WIN05 Astroparticle Physics (WG4) Summary

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WIN05 Astroparticle Physics (WG4) Summary

• Mark Vagins
• University of California, Irvine

Delphi, Greece June 6 - 11, 2005
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Thanks to Rachel Bean, my missing co-convener
(theory).
Any omissions/errors are my responsibility!
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Auger Observatory
Stephane Coutu

• 10 years 3000 km2 yields 300 -500 events gt1020
  eV
• SOURCES? Two Observatories Necessary

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The Cosmic Ray Spectrum
Fluxes rescaled by E2
gt1019 eV 1 per (km2 year sr)
gt1020 eV 1 per (km2 century sr)
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Techniques for UHECR Detection

• UHECR generate cascades (showers) in the
  atmosphere
• 1020 eV yields 1011 particles at maximum

• Shower front particles can be
• directly detected on the ground
• Showers excite nitrogen
• fluorescence, detectable on dark
• nights

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Auger Hybrid Detector
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Auger Surface Detectors
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Auger Status June 05

• 793 surface detectors deployed (755 fully
  functional)
• 3 fluorescence detector buildings completed, 1
  under construction (15 telescopes fully
  instrumented)

Completion date July 2006
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First Auger Spectrum
Total acceptance is ?? ? 1015 m2 sr s
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Astrophysical Sources
of TeV to GZK neutrinos

• Peter Mészáros
• Pennsylvania State University

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Acceleration to 1021eV? 102
Joules 0.01 MGUT

• dense regions with exceptional
• gravitational force creating relativistic
• flows of charged particles, e.g.
• coalescing black holes/neutron stars
• dense cores of exploding stars
• supermassive black holes

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GZK neutrinos
they are a guaranteed source!!

• Ultra-high energy cosmic rays
• Origin unknown, but
• Standard Model
• Ordinary charged particles accelerated by distant
  sources AGN, GRBs
• If so GZK neutrinos are the signature
• Probably necessary and sufficient to confirm
  standard GZK model

n
GZKbrick wall

• Two predictions
• 1. There is a brick wall for the highest energy
  cosmic rays. We should observe energies below
  about 1020 eV.
• 2. Reactions that limit the cosmic ray energies
  produce neutrinos as a by-product

GZK neutrinos ? probably 2nd most likely source
of UHE neutrinos!
(Courtesy A. Silvestri via D. Saltzberg)
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What do we need for a GZK n detector?
Standard model GZK Fn lt1 per km2 per day
Only 1 in 500 interact in ice
Both AMANDA-II or IceCube may expect to see 1
event every 2 years in its fiducial
volume requires astronomical level of patience!
How can we get the 100-1000 km3 sr yr exposures
needed to detect GZK neutrinos at an acceptable
rate?
QUESTION

• Askaryan process coherent radio Cherenkov
  emission
• EM cascades produce a charge asymmetry ? radio
  pulse
• Process is coherent ? Quadratic rise of power
  with cascade energy
• Neutrinos can shower in radio-transparent media
• air, ice, rock salt, etc.
• ?RF economy of scale very competitive for giant
  detectors

ANSWER
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Summary UHE ?

• GRBs ? 1020 eV protons
• - Predictions ?103 km2 area detectors
• - Experiments HiRes, Auger, EUSO/OWL
• GRBs ? 10 GeV, 1 Tev, 100 TeV, 1018 eV ?s
• - Flux ? 1 Gton detectors
• - Exps AMANDA, IceCube, Antares,
  Nestor, Nemo
• ? detection
• - GRBs CR puzzle, GRB progenitors
  physics
• - ? physics ?? ??? ? ? appearance
• - Cross sections at E gt LHC

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The Diffuse Supernova Neutrino Background
Louie Strigari The Ohio State
University
Collaborators John Beacom, Manoj Kaplinghat,
Gary Steigman, Terry Walker, Pengjie Zhang
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DSNB The Big Picture
Core Collapse of Massive Star
Gives Burst of 1058 Neutrinos

Massive Star Formation Since z 6

The Diffuse Supernova Neutrino Background (DSNB)
Cosmological background of neutrinos from all
supernovae that have occurred
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DSNB Detection
Event Rate of targets x cross section
x flux
Largest Yield from Inverse Beta
Super-Kamiokande (22.5 kton)
1.5 x 1033
Invisible
Visible
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Backgrounds to Detection
Atmosphere
Below 50 MeV, Muon is Invisible
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Super-K Upper Limit

• 4 years of data gives flux limit 1.2 cm-2
  s-1
• Detection signature is an excess of events
• Detection timescale with fiducial model is 9
  years
• Strigari, Kaplinghat, Steigman, Walker 2004

Super-Kamiokande Collaboration, PRL 90, 061101
(2003)
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DSNB Event Rate Predictions

• Modern predictions for Super-K
  3 events/yr above 18 MeV
  6 events/yr above 10 MeV
• Ando, Sato Totani 2003
• Fukugita Kawasaki 2003
• Strigari, Kaplinghat, Steigman Walker 2004
• Atmospheric Background Reduction
• Beacom Vagins 2004

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DARK ENERGY
PHENOMENOLOGY PRESENT/FUTURE OBSERVATIONS
RICHARD BATTYE
JODRELL BANK OBSERVATORY SCHOOL OF PHYSICS AND
ASTRONOMY UNIVERSITY OF MANCHESTER
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BASIC OBSERVATIONAL SITUATION
SNe Ia

2dF/SDSS
CMB
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DARK ENERGY

• PRESSURE TO DENSITY RATIO
• w-1 COSMOLOGICAL CONSTANT
• SCALAR FIELDS QUINTESSENCE
• TOPOLOGICAL DEFECT LATTICES
• MODIFICATIONS TO GRAVITY ?
• SUPER-HORIZON PERTURBATIONS !

ASSUME FLAT UNIVERSE
NB POSSIBLE NON-MINIMAL COUPLING TO GRAVITY
EASY TO MODEL GIVEN A LAGRANGIAN
MODELLED AS A RELATIVISTIC SOLID ie A FLUID WITH
RIGIDITY
COSMIC STRINGS w-1/3DOMAIN WALLS
w-2/3
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TWO CLASSES OF TESTS
GEOMETRICAL
GROWTH OF STRUCTURE
ONLY DEPENDS ON w !
GROWTH DEPENDS ON w AND ALSO ON THE PROPERTIES
OF THE DARK ENERGY
ANGULAR DIAMETER DISTANCE
LINEAR REGIME
LUMINOSITYDISTANCE
NON-LINEAR REGIME
(i) MASS FUNCTION (ii) SPHERICAL COLLAPSE
() OFTEN GEOMETRIC DEPENDENCE AS WELL
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CONCLUSIONS

• DARK ENERGY APPEARS TO EXIST
• GOOD MICROSCOPIC MODELS SCARCE
• PHENOMOLOGICAL DESCRIPTION REQUIRED
• IN PRINCIPLE MANY WAYS TO TEST IT
• MANY SYSTEMATIC ISSUES TO BE ADDRESSED
• VARIATION IN w DIFFICULT
• DARK ENERGY EXPERIMENTS COST 10 MILLION
  //EUROS

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And then
Genevieve Belanger SSM Dark Matter (WG1)
Andrew Taylor Weak Lensing
Gravity from diffuse sources distorts background
galaxy shapes into ellipses ? Powerful technique
for probing (dark) matter distributions Now using
redshift data for 3D modeling of dark matter
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Ground-based and Future Observations of the
Cosmic Microwave Background
Anthony Lasenby Astrophysics Group, Cavendish
Laboratory, Cambridge University
DelphiApril 7th 2005
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Latest CMB results - CAPMAP

• CAPMAP Cosmic Anisotropy Polarization Mapper
• Chicago, Princeton, JPL, Caltech and others
  collaboration
• Four 84 100 GHz polarization receivers mounted
  in focal plane of a Lucent 7m telescope in New
  Jersey (Crawford Hill)
• Going after E-mode anisotropy at 4 scale, in two
  wide bins
• First results reported February 2005 (Barkats et
  al, astro-ph/0409380)
• Heterodyne technology and collaboration prototype
  for QUIET (see later)

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Current Experiments - QUAD

• QUAD Quest at DASI
• Cardiff, Stanford, Chicago, Edinburgh and others
  collaboration
• 100 and 150 GHz polarization sensitive
  bolometers, feeding 2.6 m primary
• On DASI mount at South Pole
• Also going after E-mode anisotropy at 4 scale
• Data-taking now underway over-winter at South
  Pole (currently -75 degrees C!)

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New CMB projects - CLOVER

• CLOVER
• Joint project between Cambridge, Cardiff and
  Oxford
• Aim is to image B-mode polarization of the CMB
• Smoking gun tensor mode perturbations (gravity
  waves) in early universe
• Funded by PPARC construction beginning

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The NESTOR Neutrino Telescope Site
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32 m diameter 30 m between floors
20 000 m2 Effective Area for Egt10TeV
Energy threshold as low as 4 GeV
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March 2003
Successful deployment of one NESTOR star with 12
Optical Modules to 4000m using the cableship
RAYMOND CROZE (FranceTelecom) 30th of March
The first deep sea muon data transmitted to
shore through a 30km long electro-optical cable
to the Methoni counting room
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The ANTARES Collaboration
Alexander Kappes
20 institutions from 6 European countries
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The ANTARES Detector

• Hostile environment
• pressure up to 240 bar
• sea water (corrosion)

artists view (not to scale)
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Detector Infrastructure and Prototype Lines

• Deep-sea cable to shore station deployed
• Junction box deployed and connected to deep-sea
  cable
• Prototype lines deployed, connected to junction
  box and successfully recovered after 5 months
  (2003)

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New Test-Lines MILOM and Line0

• Deployed March 2005, connected April 2005

Line0 full line without electronics (test of
mechanical structure)
MILOM Mini Instrumentation Line with Optical
Modules
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ANTARES further schedule

• First full string (Line1) to be deployed and
  connected end of 2005
• Full detector installed in 2007
• From 2006 on physics analysis !

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Paolo Desiati
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First year deployment (Jan 2005) 1 IceCube
string (60 OMs) 8 IceTop Tanks (16 OMs)
IceTop 160 tanks frozen-water tanks 2 OMs / tank
1200 m

IceTop
IceCube
AMANDA
IceCube 80 strings 60 OMs/string 17 m vertical
spacing 125 m between strings

10 Hamamatsu R-7081
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n telescope AMANDA event
energy deposited in OM
time recorded on OM
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n telescope point source search
Detection of nm with time rolling search

• time window 40 / 20 days for Extragalactic /
  Galactic Objects
• angular bin 2.25-3.75

Source Nr. of n events (4 years) Expected backgr. (4 years) Period duration Nr. of doublets Chance probability
Markarian 421 6 5.58 40 days 0 1
1ES1959650 5 3.71 40 days 1 0.34
3EG J12274302 6 4.37 40 days 1 0.43
QSO 0235164 6 5.04 40 days 1 0.52
Cygnus X-3 6 5.04 20 days 0 1
GRS 1915105 6 4.76 20 days 1 0.32
GRO J042232 5 5.12 20 days 0 1
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IceCube deployment plan

• January 05
• Strings 1
• Tanks/stations 8/4
• 05/06 Plan
• Strings 10 - 12
• Tanks/stations 24/12

runway
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1st Launch in 2006!
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Super-Kamiokande
Yasuo Takeuchi

• SK-I (19962001)
• 50000ton water
• 11200 of 20inch PMTs
• Fid. vol. 22.5kt
• Photo coverage 40
• Stopped by the accident in Nov. 2001
• SK-II (Dec. 2002)
• 5200 of 20inch PMTs
• Photo coverage 19

Electronics hut
LINAC
Water and air purification system
Control room
Atotsu entrance
41.4m
Ikeno-yama Kamioka-cho, Gifu
1km (2700mwe)
2km
3km
SK
Mozumi
Atotsu
39.3m
Inner Detector (ID) 11146 of 20 inch PMTs (SK-I)
Outer Detector (OD) 1885 of 8 inch PMTs (SK-I
SK-II)
50000 ton stainless steel tank
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8B Flux
Consistent with SK-I
SK-I result 2.35 /-0.02(stat.) /-0.08(syst.)
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Energy spectrum
Consistent with SK-I
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Day / Night asymmetry
(Day-Night)
0.024 - 0.025
ADN
0.014/-0.049(stat.) (sys.)
(DayNight)/2
Preliminary
0.013
SK-I D/N Asymmetry -0.021/-0.020
- 0.012
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Future plan
NOW
1996 1997 1998 1999 2000 2001 2002 2003 2004 2005 2006 2007
SK-I
SK-II
SK-III
Accident
SK full reconstruction (plan)
DAQ stop November 2005 March 2006
ID PMT SK-II 5200 SK-III 11146
(same as SK-I) Original energy vertex
resolutions for low-energy events
Solar neutrinos below 5.0MeV with improved
analysis tools and lower Rn backgrounds
Precise study on spectrum distortion in SK-III
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Possibility of detecting spectrum distortion
ne survival probability
Recoil electron spectrum
10 upturn should be seen
P(ne ? ne)
syst. error
Dm2 (eV2) 6.3 x 10-5 4.8 x 10-5 7.2 x 10-5 10.0
x 10-5 7.2 x 10-5
tan2(q) 0.55 0.38 0.38 0.38 0.28
En (MeV)
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A future option - Gd doped SK (GADZOOKS!)
Beacom Vagins, PRL93 (2004)171101

• Gd doped SK is seriously studied as a future
  option of SK, lead by UCI group.
• Physics targets SN relic neutrinos, reactor
  anti-neutrinos, galactic SN neutrinos,
  long-baseline neutrinos, proton decay BG
  reduction,

ne p ? e n
(tag this neutron)
90 captured on Gd, gs, total Eg 8MeV 0.2 on
Cl, gs, total Eg 8.6MeV Others on p, 2.2MeV g
0.2 GdCl3
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Atsushi Takeda

• Whats XMASS

Multi purpose low-background experiment with liq.
Xe

• Xenon MASSive detector for solar neutrino
  (pp/7Be)
• Xenon neutrino MASS detector (bb decay)
• Xenon detector for Weakly Interacting MASSive
  Particles (DM search)

Dark matter
Double beta
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• Why liquid xenon

• Large Z (54)
• Self-shielding effect
• Large photon yield (42 photons/keV NaI(Tl))
• Low threshold
• High density (3 g/cm3)
• Compact detector (10 ton sphere with
  diameter of 2m)
• Purification (distillation)
• No long life radioactive isotope
• Scintillation wavelength (175 nm, detected
  directly by PMT)
• Relative high temperature (165 K)

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• Strategy of the scale-up

10 ton detector
800kg detector
100kg Prototype
With light guide
30cm
80cm
2.5m
RD
Dark matter search
We are now here
Multipurpose detector (solar neutrino, bb )
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• 100 kg prototype detector

In the Kamioka Mine (near Super-K)
2,700 m.w.e.
OFHC cubic chamber
Gamma ray shield
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Geometry design (800 kg)

• A tentative design
• (not final one)

12 pentagons / pentakisdodecahedron
This geometry has been coded in a Geant 4 based
simulator
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Dark Matter Searches - Scientific Motivation
Tim Sumner

• Cosmology is the dark matter that makes up
  22 of the Universe in the form of massive
  particles?

• Supersymmetry are these the particles
  predicted by supersymmetry?

• Galaxy formation and dynamics how do these
  particles behave within galaxes?

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Direct DM Search World Status

• Comparison between experiments made using a
  standard Galaxy model
• Separated into spin-independent (scalar)
  cross-sections and spin-dependent (axial)
  cross-sections and normalised to one nucleon

• Spin independent
• DAMA
• IGEX
• CRESST II
• CDMS I
• EDELWEISS
• ZEPLIN I
• CDMS II

N.B. Predictions extend down to 10-47 cm2!
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IGEX, DRIFTI, II
WIMP elastic nuclear recoils deposit lt 100keV of
energy at a rate 10-5 to 1 event/day/kg
? phonons, photons and charge whose relative
proportions and /or characteristics depend on
dE/dx ? particle type
CDMS, EDELWEISS
ZEPLIN II, III, MAX, XENON
NAIAD, ZEPLIN I, DAMA
CRESST I
CRESST II, ROSEBUD
World competition is intense and uses a wide
range of complementary techniques
Event-by-event particle identification requires
compound information
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ZEPLIN II data in four months
ZEPLIN III underground in 6 mon.
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• UKDMC has a unique and very strong world
  position, and is poised for rapid advances.
• Dedicated world-class well-equipped
  low-background underground laboratory.
• Competitive world limits already demonstrated.
• A new generation of competitive and scalable
  high-sensitivity instruments (ZII and ZIII) about
  to be deployed with limiting sensitivities 10-7
  to 10-8 pb.
• Upgrade paths for these instruments to extend the
  sensitivity to 10-9 pb.
• A unique and scalable directional technology
  leading to significant galactic astrophysics
  return.
• Multiple target options for confirmation and
  constraining SUSY parameter space.
• Mature plans for achieving tonne-scale targets.

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Daniel McKinsey
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CLEAN - 10 tons fiducial LNe needed for pp solar
neutrinos
Mini-CLEAN (600 kg LNe) in SNOLAB in 2007? RD
plus WIMP search
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And thats the way it was in WG4.