ARENA-2005 THE UPPER LIMIT TO THE EHE NEUTRINO FLUX FROM OBSERVATIONS OF THE MOON WITH KALYAZIN...

ARENA-2005ARENA-2005

THE UPPER LIMIT THE UPPER LIMIT TO THE EHE NEUTRINO FLUX TO THE EHE NEUTRINO FLUX

FROM OBSERVATIONS OF THE MOON FROM OBSERVATIONS OF THE MOON WITH KALYAZIN RADIO TELESCOPE. WITH KALYAZIN RADIO TELESCOPE.

A.R.Beresnyak, A.R.Beresnyak, R.D.DagkesamanskiyR.D.Dagkesamanskiy, , A.V.Kovalenko I.M.Zheleznykh A.V.Kovalenko I.M.Zheleznykh


Contents of the talkContents of the talk

1. Some milestones on the way to SHE neutrino 1. Some milestones on the way to SHE neutrino detection detection

2. Description of the Kalyazin experiment 2. Description of the Kalyazin experiment

3. Short discussion of our first results3. Short discussion of our first results 4. Plans for the future 4. Plans for the future


Some important milestonesSome important milestones on the way to SHE neutrinos detection. on the way to SHE neutrinos detection.

1961,19651961,1965 - G.Askaryan’s idea on negative charge excess of - G.Askaryan’s idea on negative charge excess of cascades in a dense dielectric medium and corresponding Cherenkov cascades in a dense dielectric medium and corresponding Cherenkov radio pulses expected. radio pulses expected.

19831983 - G.A.Gusev and I.Zheleznykh propose Radio Antarctic Muon - G.A.Gusev and I.Zheleznykh propose Radio Antarctic Muon And Neutrino Detector (RAMAND project) with the antennas And Neutrino Detector (RAMAND project) with the antennas “listening” an ice massive. “listening” an ice massive.

19881988 – I.Zheleznykh propose the RAdio Moon Hadron And Neutrino – I.Zheleznykh propose the RAdio Moon Hadron And Neutrino Detection (RAMHAND). Detection (RAMHAND).


Some important milestones (cont.)Some important milestones (cont.)

19891989 - First estimates of the Moon target volume and the - First estimates of the Moon target volume and the sensitivity of the large ground-based radio telescopes made by sensitivity of the large ground-based radio telescopes made by Dagkesamanskiy & Zheleznykh. Dagkesamanskiy & Zheleznykh.

19961996 - First search of the nanosecond pulses from the Moon with - First search of the nanosecond pulses from the Moon with 64-meter radio telescope of the Parks Radio Observatory (T.Hankins, 64-meter radio telescope of the Parks Radio Observatory (T.Hankins, R.Ekers & J.D.O’Sullivan).R.Ekers & J.D.O’Sullivan).

20002000 – Excellent results in the SLAC laboratory experiment and – Excellent results in the SLAC laboratory experiment and the first results of the GLUE project presented at RADHEP-2000 by the first results of the GLUE project presented at RADHEP-2000 by P.Gorham, D.Saltzberg and their colleagues.P.Gorham, D.Saltzberg and their colleagues.


The main parameters of our experimentThe main parameters of our experiment

- PRAO team started the monitoring of the Moon from 2002. Some of the first - PRAO team started the monitoring of the Moon from 2002. Some of the first observations were made with our 22-meter dish, but the most fruitful results have observations were made with our 22-meter dish, but the most fruitful results have been obtained with Kalyazin 64-meter radio telescope. been obtained with Kalyazin 64-meter radio telescope.

- Multi-frequency feed system of Kalyazin 64-meter radio telescope is very important - Multi-frequency feed system of Kalyazin 64-meter radio telescope is very important advantage. Indeed, delay of the signal at lower frequency due to dispersion in the advantage. Indeed, delay of the signal at lower frequency due to dispersion in the Earth ionosphere could be used to separate the signal from the Moon from local Earth ionosphere could be used to separate the signal from the Moon from local interferences.interferences. - The main frequencies are 1.4 and 2.3 GHZ.- The main frequencies are 1.4 and 2.3 GHZ. - 2 different options of simultaneous multi-frequency observations.- 2 different options of simultaneous multi-frequency observations. - trigger recording system register all suspicious events with 2 ns time resolution. - trigger recording system register all suspicious events with 2 ns time resolution.


The antenna The antenna beamwidths beamwidths are ~11are ~11'' at 1.4 GHz at 1.4 GHz and ~7and ~7'' at 2.3 GHz. at 2.3 GHz.

The expected events The expected events should be near the should be near the limb of the Moon, limb of the Moon, so the pointing was so the pointing was at 14at 14'' apart from apart from the center of the Moonthe center of the Moon

Position of the antenna beams on the MoonPosition of the antenna beams on the Moon


Receiver system block-scheme (option 1)Receiver system block-scheme (option 1)


Receiver system block-scheme (option 2)Receiver system block-scheme (option 2)


1.4 GHz1.4 GHz(LCP) (LCP)

1.4 GHz 1.4 GHz (RCP) (RCP)



Example of the suspicious event (opt.1)Example of the suspicious event (opt.1)


Our main resultsOur main results

- Option 2 (3.5 times more sensitive) is used only after mid of 2004. - Option 2 (3.5 times more sensitive) is used only after mid of 2004. - Corresponding thresholds were 13000 Jy (opt.1) and 3500 Jy (opt.2). - Corresponding thresholds were 13000 Jy (opt.1) and 3500 Jy (opt.2). - Today the total “live-time on the Moon” is slightly more than 60 hrs. - Today the total “live-time on the Moon” is slightly more than 60 hrs. - With this “exposition” we had not found any reliable radio pulse that - With this “exposition” we had not found any reliable radio pulse that could be considered as Cherenkov emission pulse. Our combined could be considered as Cherenkov emission pulse. Our combined estimate of the upper limit to the extremely-high-energy neutrino flux estimate of the upper limit to the extremely-high-energy neutrino flux (Astronomy Reports, Vol.49,No.2, 2005, p.127) is a little bit more (Astronomy Reports, Vol.49,No.2, 2005, p.127) is a little bit more conservative than GLUE’s one. conservative than GLUE’s one. Is it due to our less optimistic estimate of the effective target volume ? - Yes. Is it due to our less optimistic estimate of the effective target volume ? - Yes. or different slope adopted for neutrino spectrum above 10or different slope adopted for neutrino spectrum above 102020eV ? - May be. eV ? - May be. or there are any other differences in the model parameters ? - May be. or there are any other differences in the model parameters ? - May be.


How to improve our estimates ? How to improve our estimates ?

We consider the following ways:We consider the following ways:1.1. Increasing the “live-time on the Moon” (i.e. Increasing the “live-time on the Moon” (i.e. make more and more observations). make more and more observations). 2.2. Increasing the sensitivity (use wider receiver Increasing the sensitivity (use wider receiver bandwidths and coincidence schemes). bandwidths and coincidence schemes). 3.3. Reduce the thresholds and use some kind Reduce the thresholds and use some kind statistic analisys of the suspicious events. statistic analisys of the suspicious events. 4.4. To use not only observations of the Moon To use not only observations of the Moon with the large ground base radio telescopes, with the large ground base radio telescopes, but also the other possible space targets.but also the other possible space targets.


International cooperationInternational cooperation

The possible scheme of The possible scheme of international cooperative international cooperative observaions proposed by observaions proposed by I.Zheleznykh in 1988. I.Zheleznykh in 1988.

Such observations will Such observations will be very useful: be very useful: they improve sensitivity, they improve sensitivity, increase the reliability increase the reliability of results, and even could of results, and even could help us to determine the help us to determine the direction to the UHE direction to the UHE neutrino source. neutrino source.


That’s all. That’s all. Many thanks to Organizing Committee for Many thanks to Organizing Committee for

invitation and to all of you for your invitation and to all of you for your attention !attention !

ARENA-2005 THE UPPER LIMIT TO THE EHE NEUTRINO FLUX FROM OBSERVATIONS OF THE MOON WITH KALYAZIN...

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