Showing papers by "Liam Cunningham published in 2011"
20 May 2011
TL;DR: In this article, the conceptual design of a third generation gravitational wave observatory named the Einstein Telescope (ET) has been described with the support of the European Community's Seventh Framework Programme (FP7/2007-2013) under grant agreement n 211743.
Abstract: This document describes the Conceptual Design of a third generation gravitational wave observatory named Einstein Telescope (“ET”). The design of this new research infrastructure has been realised with the support of the European Community’s Seventh Framework Programme (FP7/2007-2013) under grant agreement n 211743. In this document are described the fundamental design options, the site requirements, the main technological solutions, a rough evaluation of the costs and a schematic time plan.
192 citations
01 Jun 2011
105 citations
TL;DR: In this paper, a low-latency analysis pipeline was used to identify and localize GW event candidates and to request images of targeted sky locations, where a catalog of nearby galaxies and Milky Way globular clusters were used to select the most promising sky positions to be imaged.
Abstract: Aims. A transient astrophysical event observed in both gravitational wave (GW) and electromagnetic (EM) channels would yield rich scientific rewards. A first program initiating EM follow-ups to possible transient GW events has been developed and exercised by the LIGO and Virgo community in association with several partners. In this paper, we describe and evaluate the methods used to promptly identify and localize GW event candidates and to request images of targeted sky locations.
Methods. During two observing periods (Dec 17 2009 to Jan 8 2010 and Sep 2 to Oct 20 2010), a low-latency analysis pipeline was used to identify GW event candidates and to reconstruct maps of possible sky locations. A catalog of nearby galaxies and Milky Way globular clusters was used to select the most promising sky positions to be imaged, and this directional information was delivered to EM observatories with time lags of about thirty minutes. A Monte Carlo simulation has been used to evaluate the low-latency GW pipeline's ability to reconstruct source positions correctly.
Results. For signals near the detection threshold, our low-latency algorithms often localized simulated GW burst signals to tens of square degrees, while neutron star/neutron star inspirals and neutron star/black hole inspirals were localized to a few hundred square degrees. Localization precision improves for moderately stronger signals. The correct sky location of signals well above threshold and originating from nearby galaxies may be observed with ~50% or better probability with a few pointings of wide-field telescopes.
104 citations
TL;DR: In this article, direct upper limits on continuous gravitational wave emission from the Vela pulsar using data from the Virgo detector's second science run were obtained using three independent methods.
Abstract: We present direct upper limits on continuous gravitational wave emission from the Vela pulsar using data from the Virgo detector's second science run. These upper limits have been obtained using three independent methods that assume the gravitational wave emission follows the radio timing. Two of the methods produce frequentist upper limits for an assumed known orientation of the star's spin axis and value of the wave polarization angle of, respectively, $1.9\ee{-24}$ and $2.2\ee{-24}$, with 95% confidence. The third method, under the same hypothesis, produces a Bayesian upper limit of $2.1\ee{-24}$, with 95% degree of belief. These limits are below the indirect {\it spin-down limit} of $3.3\ee{-24}$ for the Vela pulsar, defined by the energy loss rate inferred from observed decrease in Vela's spin frequency, and correspond to a limit on the star ellipticity of $\sim 10^{-3}$. Slightly less stringent results, but still well below the spin-down limit, are obtained assuming the star's spin axis inclination and the wave polarization angles are unknown.
78 citations
TL;DR: In this paper, the authors present a survey of the state-of-the-art work in this area, including the following: A.A. Adhikari, P.B. Abadie, B.Babak, A.C. Anderson, W.M. Brandes, M.Barriga, E.C., A.B., C.C, C.Chaibi, O.Chakrabarty, O'Brien, O.'Brien, S.Capellaro, O 'Brien, T.
Abstract: J. Abadie, B. P. Abbott, R. Abbott, M. Abernathy, T. Accadia, F. Acernese, C. Adams, R. Adhikari, P. Ajith, B. Allen, G. S. Allen, E. Amador Ceron, R. S. Amin, S. B. Anderson, W.G. Anderson, F. Antonucci, M.A. Arain, M. C. Araya, M. Aronsson, Y. Aso, S.M. Aston, P. Astone, D. Atkinson, P. Aufmuth, C. Aulbert, S. Babak, P. Baker, G. Ballardin, T. Ballinger, S. Ballmer, D. Barker, S. Barnum, F. Barone, B. Barr, P. Barriga, L. Barsotti, M. Barsuglia, M.A. Barton, I. Bartos, R. Bassiri, M. Bastarrika, J. Bauchrowitz, Th. S. Bauer, B. Behnke, M.G. Beker, A. Belletoile, M. Benacquista, A. Bertolini, J. Betzwieser, N. Beveridge, P. T. Beyersdorf, I. A. Bilenko, G. Billingsley, J. Birch, S. Birindelli, R. Biswas, M. Bitossi, M.A. Bizouard, E. Black, J. K. Blackburn, L. Blackburn, D. Blair, B. Bland, M. Blom, C. Boccara, O. Bock, T. P. Bodiya, R. Bondarescu, F. Bondu, L. Bonelli, R. Bonnand, R. Bork, M. Born, V. Boschi, S. Bose, L. Bosi, B. Bouhou, M. Boyle, S. Braccini, C. Bradaschia, P. R. Brady, V. B. Braginsky, J. E. Brau, J. Breyer, D.O. Bridges, A. Brillet, M. Brinkmann, V. Brisson, M. Britzger, A. F. Brooks, D. A. Brown, R. Budzynski, T. Bulik, H. J. Bulten, A. Buonanno, J. Burguet–Castell, O. Burmeister, D. Buskulic, C. Buy, R. L. Byer, L. Cadonati, G. Cagnoli, J. Cain, E. Calloni, J. B. Camp, E. Campagna, P. Campsie, J. Cannizzo, K. Cannon, B. Canuel, J. Cao, C. Capano, F. Carbognani, S. Caride, S. Caudill, M. Cavaglia, F. Cavalier, R. Cavalieri, G. Cella, C. Cepeda, E. Cesarini, O. Chaibi, T. Chalermsongsak, E. Chalkley, P. Charlton, E. Chassande-Mottin, S. Chelkowski, Y. Chen, A. Chincarini, N. Christensen, S. S. Y. Chua, C. T.Y. Chung, D. Clark, J. Clark, J. H. Clayton, F. Cleva, E. Coccia, C. N. Colacino, J. Colas, A. Colla, M. Colombini, R. Conte, D. Cook, T. R. Corbitt, N. Cornish, A. Corsi, C. A. Costa, J.-P. Coulon, D.M. Coward, D. C. Coyne, J. D. E. Creighton, T.D. Creighton, A.M. Cruise, R.M. Culter, A. Cumming, L. Cunningham, E. Cuoco, K. Dahl, S. L. Danilishin, R. Dannenberg, S. D’Antonio, K. Danzmann, K. Das, V. Dattilo, B. Daudert, M. Davier, G. Davies, A. Davis, E. J. Daw, R. Day, T. Dayanga, R. De Rosa, D. DeBra, G. Debreczeni, J. Degallaix, M. del Prete, V. Dergachev, R. DeRosa, R. DeSalvo, P. Devanka, S. Dhurandhar, L. Di Fiore, A. Di Lieto, I. Di Palma, M. Di Paolo Emilio, A. Di Virgilio, M. Diaz, A. Dietz, F. Donovan, K. L. Dooley, E. E. Doomes, S. Dorsher, E. S. D. Douglas, M. Drago, R.W. P. Drever, J. C. Driggers, J. Dueck, J.-C. Dumas, S. Dwyer, T. Eberle, M. Edgar, M. Edwards, A. Effler, P. Ehrens, G. Ely, R. Engel, T. Etzel, M. Evans, T. Evans, V. Fafone, S. Fairhurst, Y. Fan, B. F. Farr, D. Fazi, H. Fehrmann, D. Feldbaum, I. Ferrante, F. Fidecaro, L. S. Finn, I. Fiori, R. Flaminio, M. Flanigan, K. Flasch, S. Foley, C. Forrest, E. Forsi, L. A. Forte, N. Fotopoulos, J.-D. Fournier, J. Franc, S. Frasca, F. Frasconi, M. Frede, M. Frei, Z. Frei, A. Freise, R. Frey, T. T. Fricke, D. Friedrich, P. Fritschel, V. V. Frolov, P. Fulda, M. Fyffe, M. Galimberti, L. Gammaitoni, J. A. Garofoli, F. Garufi, M. E. Gaspar, G. Gemme, E. Genin, A. Gennai, I. Gholami, S. Ghosh, J. A. Giaime, S. Giampanis, K. D. Giardina, A. Giazotto, C. Gill, E. Goetz, L.M. Goggin, G. Gonzalez, M. L. Gorodetsky, S. Gosler, R. Gouaty, C. Graef, M. Granata, A. Grant, S. Gras, C. Gray, R. J. S. Greenhalgh, A.M. Gretarsson, C. Greverie, R. Grosso, H. Grote, S. Grunewald, G.M. Guidi, E. K. Gustafson, R. Gustafson, B. Hage, P. Hall, J.M. Hallam, D. Hammer, G. Hammond, J. Hanks, C. Hanna, J. Hanson, J. Harms, G.M. Harry, I.W. Harry, E. D. Harstad, K. Haughian, K. Hayama, J.-F. Hayau, T. Hayler, J. Heefner, H. Heitmann, P. Hello, I. S. Heng, A.W. Heptonstall, M. Hewitson, S. Hild, E. Hirose, D. Hoak, K. A. Hodge, K. Holt, D. J. Hosken, J. Hough, E. J. Howell, D. Hoyland, D. Huet, B. Hughey, S. Husa, S. H. Huttner, T. Huynh–Dinh, D. R. Ingram, R. Inta, T. Isogai, A. Ivanov, P. Jaranowski, W.W. Johnson, D. I. Jones, G. Jones, R. Jones, L. Ju, P. Kalmus, V. Kalogera, S. Kandhasamy, J. B. Kanner, E. Katsavounidis, K. Kawabe, S. Kawamura, F. Kawazoe, W. Kells, D.G. Keppel, A. Khalaidovski, F. Y. Khalili, E. A. Khazanov, H. Kim, P. J. King, D. L. Kinzel, J. S. Kissel, S. Klimenko, V. Kondrashov, R. Kopparapu, S. Koranda, I. Kowalska, D. Kozak, T. Krause, V. Kringel, S. Krishnamurthy, B. Krishnan, A. Krolak, G. Kuehn, J. Kullman, R. Kumar, P. Kwee, M. Landry, M. Lang, B. Lantz, N. Lastzka, A. Lazzarini, P. Leaci, J. Leong, I. Leonor, N. Leroy, N. Letendre, J. Li, T. G. F. Li, N. Liguori, H. Lin, P. E. Lindquist, N. A. Lockerbie, D. Lodhia, M. Lorenzini, V. Loriette, M. Lormand, G. Losurdo, P. Lu, J. Luan, M. Lubinski, A. Lucianetti, H. Luck, A.D. Lundgren, B. Machenschalk, M. MacInnis, M. Mageswaran, K. Mailand, E. Majorana, C. Mak, I. Maksimovic, N. Man, I. Mandel, V. Mandic, M. Mantovani, F. Marchesoni, F. Marion, S. Marka, Z. Marka, E. Maros, J. Marque, F. Martelli, I.W. Martin, R.M. Martin, J. N. Marx, K. Mason, A. Masserot, F. Matichard, L. Matone, R. A. Matzner, N. Mavalvala, R. McCarthy, D. E. McClelland, S. C. McGuire, G. McIntyre, G. McIvor, D. J. A. McKechan, G. Meadors, M. Mehmet, T. Meier, A. Melatos, A. C. Melissinos, G. Mendell, D. F. Menendez, R. A. Mercer, L. Merill, S. Meshkov, C. Messenger, M. S. Meyer, H. Miao, C. Michel, L. Milano, J. Miller, Y. Minenkov, Y. Mino, S. Mitra, V. P. Mitrofanov, G. Mitselmakher, R. Mittleman, B. Moe, M. Mohan, S. D. Mohanty, S. R. P. Mohapatra, D. Moraru, PHYSICAL REVIEW D 85, 089904(E) (2012)
63 citations
Posted Content•
TL;DR: Einstein gravitational-wave Telescope (ET) is a design study funded by the European Commission to explore the technological challenges of and scientific benefits from building a third generation gravitational wave detector as discussed by the authors.
Abstract: Einstein gravitational-wave Telescope (ET) is a design study funded by the European Commission to explore the technological challenges of and scientific benefits from building a third generation gravitational wave detector. The three-year study, which concluded earlier this year, has formulated the conceptual design of an observatory that can support the implementation of new technology for the next two to three decades. The goal of this talk is to introduce the audience to the overall aims and objectives of the project and to enumerate ET's potential to influence our understanding of fundamental physics, astrophysics and cosmology.
22 citations
01 Mar 2011
TL;DR: A.J. Abadie, B. Abbott, R. Adhikari, P. Allen, E. Barriga, L. Barsotti, M. Bock, T. Blair, D. Donovan, K. Frei, A. Freisinger, C. Freise, S. Fricke, J. Friedrich, P Fritschel, V. Fairhurst, Y.
9 citations
University of Glasgow1, University of Salerno2, Spanish National Research Council3, Albert Einstein Institution4, University of Southampton5, Université Paris-Saclay6, PSL Research University7, Washington State University8, University of Warsaw9, University of Naples Federico II10, University of Birmingham11, Cardiff University12, University of Rome Tor Vergata13, Moscow State University14, Leibniz University of Hanover15, California Institute of Technology16, VU University Amsterdam17, fondazione bruno kessler18, University of Cambridge19, University of Tübingen20, University of Urbino21, University of Jena22, University of Florence23, Massachusetts Institute of Technology24, University of Minnesota25, University of Savoy26, Pennsylvania State University27, University of Pisa28, Roma Tre University29, Sapienza University of Rome30, University of Mississippi31, University of the Balearic Islands32
TL;DR: The advanced interferometer network will herald a new era in observational astronomy as mentioned in this paper, and there is a very strong science case to go beyond the advanced detector network and build detectors that operate in a frequency range from 1 Hz to 10 kHz, with sensitivity a factor 10 better in amplitude.
Abstract: The advanced interferometer network will herald a new era in observational astronomy. There is a very strong science case to go beyond the advanced detector network and build detectors that operate in a frequency range from
1 Hz to 10 kHz, with sensitivity a factor 10 better in amplitude. Such detectors will be able to probe a range of topics in nuclear physics, astronomy, cosmology
and fundamental physics, providing insights into many unsolved problems in these areas.
8 citations
Journal Article•
TL;DR: In this article, the authors present a survey of the state-of-the-art work in this area: A.A. Adhikari, P. A. Ajith, B. Barriga, S.A., A.B. Bennett, J.C. Dooley, E.M. Brandt, J-C. Hohenberger, M.E.Charlton, N.C., C.Chua, C.C, T.Chung, D.Chakrabarty, D-C., D.
Abstract: J. Abadie, B. P. Abbott, R. Abbott, R. Adhikari, P. Ajith, B. Allen, G. Allen, E. Amador Ceron, R. S. Amin, S. B. Anderson, W.G. Anderson, M.A. Arain, M. Araya, Y. Aso, S. Aston, P. Aufmuth, C. Aulbert, S. Babak, P. Baker, S. Ballmer, D. Barker, B. Barr, P. Barriga, L. Barsotti, M.A. Barton, I. Bartos, R. Bassiri, M. Bastarrika, B. Behnke, M. Benacquista, M. F. Bennett, J. Betzwieser, P. T. Beyersdorf, I. A. Bilenko, G. Billingsley, R. Biswas, E. Black, J. K. Blackburn, L. Blackburn, D. Blair, B. Bland, O. Bock, T. P. Bodiya, R. Bondarescu, R. Bork, M. Born, S. Bose, P. R. Brady, V. B. Braginsky, J. E. Brau, J. Breyer, D.O. Bridges, M. Brinkmann, M. Britzger, A. F. Brooks, D.A. Brown, A. Bullington, A. Buonanno, O. Burmeister, R. L. Byer, L. Cadonati, J. Cain, J. B. Camp, J. Cannizzo, K. C. Cannon, J. Cao, C. Capano, L. Cardenas, S. Caudill, M. Cavaglià, C. Cepeda, T. Chalermsongsak, E. Chalkley, P. Charlton, S. Chatterji, S. Chelkowski, Y. Chen, N. Christensen, S. S. Y. Chua, C. T. Y. Chung, D. Clark, J. Clark, J. H. Clayton, R. Conte, D. Cook, T. R. C. Corbitt, N. Cornish, D. Coward, D. C. Coyne, J. D. E. Creighton, T. D. Creighton, A.M. Cruise, R.M. Culter, A. Cumming, L. Cunningham, K. Dahl, S. L. Danilishin, K. Danzmann, B. Daudert, G. Davies, E. J. Daw, T. Dayanga, D. DeBra, J. Degallaix, V. Dergachev, R. DeSalvo, S. Dhurandhar, M. Dı́az, F. Donovan, K. L. Dooley, E. E. Doomes, R.W. P. Drever, J. Driggers, J. Dueck, I. Duke, J.-C. Dumas, S. Dwyer, M. Edgar, M. Edwards, A. Effler, P. Ehrens, T. Etzel, M. Evans, T. Evans, S. Fairhurst, Y. Faltas, Y. Fan, D. Fazi, H. Fehrmann, L. S. Finn, K. Flasch, S. Foley, C. Forrest, N. Fotopoulos, M. Frede, M. Frei, Z. Frei, A. Freise, R. Frey, T. T. Fricke, D. Friedrich, P. Fritschel, V. V. Frolov, P. Fulda, M. Fyffe, J. A. Garofoli, S. Ghosh, J. A. Giaime, S. Giampanis, K.D. Giardina, E. Goetz, L.M. Goggin, G. González, S. Goßler, A. Grant, S. Gras, C. Gray, R. J. S. Greenhalgh, A.M. Gretarsson, R. Grosso, H. Grote, S. Grunewald, E. K. Gustafson, R. Gustafson, B. Hage, J.M. Hallam, D. Hammer, G. D. Hammond, C. Hanna, J. Hanson, J. Harms, G.M. Harry, I.W. Harry, E. D. Harstad, K. Haughian, K. Hayama, T. Hayler, J. Heefner, I. S. Heng, A. Heptonstall, M. Hewitson, S. Hild, E. Hirose, D. Hoak, K. A. Hodge, K. Holt, D. J. Hosken, J. Hough, E. Howell, D. Hoyland, B. Hughey, S. Husa, S. H. Huttner, D. R. Ingram, T. Isogai, A. Ivanov, W.W. Johnson, D. I. Jones, G. Jones, R. Jones, L. Ju, P. Kalmus, V. Kalogera, S. Kandhasamy, J. Kanner, E. Katsavounidis, K. Kawabe, S. Kawamura, F. Kawazoe, W. Kells, D. G. Keppel, A. Khalaidovski, F. Y. Khalili, R. Khan, E. Khazanov, H. Kim, P. J. King, J. S. Kissel, S. Klimenko, K. Kokeyama, V. Kondrashov, R. Kopparapu, S. Koranda, D. Kozak, V. Kringel, B. Krishnan, G. Kuehn, J. Kullman, R. Kumar, P. Kwee, P. K. Lam, M. Landry, M. Lang, B. Lantz, N. Lastzka, A. Lazzarini, P. Leaci, M. Lei, N. Leindecker, I. Leonor, H. Lin, P. E. Lindquist, T. B. Littenberg, N.A. Lockerbie, D. Lodhia, M. Lormand, P. Lu, M. Lubinski, A. Lucianetti, H. Lück, A. Lundgren, B. Machenschalk, M. MacInnis, M. Mageswaran, K. Mailand, C. Mak, I. Mandel, V. Mandic, S. Márka, Z. Márka, A. Markosyan, J. Markowitz, E. Maros, I.W. Martin, R.M. Martin, J. N. Marx, K. Mason, F. Matichard, L. Matone, R. A. Matzner, N. Mavalvala, R. McCarthy, D. E. McClelland, S. C. McGuire, G. McIntyre, D. J. A. McKechan, M. Mehmet, A. Melatos, A. C. Melissinos, G. Mendell, D. F. Menéndez, R. A. Mercer, L. Merrill, S. Meshkov, C. Messenger, M. S. Meyer, H. Miao, J. Miller, Y. Mino, S. Mitra, V. P. Mitrofanov, G. Mitselmakher, R. Mittleman, O. Miyakawa, B. Moe, S. D. Mohanty, S. R. P. Mohapatra, G. Moreno, K. Mors, K. Mossavi, C. MowLowry, G. Mueller, H. Müller-Ebhardt, S. Mukherjee, A. Mullavey, J. Munch, P. G. Murray, T. Nash, R. Nawrodt, J. Nelson, G. Newton, E. Nishida, A. Nishizawa, J. O’Dell, B. O’Reilly, R. O’Shaughnessy, E. Ochsner, G.H. Ogin, R. Oldenburg, D. J. Ottaway, R. S. Ottens, H. Overmier, B. J. Owen, A. Page, Y. Pan, C. Pankow, M.A. Papa, P. Patel, D. Pathak, M. Pedraza, L. Pekowsky, S. Penn, C. Peralta, A. Perreca, M. Pickenpack, I.M. Pinto, M. Pitkin, H. J. Pletsch, M.V. Plissi, F. Postiglione, M. Principe, R. Prix, L. Prokhorov, O. Puncken, V. Quetschke, F. J. Raab, D. S. Rabeling, H. Radkins, P. Raffai, Z. Raics, M. Rakhmanov, V. Raymond, C.M. Reed, T. Reed, H. Rehbein, S. Reid, D.H. Reitze, R. Riesen, K. Riles, P. Roberts, N.A. Robertson, C. Robinson, E. L. Robinson, S. Roddy, C. Röver, J. Rollins, J. D. Romano, J. H. Romie, S. Rowan, A. Rüdiger, K. Ryan, S. Sakata, L. Sammut, L. Sancho de la Jordana, V. Sandberg, V. Sannibale, L. Santamarı́a, G. Santostasi, S. Saraf, P. Sarin, B. S. Sathyaprakash, S. Sato, M. Satterthwaite, P. R. Saulson, R. Savage, R. Schilling, R. Schnabel, R. Schofield, B. Schulz, B. F. Schutz, P. Schwinberg, J. Scott, S.M. Scott, A. C. Searle, F. Seifert, D. Sellers, A. S. Sengupta, A. Sergeev, B. Shapiro, PHYSICAL REVIEW D 83, 042001 (2011)
7 citations
Posted Content•
TL;DR: In this paper, the authors presented 90% confidence level (CL) upper-limit maps of GW strain power with typical values between 2-20x10^-50 strain and 5-35x10−49 strain for pointlike and extended sources respectively.
Abstract: The gravitational-wave (GW) sky may include nearby pointlike sources as well as astrophysical and cosmological stochastic backgrounds. Since the relative strength and angular distribution of the many possible sources of GWs are not well constrained, searches for GW signals must be performed in a model-independent way. To that end we perform two directional searches for persistent GWs using data from the LIGO S5 science run: one optimized for pointlike sources and one for arbitrary extended sources. The latter result is the first of its kind. Finding no evidence to support the detection of GWs, we present 90% confidence level (CL) upper-limit maps of GW strain power with typical values between 2-20x10^-50 strain^2 Hz^-1 and 5-35x10^-49 strain^2 Hz^-1 sr^-1 for pointlike and extended sources respectively. The limits on pointlike sources constitute a factor of 30 improvement over the previous best limits. We also set 90% CL limits on the narrow-band root-mean-square GW strain from interesting targets including Sco X-1, SN1987A and the Galactic Center as low as ~7x10^-25 in the most sensitive frequency range near 160 Hz. These limits are the most constraining to date and constitute a factor of 5 improvement over the previous best limits.
2 citations