1 / 25

RICE Status Report

RICE Status Report. 1) Technique & calibration 2) UHE neutrino limits (soon-to-be-released-once-the-mud-wrestling-is-over) 3) Low-scale gravity UL’s 4) RICE-II: Duty now for the future. 17 underice Rx dipoles + 3 surface horn Rx + 5 Tx dipoles 200x200x200 m cube above AMANDA

curt
Download Presentation

RICE Status Report

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. RICE Status Report 1) Technique & calibration 2) UHE neutrino limits (soon-to-be-released-once-the-mud-wrestling-is-over) 3) Low-scale gravity UL’s 4) RICE-II: Duty now for the future

  2. 17 underice Rx dipoles + 3 surface horn Rx + 5 Tx dipoles 200x200x200 m cube above AMANDA 200500 MHz bandpass Digital scope DAQ 8.192 us waveform capture/event “Forced”=“Unbiased” triggers to capture background conditions Data-taking since 1999 RICE at a glance

  3. Transmitter Location Reconstruction True (known) Transmitter Depth

  4. Single Channel Absolute Gain Calib. • NWAcableTxRxampcableNWA • antenna + amplifier calibrations • cable (TX, RX) and filter • relative geometry of TX/RX 200-500 MHz: <3 dB (E), Likely better for pulses

  5. Glaciology-n(z) by TxRx t=c/n

  6. Data – surface reflections (03 data)

  7. Bottom echo measures atten Bottom echo visible thru 5.6 km! (20 dB noise reduction [averaging]) Bedrock/2850m

  8. Absorption (Im(eps)) at SP

  9. Ray Tracing

  10. WAVEFORMS:Tx → Rx simulation vs. data:Data bandwidth slightly better than MC prediction MC Simulations simulated data

  11. MC simulations: Angular Resolution +Energy resolution~50% for r<1 km

  12. Generate expected waveforms from nNshower Embed waveforms in “forced” trigger data Sample over course of data-taking Smear MC by timing uncertainty (s~10 ns) Double-counting? Reconstruct with cuts as if data Efficiency~50% Monte Carlo efficiency

  13. Irreducible (thermal) bkgnds – ~50% of triggers when “RF-quiet” Compare vx/vy/vz for 4-hit data vs 4-random time Data more peaked @ cntr Remaining bkgnds: dominantly surface transients

  14. Data Summary – 1999April 2005 Total of ~1.5 yrs. Livetime for current analysis

  15. Old vs. New (corrected ray-tracing + other refinements) effective volume Aside: “The energy has to go somewhere”. Compensating effect of caustics, or after-pulses NOT included in Veff calc.

  16. RICE (2000-2004) BOUNDS ON FLUXES

  17. neutrino 1. PDFs have not been measured in the required (x,Q) range. (10-3>x>10-9) – extrapolate (CTEQ5) into low x-regime 2. Look for anomalous enhancements in neutrino-nucleon cross-section. nucleon Example: Charged current Weak interaction (nu-nucleon) (Q=-|q|)=momentum transfer

  18. Low scale gravity interactions • Assume there are large compact extra dimensions. Only graviton sees these dimensions: • gravity may become strong around electroweak scale (E(c.m.)~ O(1TeV)). Above the mass scale M_D, expect graviton exchangeand microblack hole formation; expect enhancement of the neutrino-nucleon cross-sections. • FREE PARAMETERS: • number of extra dimensions (n); • mass scale (M_D); minimum mass (M_BH0) • required for black hole formation. • => for UHE neutrinos….

  19. An example: LSG VS SM LSG MAY BECOME DOMINANT ABOVE A FEW PeV

  20. WEAKEST STRONGEST BOUNDS ON LOW SCALE GRAVITY

  21. Paper release being held up internally pending completion of evaluation of systematic errors: Uncertainty in attenuation length (most corrections drive Latten up) Uncertainty in ray tracing (enhancement due to focusing being studied, although not to be included in results) Smaller: Pattern recognition/vertexing within limits of amplitude and timing uncertainties Transfer function uncertainties

  22. GRB coincidences (BATSE catalog+), Air Shower coincidences using SPASE coincidence trigger, SGR1806 (27 Dec 2004) flare, muon bremstrahlung (your model here)… Next: monopole search: M=1 PeV monopole, g~104 loses ~20 PeV/km via photonuclear and pair production Other things that we didn’t find

  23. RICE-II / Hardware ready for deployment Nov., 2005… RxDAQ hardware scheme

  24. Transient Response Input signal size into OF linkS:kT noise = 3:1 = local trigger requirement

  25. Current Hardware will operate thru 2007 (MAPO elevation) RICERICE-II transition: “When you see a fork in the road, take it”. To get to “next level”, need hardware improvements + bigger footprint (see Justin talk tomorrow on projected neutrino sensitivity improvement). UHE nu+BH results “in the mail”

More Related