Upper limits from the LIGO and TAMA detectors on the rate of gravitational-wave bursts
We report on the first joint search for gravitational waves by the TAMA and LIGO collaborations. We looked for millisecond-duration unmodeled gravitational-wave bursts in 473 hr of coincident data collected during early 2003. No candidate signals were found. We set an upper limit of 0.12 events per...
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Veröffentlicht in: | Physical review. D, Particles and fields Particles and fields, 2005-12, Vol.72 (12), Article 122004 |
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creator | Abbott, B. Abbott, R. Adhikari, R. Ageev, A. Agresti, J. Ajith, P. Allen, B. Allen, J. Amin, R. Anderson, S. B. Anderson, W. G. Araya, M. Armandula, H. Ashley, M. Asiri, F. Aufmuth, P. Aulbert, C. Babak, S. Balasubramanian, R. Ballmer, S. Barish, B. C. Barker, C. Barker, D. Barnes, M. Barr, B. Barton, M. A. Bayer, K. Beausoleil, R. Belczynski, K. Bennett, R. Berukoff, S. J. Betzwieser, J. Bhawal, B. Bilenko, I. A. Billingsley, G. Black, E. Blackburn, K. Blackburn, L. Bland, B. Bochner, B. Bogue, L. Bork, R. Bose, S. Brady, P. R. Braginsky, V. B. Brau, J. E. Brown, D. A. Bullington, A. Bunkowski, A. Buonanno, A. Burgess, R. Busby, D. Butler, W. E. Byer, R. L. Cadonati, L. Cagnoli, G. Camp, J. B. Cannizzo, J. Cannon, K. Cantley, C. A. Cao, J. Cardenas, L. Carter, K. Casey, M. M. Castiglione, J. Chandler, A. Chapsky, J. Charlton, P. Chatterji, S. Chelkowski, S. Chen, Y. Chickarmane, V. Chin, D. Christensen, N. Churches, D. Cokelaer, T. Colacino, C. Coldwell, R. Coles, M. Cook, D. Corbitt, T. Coyne, D. Creighton, J. D. E. Creighton, T. D. Crooks, D. R. M. Csatorday, P. Cusack, B. J. Cutler, C. Dalrymple, J. D’Ambrosio, E. Danzmann, K. Davies, G. Daw, E. DeBra, D. Delker, T. Dergachev, V. Desai, S. DeSalvo, R. Dhurandhar, S. Di Credico, A. |
description | We report on the first joint search for gravitational waves by the TAMA and LIGO collaborations. We looked for millisecond-duration unmodeled gravitational-wave bursts in 473 hr of coincident data collected during early 2003. No candidate signals were found. We set an upper limit of 0.12 events per day on the rate of detectable gravitational-wave bursts, at 90% confidence level. From software simulations, we estimate that our detector network was sensitive to bursts with root-sum-square strain amplitude above approximately 1-3x10{sup -19} Hz{sup -1/2} in the frequency band 700-2000 Hz. We describe the details of this collaborative search, with particular emphasis on its advantages and disadvantages compared to searches by LIGO and TAMA separately using the same data. Benefits include a lower background and longer observation time, at some cost in sensitivity and bandwidth. We also demonstrate techniques for performing coincidence searches with a heterogeneous network of detectors with different noise spectra and orientations. These techniques include using coordinated software signal injections to estimate the network sensitivity, and tuning the analysis to maximize the sensitivity and the livetime, subject to constraints on the background. |
doi_str_mv | 10.1103/PhysRevD.72.122004 |
format | Article |
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B. ; Anderson, W. G. ; Araya, M. ; Armandula, H. ; Ashley, M. ; Asiri, F. ; Aufmuth, P. ; Aulbert, C. ; Babak, S. ; Balasubramanian, R. ; Ballmer, S. ; Barish, B. C. ; Barker, C. ; Barker, D. ; Barnes, M. ; Barr, B. ; Barton, M. A. ; Bayer, K. ; Beausoleil, R. ; Belczynski, K. ; Bennett, R. ; Berukoff, S. J. ; Betzwieser, J. ; Bhawal, B. ; Bilenko, I. A. ; Billingsley, G. ; Black, E. ; Blackburn, K. ; Blackburn, L. ; Bland, B. ; Bochner, B. ; Bogue, L. ; Bork, R. ; Bose, S. ; Brady, P. R. ; Braginsky, V. B. ; Brau, J. E. ; Brown, D. A. ; Bullington, A. ; Bunkowski, A. ; Buonanno, A. ; Burgess, R. ; Busby, D. ; Butler, W. E. ; Byer, R. L. ; Cadonati, L. ; Cagnoli, G. ; Camp, J. B. ; Cannizzo, J. ; Cannon, K. ; Cantley, C. A. ; Cao, J. ; Cardenas, L. ; Carter, K. ; Casey, M. M. ; Castiglione, J. ; Chandler, A. ; Chapsky, J. ; Charlton, P. ; Chatterji, S. ; Chelkowski, S. ; Chen, Y. ; Chickarmane, V. ; Chin, D. ; Christensen, N. ; Churches, D. ; Cokelaer, T. ; Colacino, C. ; Coldwell, R. ; Coles, M. ; Cook, D. ; Corbitt, T. ; Coyne, D. ; Creighton, J. D. E. ; Creighton, T. D. ; Crooks, D. R. M. ; Csatorday, P. ; Cusack, B. J. ; Cutler, C. ; Dalrymple, J. ; D’Ambrosio, E. ; Danzmann, K. ; Davies, G. ; Daw, E. ; DeBra, D. ; Delker, T. ; Dergachev, V. ; Desai, S. ; DeSalvo, R. ; Dhurandhar, S. ; Di Credico, A.</creator><creatorcontrib>Abbott, B. ; Abbott, R. ; Adhikari, R. ; Ageev, A. ; Agresti, J. ; Ajith, P. ; Allen, B. ; Allen, J. ; Amin, R. ; Anderson, S. B. ; Anderson, W. G. ; Araya, M. ; Armandula, H. ; Ashley, M. ; Asiri, F. ; Aufmuth, P. ; Aulbert, C. ; Babak, S. ; Balasubramanian, R. ; Ballmer, S. ; Barish, B. C. ; Barker, C. ; Barker, D. ; Barnes, M. ; Barr, B. ; Barton, M. A. ; Bayer, K. ; Beausoleil, R. ; Belczynski, K. ; Bennett, R. ; Berukoff, S. J. ; Betzwieser, J. ; Bhawal, B. ; Bilenko, I. A. ; Billingsley, G. ; Black, E. ; Blackburn, K. ; Blackburn, L. ; Bland, B. ; Bochner, B. ; Bogue, L. ; Bork, R. ; Bose, S. ; Brady, P. R. ; Braginsky, V. B. ; Brau, J. E. ; Brown, D. A. ; Bullington, A. ; Bunkowski, A. ; Buonanno, A. ; Burgess, R. ; Busby, D. ; Butler, W. E. ; Byer, R. L. ; Cadonati, L. ; Cagnoli, G. ; Camp, J. B. ; Cannizzo, J. ; Cannon, K. ; Cantley, C. A. ; Cao, J. ; Cardenas, L. ; Carter, K. ; Casey, M. M. ; Castiglione, J. ; Chandler, A. ; Chapsky, J. ; Charlton, P. ; Chatterji, S. ; Chelkowski, S. ; Chen, Y. ; Chickarmane, V. ; Chin, D. ; Christensen, N. ; Churches, D. ; Cokelaer, T. ; Colacino, C. ; Coldwell, R. ; Coles, M. ; Cook, D. ; Corbitt, T. ; Coyne, D. ; Creighton, J. D. E. ; Creighton, T. D. ; Crooks, D. R. M. ; Csatorday, P. ; Cusack, B. J. ; Cutler, C. ; Dalrymple, J. ; D’Ambrosio, E. ; Danzmann, K. ; Davies, G. ; Daw, E. ; DeBra, D. ; Delker, T. ; Dergachev, V. ; Desai, S. ; DeSalvo, R. ; Dhurandhar, S. ; Di Credico, A.</creatorcontrib><description>We report on the first joint search for gravitational waves by the TAMA and LIGO collaborations. We looked for millisecond-duration unmodeled gravitational-wave bursts in 473 hr of coincident data collected during early 2003. No candidate signals were found. We set an upper limit of 0.12 events per day on the rate of detectable gravitational-wave bursts, at 90% confidence level. From software simulations, we estimate that our detector network was sensitive to bursts with root-sum-square strain amplitude above approximately 1-3x10{sup -19} Hz{sup -1/2} in the frequency band 700-2000 Hz. We describe the details of this collaborative search, with particular emphasis on its advantages and disadvantages compared to searches by LIGO and TAMA separately using the same data. Benefits include a lower background and longer observation time, at some cost in sensitivity and bandwidth. We also demonstrate techniques for performing coincidence searches with a heterogeneous network of detectors with different noise spectra and orientations. These techniques include using coordinated software signal injections to estimate the network sensitivity, and tuning the analysis to maximize the sensitivity and the livetime, subject to constraints on the background.</description><identifier>ISSN: 1550-7998</identifier><identifier>ISSN: 0556-2821</identifier><identifier>EISSN: 1550-2368</identifier><identifier>EISSN: 1089-4918</identifier><identifier>DOI: 10.1103/PhysRevD.72.122004</identifier><language>eng</language><publisher>United States</publisher><subject>AMPLITUDES ; COMPUTER CODES ; COMPUTERIZED SIMULATION ; COSMOLOGY ; GRAVITATIONAL WAVE DETECTORS ; GRAVITATIONAL WAVES ; INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND TECHNOLOGY ; INTERFEROMETRY ; ORIENTATION ; PHYSICS OF ELEMENTARY PARTICLES AND FIELDS ; SENSITIVITY ; VISIBLE RADIATION</subject><ispartof>Physical review. D, Particles and fields, 2005-12, Vol.72 (12), Article 122004</ispartof><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c429t-381f85968e3afb2936f6c8a1d43d59a791b85ab52e14281eb4ada579e1f0d46a3</citedby><cites>FETCH-LOGICAL-c429t-381f85968e3afb2936f6c8a1d43d59a791b85ab52e14281eb4ada579e1f0d46a3</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>230,314,776,780,881,2863,2864,27901,27902</link.rule.ids><backlink>$$Uhttps://www.osti.gov/biblio/20774492$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>Abbott, B.</creatorcontrib><creatorcontrib>Abbott, R.</creatorcontrib><creatorcontrib>Adhikari, R.</creatorcontrib><creatorcontrib>Ageev, A.</creatorcontrib><creatorcontrib>Agresti, J.</creatorcontrib><creatorcontrib>Ajith, P.</creatorcontrib><creatorcontrib>Allen, B.</creatorcontrib><creatorcontrib>Allen, J.</creatorcontrib><creatorcontrib>Amin, R.</creatorcontrib><creatorcontrib>Anderson, S. 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M.</creatorcontrib><creatorcontrib>Csatorday, P.</creatorcontrib><creatorcontrib>Cusack, B. J.</creatorcontrib><creatorcontrib>Cutler, C.</creatorcontrib><creatorcontrib>Dalrymple, J.</creatorcontrib><creatorcontrib>D’Ambrosio, E.</creatorcontrib><creatorcontrib>Danzmann, K.</creatorcontrib><creatorcontrib>Davies, G.</creatorcontrib><creatorcontrib>Daw, E.</creatorcontrib><creatorcontrib>DeBra, D.</creatorcontrib><creatorcontrib>Delker, T.</creatorcontrib><creatorcontrib>Dergachev, V.</creatorcontrib><creatorcontrib>Desai, S.</creatorcontrib><creatorcontrib>DeSalvo, R.</creatorcontrib><creatorcontrib>Dhurandhar, S.</creatorcontrib><creatorcontrib>Di Credico, A.</creatorcontrib><title>Upper limits from the LIGO and TAMA detectors on the rate of gravitational-wave bursts</title><title>Physical review. D, Particles and fields</title><description>We report on the first joint search for gravitational waves by the TAMA and LIGO collaborations. We looked for millisecond-duration unmodeled gravitational-wave bursts in 473 hr of coincident data collected during early 2003. No candidate signals were found. We set an upper limit of 0.12 events per day on the rate of detectable gravitational-wave bursts, at 90% confidence level. From software simulations, we estimate that our detector network was sensitive to bursts with root-sum-square strain amplitude above approximately 1-3x10{sup -19} Hz{sup -1/2} in the frequency band 700-2000 Hz. We describe the details of this collaborative search, with particular emphasis on its advantages and disadvantages compared to searches by LIGO and TAMA separately using the same data. Benefits include a lower background and longer observation time, at some cost in sensitivity and bandwidth. We also demonstrate techniques for performing coincidence searches with a heterogeneous network of detectors with different noise spectra and orientations. These techniques include using coordinated software signal injections to estimate the network sensitivity, and tuning the analysis to maximize the sensitivity and the livetime, subject to constraints on the background.</description><subject>AMPLITUDES</subject><subject>COMPUTER CODES</subject><subject>COMPUTERIZED SIMULATION</subject><subject>COSMOLOGY</subject><subject>GRAVITATIONAL WAVE DETECTORS</subject><subject>GRAVITATIONAL WAVES</subject><subject>INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND TECHNOLOGY</subject><subject>INTERFEROMETRY</subject><subject>ORIENTATION</subject><subject>PHYSICS OF ELEMENTARY PARTICLES AND FIELDS</subject><subject>SENSITIVITY</subject><subject>VISIBLE RADIATION</subject><issn>1550-7998</issn><issn>0556-2821</issn><issn>1550-2368</issn><issn>1089-4918</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2005</creationdate><recordtype>article</recordtype><recordid>eNo1kE1LAzEYhIMoWKt_wFPA86752k1yLFVroVKR1mt4dzexkXZTkljpv7faepqBGYbhQeiWkpJSwu9fV_v0ZncPpWQlZYwQcYYGtKpIwXitzk9eaq0u0VVKn4RwVks5QO_L7dZGvPYbnxN2MWxwXlk8m07mGPoOL0YvI9zZbNscYsKh_4sjZIuDwx8Rdj5D9qGHdfENO4ubr5hyukYXDtbJ3px0iJZPj4vxczGbT6bj0axoBdO54Io6VelaWQ6uYZrXrm4V0E7wrtIgNW1UBU3FLBVMUdsI6KCS2lJHOlEDH6K7425I2ZvU-sPRVRv6_vDXMCKlEJodWuzYamNIKVpnttFvIO4NJeaXn_nnZyQzR378BySlZL0</recordid><startdate>20051201</startdate><enddate>20051201</enddate><creator>Abbott, B.</creator><creator>Abbott, R.</creator><creator>Adhikari, R.</creator><creator>Ageev, A.</creator><creator>Agresti, J.</creator><creator>Ajith, P.</creator><creator>Allen, B.</creator><creator>Allen, J.</creator><creator>Amin, R.</creator><creator>Anderson, S. 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J.</creator><creator>Cutler, C.</creator><creator>Dalrymple, J.</creator><creator>D’Ambrosio, E.</creator><creator>Danzmann, K.</creator><creator>Davies, G.</creator><creator>Daw, E.</creator><creator>DeBra, D.</creator><creator>Delker, T.</creator><creator>Dergachev, V.</creator><creator>Desai, S.</creator><creator>DeSalvo, R.</creator><creator>Dhurandhar, S.</creator><creator>Di Credico, A.</creator><scope>AAYXX</scope><scope>CITATION</scope><scope>OTOTI</scope></search><sort><creationdate>20051201</creationdate><title>Upper limits from the LIGO and TAMA detectors on the rate of gravitational-wave bursts</title><author>Abbott, B. ; Abbott, R. ; Adhikari, R. ; Ageev, A. ; Agresti, J. ; Ajith, P. ; Allen, B. ; Allen, J. ; Amin, R. ; Anderson, S. B. ; Anderson, W. G. ; Araya, M. ; Armandula, H. ; Ashley, M. ; Asiri, F. ; Aufmuth, P. ; Aulbert, C. ; Babak, S. ; Balasubramanian, R. ; Ballmer, S. ; Barish, B. C. ; Barker, C. ; Barker, D. ; Barnes, M. ; Barr, B. ; Barton, M. A. ; Bayer, K. ; Beausoleil, R. ; Belczynski, K. ; Bennett, R. ; Berukoff, S. J. ; Betzwieser, J. ; Bhawal, B. ; Bilenko, I. A. ; Billingsley, G. ; Black, E. ; Blackburn, K. ; Blackburn, L. ; Bland, B. ; Bochner, B. ; Bogue, L. ; Bork, R. ; Bose, S. ; Brady, P. R. ; Braginsky, V. B. ; Brau, J. E. ; Brown, D. A. ; Bullington, A. ; Bunkowski, A. ; Buonanno, A. ; Burgess, R. ; Busby, D. ; Butler, W. E. ; Byer, R. L. ; Cadonati, L. ; Cagnoli, G. ; Camp, J. B. ; Cannizzo, J. ; Cannon, K. ; Cantley, C. A. ; Cao, J. ; Cardenas, L. ; Carter, K. ; Casey, M. M. ; Castiglione, J. ; Chandler, A. ; Chapsky, J. ; Charlton, P. ; Chatterji, S. ; Chelkowski, S. ; Chen, Y. ; Chickarmane, V. ; Chin, D. ; Christensen, N. ; Churches, D. ; Cokelaer, T. ; Colacino, C. ; Coldwell, R. ; Coles, M. ; Cook, D. ; Corbitt, T. ; Coyne, D. ; Creighton, J. D. E. ; Creighton, T. D. ; Crooks, D. R. M. ; Csatorday, P. ; Cusack, B. J. ; Cutler, C. ; Dalrymple, J. ; D’Ambrosio, E. ; Danzmann, K. ; Davies, G. ; Daw, E. ; DeBra, D. ; Delker, T. ; Dergachev, V. ; Desai, S. ; DeSalvo, R. ; Dhurandhar, S. ; Di Credico, A.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c429t-381f85968e3afb2936f6c8a1d43d59a791b85ab52e14281eb4ada579e1f0d46a3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2005</creationdate><topic>AMPLITUDES</topic><topic>COMPUTER CODES</topic><topic>COMPUTERIZED SIMULATION</topic><topic>COSMOLOGY</topic><topic>GRAVITATIONAL WAVE DETECTORS</topic><topic>GRAVITATIONAL WAVES</topic><topic>INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND TECHNOLOGY</topic><topic>INTERFEROMETRY</topic><topic>ORIENTATION</topic><topic>PHYSICS OF ELEMENTARY PARTICLES AND FIELDS</topic><topic>SENSITIVITY</topic><topic>VISIBLE RADIATION</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Abbott, B.</creatorcontrib><creatorcontrib>Abbott, R.</creatorcontrib><creatorcontrib>Adhikari, R.</creatorcontrib><creatorcontrib>Ageev, A.</creatorcontrib><creatorcontrib>Agresti, J.</creatorcontrib><creatorcontrib>Ajith, P.</creatorcontrib><creatorcontrib>Allen, B.</creatorcontrib><creatorcontrib>Allen, J.</creatorcontrib><creatorcontrib>Amin, R.</creatorcontrib><creatorcontrib>Anderson, S. B.</creatorcontrib><creatorcontrib>Anderson, W. G.</creatorcontrib><creatorcontrib>Araya, M.</creatorcontrib><creatorcontrib>Armandula, H.</creatorcontrib><creatorcontrib>Ashley, M.</creatorcontrib><creatorcontrib>Asiri, F.</creatorcontrib><creatorcontrib>Aufmuth, P.</creatorcontrib><creatorcontrib>Aulbert, C.</creatorcontrib><creatorcontrib>Babak, S.</creatorcontrib><creatorcontrib>Balasubramanian, R.</creatorcontrib><creatorcontrib>Ballmer, S.</creatorcontrib><creatorcontrib>Barish, B. C.</creatorcontrib><creatorcontrib>Barker, C.</creatorcontrib><creatorcontrib>Barker, D.</creatorcontrib><creatorcontrib>Barnes, M.</creatorcontrib><creatorcontrib>Barr, B.</creatorcontrib><creatorcontrib>Barton, M. A.</creatorcontrib><creatorcontrib>Bayer, K.</creatorcontrib><creatorcontrib>Beausoleil, R.</creatorcontrib><creatorcontrib>Belczynski, K.</creatorcontrib><creatorcontrib>Bennett, R.</creatorcontrib><creatorcontrib>Berukoff, S. J.</creatorcontrib><creatorcontrib>Betzwieser, J.</creatorcontrib><creatorcontrib>Bhawal, B.</creatorcontrib><creatorcontrib>Bilenko, I. A.</creatorcontrib><creatorcontrib>Billingsley, G.</creatorcontrib><creatorcontrib>Black, E.</creatorcontrib><creatorcontrib>Blackburn, K.</creatorcontrib><creatorcontrib>Blackburn, L.</creatorcontrib><creatorcontrib>Bland, B.</creatorcontrib><creatorcontrib>Bochner, B.</creatorcontrib><creatorcontrib>Bogue, L.</creatorcontrib><creatorcontrib>Bork, R.</creatorcontrib><creatorcontrib>Bose, S.</creatorcontrib><creatorcontrib>Brady, P. R.</creatorcontrib><creatorcontrib>Braginsky, V. B.</creatorcontrib><creatorcontrib>Brau, J. E.</creatorcontrib><creatorcontrib>Brown, D. A.</creatorcontrib><creatorcontrib>Bullington, A.</creatorcontrib><creatorcontrib>Bunkowski, A.</creatorcontrib><creatorcontrib>Buonanno, A.</creatorcontrib><creatorcontrib>Burgess, R.</creatorcontrib><creatorcontrib>Busby, D.</creatorcontrib><creatorcontrib>Butler, W. E.</creatorcontrib><creatorcontrib>Byer, R. L.</creatorcontrib><creatorcontrib>Cadonati, L.</creatorcontrib><creatorcontrib>Cagnoli, G.</creatorcontrib><creatorcontrib>Camp, J. B.</creatorcontrib><creatorcontrib>Cannizzo, J.</creatorcontrib><creatorcontrib>Cannon, K.</creatorcontrib><creatorcontrib>Cantley, C. A.</creatorcontrib><creatorcontrib>Cao, J.</creatorcontrib><creatorcontrib>Cardenas, L.</creatorcontrib><creatorcontrib>Carter, K.</creatorcontrib><creatorcontrib>Casey, M. M.</creatorcontrib><creatorcontrib>Castiglione, J.</creatorcontrib><creatorcontrib>Chandler, A.</creatorcontrib><creatorcontrib>Chapsky, J.</creatorcontrib><creatorcontrib>Charlton, P.</creatorcontrib><creatorcontrib>Chatterji, S.</creatorcontrib><creatorcontrib>Chelkowski, S.</creatorcontrib><creatorcontrib>Chen, Y.</creatorcontrib><creatorcontrib>Chickarmane, V.</creatorcontrib><creatorcontrib>Chin, D.</creatorcontrib><creatorcontrib>Christensen, N.</creatorcontrib><creatorcontrib>Churches, D.</creatorcontrib><creatorcontrib>Cokelaer, T.</creatorcontrib><creatorcontrib>Colacino, C.</creatorcontrib><creatorcontrib>Coldwell, R.</creatorcontrib><creatorcontrib>Coles, M.</creatorcontrib><creatorcontrib>Cook, D.</creatorcontrib><creatorcontrib>Corbitt, T.</creatorcontrib><creatorcontrib>Coyne, D.</creatorcontrib><creatorcontrib>Creighton, J. D. E.</creatorcontrib><creatorcontrib>Creighton, T. D.</creatorcontrib><creatorcontrib>Crooks, D. R. M.</creatorcontrib><creatorcontrib>Csatorday, P.</creatorcontrib><creatorcontrib>Cusack, B. J.</creatorcontrib><creatorcontrib>Cutler, C.</creatorcontrib><creatorcontrib>Dalrymple, J.</creatorcontrib><creatorcontrib>D’Ambrosio, E.</creatorcontrib><creatorcontrib>Danzmann, K.</creatorcontrib><creatorcontrib>Davies, G.</creatorcontrib><creatorcontrib>Daw, E.</creatorcontrib><creatorcontrib>DeBra, D.</creatorcontrib><creatorcontrib>Delker, T.</creatorcontrib><creatorcontrib>Dergachev, V.</creatorcontrib><creatorcontrib>Desai, S.</creatorcontrib><creatorcontrib>DeSalvo, R.</creatorcontrib><creatorcontrib>Dhurandhar, S.</creatorcontrib><creatorcontrib>Di Credico, A.</creatorcontrib><collection>CrossRef</collection><collection>OSTI.GOV</collection><jtitle>Physical review. D, Particles and fields</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Abbott, B.</au><au>Abbott, R.</au><au>Adhikari, R.</au><au>Ageev, A.</au><au>Agresti, J.</au><au>Ajith, P.</au><au>Allen, B.</au><au>Allen, J.</au><au>Amin, R.</au><au>Anderson, S. B.</au><au>Anderson, W. G.</au><au>Araya, M.</au><au>Armandula, H.</au><au>Ashley, M.</au><au>Asiri, F.</au><au>Aufmuth, P.</au><au>Aulbert, C.</au><au>Babak, S.</au><au>Balasubramanian, R.</au><au>Ballmer, S.</au><au>Barish, B. C.</au><au>Barker, C.</au><au>Barker, D.</au><au>Barnes, M.</au><au>Barr, B.</au><au>Barton, M. A.</au><au>Bayer, K.</au><au>Beausoleil, R.</au><au>Belczynski, K.</au><au>Bennett, R.</au><au>Berukoff, S. J.</au><au>Betzwieser, J.</au><au>Bhawal, B.</au><au>Bilenko, I. A.</au><au>Billingsley, G.</au><au>Black, E.</au><au>Blackburn, K.</au><au>Blackburn, L.</au><au>Bland, B.</au><au>Bochner, B.</au><au>Bogue, L.</au><au>Bork, R.</au><au>Bose, S.</au><au>Brady, P. R.</au><au>Braginsky, V. B.</au><au>Brau, J. E.</au><au>Brown, D. A.</au><au>Bullington, A.</au><au>Bunkowski, A.</au><au>Buonanno, A.</au><au>Burgess, R.</au><au>Busby, D.</au><au>Butler, W. E.</au><au>Byer, R. L.</au><au>Cadonati, L.</au><au>Cagnoli, G.</au><au>Camp, J. B.</au><au>Cannizzo, J.</au><au>Cannon, K.</au><au>Cantley, C. A.</au><au>Cao, J.</au><au>Cardenas, L.</au><au>Carter, K.</au><au>Casey, M. M.</au><au>Castiglione, J.</au><au>Chandler, A.</au><au>Chapsky, J.</au><au>Charlton, P.</au><au>Chatterji, S.</au><au>Chelkowski, S.</au><au>Chen, Y.</au><au>Chickarmane, V.</au><au>Chin, D.</au><au>Christensen, N.</au><au>Churches, D.</au><au>Cokelaer, T.</au><au>Colacino, C.</au><au>Coldwell, R.</au><au>Coles, M.</au><au>Cook, D.</au><au>Corbitt, T.</au><au>Coyne, D.</au><au>Creighton, J. D. E.</au><au>Creighton, T. D.</au><au>Crooks, D. R. M.</au><au>Csatorday, P.</au><au>Cusack, B. J.</au><au>Cutler, C.</au><au>Dalrymple, J.</au><au>D’Ambrosio, E.</au><au>Danzmann, K.</au><au>Davies, G.</au><au>Daw, E.</au><au>DeBra, D.</au><au>Delker, T.</au><au>Dergachev, V.</au><au>Desai, S.</au><au>DeSalvo, R.</au><au>Dhurandhar, S.</au><au>Di Credico, A.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Upper limits from the LIGO and TAMA detectors on the rate of gravitational-wave bursts</atitle><jtitle>Physical review. D, Particles and fields</jtitle><date>2005-12-01</date><risdate>2005</risdate><volume>72</volume><issue>12</issue><artnum>122004</artnum><issn>1550-7998</issn><issn>0556-2821</issn><eissn>1550-2368</eissn><eissn>1089-4918</eissn><abstract>We report on the first joint search for gravitational waves by the TAMA and LIGO collaborations. We looked for millisecond-duration unmodeled gravitational-wave bursts in 473 hr of coincident data collected during early 2003. No candidate signals were found. We set an upper limit of 0.12 events per day on the rate of detectable gravitational-wave bursts, at 90% confidence level. From software simulations, we estimate that our detector network was sensitive to bursts with root-sum-square strain amplitude above approximately 1-3x10{sup -19} Hz{sup -1/2} in the frequency band 700-2000 Hz. We describe the details of this collaborative search, with particular emphasis on its advantages and disadvantages compared to searches by LIGO and TAMA separately using the same data. Benefits include a lower background and longer observation time, at some cost in sensitivity and bandwidth. We also demonstrate techniques for performing coincidence searches with a heterogeneous network of detectors with different noise spectra and orientations. These techniques include using coordinated software signal injections to estimate the network sensitivity, and tuning the analysis to maximize the sensitivity and the livetime, subject to constraints on the background.</abstract><cop>United States</cop><doi>10.1103/PhysRevD.72.122004</doi><oa>free_for_read</oa></addata></record> |
fulltext | fulltext |
identifier | ISSN: 1550-7998 |
ispartof | Physical review. D, Particles and fields, 2005-12, Vol.72 (12), Article 122004 |
issn | 1550-7998 0556-2821 1550-2368 1089-4918 |
language | eng |
recordid | cdi_osti_scitechconnect_20774492 |
source | American Physical Society Journals |
subjects | AMPLITUDES COMPUTER CODES COMPUTERIZED SIMULATION COSMOLOGY GRAVITATIONAL WAVE DETECTORS GRAVITATIONAL WAVES INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND TECHNOLOGY INTERFEROMETRY ORIENTATION PHYSICS OF ELEMENTARY PARTICLES AND FIELDS SENSITIVITY VISIBLE RADIATION |
title | Upper limits from the LIGO and TAMA detectors on the rate of gravitational-wave bursts |
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