Protein A (RPA) Hampers the Processive Action of APOBEC3G Cytosine Deaminase on Single-Stranded DNA
deamination assays and expression of A3G in yeast, we show that replication protein A (RPA), the eukaryotic single-stranded DNA (ssDNA) binding protein, severely inhibits the deamination activity and processivity of A3G. on long ssDNA regions. This resembles the âhit and runâ single base substitution events observed in yeast., we propose that RPA plays a role in the protection of the human genome cell from A3G and other deaminases when they are inadvertently diverged from their natural targets. We propose a model where RPA serves as one of the guardians of the genome that protects ssDNA from the destructive processive activity of deaminases by non-specific steric hindrance
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 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. CalderĂłn; Callaghan, J.âD.; Callister, T.âA.; Calloni, E.; Cameron, J.; Camp, J.âB.; Canepa, M.; Canevarolo, S.; Cannavacciuolo, M.; Cannon, K.âC.; Cao, H.; Capote, E.; Carapella, G.; Carbognani, F.; Carlin, J.âB.; Carney, M.âF.; Carpinelli, M.; Carrillo, G.; Carullo, G.; Carver, T.âL.; Diaz, J. Casanueva; Casentini, C.; Castaldi, G.; Caudill, S.; CavagliĂ , M.; Cavalier, F.; Cavalieri, R.; Ceasar, M.; Cella, G.; CerdĂĄ-DurĂĄn, P.; Cesarini, E.; Chaibi, W.; Chakravarti, K.; Subrahmanya, S. 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. Lopez; Lorenzini, M.; Loriette, V.; Lormand, M.; Losurdo, G.; Lott, T.âP.; Lough, J.âD.; Lousto, C.âO.; Lovelace, G.; Lucaccioni, J.âF.; LĂŒck, H.; Lumaca, D.; Lundgren, A.âP.; Lynam, J.âE.; Macas, R.; MacInnis, M.; Macleod, D.âM.; MacMillan, I.âA.âO.; Macquet, A.; Hernandez, I. Magaña; MagazzĂč, C.; Magee, R.âM.; Maggiore, R.; Magnozzi, M.; Mahesh, S.; Majorana, E.; Makarem, C.; Maksimovic, I.; Maliakal, S.; Malik, A.; Man, N.; Mandic, V.; Mangano, V.; Mango, J.âL.; Mansell, G.âL.; Manske, M.; Mantovani, M.; Mapelli, M.; Marchesoni, F.; Marion, F.; Mark, Z.; MĂĄrka, S.; MĂĄrka, Z.; Markakis, C.; Markosyan, A.âS.; Markowitz, A.; Maros, E.; Marquina, A.; Marsat, S.; Martelli, F.; Martin, I.âW.; Martin, R.âM.; Martinez, M.; Martinez, V.âA.; Martinez, V.; Martinovic, K.; Martynov, D.âV.; Marx, E.âJ.; Masalehdan, H.; Mason, K.; Massera, E.; Masserot, A.; Massinger, T.âJ.; Masso-Reid, M.; Mastrogiovanni, S.; Matas, A.; Mateu-Lucena, M.; Matichard, F.; Matiushechkina, M.; Mavalvala, N.; McCann, J.âJ.; McCarthy, R.; McClelland, D.âE.; McClincy, P.âK.; McCormick, S.; McCuller, L.; McGhee, G.âI.; McGuire, S.âC.; McIsaac, C.; McIver, J.; McRae, T.; McWilliams, S.âT.; Meacher, D.; Mehmet, M.; Mehta, A.âK.; Meijer, Q.; Melatos, A.; Melchor, D.âA.; Mendell, G.; Menendez-Vazquez, A.; Menoni, C.âS.; Mercer, R.âA.; Mereni, L.; Merfeld, K.; Merilh, E.âL.; Merritt, J.âD.; Merzougui, M.; Meshkov, S.; Messenger, C.; Messick, C.; Meyers, P.âM.; Meylahn, F.; Mhaske, A.; Miani, A.; Miao, H.; Michaloliakos, I.; Michel, C.; Middleton, H.; Milano, L.; Miller, A.; Miller, A.âL.; Miller, B.; Millhouse, M.; Mills, J.âC.; Milotti, E.; Minazzoli, O.; Minenkov, Y.; Mir, Ll.âM.; Miravet-TenĂ©s, M.; Mishra, C.; Mishra, T.; Mistry, T.; Mitra, S.; Mitrofanov, V.âP.; Mitselmakher, G.; Mittleman, R.; Mo, Geoffrey; Moguel, E.; Mogushi, K.; Mohapatra, S.âR.âP.; Mohite, S.âR.; Molina, I.; Molina-Ruiz, M.; Mondin, M.; Montani, M.; Moore, C.âJ.; Moraru, D.; Morawski, F.; More, A.; Moreno, C.; Moreno, G.; Morisaki, S.; Mours, B.; Mow-Lowry, C.âM.; Mozzon, S.; Muciaccia, F.; Mukherjee, Arunava; Mukherjee, D.; Mukherjee, Soma; Mukherjee, Subroto; Mukherjee, Suvodip; Mukund, N.; Mullavey, A.; Munch, J.; Muñiz, E.âA.; Murray, P.âG.; Musenich, R.; Muusse, S.; Nadji, S.âL.; Nagar, A.; Napolano, V.; Nardecchia, I.; 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The population of merging compact binaries inferred using gravitational waves through GWTC-3
We report on the population properties of 76 compact binary mergers detected with gravitational waves below a false alarm rate of 1 per year through GWTC-3. The catalog contains three classes of binary mergers: BBH, BNS, and NSBH mergers. We infer the BNS merger rate to be between 10 and 1700 and the NSBH merger rate to be between 7.8 and 140 , assuming a constant rate density versus comoving volume and taking the union of 90% credible intervals for methods used in this work. Accounting for the BBH merger rate to evolve with redshift, we find the BBH merger rate to be between 17.9 and 44 at a fiducial redshift (z=0.2). We obtain a broad neutron star mass distribution extending from to . We can confidently identify a rapid decrease in merger rate versus component mass between neutron star-like masses and black-hole-like masses, but there is no evidence that the merger rate increases again before 10 . We also find the BBH mass distribution has localized over- and under-densities relative to a power law distribution. While we continue to find the mass distribution of a binary's more massive component strongly decreases as a function of primary mass, we observe no evidence of a strongly suppressed merger rate above . The rate of BBH mergers is observed to increase with redshift at a rate proportional to with for . Observed black hole spins are small, with half of spin magnitudes below . We observe evidence of negative aligned spins in the population, and an increase in spin magnitude for systems with more unequal mass ratio
Population of Merging Compact Binaries Inferred Using Gravitational Waves through GWTC-3
We report on the population properties of compact binary mergers inferred from gravitational-wave observations of these systems during the first three LIGO-Virgo observing runs. The Gravitational-Wave Transient Catalog 3 (GWTC-3) contains signals consistent with three classes of binary mergers: binary black hole, binary neutron star, and neutron star-black hole mergers. We infer the binary neutron star merger rate to be between 10 and 1700 Gpc-3 yr-1 and the neutron star-black hole merger rate to be between 7.8 and 140 Gpc-3 yr-1, assuming a constant rate density in the comoving frame and taking the union of 90% credible intervals for methods used in this work. We infer the binary black hole merger rate, allowing for evolution with redshift, to be between 17.9 and 44 Gpc-3 yr-1 at a fiducial redshift (z=0.2). The rate of binary black hole mergers is observed to increase with redshift at a rate proportional to (1+z)Îș with Îș=2.9-1.8+1.7 for zâČ1. Using both binary neutron star and neutron star-black hole binaries, we obtain a broad, relatively flat neutron star mass distribution extending from 1.2-0.2+0.1 to 2.0-0.3+0.3Mâ. We confidently determine that the merger rate as a function of mass sharply declines after the expected maximum neutron star mass, but cannot yet confirm or rule out the existence of a lower mass gap between neutron stars and black holes. We also find the binary black hole mass distribution has localized over- and underdensities relative to a power-law distribution, with peaks emerging at chirp masses of 8.3-0.5+0.3 and 27.9-1.8+1.9Mâ. While we continue to find that the mass distribution of a binary's more massive component strongly decreases as a function of primary mass, we observe no evidence of a strongly suppressed merger rate above approximately 60Mâ, which would indicate the presence of a upper mass gap. Observed black hole spins are small, with half of spin magnitudes below Ïiâ0.25. While the majority of spins are preferentially aligned with the orbital angular momentum, we infer evidence of antialigned spins among the binary population. We observe an increase in spin magnitude for systems with more unequal-mass ratio. We also observe evidence of misalignment of spins relative to the orbital angular momentum
Constraints on dark photon dark matter using data from LIGO's and Virgo's third observing run
We present a search for dark photon dark matter that could couple to
gravitational-wave interferometers using data from Advanced LIGO and Virgo's
third observing run. To perform this analysis, we use two methods, one based on
cross-correlation of the strain channels in the two nearly aligned LIGO
detectors, and one that looks for excess power in the strain channels of the
LIGO and Virgo detectors. The excess power method optimizes the Fourier
Transform coherence time as a function of frequency, to account for the
expected signal width due to Doppler modulations. We do not find any evidence
of dark photon dark matter with a mass between eV/, which corresponds to frequencies between 10-2000
Hz, and therefore provide upper limits on the square of the minimum coupling of
dark photons to baryons, i.e. dark matter. For the
cross-correlation method, the best median constraint on the squared coupling is
at eV/; for the
other analysis, the best constraint is at eV/. These limits improve upon those obtained
in direct dark matter detection experiments by a factor of for
eV/, and are, in absolute terms, the
most stringent constraint so far in a large mass range eV/.Comment: 20 pages, 7 figure
All-sky search for long-duration gravitational-wave bursts in the third Advanced LIGO and Advanced Virgo run
After the detection of gravitational waves from compact binary coalescences, the search for transient gravitational-wave signals with less well-defined waveforms for which matched filtering is not well suited is one of the frontiers for gravitational-wave astronomy. Broadly classified into âshortâ âČ1ââs and âlongâ âł1ââs duration signals, these signals are expected from a variety of astrophysical processes, including non-axisymmetric deformations in magnetars or eccentric binary black hole coalescences. In this work, we present a search for long-duration gravitational-wave transients from Advanced LIGO and Advanced Virgoâs third observing run from April 2019 to March 2020. For this search, we use minimal assumptions for the sky location, event time, waveform morphology, and duration of the source. The search covers the range of 2â500 s in duration and a frequency band of 24â2048 Hz. We find no significant triggers within this parameter space; we report sensitivity limits on the signal strength of gravitational waves characterized by the root-sum-square amplitude hrss as a function of waveform morphology. These hrss limits improve upon the results from the second observing run by an average factor of 1.8
Search for subsolar-mass black hole binaries in the second part of Advanced LIGOâs and Advanced Virgoâs third observing run
We describe a search for gravitational waves from compact binaries with at least one component with mass 0.2âMââ1.0âMâ and mass ratio q â„ 0.1 in Advanced LIGO and Advanced Virgo data collected between 1 November 2019, 15:00 UTC and 27 March 2020, 17:00 UTC. No signals were detected. The most significant candidate has a false alarm rate of 0.2yrâ1
â . We estimate the sensitivity of our search over the entirety of Advanced LIGOâs and Advanced Virgoâs third observing run, and present the most stringent limits to date on the merger rate of binary black holes with at least one subsolar-mass component. We use the upper limits to constrain two fiducial scenarios that could produce subsolar-mass black holes: primordial black holes (PBH) and a model of dissipative dark matter. The PBH model uses recent prescriptions for the merger rate of PBH binaries that include a rate suppression factor to effectively account for PBH early binary disruptions. If the PBHs are monochromatically distributed, we can exclude a dark matter fraction in PBHs fPBH âłâ0.6 (at 90% confidence) in the probed subsolar-mass range. However, if we allow for broad PBH mass distributions we are unable to rule out fPBH = 1. For the dissipative model, where the dark matter has chemistry that allows a small fraction to cool and collapse into black holes, we find an upper bound fDBH < 10â5 on the fraction of atomic dark matter collapsed into black holes
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