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19 results on '"A. Castellina"'

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

Author

Aglietta, M., Alyea, E. D., Antonioli, P., Badino, G., Bari, G., Basile, M., Berezinsky, V. S., Bersani, F., Bertaina, M., Bertoni, R., Bruni, G., Cara Romeo, G., Castagnoli, C., Castellina, A., Chiavassa, A., Chinellato, J. A., Cifarelli, L., Cindolo, F., Contin, A., Dadykin, V. L., Dos Santos, L. G., Enikeev, R. I., Fulgione, W., Galeotti, P., Ghia, P. L., Giusti, P., Grianti, F., Iacobucci, G., Kemp, E., Khalchukov, F. F., Korolkova, E. V., Korchaguin, P. V., Korchaguin, V. B., Kudryavtsev, V. A., Luvisetto, M., Malguin, A. S., Massam, T., Mengotti Silva, N., Morello, C., Nania, R., Navarra, G., Periale, L., Pesci, A., Picchi, P., Pless, I. A., Ryasny, V. G., Ryazhskaya, O. G., Saavedra, O., Saitoh, K., Sartorelli, G., Selvi, M., Taborgna, N., Takahashi, N., Talochkin, V. P., Trinchero, G. C., Tsuji, S., Turtelli, A., Vallania, P., Vernetto, S., Vigorito, C., Votano, L., Wada, T., Weinstein, R., Widgoff, M., Yakushev, V. F., Yamamoto, I., Zatsepin, G. T., Zichichi, A., Aglietta, M., Alyea, E. D., Antonioli, P., Badino, G., Bari, G., Basile, M., Berezinsky, V. S., Bersani, F., Bertaina, M., Bertoni, R., Bruni, G., Cara Romeo, G., Castagnoli, C., Castellina, A., Chiavassa, A., Chinellato, J. A., Cifarelli, L., Cindolo, F., Contin, A., Dadykin, V. L., Dos Santos, L. G., Enikeev, R. I., Fulgione, W., Galeotti, P., Ghia, P. L., Giusti, P., Grianti, F., Iacobucci, G., Kemp, E., Khalchukov, F. F., Korolkova, E. V., Korchaguin, P. V., Korchaguin, V. B., Kudryavtsev, V. A., Luvisetto, M., Malguin, A. S., Massam, T., Mengotti Silva, N., Morello, C., Nania, R., Navarra, G., Periale, L., Pesci, A., Picchi, P., Pless, I. A., Ryasny, V. G., Ryazhskaya, O. G., Saavedra, O., Saitoh, K., Sartorelli, G., Selvi, M., Taborgna, N., Takahashi, N., Talochkin, V. P., Trinchero, G. C., Tsuji, S., Turtelli, A., Vallania, P., Vernetto, S., Vigorito, C., Votano, L., Wada, T., Weinstein, R., Widgoff, M., Yakushev, V. F., Yamamoto, I., Zatsepin, G. T., and Zichichi, A.

Abstract

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 νemission 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.

Published
2001
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10. Search for low energyνe,μ,τ andve,μ,τ in coincidence with BATSE gamma ray bursts

Author

Aglietta, M., Antonioli, P., Badino, G., Bologna, G., Castagnoli, C., Castellina, A., Dadykin, V. L., Fulgione, W., Galeotti, P., Khalchukov, F. F., Korolkova, E. V., Kortchaguin, P. V., Kortchaguin, V. B., Kudryavtsev, V. A., Malguin, A. S., Periale, L., Ryassny, V. G., Ryazhskaya, O. G., Saavedra, O., Trinchero, G., Vernetto, S., Vigorito, C., Yakushev, V. F., and Zatsepin, G. T.

Abstract

A search for low energy neutrinos of all flavours in correlation with 553 γ ray bursts detected by BATSE aboard the Compton Observatory has been performed by the LSD (Liquid Scintillator Detector) neutrino telescope. No excess ofνe,μ,τ orve,μ,τ candidate has been detected by LSD during the time interval in which BATSE detected the 90% of the photon flux for any of the GRBs analyzed. Upper limits on the neutrino fluxes are given in the paper.

Published
1995
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11. Search for Gamma Ray Bursts of energy Eγ ≥10 GeV and Eγ ≥ 100 TeV in correlation with BATSE events

Author

Aglietta, M., Alessandro, B., Antonioli, P., Arneodo, F., Bergamasco, L., Bertaina, M., Campos Fauth, A., Castellina, A., Castagnoli, C., Chiavassa, A., Cini, G., D'Ettorre Piazzoli, B., Di Sciascio, G., Fulgione, W., Galeotti, P., Ghia, P. L., Iacovacci, M., Mannocchi, G., Melagrana, C., Morello, C., Navarra, G., Riccati, L., Saavedra, O., Trinchero, G. C., Vallania, P., and Vernetto, S.

Abstract

We present the results of a search for Gamma Ray Bursts at energies Eγ ≥ 10 GeV and Eγ ≥ 100 TeV made by the EAS-TOP Air Shower Array in correlation with ∼ 50 events detected by BATSE in the last 3 years.

Published
1995
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12. Underground muon energy spectrum and its relevance for muon astronomy

Author

Castellina, A., Piazzoli, B. D’Ettorre, Mannocchi, G., Picchi, P., Vernetto, S., Bilokon, H., and Meroni, E.

Abstract

A striking result from the NUSEX (1) and SOUDAN (2) experiments is the discovery of a high flux of muons from the direction of Cygnus X-3 displaying the typical 4.8 hour time modulation of this source. The differential energy spectrum of these muons is much flatter (γ∼2) than that for ordinary atmospheric muons (γ∼3.71). This implies a very different shape for the local deep underground muon energy spectrum. We show that a measurement of the content of high-energy muons (> 500 GeV) in underground experiments is a strong signature of their origin.

Published
1985
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13. The high-energy muon flux in air showers from Cygnus X-3

Author

Castellina, A., Piazzoli, B. D’Ettorre, Mannocchi, G., Picchi, P., Vernetto, S., Bilokon, H., and Meroni, E.

Abstract

The underground muon intensity induced by the primaries producing the air shower signal from Cygnus X-3 has been calculated, in both hypothesis of their hadronic or photonic nature. The muon flux measured in NUSEX and SOUDAN experiments is found to be considerably higher than that expected from conventional interactions of the primaries. It is, therefore, impossible to explain both air shower and underground muon fluxes in the frame of conventional interactions.

Published
1985
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14. Correlation between the Maryland and Rome gravitational-wave detectors and the Mont Blanc, Kamioka and IMB particle detectors during SN 1987 A

Author

Aglietta, M., Castellina, A., Fulgione, W., Trinchero, G., Vernetto, S., Astone, P., Badino, G., Bologna, G., Bassan, M., Coccia, E., Modena, I., Bonifazi, P., Castellano, M. G., Visco, M., Castagnoli, C., Galeotti, P., Saavedra, O., Cosmelli, C., Frasca, S., Pallottino, G. V., Pizzella, G., Rapagnani, P., Ricci, F., Majorana, E., Gretz, D., Weber, J., and Wilmot, G.

Abstract

Following a previously found correlation between the gravitational-wave detectors and the Mont Blanc particle detector, we have searched for a similar correlation between the data of the experiments mentioned in the title. We have found that both the Kamioka and the IMB data have a correlation with the gravitational-wave data that occurs with the same characteristics and at the same time of that already found with Mont Blanc. This correlation extends for a period of one or two hours centred at the hour 2∶45 UT of 23 February 1987. It shows that the particle detector signals are delayed with respect to the gravitational-wave detector signals by (1.2±0.5) s. The probability that the additional correlation due to Kamioka and IMB is only accidental is estimated of the order of 10−3or 10−4.

Published
1991
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15. Search for high energy GRBs with EASTOP

Author

Aglietta, M., Alessandro, B., Antonioli, P., Arneodo, F., Bergamasco, L., Bertaina, M., Castagnoli, C., Castellina, A., Chiavassa, A., Cini, G., D'Ettorre Piazzoli, B., Di Sciascio, G., Fulgione, W., Galeotti, P., Ghia, P. L., Iacovacci, M., Mannocchi, G., Morello, C., Navarra, G., Saavedra, O., Trinchero, G. C., Vallania, P., Vernetto, S., Vigorito, C., Aglietta, M., Alessandro, B., Antonioli, P., Arneodo, F., Bergamasco, L., Bertaina, M., Castagnoli, C., Castellina, A., Chiavassa, A., Cini, G., D'Ettorre Piazzoli, B., Di Sciascio, G., Fulgione, W., Galeotti, P., Ghia, P. L., Iacovacci, M., Mannocchi, G., Morello, C., Navarra, G., Saavedra, O., Trinchero, G. C., Vallania, P., Vernetto, S., and Vigorito, C.

Abstract

A search for GRBs of energy $E>10$GeV has been performed by studying the single particle counting rate of the EAS array EASTOP. No candidates have been observed in coincidence with 292 BATSE GRBs and the typical upper limits obtained on the energy fluence are $F(10~{\rm GeV}\div 1~{\rm TeV})\sim 10 ^{-4}\div 10^{-3}~{\rm erg}~{\rm cm}^{-2}$for the events with zenith angle $\theta<30^{\circ}$. A single candidate has been observed in the "all sky" survey mode during 1.5 103days.

Published
1999
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16. Search for GeV GRBs with the INCA experiment

Author

Cabrera, R., Castellina, A., Ghia, P. L., Kakimoto, F., Kaneko, T., Morello, C., Navarra, G., Nishi, K., Saavedra, O., Trinchero, G., Urzagasti, D., Vallania, P., Velarde, A., Vernetto, S., Yoshii, H., Cabrera, R., Castellina, A., Ghia, P. L., Kakimoto, F., Kaneko, T., Morello, C., Navarra, G., Nishi, K., Saavedra, O., Trinchero, G., Urzagasti, D., Vallania, P., Velarde, A., Vernetto, S., and Yoshii, H.

Abstract

INCA is an air shower array located at Mount Chacaltaya in Bolivia, at 5200 m a.s.l., searching for Gamma Ray Bursts of energy $E>1$GeV. The results presented here concern a GRB search made in correlation with 70 events recorded by BATSE since December 1996 to August 1998. For every burst, the INCA counting rate has been studied both during the BATSE detection time and in 2 hours around. No significant excess has been found in any of the trials. Assuming for the burst a power low energy spectrum extending up to 1 TeV with a slope $\alpha = -2$and a time duration of 10 s, the obtained $1~{\rm GeV}\div 1~{\rm TeV}$energy fluence upper limits range from $5.3 \ 10^{-5}~{\rm erg}~{\rm cm}^{-2}$to $2.9 \ 10^{-2}~{\rm erg}~{\rm cm}^{-2}$depending on the event zenith angle.

Published
1999
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