Cumulative analysis of the association between the data of the gravitational wave detectors NAUTILUS and EXPLORER and the gamma ray bursts detected by BATSE and BeppoSAX

Physical Review D - Particles, Fields, Gravitation and Cosmology

Volumn 71, Issue 4, 2005, Pages

  Astone, P ^a   Babusci, D ^b   Bassan, M ^a,c   Carelli, P ^a,d   Coccia, E ^a,c,e   Cosmelli, C ^a,f   D'Antonio, S ^a   Fafone, V ^b   Frontera, F ^g,h   Giordano, G ^b   Guidorzi, C ^g   Marini, A ^b   Minenkov, Y ^a,c   Modena, I ^a,c   Modestino, G ^b   Moleti, A ^a,c   Montanari, E ^g,i   Pallottino, G V ^a,f   Pizzella, G ^b,c   Quintieri, L ^b   Rocchi, A ^b,c   Ronga, F ^b   Sperandio, L ^b   Terenzi, R ^a,h   Torrioli, G ^f   Visco, M ^a,h   more..

^a INFN SEZIONE DI ROMA   (Italy)

^b INFN LABORATORI NAZIONALI DI FRASCATI   (Italy)

^c UNIVERSITY OF ROME TOR VERGATA   (Italy)

^d UNIVERSITY OF L'AQUILA   (Italy)

^e LABORATORI NAZIONALI DEL GRAN SASSO   (Italy)

^f UNIVERSITÀ DI ROMA LA SAPIENZA   (Italy)

^g UNIVERSITY OF FERRARA   (Italy)

^h CNR   (Italy)

ⁱ ISA A Venturi   (Italy)

Author keywords

[No Author keywords available]

Indexed keywords

ALGORITHM; ARTICLE; ENERGY; GAMMA RADIATION; GRAVITY; MATHEMATICAL ANALYSIS; MATHEMATICAL MODEL; QUANTUM THEORY;

EID: 84927710503     PISSN: 15507998     EISSN: 15502368     Source Type: Journal    
DOI: 10.1103/PhysRevD.71.042001     Document Type: Article

References (34)

1. G. J. Fishman and C. A. Meegan, Annu. Rev. Astron. Astrophys. 33, 415 (1995).
2. M. S. Briggs et al., Astrophys. J. 459, 40 (1996).
3. G. Boella et al., Astron. Astrophys. Suppl. Ser. 122, 299 (1997).
4. E. Costa et al., Nature (London), 387, 783 (1997).
5. W. S. Paciesas et al., Astrophys. J. Suppl. Ser. 122, 465 (1999).
6. C. Guidorzi et al., in Gamma-Ray Bursts in the Afterglow Era, edited by E. Costa, F. Frontera, and J. Hjorth (Springer-Verlag, Berlin, 2001), p. 43.
7. http://gammaray.msfc.nasa.gov/batse/grb/catalog/
8. L. S. Finn, S. D. Mohanty, and J. D. Romano, Phys. Rev. D 60, 121101 (1999).
9. G. Modestino and G. Pizzella, Astron. Astrophys. 364, 419 (2000).
10. M. T. Murphy, J. K. Webb, and I. S. Heng, Mon. Not. R. Astron. Soc. 316, 657 (2000).
11. P. Bonifazi et al., Astronomical and Astrophysical Transactions 22, 557 (2003).
12. G. Modestino and A. Moleti, Phys. Rev. D 65, 022005 (2002).
13. P. Astone et al., Phys. Rev. D 66, 102002 (2002).
14. M. J. Rees and P. Mészáros, Astrophys. J., Lett. Ed. 430, L93 (1994).
15. T. Piran, Phys. Rep. 314, 575 (1999).
16. P. Mészáros, Science 291, 79 (2001).
17. B. Zhang and P. Mészáros, Int. J. Mod. Phys. A 19, 2385 (2004).
18. A. De Rujúla, astro-ph/0207033.
19. S. Kobayashi and P. Mészáros, Astrophys. J. 589, 861 (2003).
20. M. H. P. M. van Putten, Phys. Rep. 345, 1 (2001); M. H. P. M. van Putten et al., Phys. Rev. D 69, 044007 (2004).
21. M. H. P. M. van Putten, Phys. Rep. 345, 1 (2001); M. H. P. M. van Putten et al., Phys. Rev. D 69, 044007 (2004).
22. F. Frontera et al., Astrophys. J. Suppl. Ser. 127, 59 (2000).
23. F. Frontera, Lecture Notes in Physics, (Springer, Berlin, Heidelberg, 2003), edited by K. W. Weiler vol. 598, p. 317.
24. R. Sari, T. Piran, and R. Narayan, Astrophys. J., Lett. Ed. 497, L17 (1998).
25. G. Modestino et al., in Proceedings of Gravitational Wave Data Analysis Workshop 2, Orsay, 1997, edited by M. Davier and P. Hello, p. 187.
26. G. Modestino et al., in Proceedings of Frontier Objects in Astrophysics and Particle Physics, Vulcano, 1998, edited by F. Giovannelli and G. Mannocchi, p. 295.
27. P. Tricarico et al., Phys. Rev. D 63, 082002 (2001).
28. P. Astone et al., Classical Quantum Gravity 19, 5449 (2002).
29. S. D. Márka, talk given at Gravitational Wave Data Analysis Workshop 8, Milwaukee, Wisconsin, 2003 (unpublished).
30. A preliminary analysis of these data was presented at the 2003 Amaldi conference: P. Astone et al., Classical Quantum Gravity 21, S759 (2004).
31. P. Astone, P. Bonifazi, G. V. Pallottino, and G. Pizzella, Nuovo Cimento Soc. Ital. Fis. C 17, 713 (1994).
32. W. T. Eadie, D. Drijard, F.L. James, and B. Saudoulet, Statistical Method in Experimental Physics (North-Holland Publishing Company, Amsterdam, 1971).
33. The choice of 10 s as integration interval comes from estimating the possible differences between the true GRB arrival time and the flux peak time, and from the time resolution of our data. In principle, the optimal choice is to have an integration interval of the same order of the overall time uncertainty. This choice will imply losing sensitivity when the GW detector decay time is smaller than 10 s, which occurs about 50% of the times.
34. G. D'Agostini, Bayesian Reasoning in Data analysis (World Scientific, Singapore, 2003).