1 / 13

The ν Moon project: Detecting UHE cosmic-rays and neutrinos hitting the Moon

The ν Moon project: Detecting UHE cosmic-rays and neutrinos hitting the Moon. ν Moon Collaboration: J. Bacelar (KVI) R.Braun (ASTRON) G. de Bruyn (ASTRON) H. Falcke (ASTRON) O. Scholten (KVI) B. Stappers (ASTRON) R. Strom (ASTRON). Neutrino detection needs large detector volumes!.

addison
Download Presentation

The ν Moon project: Detecting UHE cosmic-rays and neutrinos hitting the Moon

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. The νMoon project: Detecting UHE cosmic-rays and neutrinos hitting the Moon νMoon Collaboration:J. Bacelar (KVI) R.Braun (ASTRON) G. de Bruyn (ASTRON) H. Falcke (ASTRON) O. Scholten (KVI) B. Stappers (ASTRON) R. Strom (ASTRON)

  2. Neutrino detection needs large detector volumes! Use the moon …

  3. Cosmic Ray Westerbork antennas 100 MHz Radio Waves

  4. Vacuum Moon n=1.5-1.8 θc ≈ 560 Cosmic particle interaction • Particle hits Moon (radius=1700 km; area = 6×106 km2): • Interacts: protons within meters, V • Askaryan effect -> Coherent Cherenkov emission • Shower development -> including LPM effect • Transmission through Moon material λr= 15[m] /  [GHz] = 7m (at 2.2 GHz) • Transmissivity across Moon surface – vacuum boundary 60 km @ 1021 eV 6 km @ 1024 eV Vacuum Moon n=1.5-1.8 Spread emitted power density in a gaussian of width Δθc≈λ/ℓ Hadronic component: Δθc= 2.5 (3/) = 3.50 (at 2.2 GHz) EM component Δθc= 2.5 (3/)(4.1014 / E)1/3 = 0.0250 θc ≈ 560 θc 2.2 GHz

  5. Vacuum Moon n=1.5-1.8 θc ≈ 560 Cosmic particle interaction • Particle hits Moon (radius=1700 km; area = 6×106 km2): • Interacts: protons within meters, V • Askaryan effect -> Coherent Cherenkov emission • Shower development -> including LPM effect • Transmission through Moon material λr= 15[m] /  [GHz] = 150 m (at 0.1 GHz) • Transmissivity across Moon surface – vacuum boundary 60 km @ 1021 eV 6 km @ 1024 eV Spread emitted power density in a gaussian of width Δθc≈λ/ℓ Hadronic component: Δθc= 2.5 (3/) = 750 (at 0.1 GHz) EM component Δθc= 2.5 (3/)(4.1014 / E)1/3 = 0.50 θc 100 MHz

  6. Where can one do this experiment at 150 MHz ? • GMRT in India (30 dishes 45m diameter) • Problem: Data acquisition, Ionosphere, Interference,separation between telescopes • WSRT Westerbork – available at present (14 dishes 25 m diameter) • Use “PUMA II” backend for pulsar observations • LOFAR – available in the future • Dedicated mode for moon experiment

  7. Westerbork (WSRT) Experiment • Basic Properties: • 14 x 25 m diameter dishes • 12 dishes phased-up • 110 hour observation time • 40 M samples/sec (PuMa II) • Full Polarization information • 117-175 MHz band • 8 dual-pol bands of 20 MHz • 3×1020 eV would give 15 σ peak (req.) • 2 separate 4’ × 6° pencil beams • covering 50% of moon Westerbork Synthesis Radio Telescope

  8. Westerbork (WSRT) Experiment 4 freq.bands 4 freq.bands Westerbork Synthesis Radio Telescope

  9. Schedule • Pilot experiment at WSRT, followed by campaign at LOFAR • First: Director’s time at WSRT • 2005, 14th June 17:00-19:00 several different daq. Options tried (PuMa I) • 2005, 8th July 07:00-09:00 measurements at 117 and 162 MHz (PuMa I) • 2006, 20th Feb. 06 05:00-06:00 measurement with PuMaII • 2006: νMoon approved as Long-Term Project • First 110 hrs granted, starting July 15, 2006 • A total of 510 hrs requested for subsequent years • Currently observed 24 hrs / 12 hrs of useful data

  10. Processing Pipeline Spectrum before & after interference excision • 18 TB raw data per 6 hr slot • Excision of narrow-band interference • De-Dispersion of ionosphere with GPS TEC values • Indentification of peaks • 100:1 to 180 GB

  11. First Data Products: Noise Distribution & Power Spectra Simulation of data for 15 events within 1 hour data taking Noise is Gaussian down to 10-7 10 s of data

  12. Expected Sensitivity Cosmic Rays Neutrinos TDs GZK ν´s Scholten et al. (NuMoon Collab.) 2006, Astropart. Phys., in press

  13. Summary • Low-Frequency radio observations are ideal to study super-GZK particles. • Westerbork experiment has just begun • Data pipeline is working • 100 hrs granted, 500 hrs expected in total • Search for pulses is next … • Very interesting first limit within one year!? • LOFAR will improve limits(?) even more

More Related