TIPP 20111 A Testable Conventional Hypothesis for the DAMA-LIBRA Annual Modulation Signal David Nygren LBNL.

Slides:



Advertisements
Similar presentations
NUCP 2371 Radiation Measurements II
Advertisements

 At the time theories regarding light were being developed, scientists knew that light:  Refracted  Travels in a straight line  Reflects.
Radiation:.
Combined Energy Spectra of Flux and Anisotropy Identifying Anisotropic Source Populations of Gamma-rays or Neutrinos Sheldon Campbell The Ohio State University.
Searching for Dark Matter with the CoGeNT and C4 Detectors
正および負電荷の ミューオンの物質中での寿命 July 1 st, 2014 Suguru Tamamushi List of Contents 1.Purpose 2.Decay of Positive and Negative Muons 3.Experimental Procedure and.
By Miriam Aczel. What are neutrinos? They are almost massless— hardly feel the force of gravity They have no electric charge— don’t feel the electromagnetic.
Scientific Method.
Status of Ultra-low Energy HPGe Detector for low-mass WIMP search Li Xin (Tsinghua University) KIMS collaboration Oct.22nd, 2005.
A Muon Veto for the Ultra Cold Neutron Asymmetry Experiment Vince Bagnulo with Dr. Jeff Martin Electrons Ultra Cold Neutrons Cosmic Ray Muons Protons Pions.
Working Group 2 - Ion acceleration and interactions.
MAGNETIC MONOPOLES Andrey Shmakov Physics 129 Fall 2010 UC Berkeley.
RHESSI/GOES Observations of the Non-flaring Sun from 2002 to J. McTiernan SSL/UCB.
Collecting and Mapping Planetary Data. Direct measurements (in situ) Collecting data directly at the site of scientific interest Ground stations on Earth.
Relative and (maybe) Absolute RHESSI Detector Efficiency: J.McTiernan 2-dec-2009.
Energy Reconstruction Algorithms for the ANTARES Neutrino Telescope J.D. Zornoza 1, A. Romeyer 2, R. Bruijn 3 on Behalf of the ANTARES Collaboration 1.
MACRO Atmospheric Neutrinos Barry Barish 5 May 00 1.Neutrino oscillations 2.WIMPs 3.Astrophysical point sources.
30 Ge & Si Crystals Arranged in verticals stacks of 6 called “towers” Shielding composed of lead, poly, and a muon veto not described. 7.6 cm diameter.
Stopping Power The linear stopping power S for charged particles in a given absorber is simply defined as the differential energy loss for that particle.
Luminous Dark Matter Brian Feldstein arXiv: B.F., P. Graham and S. Rajendran.
Coincidence analysis in ANTARES: Potassium-40 and muons  Brief overview of ANTARES experiment  Potassium-40 calibration technique  Adjacent floor coincidences.
Form Factor Dark Matter Brian Feldstein Boston University In Preparation -B.F., L. Fitzpatrick and E. Katz In Preparation -B.F., L. Fitzpatrick, E. Katz.
880.P20 Winter 2006 Richard Kass 1 Confidence Intervals and Upper Limits Confidence intervals (CI) are related to confidence limits (CL). To calculate.
Radiation The emission of energetic particles The study of it and the processes that produce it is called nuclear chemistry. Unlike the chemistry we have.
Genuine random number generator demo software explanation What happens in this demo LeTech Co.,ltd.
探测器自身放射性本底 CsI crystal CsI Powder. 脉冲形状甄别 PSD Pulse Shape Discrimination.
UKDMC Dark Matter Search with inorganic scintillators Vitaly A. Kudryavtsev University of Sheffield IDM2000 York, UK September 19, 2000.
Petten 29/10/99 ANTARES an underwater neutrino observatory Contents: – Introduction – Neutrino Astronomy and Physics the cosmic ray spectrum sources of.
T. Frank for the CRESST collaboration Laboratori Nazionali del Gran Sasso C. Bucci Max-Planck-Institut für Physik M. Altmann, M. Bruckmayer, C. Cozzini,
14/02/2007 Paolo Walter Cattaneo 1 1.Trigger analysis 2.Muon rate 3.Q distribution 4.Baseline 5.Pulse shape 6.Z measurement 7.Att measurement OUTLINE.
Toby Shoobridge David Benham NERC Space Geodesy Facility Herstmonceux, UK
Annual Modulation Study of Dark Matter Using CsI(Tl) Crystals In KIMS Experiment J.H. Choi (Seoul National University) SUSY2012, Beijing.
The Particlelike Properties of Electromagnetics Radiation Wei-Li Chen 10/27/2014.
What is it? A tool used by scientists to gather information about scientific observations and questions.
Dark Matter Search with Direction Sensitive Scintillators NOON2004 Work Shop February 14, 2004, Odaiba H. Sekiya University of Tokyo M.Minowa, Y.Shimizu,
Neutron scattering systems for calibration of dark matter search and low-energy neutrino detectors A.Bondar, A.Buzulutskov, A.Burdakov, E.Grishnjaev, A.Dolgov,
Ian Ross Rose-Hulman Institute of Technology Mentor: Dr. Richard Teuscher University of Toronto ATLAS Group ATLAS Calorimetery: Cosmic Ray Commissioning.
Iwha Womans University 2005/04/22 Hyunsu Lee & Jungwon Kwak Current Limit of WIMP search with CsI(Tl) crystal in KIMS 이현수 *, 곽정원, 김상열, 김선기, 김승천,
Issues concerning the interpretation of statistical significance tests.
Hypothesis Testing An understanding of the method of hypothesis testing is essential for understanding how both the natural and social sciences advance.
The IceCube Neutrino Observatory is a cubic kilometer detector at the geographic South Pole. We give an overview of searches for time-variable neutrino.
1 水质契仑科夫探测器中的中子识别 张海兵 清华大学 , 南京 First Study of Neutron Tagging with a Water Cherenkov Detector.
NoRH Observations of RHESSI Microflares M.R. Kundu, Dept. of Astronomy, University of Maryland, College Park, MD E.J.Schmahl, Dept. of Astronomy, University.
MaGe framework for Monte Carlo simulations MaGe is a Geant4-based Monte Carlo simulation package dedicated to experiments searching for 0 2  decay of.
Study of the Atmospheric Muon and Neutrinos for the IceCube Observatory Ryan Birdsall Paolo Desiati, Patrick Berghaus,
PHY418 Particle Astrophysics
Dark Matter Search with Direction Sensitive Scintillators The10th ICEPP Symposium February 16, 2004, Hakuba H. Sekiya University of Tokyo.
Daily Modulation of the Dark Matter Signal in Crystalline Detectors Nassim Bozorgnia UCLA TexPoint fonts used in EMF. Read the TexPoint manual before you.
Implications of CoGeNT's New Results For Dark Matter Chris Kelso University of Chicago DESY Theory Workshop Sep. 28, 2011.
WIMP search Result from KIMS experiments Kim Seung Cheon (DMRC,SNU)
? At Yangyang beach, looking for something in the swamp of particles and waves. 1 The recent results from KIMS Seung Cheon Kim (Seoul National University)
5 June 2002DAQ System Engineering Requirements 1 DAQ System Requirements DOM Main Board Engineering Requirements Review David Nygren.
Medium baseline neutrino oscillation searches Andrew Bazarko, Princeton University Les Houches, 20 June 2001 LSND: MeVdecay at rest MeVdecay in flight.
KIMS Seoul National University Juhee Lee 1 KPS in Changwon.
Some EOVSA Science Issues Gregory Fleishman 26 April 2011.
Chapter 10: States of Matter Changes of State. Objectives Explain the relationship between equilibrium and changes of state. Interpret phase diagrams.
PyungChang 2006/02/06 HYUNSU LEE CsI(Tl) crystals for WIMP search Hyun Su Lee Seoul National University (For The KIMS Collaboration)
Potential for Dark Matter Direct Searches in Australia Professor Elisabetta Barberio The University of Melbourne.
11 ELECTROMAGNETIC RADIATION. 22 EM RADIATION II ALSO CALLED RADIANT ENERGY ONLY A PORTION IS CALLED LIGHT TRAVELS IN WAVES TRAVELS THROUGH SPACE (VACUUM)
1 CRESST Cryogenic Rare Event Search with Superconducting Thermometers Jens Schmaler for the CRESST group at MPI MPI Project Review December 14, 2009.
Observation Gamma rays from neutral current quasi-elastic in the T2K experiment Huang Kunxian for half of T2K collaboration Mar. 24, Univ.
Alex Howard, Imperial College Slide 1 July 2 nd 2001 Underground Project UNDERGROUND PROJECT – Overview and Goals Alex Howard Imperial College, London.
KIMS & Inelastic DarK Matter(iDM)
Cosmogenic Muon Background
The Antares Neutrino Telescope
Sterile Neutrinos and WDM
The Candle Flame Measuring the temperature of a flame according to the “three zones model”
CRESST Cryogenic Rare Event Search with Superconducting Thermometers
Constraining neutrino electromagnetic properties using Xenon detectors
Detecting WIMPs using Au-DNA Microarrays
Presentation transcript:

TIPP A Testable Conventional Hypothesis for the DAMA-LIBRA Annual Modulation Signal David Nygren LBNL

TIPP S is modulation signal amplitude: S =  (2-5 keV)

TIPP from: arXiv known background: potassium

TIPP Signal or Background: n, , , or ? High energy neutrons calculated to be weak by two to three orders of magnitude; –Ralston argues that epithermal neutrons have been under-appreciated: arXiv: v1 Multi-hit events show no modulation in D-L –Why not? Icarus sees ~4% neutron modulation –Are multi-hit events all  -rays? Can’t be atmospheric neutrinos (  ~ 1 mb)

TIPP Did the muons really do it? Muons in Gran Sasso display modulation –S muons ~0.015  according to LVD –Phase (LVD): 15 July  15 days Muons strike D-L about times a day –about 2,000,000 keV are deposited/day –D-L modulation signal: 3,000 keV/day Muons deposit ~600 times more energy

TIPP The delayed pulse hypothesis From St. Gobain Technical note #527 on exposure of NaI(Tl) crystals to UV : “ With mild exposure several pulses/second can be seen in the 6-10 keV region of a spectrum. If the crystal is stored in a dark area, this mild UV exposure will eventually disappear, although it may take from several hours to several days for the effects to stop.” (Emphasis added). Here, the manufacturer of the D-L crystals suggests that a delayed phosphorescence phenomenon can produce pulses in the approximate energy range of interest for D-L!

TIPP Plausible or implausible? keV is not exactly the right range... –but, maybe, D-L is uniquely able to see pulses below 6 keV due to extreme radiopurity. Does NaI(Tl) display phosphorescence? –Yes, time constants of 0.15 s to hours, days –NaI displays strong temperature dependence indicating thermal activation energies exist, also with non-luminescent pathways

TIPP Plausible or implausible? What does UV have to do with muons? –Herbert N. Hersh, Phys. Rev. 148(2) (1966) p928 argues that UV, x-rays, high-energy ionizing particles have very similar production of excitons within alkali halide crystal lattice. –These excitons can migrate through the lattice, sometimes leading to defects and color centers –Muons may evoke phosphorescence.

TIPP Plausible or implausible? But, how does the NaI crystal turn stored energy into pulses of light? –Not clear, but not implausible –Excitonic migration exists, then aggregation along muonic ionization path may occur –Smaller pulses seem more likely than large ones –Worthy of attention: “...the effects of UV light to NaI have never been closely studied...” - St. Gobain, #527

TIPP Amplitude OK? D-L: –modulation amplitude of  LVD: –modulation amplitude of  (  ) Icarus: –modulation amplitude of 4% (neutrons) Water content of Gran Sasso varies Not clear how to interpret disparities

TIPP Phase OK? D-L: Phase is June 2 ±7 days LVD: Phase is July 15 ±15 days D-L’s assertion that the discrepancy is ~6  ignores the error quoted by LVD! Also, the 7 day phase error is obtained only if the period is fixed in the fit; including period in the fit increases phase error by ~ 3. Phase discrepancy appears to be less than 2.5 

TIPP What to do? D-L could search for space-time correlation in their data; which crystals were hit by muons, followed by a “signal event” –any level of correlation is a red flag! D-L could run with a substantially lower temperature, “freezing out” delayed phosphorescence effects discussed here. –easier than building new detector or moving

TIPP What to do? D-L could expose a crystal in their detector to a  -ray source to evoke phosphorescence; –test could possibly disprove this hypothesis Others could also perform this test if their setup is sufficiently radio-pure to see 3 keV –underground muons at x10 level of D-L OK

TIPP Summary : An obligation endures to ensure that no conventional explanation can satisfy all the requirements of D-L for a WIMP signal The delayed pulse hypothesis may provide at least part of a conventional explanation. Easier to test than a completely new cycle of running or construction!

TIPP