Mostrando recursos 1 - 20 de 756

  1. The characterization of the gamma-ray signal from the central Milky Way: A case for annihilating dark matter

    Daylan, Tansu; Finkbeiner, Douglas P.; Hooper, Dan; Linden, Tim; Portillo, Stephen K.N.; Rodd, Nicholas Llewellyn; Slatyer, Tracy Robyn
    Past studies have identified a spatially extended excess of ~1-3 GeV gamma rays from the region surrounding the Galactic Center, consistent with the emission expected from annihilating dark matter. We revisit and scrutinize this signal with the intention of further constraining its characteristics and origin. By applying cuts to the Fermi event parameter CTBCORE, we suppress the tails of the point spread function and generate high resolution gamma-ray maps, enabling us to more easily separate the various gamma-ray components. Within these maps, we find the GeV excess to be robust and highly statistically significant, with a spectrum, angular distribution, and...

  2. ¿Qué puede una historia del arte cuir?

    Poggio, Catalina
    Fantasear una historia del arte hereje, blasfema. Una historia sacrílega, iconoclasta, que pervierta la intocable madona con el niño, la niña, la madre y la señora, siempre virgen, santa, sumisa, entregada, sometida. Desear una historia del arte sucia, pornográfica, degenerada, que desborde, deforme, travista las ficciones somáticas administradas por la escritura cis, heterosexual de la blancura académica. Ansiar una historia del arte hacker, cyborg, protésica, que desmonte la relación histérica y carnal entre imagen y poder. Pulsar una escritura de la historia del arte cuir como resistencia a la normalización, contra el dogmatismo del lenguaje académico.

  3. Disentangling hadronic from leptonic emission in the composite SNR G326.3$-$1.8

    Devin , J.; Acero , F.; Ballet , J.; Schmid , J.
    G326.3$-$1.8 (also known as MSH 15$-$56) has been detected in radio as a middle-aged composite supernova remnant (SNR) consisting of an SNR shell and a pulsar wind nebula (PWN), which has been crushed by the SNR's reverse shock. Previous $\gamma$-ray studies of SNR G326.3$-$1.8 revealed bright and extended emission with uncertain origin. Understanding the nature of the $\gamma$-ray emission allows probing the population of high-energy particles (leptons or hadrons) but can be challenging for sources of small angular extent. With the recent $\textit{Fermi}$ Large Area Telescope data release Pass 8, we investigate the morphology of this SNR to disentangle the...

  4. Inter-relações: nóis é nóis: construções identitárias no futebol de várzea paulistano

    Oliveira, Ana Claudia de; Rovina Castro Pereira, Tatiana
    São Paulo, capital. Um sábado ou domingo qualquer, tão importante quanto todos os fins de semana do ano. Nos campos, a bola rola, balança a rede, com clima de decisão. A torcida vibra, xinga, batuca onde nem sempre há arquibancada – e, às vezes, sequer gramado. Mas essas condições não diminuem o amor pelo futebol, que une “todos juntos em uma mesma emoção”. Longe dos estádios e dos times milionários, dos craques espetacularizados e das torcidas organizadas oficiais, o futebol amador faz pulsar as quebradas. No coração das comunidades, espalhadas pelos quatro cantos da metrópole, o grito de gol, que não falta, ecoa, integrando-as (...)

  5. Cidade sensível, cidade de areia, Cidade Nova

    Nóbrega Ferreira, Felipe; Duarte Pedroso, Ticiano
    As cidades e as sensibilidades se coadunaram junto à História Cultural – essa consolidada enquanto abordagem no campo da História no decorrer dos anos 1990 - a partir de obras que se preocupavam em aproximar o universo do sensível ao pulsar urbano. A partir desse reposicionamento, seja do entendimento das cidades enquanto objeto, ou da abertura do entendimento das sensibilidades, apresentamos um diálogo em que o objetivo é adentrar as camadas sensíveis presentes na constituição de um espaço urbano que passa por transformações contundentes: de território limítrofe de uma cidade, tomado por areias, a bairro ocupado por sujeitos alijados do...

  6. La aportación de Lluís Bel al desarrollo de la física relativista en España

    Soler Ferrán, Pablo
    Se muestra la aportación del físico Lluís Bel al desarrollo de la física relativista en España desde los años 1970, en concreto con la formación de uno de los grupos de investigación sobre relatividad, el de la Universidad Autónoma de Madrid (UAM). Bel venía desarrollando su carrera investigadora en Francia, principalmente en radiación gravitacional, cuando en 1971 fue invitado a la UAM, hecho que se enmarca en el intento de renovación de la ciencia española en esos años. Diferentes problemas motivaron que solo permaneciera en España dos años, pero en ese tiempo se logró consolidar de forma estable un grupo...

  7. An observational test for the existence of a planetary system orbiting PSR1257 + 12

    Rasio, F. A.; Nicholson, P. D.; Shapiro, S. L.; Teukolsky, S. A.
    FOLLOWING the first report of an object of planetary mass orbiting a pulsar, Wolszczan and Frail have now reported the even more surprising discovery of two planet-size companions in orbit around the nearby millisecond pulsar PSR1257+12. The orbital periods of the two planets are about 98 days and 67 days, very close to a 3:2 ratio. Here we point out that, because of this near commensurability, the mutual gravitational perturbations of the two planets should produce not only small secular changes, but also larger periodic changes in their orbital elements. In particular, we find that changes in the eccentricities and...

  8. Formation of a 'planet' by rapid evaporation of a pulsar's companion

    Rasio, F. A.; Shapiro, S. L.; Teukolsky, S. A.
    A planet-size object in circular orbit around a pulsar could be formed as the result of rapid evaporation of a more massive binary companion by the pulsar's radiation.

  9. Spin-up of a rapidly rotating star by angular momentum loss

    Shapiro, Stuart L.; Teukolsky, Saul A.; Nakamura, Takashi
    Can a rotating star spin up by radiating away its angular momentum? And if so, what can we infer about the properties of such a star? We show that the spin of a rapidly rotating star like a pulsar can indeed increase as it radiates away energy and angular momentum. For this to happen the adiabatic index governing the equation of state must be very close to 4/3 if the star is rotating uniformly. Otherwise the star must be rotating differentially.

  10. The 30-Year Search for the Compact Object in SN 1987A

    Alp , Dennis; Larsson , Josefin; Fransson , Claes; Indebetouw , Remy; Jerkstrand , Anders; Ahola , Antero; Burrows , David; Challis , Peter; Cigan , Phil; Cikota , Aleksandar; Kirshner , Robert; van Loon , Jacco; Mattila , Seppo; Ng , C.-Y.; Park , Sangwook; Spyromilio , Jason; Woosley , Stan; Baes , Maarten; Bouchet , Patrice; Chevalier , Roger; Frank , Kari; Gaensler , B.M.; Gomez , Haley; Janka , Hans-Thomas; Leibundgut , Bruno; Lundqvist , Peter; Marcaide , Jon; Matsuura , Mikako; Sollerman , Jesper; Sonneborn , George; Staveley-Smith , Lister; Zanardo , Giovanna; Gabler , Michael; Taddia , Francesco; Wheeler , J.
    Despite more than 30 years of searches, the compact object in Supernova (SN) 1987A has not yet been detected. We present new limits on the compact object in SN 1987A using millimeter, near-infrared, optical, ultraviolet, and X-ray observations from ALMA, VLT, HST, and Chandra. The limits are approximately 0.1 mJy ($0.1\times 10^{-26}$ erg s$^{-1}$ cm$^{-2}$ Hz$^{-1}$) at 213 GHz, 1 Lsun ($6\times 10^{-29}$ erg s$^{-1}$ cm$^{-2}$ Hz$^{-1}$) in optical if our line-of-sight is free of ejecta dust, and $10^{36}$ erg s$^{-1}$ ($2\times 10^{-30}$ erg s$^{-1}$ cm$^{-2}$ Hz$^{-1}$) in 2-10 keV X-rays. Our X-ray limits are an order of magnitude less...

  11. The NANOGrav 11 Year Data Set: Pulsar-timing Constraints on the Stochastic Gravitational-wave Background

    Arzoumanian, Z.; Lazio, T. J. W.; Taylor, S. R.; Vallisneri, M.
    We search for an isotropic stochastic gravitational-wave background (GWB) in the newly released 11 year data set from the North American Nanohertz Observatory for Gravitational Waves (NANOGrav). While we find no evidence for a GWB, we place constraints on a population of inspiraling supermassive black hole (SMBH) binaries, a network of decaying cosmic strings, and a primordial GWB. For the first time, we find that the GWB constraints are sensitive to the solar system ephemeris (SSE) model used and that SSE errors can mimic a GWB signal. We developed an approach that bridges systematic SSE differences, producing the first pulsar-timing...

  12. The geometric distance and binary orbit of PSR B1259-63

    Miller-Jones , J.C.; Deller , A.T.; Shannon , R.M.; Dodson , R.; Moldón , J.; Ribó , M.; Dubus , G.; Johnston , S.; Paredes , J.M.; Ransom , S.M.; Tomsick , J.A.
    The pulsar/massive star binary system PSR B1259-63 / LS 2883 is one of the best-studied gamma-ray binaries, a class of systems whose bright gamma-ray flaring can provide important insights into high-energy physics. Using the Australian Long Baseline Array we have conducted very long baseline interferometric observations of PSR B1259-63 over 4.4 years, fully sampling the 3.4-year orbital period. Inverting our measured parallax gives a distance of $2.59^{+0.37}_{-0.28}$ kpc, which when modified to account for the Lutz-Kelker bias gives a corrected distance of $2.70^{+0.41}_{-0.31}$ kpc. We find that the binary orbit is viewed at an angle of $153.4^{+3.2}_{-3.0}$ degrees to the...

  13. Improving timing sensitivity in the microhertz frequency regime: limits from PSR J1713$+$0747 on gravitational waves produced by super-massive black-hole binaries

    Perera , B.B.P.; Stappers , B.W.; Babak , S.; Keith , M.J.; Antoniadis , J.; Bassa , C.G.; Caballero , R.N.; Champion , D.J.; Cognard , I.; Desvignes , G.; Graikou , E.; Guillemot , L.; Janssen , G.H.; Karuppusamy , R.; Kramer , M.; Lazarus , P.; Lentati , L.; Liu , K.; Lyne , A.G.; McKee , J.W.; Osłowski , S.; Perrodin , D.; Sanidas , S.A.; Sesana , A.; Shaifullah , G.; Theureau , G.; Verbiest , J.P.W.; Taylor , S.R.
    We search for continuous gravitational waves (CGWs) produced by individual super-massive black-hole binaries (SMBHBs) in circular orbits using high-cadence timing observations of PSR J1713$+$0747. We observe this millisecond pulsar using the telescopes in the European Pulsar Timing Array (EPTA) with an average cadence of approximately 1.6 days over the period between April 2011 and July 2015, including an approximately daily average between February 2013 and April 2014. The high-cadence observations are used to improve the pulsar timing sensitivity across the GW frequency range of $0.008-5$ $\mu$Hz. We use two algorithms in the analysis, including a spectral fitting method and a...

  14. Einstein@Home discovers a radio-quiet gamma-ray millisecond pulsar

    Clark , Colin; Pletsch , Holger; Wu , Jason; Guillemot , Lucas; Kerr , Matthew; Johnson , Tyrel; Camilo , Fernando; Salvetti , David; Allen , Bruce; Anderson , David; Aulbert , Carsten; Beer , Christian; Bock , Oliver; Cuéllar , Andres; Eggenstein , Heinz-Bernd; Fehrmann , Henning; Kramer , Michael; Kwang , Shawn; Machenschalk , Bernd; Nieder , Lars; Ackermann , Markus; Ajello , Marco; Baldini , Luca; Ballet , Jean; Barbiellini , Guido; Bastieri , Denis; Bellazzini , Ronaldo; Bissaldi , Elisabetta; Blandford , Roger; Bloom , Elliott; Bonino , Raffaella; Bottacini , Eugenio; Brandt , Terri; Bregeon , Johan; Bruel , Philippe; Buehler , Rolf; Burnett , Toby; Buson , Sara; Cameron , Rob; Caputo , Regina; Caraveo , Patrizia; Cavazzuti , Elisabetta; Cecchi , Claudia; Charles , Eric; Chekhtman , Alexandre; Ciprini , Stefano; Cominsky , Lynn; Costantin , Denise; Cutini , Sara; D'Ammando , Filippo; De Luca , Andrea; Desiante , Rachele; Di Venere , Leonardo; Di Mauro , Mattia; Di Lalla , Niccolò; Digel , Seth; Favuzzi , Cecilia; Ferrara , Elizabeth; Franckowiak , Anna; Fukazawa , Yasushi; Funk , Stefan; Fusco , Piergiorgio; Gargano , Fabio; Gasparrini , Dario; Giglietto , Nico; Giordano , Francesco; Giroletti , Marcello; Gomez-Vargas , Germán; Green , David; Grenier , Isabelle; Guiriec , Sylvain; Harding , Alice; Hewitt , John; Horan , Deirdre; Jóhannesson , Guðlaugur; Kensei , Shiki; Kuss , Michael; La Mura , Giovanni; Larsson , Stefan; Latronico , Luca; Li , Jian; Longo , Francesco; Loparco , Francesco; Lovellette , Michael; Lubrano , Pasquale; Magill , Jeffrey; Maldera , Simone; Manfreda , Alberto; Mazziotta , Mario; McEnery , Julie; Michelson , Peter; Mirabal , Nestor; Mitthumsiri , Warit; Mizuno , Tsunefumi; Monzani , Maria; Morselli , Aldo; Moskalenko , Igor; Nuss , Eric; Ohsugi , Takashi; Omodei , Nicola; Orienti , Monica; Orlando , Elena; Palatiello , Michele; Paliya , Vaidehi; De Palma , Francesco; Paneque , David; Perkins , Jeremy; Persic , Massimo; Pesce-Rollins , Melissa; Porter , Troy; Principe , Giacomo; Rainò , Silvia; Rando , Riccardo; Ray , Paul; Razzano , Massimiliano; Reimer , Anita; Reimer , Olaf; Romani , Roger; Saz Parkinson , Pablo; Sgrò , Carmelo; Siskind , Eric; Smith , David; Spada , Francesca; Spandre , Gloria; Spinelli , Paolo; Thayer , Jana; Thompson , David; Torres , Diego; Troja , Eleonora; Vianello , Giacomo; Wood , Kent; Wood , Matthew
    International audience

  15. A tale of two periods: determination of the orbital ephemeris of the super-Eddington pulsar NGC 7793 P13

    Fürst, F.; Walton, D. J.; Heida, M.; Harrison, F. A.; Barret, D.; Brightman, M.; Fabian, A. C.; Middleton, M. J.; Pinto, C.; Rana, V.; Tramper, F.; Webb, N.; Kretschmar, P.
    We present a timing analysis of multiple XMM-Newton and NuSTAR observations of the ultra-luminous pulsar NGC 7793 P13 spread over its 65d variability period. We use the measured pulse periods to determine the orbital ephemeris, confirm a long orbital period with P_orb = 63.9 (+0.5,-0.6) d, and find an eccentricity of e <= 0.15. The orbital signature is imprinted on top of a secular spin-up, which seems to get faster as the source becomes brighter. We also analyse data from dense monitoring of the source with Swift and find an optical photometric period of 63.9 +/- 0.5 d and an X-ray flux period of 66.8 +/- 0.4 d....

  16. Hitomi X-ray studies of giant radio pulses from the Crab pulsar

    Aharonian , Felix; Akamatsu , Hiroki; Akimoto , Fumie; Allen , Steven; Angelini , Lorella; Audard , Marc; Awaki , Hisamitsu; Axelsson , Magnus; Bamba , Aya; Bautz , Marshall; Blandford , Roger; Brenneman , Laura; Brown , Gregory; Bulbul , Esra; Cackett , Edward; Chernyakova , Maria; Chiao , Meng; Coppi , Paolo; Costantini , Elisa; De Plaa , Jelle; De Vries , Cor; Herder , Jan-Willem; Done , Chris; Dotani , Tadayasu; Ebisawa , Ken; Eckart , Megan; Enoto , Teruaki; Ezoe , Yuichiro; Fabian , Andrew; Ferrigno , Carlo; Foster , Adam; Fujimoto , Ryuichi; Fukazawa , Yasushi; Furuzawa , Akihiro; Galeazzi , Massimiliano; Gallo , Luigi; Gandhi , Poshak; Giustini , Margherita; Goldwurm , Andrea; Gu , Liyi; Guainazzi , Matteo; Haba , Yoshito; Hagino , Kouichi; Hamaguchi , Kenji; Harrus , Ilana; Hatsukade , Isamu; Hayashi , Katsuhiro; Hayashi , Takayuki; Hayashida , Kiyoshi; Hiraga , Junko; Hornschemeier , Ann; Hoshino , Akio; Hughes , John; Ichinohe , Yuto; Iizuka , Ryo; Inoue , Hajime; Inoue , Yoshiyuki; Ishida , Manabu; Ishikawa , Kumi; Ishisaki , Yoshitaka; Iwai , Masachika; Kaastra , Jelle; Kallman , Tim; Kamae , Tsuneyoshi; Kataoka , Jun; Katsuda , Satoru; Kawai , Nobuyuki; Kelley , Richard; Kilbourne , Caroline; Kitaguchi , Takao; Kitamoto , Shunji; Kitayama , Tetsu; Kohmura , Takayoshi; Kokubun , Motohide; Koyama , Katsuji; Koyama , Shu; Kretschmar , Peter; Krimm , Hans; Kubota , Aya; Kunieda , Hideyo; Laurent , Philippe; Lee , Shiu-Hang; Leutenegger , Maurice; Limousin , Olivier; Loewenstein , Michael; Long , Knox; Lumb , David; Madejski , Greg; Maeda , Yoshitomo; Maier , Daniel; Makishima , Kazuo; Markevitch , Maxim; Matsumoto , Hironori; Matsushita , Kyoko; Mccammon , Dan; McNamara , Brian; Mehdipour , Missagh; Miller , Eric; Miller , Jon; Mineshige , Shin; Mitsuda , Kazuhisa; Mitsuishi , Ikuyuki; Miyazawa , Takuya; Mizuno , Tsunefumi; Mori , Hideyuki; Mori , Koji; Mukai , Koji; Murakami , Hiroshi; Mushotzky , Richard; Nakagawa , Takao; Nakajima , Hiroshi; Nakamori , Takeshi; Nakashima , Shinya; Nakazawa , Kazuhiro; Nobukawa , Kumiko; Nobukawa , Masayoshi; Noda , Hirofumi; Odaka , Hirokazu; Ohashi , Takaya; Ohno , Masanori; Okajima , Takashi; Oshimizu , Kenya; Ota , Naomi; Ozaki , Masanobu; Paerels , Frits; Paltani , Stéphane; Petre , Robert; Pinto , Ciro; Porter , Frederick; Pottschmidt , Katja; Reynolds , Christopher; Safi-Harb , Samar; Saito , Shinya; Sakai , Kazuhiro; Sasaki , Toru; Sato , Goro; Sato , Kosuke; Sato , Rie; Sawada , Makoto; Schartel , Norbert; Serlemtsos , Peter; Seta , Hiromi; Shidatsu , Megumi; Simionescu , Aurora; Smith , Randall; Soong , Yang; Stawarz , Ł; Sugawara , Yasuharu; Sugita , Satoshi; Szymkowiak , Andrew; Tajima , Hiroyasu; Takahashi , Hiromitsu; Takahashi , Tadayuki; Takeda , Shiníchiro; Takei , Yoh; Tamagawa , Toru; Tamura , Takayuki; Tanaka , Takaaki; Tanaka , Yasuo; Tanaka , Yasuyuki; Tashiro , Makoto; Tawara , Yuzuru; Terada , Yukikatsu; Terashima , Yuichi; Tombesi , Francesco; Tomida , Hiroshi; Tsuboi , Yohko; Tsujimoto , Masahiro; Tsunemi , Hiroshi; Tsuru , Takeshi; Uchida , Hiroyuki; Uchiyama , Hideki; Uchiyama , Yasunobu; Ueda , Shutaro; Ueda , Yoshihiro; Uno , Shiníchiro; Urry , C.; Ursino , Eugenio; Watanabe , Shin; Werner , Norbert; Wilkins , Dan; Williams , Brian; Yamada , Shinya; Yamaguchi , Hiroya; Yamaoka , Kazutaka; Yamasaki , Noriko; Yamauchi , Makoto; Yamauchi , Shigeo; Yaqoob , Tahir; Yatsu , Yoichi; Yonetoku , Daisuke; Zhuravleva , Irina; Zoghbi , Abderahmen; Terasawa , Toshio; Sekido , Mamoru; Takefuji , Kazuhiro; Kawai , Eiji; Misawa , Hiroaki; Tsuchiya , Fuminori; Yamazaki , Ryo; Kobayashi , Eiji; Kisaka , Shota; Aoki , Takahiro
    International audience

  17. Estudio del estado evolutivo del sistema binario PSR J1227-4853

    González, Julián
    En esta tesis describiremos los objetos conocidos como black widows y redbacks en el marco de los sistemas binarios interactuantes, y, en particular, el estado evolutivo del sistema binario eclipsante que contiene al púlsar PSR J1227-4853. Los resultados se obtuvieron utilizando el código de evolución binaria desarrollado por mis directores. Para ello hicimos los cálculos evolutivos de posibles progenitores del sistema hasta encontrar coincidencia con los parámetros –masas de las componentes, período orbital y cociente de masas– que presenta hoy en día el sistema. Finalmente, se analiza el efecto de la irradiación mutua en este caso en particular.

  18. Constraints on cosmic strings using data from the first Advanced LIGO observing run

    Abbott, B. P.; Abbott, R.; Abbott, T. D.; Acernese, F.; Ackley, K.; Adams, C.; Adams, T.; Addesso, P.; Adhikari, R. X.; Adya, V. B.; Affeldt, C.; Afrough, M.; Agarwal, B.; Agathos, M.; Agatsuma, K.; Aguiar, O. D.; Aiello, L.; Ain, A.; Ajith, P.; Allen, B.; Allen, G.; Allocca, A.; Altin, P. A.; Amato, A.; Ananyeva, A.; Anderson, S. B.; Anderson, W. G.; Antier, S.; Appert, S.; Arai, K.; Araya, M. C.; Areeda, J. S.; Arnaud, N.; Arun, K. G.; Ascenzi, S.; Ashton, G.; Ast, M.; Aston, S. M.; Astone, P.; Aufmuth, P.; Aulbert, C.; AultONeal, K.; Avila-Alvarez, A.; Babak, S.; Bacon, P.; Bader, M. K. M.; Bae, S.; Baker, P. T.; Baldaccini, F.; Ballardin, G.; Ballmer, S. W.; Banagiri, S.; Barayoga, J. C.; Barclay, S. E.; Barish, B. C.; Barker, D.; Barone, F.; Barr, B.; Barsuglia, M.; Barta, D.; Bartlett, J.; Bartos, I.; Bassiri, R.; Basti, A.; Batch, J. C.; Baune, C.; Bawaj, M.; Bazzan, M.; Bécsy, B.; Beer, C.; Bejger, M.; Belahcene, I.; Bell, A. S.; Berger, B. K.; Bergmann, G.; Berry, C. P. L.; Bersanetti, D.; Bertolini, A.; Betzwieser, J.; Bhagwat, S.; Bhandare, R.; Bilenko, I. A.; Billingsley, G.; Billman, C. R.; Birch, J.; Birney, R.; Birnholtz, O.; Bisht, A.; Bitossi, M.; Biwer, C.; Bizouard, M. A.; Blackburn, J. K.; Blackman, J.; Blair, C. D.; Blair, D. G.; Blair, R. M.; Bloemen, S.; Bock, O.; Bode, N.; Boer, M.; Bogaert, G.; Bohe, A.; Bondu, F.; Bonnand, R.; Boom, B. A.; Bork, R.; Boschi, V.; Bose, S.; Bouffanais, Y.; Bozzi, A.; Bradaschia, C.; Brady, P. R.; Braginsky, V. B.; Branchesi, M.; Brau, J. E.; Briant, T.; Brillet, A.; Brinkmann, M.; Brisson, V.; Brockill, P.; Broida, J. E.; Brooks, A. F.; Brown, D. A.; Brown, D. D.; Brunett, S.; Buchanan, C. C.; Bulik, T.; Bulten, H. J.; Buonanno, A.; Buskulic, D.; Buy, C.; Byer, R. L.; Cabero, M.; Cadonati, L.; Cagnoli, G.; Cahillane, C.; Calderón Bustillo, J.; Callister, T. A.; Calloni, E.; Camp, J. B.; Canepa, M.; Canizares, P.; Cannon, K. C.; Cao, H.; Cao, J.; Capano, C. D.; Capocasa, E.; Carbognani, F.; Caride, S.; Carney, M. F.; Casanueva Diaz, J.; Casentini, C.; Caudill, S.; Cavaglià, M.; Cavalier, F.; Cavalieri, R.; Cella, G.; Cepeda, C. B.; Cerboni Baiardi, L.; Cerretani, G.; Cesarini, E.; Chamberlin, S. J.; Chan, M.; Chao, S.; Charlton, P.; Chassande-Mottin, E.; Chatterjee, D.; Cheeseboro, B. D.; Chen, H. Y.; Chen, Y.; Cheng, H.-P.; Chincarini, A.; Chiummo, A.; Chmiel, T.; Cho, H. S.; Cho, M.; Chow, J. H.; Christensen, N.; Chu, Q.; Chua, A. J. K.; Chua, S.; Chung, A. K. W.; Chung, S.; Ciani, G.; Ciolfi, R.; Cirelli, C. E.; Cirone, A.; Clara, F.; Clark, J. A.; Cleva, F.; Cocchieri, C.; Coccia, E.; Cohadon, P.-F.; Colla, A.; Collette, C. G.; Cominsky, L. R.; Constancio, M.; Conti, L.; Cooper, S. J.; Corban, P.; Corbitt, T. R.; Corley, K. R.; Cornish, N.; Corsi, A.; Cortese, S.; Costa, C. A.; Coughlin, M. W.; Coughlin, S. B.; Coulon, J.-P.; Countryman, S. T.; Couvares, P.; Covas, P. B.; Cowan, E. E.; Coward, D. M.; Cowart, M. J.; Coyne, D. C.; Coyne, R.; Creighton, J. D. E.; Creighton, T. D.; Cripe, J.; Crowder, S. G.; Cullen, T. J.; Cumming, A.; Cunningham, L.; Cuoco, E.; Dal Canton, T.; Danilishin, S. L.; D’Antonio, S.; Danzmann, K.; Dasgupta, A.; Da Silva Costa, C. F.; Dattilo, V.; Dave, I.; Davier, M.; Davis, D.; Daw, E. J.; Day, B.; De, S.; DeBra, D.; Degallaix, J.; De Laurentis, M.; Deléglise, S.; Del Pozzo, W.; Denker, T.; Dent, T.; Dergachev, V.; De Rosa, R.; DeRosa, R. T.; DeSalvo, R.; Devenson, J.; Devine, R. C.; Dhurandhar, S.; Díaz, M. C.; Di Fiore, L.; Di Giovanni, M.; Di Girolamo, T.; Di Lieto, A.; Di Pace, S.; Di Palma, I.; Di Renzo, F.; Doctor, Z.; Dolique, V.; Dooley, K. L.; Doravari, S.; Dorrington, I.; Douglas, R.; Dovale Álvarez, M.; Downes, T. P.; Drago, M.; Drever, R. W. P.; Driggers, J. C.; Du, Z.; Ducrot, M.; Duncan, J.; Dwyer, S. E.; Edo, T. B.; Edwards, M. C.; Effler, A.; Eggenstein, H.-B.; Ehrens, P.; Eichholz, J.; Eikenberry, S. S.; Etienne, Z. B.; Etzel, T.; Evans, T. M.; Factourovich, M.; Fafone, V.; Fair, H.; Fairhurst, S.; Fan, X.; Farinon, S.; Farr, B.; Farr, W. M.; Fauchon-Jones, E. J.; Favata, M.; Fays, M.; Fehrmann, H.; Feicht, J.; Fejer, M. M.; Ferrante, I.; Ferreira, E. C.; Ferrini, F.; Fidecaro, F.; Fiori, I.; Fiorucci, D.; Fisher, R. P.; Fitz-Axen, M.; Flaminio, R.; Fletcher, M.; Fong, H.; Forsyth, P. W. F.; Forsyth, S. S.; Fournier, J.-D.; Frasca, S.; Frasconi, F.; Frei, Z.; Freise, A.; Frey, R.; Frey, V.; Fries, E. M.; Frolov, V. V.; Fulda, P.; Fyffe, M.; Gabbard, H.; Gabel, M.; Gadre, B. U.; Gaebel, S. M.; Gair, J. R.; Gammaitoni, L.; Ganija, M. R.; Gaonkar, S. G.; Garufi, F.; Gaudio, S.; Gaur, G.; Gayathri, V.; Gehrels, N.; Gemme, G.; Genin, E.; Gennai, A.; George, D.; George, J.; Gergely, L.; Germain, V.; Ghonge, S.; Ghosh, Abhirup; Ghosh, Archisman; Ghosh, S.; Giaime, J. A.; Giardina, K. D.; Giazotto, A.; Gill, K.; Glover, L.; Goetz, E.; Goetz, R.; Gomes, S.; González, G.; Gonzalez Castro, J. M.; Gopakumar, A.; Gorodetsky, M. L.; Gossan, S. E.; Gosselin, M.; Gouaty, R.; Grado, A.; Graef, C.; Granata, M.; Grant, A.; Gray, C.; Greco, G.; Green, A. C.; Groot, P.; Grote, H.; Grunewald, S.; Gruning, P.; Guidi, G. M.; Guo, X.; Gupta, A.; Gupta, M. K.; Gushwa, K. E.; Gustafson, E. K.; Gustafson, R.; Hall, B. R.; Hall, E. D.; Hammond, G.; Haney, M.; Hanke, M. M.; Hanks, J.; Hanna, C.; Hannam, M. D.; Hannuksela, O. A.; Hanson, J.; Hardwick, T.; Harms, J.; Harry, G. M.; Harry, I. W.; Hart, M. J.; Haster, C.-J.; Haughian, K.; Healy, J.; Heidmann, A.; Heintze, M. C.; Heitmann, H.; Hello, P.; Hemming, G.; Hendry, M.; Heng, I. S.; Hennig, J.; Henry, J.; Heptonstall, A. W.; Heurs, M.; Hild, S.; Hoak, D.; Hofman, D.; Holt, K.; Holz, D. E.; Hopkins, P.; Horst, C.; Hough, J.; Houston, E. A.; Howell, E. J.; Hu, Y. M.; Huerta, E. A.; Huet, D.; Hughey, B.; Husa, S.; Huttner, S. H.; Huynh-Dinh, T.; Indik, N.; Ingram, D. R.; Inta, R.; Intini, G.; Isa, H. N.; Isac, J.-M.; Isi, M.; Iyer, B. R.; Izumi, K.; Jacqmin, T.; Jani, K.; Jaranowski, P.; Jawahar, S.; Jiménez-Forteza, F.; Johnson, W. W.; Jones, D. I.; Jones, R.; Jonker, R. J. G.; Ju, L.; Junker, J.; Kalaghatgi, C. V.; Kalogera, V.; Kandhasamy, S.; Kang, G.; Kanner, J. B.; Karki, S.; Karvinen, K. S.; Kasprzack, M.; Katolik, M.; Katzman, W.; Kaufer, S.; Kawabe, K.; Kéfélian, F.; Keitel, D.; Kemball, A. J.; Kennedy, R.; Kent, C.; Key, J. S.; Khalili, F. Y.; Khan, I.; Khan, S.; Khan, Z.; Khazanov, E. A.; Kijbunchoo, N.; Kim, Chunglee; Kim, J. C.; Kim, W.; Kim, W. S.; Kim, Y.-M.; Kimbrell, S. J.; King, E. J.; King, P. J.; Kirchhoff, R.; Kissel, J. S.; Kleybolte, L.; Klimenko, S.; Koch, P.; Koehlenbeck, S. M.; Koley, S.; Kondrashov, V.; Korobko, M.; Korth, W. Z.; Kowalska, I.; Kozak, D. B.; Krämer, C.; Kringel, V.; Krishnan, B.; Królak, A.; Kuehn, G.; Kumar, P.; Kumar, R.; Kumar, S.; Kuo, L.; Kutynia, A.; Kwang, S.; Lackey, B. D.; Lai, K. H.; Landry, M.; Lang, R. N.; Lange, J.; Lantz, B.; Lartaux-Vollard, A.; Lasky, P. D.; Laxen, M.; Lazzarini, A.; Lazzaro, C.; Leaci, P.; Leavey, S.; Lee, C. H.; Lee, H. K.; Lee, H. M.; Lee, H. W.; Lee, K.; Lehmann, J.; Lenon, A.; Leonardi, M.; Leroy, N.; Letendre, N.; Levin, Y.; Li, T. G. F.; Littenberg, T. B.; Liu, J.; Lo, R. K. L.; Lockerbie, N. A.; London, L. T.; Lord, J. E.; Lorenzini, M.; Loriette, V.; Lormand, M.; Losurdo, G.; Lough, J. D.; Lousto, C. O.; Lovelace, G.; Lück, H.; Lumaca, D.; Lundgren, A. P.; Ma, Y.; Macfoy, S.; Machenschalk, B.; Macleod, D. M.; Magaña Hernandez, I.; Magaña-Sandoval, F.; Magaña Zertuche, L.; Magee, R. M.; Majorana, E.; Maksimovic, I.; Man, N.; Mandic, V.; Mangano, V.; Mansell, G. L.; Manske, M.; Mantovani, M.; Marchesoni, F.; Marion, F.; Márka, S.; Márka, Z.; Markakis, C.; Markosyan, A. S.; Maros, E.; Martelli, F.; Martellini, L.; Martin, I. W.; Masserot, A.; Massinger, T. J.; Masso-Reid, M.; Mastrogiovanni, S.; Matas, A.; Matone, L.; Mazumder, N.; McCarthy, R.; McClelland, D. E.; McCormick, S.; McGuire, S. C.; McIntyre, G.; McIver, J.; McManus, D. J.; McRae, T.; McWilliams, S. T.; Meacher, D.; Meadors, G. D.; Meidam, J.; Mejuto-Villa, E.; Melatos, A.; Mendell, G.; Mercer, R. A.; Merilh, E. L.; Merzougui, M.; Meshkov, S.; Messenger, C.; Messick, C.; Metzdorff, R.; Meyers, P. M.; Mezzani, F.; Miao, H.; Michel, C.; Middleton, H.; Mikhailov, E. E.; Milano, L.; Miller, A. L.; Miller, A.; Miller, B. B.; Millhouse, M.; Minazzoli, O.; Minenkov, Y.; Ming, J.; Mishra, C.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher, G.; Moggi, A.; Mohan, M.; Montani, M.; Moore, B. C.; Moore, C. J.; Moraru, D.; Moreno, G.; Morriss, S. R.; Mours, B.; Mow-Lowry, C. M.; Mueller, G.; Muir, A. W.; Mukherjee, Arunava; Mukherjee, D.; Mukherjee, S.; Mukund, N.; Mullavey, A.; Munch, J.; Muniz, E. A. M.; Murray, P. G.; Napier, K.; Nardecchia, I.; Naticchioni, L.; Nayak, R. K.; Nelemans, G.; Nelson, T. J. N.; Neri, M.; Nery, M.; Neunzert, A.; Newport, J. M.; Newton, G.; Ng, K. K. Y.; Nguyen, T. T.; Nichols, D.; Nielsen, A. B.; Nissanke, S.; Nitz, A.; Noack, A.; Nocera, F.; Nolting, D.; Normandin, M. E. N.; Nuttall, L. K.; Oberling, J.; Ochsner, E.; Ogin, G. H.; Oh, J. J.; Oh, S. H.; Ohme, F.; Oliver, M.; Oppermann, P.; Oram, Richard J.; O’Reilly, B.; Ormiston, R.; Ortega, L. F.; O’Shaughnessy, R.; Ottaway, D. J.; Overmier, H.; Owen, B. J.; Pace, A. E.; Page, J.; Page, M. A.; Pai, A.; Pai, S. A.; Palamos, J. R.; Palashov, O.; Palomba, C.; Pal-Singh, A.; Pan, H.; Pang, B.; Pang, P. T. H.; Pankow, C.; Pannarale, F.; Pant, B. C.; Paoletti, F.; Paoli, A.; Papa, M. A.; Paris, H. R.; Parker, W.; Pascucci, D.; Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Patricelli, B.; Pearlstone, B. L.; Pedraza, M.; Pedurand, R.; Pekowsky, L.; Pele, A.; Penn, S.; Perez, C. J.; Perreca, A.; Perri, L. M.; Pfeiffer, H. P.; Phelps, M.; Piccinni, O. J.; Pichot, M.; Piergiovanni, F.; Pierro, V.; Pillant, G.; Pinard, L.; Pinto, I. M.; Pitkin, M.; Poggiani, R.; Popolizio, P.; Porter, E. K.; Post, A.; Powell, J.; Prasad, J.; Pratt, J. W. W.; Predoi, V.; Prestegard, T.; Prijatelj, M.; Principe, M.; Privitera, S.; Prix, R.; Prodi, G. A.; Prokhorov, L. G.; Puncken, O.; Punturo, M.; Puppo, P.; Pürrer, M.; Qi, H.; Qin, J.; Qiu, S.; Quetschke, V.; Quintero, E. A.; Quitzow-James, R.; Raab, F. J.; Rabeling, D. S.; Radkins, H.; Raffai, P.; Raja, S.; Rajan, C.; Rakhmanov, M.; Ramirez, K. E.; Rapagnani, P.; Raymond, V.; Razzano, M.; Read, J.; Regimbau, T.; Rei, L.; Reid, S.; Reitze, D. H.; Rew, H.; Reyes, S. D.; Ricci, F.; Ricker, P. M.; Rieger, S.; Riles, K.; Rizzo, M.; Robertson, N. A.; Robie, R.; Robinet, F.; Rocchi, A.; Rolland, L.; Rollins, J. G.; Roma, V. J.; Romano, J. D.; Romano, R.; Romel, C. L.; Romie, J. H.; Rosińska, D.; Ross, M. P.; Rowan, S.; Rüdiger, A.; Ruggi, P.; Ryan, K.; Sachdev, S.; Sadecki, T.; Sadeghian, L.; Sakellariadou, M.; Salconi, L.; Saleem, M.; Salemi, F.; Samajdar, A.; Sammut, L.; Sampson, L. M.; Sanchez, E. J.; Sandberg, V.; Sandeen, B.; Sanders, J. R.; Sassolas, B.; Saulson, P. R.; Sauter, O.; Savage, R. L.; Sawadsky, A.; Schale, P.; Scheuer, J.; Schmidt, E.; Schmidt, J.; Schmidt, P.; Schnabel, R.; Schofield, R. M. S.; Schönbeck, A.; Schreiber, E.; Schuette, D.; Schulte, B. W.; Schutz, B. F.; Schwalbe, S. G.; Scott, J.; Scott, S. M.; Seidel, E.; Sellers, D.; Sengupta, A. S.; Sentenac, D.; Sequino, V.; Sergeev, A.; Shaddock, D. A.; Shaffer, T. J.; Shah, A. A.; Shahriar, M. S.; Shao, L.; Shapiro, B.; Shawhan, P.; Sheperd, A.; Shoemaker, D. M.; Siellez, K.; Siemens, X.; Sieniawska, M.; Sigg, D.; Silva, A. D.; Singer, A.; Singer, L. P.; Singh, A.; Singh, R.; Singhal, A.; Sintes, A. M.; Slagmolen, B. J. J.; Smith, B.; Smith, J. R.; Smith, R. J. E.; Son, E. J.; Sonnenberg, J. A.; Sorazu, B.; Sorrentino, F.; Souradeep, T.; Spencer, A. P.; Srivastava, A. K.; Staley, A.; Steer, D. A.; Steinke, M.; Steinlechner, J.; Steinlechner, S.; Steinmeyer, D.; Stephens, B. C.; Stone, R.; Strain, K. A.; Stratta, G.; Strigin, S. E.; Sturani, R.; Stuver, A. L.; Summerscales, T. Z.; Sun, L.; Sunil, S.; Sutton, P. J.; Swinkels, B. L.; Szczepańczyk, M. J.; Tacca, M.; Talukder, D.; Tanner, D. B.; Tápai, M.; Taracchini, A.; Taylor, J. A.; Taylor, R.; Theeg, T.; Thomas, E. G.; Thomas, M.; Thomas, P.; Thorne, K. A.; Thorne, K. S.; Thrane, E.; Tiwari, S.; Tiwari, V.; Tokmakov, K. V.; Toland, K.; Tonelli, M.; Tornasi, Z.; Torrie, C. I.; Töyrä, D.; Travasso, F.; Traylor, G.; Trifirò, D.; Trinastic, J.; Tringali, M. C.; Trozzo, L.; Tsang, K. W.; Tso, R.; Tuyenbayev, D.; Ueno, K.; Ugolini, D.; Unnikrishnan, C. S.; Urban, A. L.; Usman, S. A.; Vahlbruch, H.; Vajente, G.; Valdes, G.; Vallisneri, M.; van Bakel, N.; van Beuzekom, M.; van den Brand, J. F. J.; Van Den Broeck, C.; Vander-Hyde, D. C.; van der Schaaf, L.; van Heijningen, J. V.; van Veggel, A. A.; Vardaro, M.; Varma, V.; Vass, S.; Vasúth, M.; Vecchio, A.; Vedovato, G.; Veitch, J.; Veitch, P. J.; Venkateswara, K.; Venugopalan, G.; Verkindt, D.; Vetrano, F.; Viceré, A.; Viets, A. D.; Vinciguerra, S.; Vine, D. J.; Vinet, J.-Y.; Vo, T.; Vocca, H.; Vorvick, C.; Voss, D. V.; Vousden, W. D.; Vyatchanin, S. P.; Wade, A. R.; Wade, L. E.; Wade, M.; Walet, R.; Walker, M.; Wallace, L.; Walsh, S.; Wang, G.; Wang, H.; Wang, J. Z.; Wang, M.; Wang, Y.-F.; Wang, Y.; Ward, R. L.; Warner, J.; Was, M.; Watchi, J.; Weaver, B.; Wei, L.-W.; Weinert, M.; Weinstein, A. J.; Wen, L.; Wessel, E. K.; Weßels, P.; Westphal, T.; Wette, K.; Whelan, J. T.; Whiting, B. F.; Whittle, C.; Williams, D.; Williams, R. D.; Williamson, A. R.; Willis, J. L.; Willke, B.; Wimmer, M. H.; Winkler, W.; Wipf, C. C.; Wittel, H.; Woan, G.; Woehler, J.; Wofford, J.; Wong, K. W. K.; Worden, J.; Wright, J. L.; Wu, D. S.; Wu, G.; Yamamoto, H.; Yancey, C. C.; Yap, M. J.; Yvert, M.; Zadrożny, A.; Zanolin, M.; Zelenova, T.; Zendri, J.-P.; Zevin, M.; Zhang, L.; Zhang, M.; Zhang, T.; Zhang, Y.-H.; Zhao, C.; Zhou, M.; Zhou, Z.; Zhu, S. J.; Zhu, X. J.; Zweizig, J.; LIGO Scientific Collaboration; Virgo Collaboration; Aggarwal, Nancy; Barsotti, Lisa; Biscans, Sebastien; Brown, N. M.; Buikema, Aaron; Donovan, Frederick J; Eisenstein, Robert Alan; Essick, Reed Clasey; Evans, Matthew J; Fernandez Galiana, Alvaro-Miguel; Fritschel, Peter K; Gras, Slawomir; Katsavounidis, Erotokritos; Kontos, Antonios; Lanza Jr, Robert K; Libson, Adam A.; Lynch, Ryan Christopher; MacInnis, Myron E; Martynov, Denis; Mason, Kenneth R; Matichard, Fabrice; Mavalvala, Nergis; McCuller, Lee P; Miller, John; Mittleman, Richard K; Ray Pitambar Mohapatra, Satyanarayan; Oelker, Eric Glenn; Shoemaker, David H; Tse, Maggie; Vitale, Salvatore; Weiss, Rainer; Yam, William; Yu, Hang; Yu, Haocun; Zucker, Michael E
    Cosmic strings are topological defects which can be formed in grand unified theory scale phase transitions in the early universe. They are also predicted to form in the context of string theory. The main mechanism for a network of Nambu-Goto cosmic strings to lose energy is through the production of loops and the subsequent emission of gravitational waves, thus offering an experimental signature for the existence of cosmic strings. Here we report on the analysis conducted to specifically search for gravitational-wave bursts from cosmic string loops in the data of Advanced LIGO 2015-2016 observing run (O1). No evidence of such...

  19. Constraints on cosmic strings using data from the first Advanced LIGO observing run

    Abbott, B. P.; Abbott, R.; Adhikari, R. X.; Ananyeva, A.; Anderson, S. B.; Appert, S.; Arai, K.; Araya, M. C.; Barayoga, J. C.; Barish, B. C.; Berger, B. K.; Billingsley, G.; Blackburn, J. K.; Bork, R.; Brooks, A. F.; Brunett, S.; Cahillane, C.; Callister, T. A.; Cepeda, C. B.; Couvares, P.; Coyne, D. C.; Drever, R. W. P.; Ehrens, P.; Eichholz, J.; Etzel, T.; Feicht, J.; Fries, E. M.; Gossan, S. E.; Gushwa, K. E.; Gustafson, E. K.; Hall, E. D.; Heptonstall, A. W.; Isi, M.; Kanner, J. B.; Kondrashov, V.; Korth, W. Z.; Kozak, D. B.; Lazzarini, A.; Maros, E.; Massinger, T. J.; McIntyre, G.; McIver, J.; Meshkov, S.; Pedraza, M.; Quintero, E. A.; Reitze, D. H.; Robertson, N. A.; Rollins, J. G.; Sachdev, S.; Sanchez, E. J.; Schmidt, P.; Singer, A.; Smith, R. J. E.; Taylor, R.; Torrie, C. I.; Tso, R.; Urban, A. L.; Vajente, G.; Vass, S.; Venugopalan, G.; Wade, A. R.; Wallace, L.; Weinstein, A. J.; Williams, R. D.; Wipf, C. C.; Yamamoto, H.; Zhang, L.; Zucker, M. E.; Zweizig, J.; Blackman, J.; Chen, Y.; Ma, Y.; Pang, B.; Thorne, K. S.; Vallisneri, M.; Varma, V.
    Cosmic strings are topological defects which can be formed in grand unified theory scale phase transitions in the early universe. They are also predicted to form in the context of string theory. The main mechanism for a network of Nambu-Goto cosmic strings to lose energy is through the production of loops and the subsequent emission of gravitational waves, thus offering an experimental signature for the existence of cosmic strings. Here we report on the analysis conducted to specifically search for gravitational-wave bursts from cosmic string loops in the data of Advanced LIGO 2015-2016 observing run (O1). No evidence of such...

  20. Constraining Alternative Theories of Gravity Using Pulsar Timing Arrays

    Cornish, Neil J.; O’Beirne, Logan; Taylor, Stephen R.; Yunes, Nicolás
    The opening of the gravitational wave window by ground-based laser interferometers has made possible many new tests of gravity, including the first constraints on polarization. It is hoped that, within the next decade, pulsar timing will extend the window by making the first detections in the nanohertz frequency regime. Pulsar timing offers several advantages over ground-based interferometers for constraining the polarization of gravitational waves due to the many projections of the polarization pattern provided by the different lines of sight to the pulsars, and the enhanced response to longitudinal polarizations. Here, we show that existing results from pulsar timing arrays...

Aviso de cookies: Usamos cookies propias y de terceros para mejorar nuestros servicios, para análisis estadístico y para mostrarle publicidad. Si continua navegando consideramos que acepta su uso en los términos establecidos en la Política de cookies.