1,803 research outputs found
The ISLAndS project II: The Lifetime Star Formation Histories of Six Andromeda dSphs
The Initial Star formation and Lifetimes of Andromeda Satellites (ISLAndS)
project uses Hubble Space Telescope imaging to study a representative sample of
six Andromeda dSph satellite companion galaxies. The main goal of the program
is to determine whether the star formation histories (SFHs) of the Andromeda
dSph satellites demonstrate significant statistical differences from those of
the Milky Way, which may be attributable to the different properties of their
local environments. Our observations reach the oldest main sequence turn-offs,
allowing a time resolution at the oldest ages of ~ 1 Gyr, which is comparable
to the best achievable resolution in the MW satellites. We find that the six
dSphs present a variety of SFHs that are not strictly correlated with
luminosity or present distance from M31. Specifically, we find a significant
range in quenching times (lookback times from 9 to 6 Gyr), but with all
quenching times more than ~ 6 Gyr ago. In agreement with observations of Milky
Way companions of similar mass, there is no evidence of complete quenching of
star formation by the cosmic UV background responsible for reionization, but
the possibility of a degree of quenching at reionization cannot be ruled out.
We do not find significant differences between the SFHs of the three members of
the vast, thin plane of satellites and the three off-plane dSphs. The primary
difference between the SFHs of the ISLAndS dSphs and Milky Way dSph companions
of similar luminosities and host distances is the absence of very late
quenching (< 5 Gyr ago) dSphs in the ISLAndS sample. Thus, models that can
reproduce satellite populations with and without late quenching satellites will
be of extreme interest.Comment: 24 pages, 11 figures, 3 tables, submitted to the Ap
Latino Communities in the United States: Place-Making in the Pre-World War II, Postwar, and Contemporary City
Scholarship on Latino communities in the United States has yet to catch up with the rapid growth of this ethnic population in the country. Understanding the Latino urban experience and developing plans to better respond to both the needs of Latino communities and their integration within society is not only relevant, but also urgently necessary. Using the city of Los Angeles as a main lens, in addition to a general look at the urban Southwest, we contribute to the scholarship on the subject with a review of literature on Latino communities. We structure the review as an assessment of the various challenges and opportunities for urban Latinos in the pre-war, postwar, and contemporary city. Focusing on space, culture, economy, and governance, we chart the various roles both the private and public sectors play in meeting these challenges. Our reading of the literature shows that particular government actions in the economic and governance domains in the past had positive impacts on Latino integration, and we call for a similar effort today in addressing contemporary challenges. We conclude by suggesting that future planning scholarship on Latino communities engage the wider urban studies literature, focus on emerging forms of urbanization, and call on planners to sustain increased academic and practical interest in the topic
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. 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.; 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Rana, J.; Rapagnani, P.; Rapol, U.âD.; Ray, A.; Raymond, V.; Raza, N.; Razzano, M.; Read, J.; Rees, L.âA.; Regimbau, T.; Rei, L.; Reid, S.; Reid, S.âW.; Reitze, D.âH.; Relton, P.; Renzini, A.; Rettegno, P.; Rezac, M.; Ricci, F.; Richards, D.; Richardson, J.âW.; Richardson, L.; Riemenschneider, G.; Riles, K.; Rinaldi, S.; Rink, K.; Rizzo, M.; Robertson, N.âA.; Robie, R.; Robinet, F.; Rocchi, A.; Rodriguez, S.; Rolland, L.; Rollins, J.âG.; Romanelli, M.; Romano, R.; Romel, C.âL.; Romero-RodrĂguez, A.; Romero-Shaw, I.âM.; Romie, J.âH.; Ronchini, S.; Rosa, L.; Rose, C.âA.; RosiĆska, D.; Ross, M.âP.; Rowan, S.; Rowlinson, S.âJ.; Roy, S.; Roy, Santosh; Roy, Soumen; Rozza, D.; Ruggi, P.; Ryan, K.; Sachdev, S.; Sadecki, T.; Sadiq, J.; Sakellariadou, M.; Salafia, O.âS.; Salconi, L.; Saleem, M.; Salemi, F.; Samajdar, A.; Sanchez, E.âJ.; Sanchez, J.âH.; Sanchez, L.âE.; Sanchis-Gual, N.; Sanders, J.âR.; Sanuy, A.; Saravanan, T.âR.; Sarin, N.; Sassolas, B.; Satari, H.; Sathyaprakash, B.âS.; Sauter, O.; Savage, R.âL.; Sawant, D.; Sawant, H.âL.; Sayah, S.; Schaetzl, D.; Scheel, M.; Scheuer, J.; Schiworski, M.; Schmidt, P.; Schmidt, S.; Schnabel, R.; Schneewind, M.; Schofield, R.âM.âS.; Schönbeck, A.; Schulte, B.âW.; Schutz, B.âF.; Schwartz, E.; Scott, J.; Scott, S.âM.; Seglar-Arroyo, M.; Sellers, D.; Sengupta, A.âS.; Sentenac, D.; Seo, E.âG.; Sequino, V.; Sergeev, A.; Setyawati, Y.; Shaffer, T.; Shahriar, M.âS.; Shams, B.; Sharma, A.; Sharma, P.; Shawhan, P.; Shcheblanov, N.âS.; Shikauchi, M.; Shoemaker, D.âH.; Shoemaker, D.âM.; ShyamSundar, S.; Sieniawska, M.; Sigg, D.; Singer, L.âP.; Singh, D.; Singh, N.; Singha, A.; Sintes, A.âM.; Sipala, V.; Skliris, V.; Slagmolen, B.âJ.âJ.; Slaven-Blair, T.âJ.; Smetana, J.; Smith, J.âR.; Smith, R.âJ.âE.; Soldateschi, J.; Somala, S.âN.; Son, E.âJ.; Soni, K.; Soni, S.; Sordini, V.; Sorrentino, F.; Sorrentino, N.; Soulard, R.; Souradeep, T.; Sowell, E.; Spagnuolo, V.; Spencer, A.âP.; Spera, M.; Srinivasan, R.; Srivastava, A.âK.; Srivastava, V.; Staats, K.; 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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
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
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
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