EDP Sciences
Free access
Volume 366, Number 2, February I 2001
Page(s) 573 - 577
Section Formation, structure and evolution of stars
DOI http://dx.doi.org/10.1051/0004-6361:20000233

A&A 366, 573-577 (2001)
DOI: 10.1051/0004-6361:20000233

Upper limits to low energy $\bar\nu_\mathrm{e}$ flux from GRB 990705

M. Aglietta1, E. D. Alyea2, P. Antonioli3, G. Badino1, G. Bari3, M. Basile3, V. S. Berezinsky4, F. Bersani3, M. Bertaina1, R. Bertoni1, G. Bruni3, G. Cara Romeo3, C. Castagnoli1, A. Castellina1, A. Chiavassa1, J. A. Chinellato5, L. Cifarelli3, F. Cindolo3, A. Contin3, V. L. Dadykin4, L. G. Dos Santos5, R. I. Enikeev4, W. Fulgione1, P. Galeotti1, P. L. Ghia1, P. Giusti3, F. Grianti3, G. Iacobucci3, E. Kemp5, F. F. Khalchukov4, E. V. Korolkova4, P. V. Korchaguin4, V. B. Korchaguin4, V. A. Kudryavtsev4, M. Luvisetto3, A. S. Malguin4, T. Massam3, N. Mengotti Silva5, C. Morello1, R. Nania3, G. Navarra1, L. Periale1, A. Pesci3, P. Picchi1, I. A. Pless6, V. G. Ryasny4, O. G. Ryazhskaya4, O. Saavedra1, K. Saitoh7, G. Sartorelli3, M. Selvi3, N. Taborgna8, N. Takahashi9, V. P. Talochkin4, G. C. Trinchero1, S. Tsuji10, A. Turtelli5, P. Vallania1, S. Vernetto1, C. Vigorito1, L. Votano11, T. Wada10, R. Weinstein12, M. Widgoff13, V. F. Yakushev4, I. Yamamoto14, G. T. Zatsepin4 and A. Zichichi3

1  Institute of Cosmo-Geophysics, CNR, Torino, University of Torino and INFN-Torino, Italy
2  Indiana University, Bloomington, USA
3  University of Bologna and INFN-Bologna, Italy
4  Institute for Nuclear Research, Russian Academy of Sciences, Moscow, Russia
5  University of Campinas, Campinas, Brazil
6  Massachusetts Institute of Technology, Cambridge, USA
7  Ashikaga Institute of Technology, Ashikaga, Japan
8  INFN-LNGS, Assergi, Italy
9  Hirosaki University, Hirosaki, Japan
10  Okayama University, Okayama, Japan
11  INFN-LNF, Frascati, Italy
12  University of Houston, Houston, USA
13  Brown University, Providence, USA
14  Okayama University of Science, Okayama, Japan

(Received 16 June 2000 /Accepted 9 November 2000 )

The detection of Gamma Ray Burst GRB 990705 on 1999, July 5.66765 UT, pointing to the Large Magellanic Clouds, suggested the search for a possible neutrino counterpart, both in coincidence with and slightly before (or after) the photon burst. We exploited such a possibility by means of the LVD neutrino telescope (National Gran Sasso Laboratory, Italy), which has the capability to study low-energy cosmic neutrinos. No evidence for any neutrino signal, over a wide range of time durations, has been found, at the occurrence of GRB 990705. Due to the lack of information about both the source distance and its emission spectrum, the results of the search are expressed in terms of upper limits, at the Earth, to the $\bar\nu_\mathrm{e}$ flux $\cdot$ cross-section, integrated over different time durations, $\int \int \Phi_{\bar \nu_\mathrm{e}}\sigma {\rm d}E {\rm d}t$. Moreover, assuming thermal $\bar\nu_\mathrm{e}$ spectra at the source, upper limits to the $\bar\nu_\mathrm{e}$ flux, integrated over time duration, for different spectral temperatures, are obtained. Based on these limits and on the expectations for $\nu$ emission from collapsing astrophysical objects, the occurrence of a gravitational stellar collapse can be excluded up to a distance $r \approx 50$ kpc, in the case of time coincidence with GRB 990705, and $r \approx 20$ kpc, for the 24 hours preceding it.

Key words: stars: supernovae -- gamma ray bursts

Offprint request: W. Fulgione, fulgione@to.infn.it

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