Search for gravitational waves from galactic and extra-galactic binary neutron stars -: art. no. 082001

被引：122

作者：

Abbott, B ^{[1
]}

Abbott, R

Adhikari, R

Ageev, A

Allen, B

Amin, R

Anderson, SB

Anderson, WG

Araya, M

Armandula, H

Ashley, M

Asiri, F

Aufmuth, P

Aulbert, C

Babak, S

Balasubramanian, R

Ballmer, S

Barish, BC

Barker, C

Barker, D

Barnes, M

Barr, B

Barton, MA

Bayer, K

Beausoleil, R

Belczynski, K

Bennett, R

Berukoff, SJ

Betzwieser, J

Bhawal, B

Bilenko, IA

Billingsley, G

Black, E

Blackburn, K

Blackburn, L

Bland, B

Bochner, B

Bogue, L

Bork, R

Bose, S

Brady, PR

Braginsky, VB

Brau, JE

Brown, DA

Bullington, A

Bunkowski, A

Buonanno, A

Burgess, R

Busby, D

Butler, WE

机构：

[1] CALTECH, LIGO, Pasadena, CA 91125 USA

[2] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany

[3] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany

[4] Australian Natl Univ, Canberra, ACT 0200, Australia

[5] Calif State Univ Dominguez Hills, Carson, CA 90747 USA

[6] CALTECH, CaRT, Pasadena, CA 91125 USA

[7] Cardiff Univ, Cardiff CF2 3YB, Wales

[8] Carleton Coll, Northfield, MN 55057 USA

[9] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA

[10] Hobart & William Smith Coll, Geneva, NY 14456 USA

[11] Inter Univ Ctr Astron & Astrophys, Pune 411007, Maharashtra, India

[12] MIT, LIGO, Cambridge, MA 02139 USA

[13] LIGO Hanford Observ, Richland, WA 99352 USA

[14] LIGO Livingston Observ, Livingston, LA USA

[15] Louisiana State Univ, Baton Rouge, LA 70803 USA

[16] Louisiana Tech Univ, Ruston, LA 71272 USA

[17] Loyola Univ, New Orleans, LA 70118 USA

[18] Max Planck Inst Quantum Opt, D-85748 Garching, Germany

[19] Moscow MV Lomonosov State Univ, Moscow 119992, Russia

[20] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[21] Natl Astron Observ Japan, Tokyo 1818588, Japan

[22] Northwestern Univ, Evanston, IL 60208 USA

[23] Salish Kootenai Coll, Pablo, MT 59855 USA

[24] SE Louisiana Univ, Hammond, LA 70402 USA

[25] Stanford Univ, Stanford, CA 94305 USA

[26] Syracuse Univ, Syracuse, NY 13244 USA

[27] Penn State Univ, University Pk, PA 16802 USA

[28] Univ Texas Brownsville, Brownsville, TX 78520 USA

[29] Texas Southmost Coll, Brownsville, TX 78520 USA

[30] Trinity Univ, San Antonio, TX 78212 USA

[31] Leibniz Univ Hannover, D-30167 Hannover, Germany

[32] Univ Illes Balears, E-07122 Palma de Mallorca, Spain

[33] Univ Birmingham, Birmingham B15 2TT, W Midlands, England

[34] Univ Florida, Gainesville, FL 32611 USA

[35] Univ Glasgow, Glasgow G12 8QQ, Lanark, Scotland

[36] Univ Michigan, Ann Arbor, MI 48109 USA

[37] Univ Oregon, Eugene, OR 97403 USA

[38] Univ Rochester, Rochester, NY 14627 USA

[39] Univ Wisconsin, Milwaukee, WI 53201 USA

[40] Washington State Univ, Pullman, WA 99164 USA

[41] HP Labs, Palo Alto, CA USA

[42] CNRS, Inst Astrophys Paris, GReCO, F-75700 Paris, France

[43] Columbia Univ, New York, NY 10027 USA

[44] Univ Tokyo, Inst Cosm Ray Res, Tokyo, Japan

[45] Univ Coll Dublin, Dublin, Ireland

[46] IBM Canada Ltd, Markham, ON, Canada

[47] CALTECH, Jet Prop Lab, Pasadena, CA USA

来源：

PHYSICAL REVIEW D | 2005年 / 72卷 / 08期

关键词：

D O I：

10.1103/PhysRevD.72.082001

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We use 373 hours (approximate to 15 days) of data from the second science run of the LIGO gravitational-wave detectors to search for signals from binary neutron star coalescences within a maximum distance of about 1.5 Mpc, a volume of space which includes the Andromeda Galaxy and other galaxies of the Local Group of galaxies. This analysis requires a signal to be found in data from detectors at the two LIGO sites, according to a set of coincidence criteria. The background (accidental coincidence rate) is determined from the data and is used to judge the significance of event candidates. No inspiral gravitational-wave events were identified in our search. Using a population model which includes the Local Group, we establish an upper limit of less than 47 inspiral events per year per Milky Way equivalent galaxy with 90% confidence for nonspinning binary neutron star systems with component masses between 1 and 3M.

引用

页数：22

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