Neutrino astronomy with AMANDA and IceCube

1
Neutrino astronomywithAMANDA and IceCube

• Per Olof Hulth
• Stockholm University
• hulth_at_physto.se

2
Content

• Introduction
• AMANDA results
• IceCube expectations
• Summary

3
Short summary of neutrinos for pedestrians

• There are three different families of leptons
• Electron neutrino (?e) and the electron (e-)
• Muon neutrino (??) and the muon (?-)
• Tau neutrino (??) and the tau (?-)
• The neutrinos penetrates huge amount of matter
  without being absorbed
• E.g. a 1 MeV neutrino from the sun has an
  absorption length of 20 light years in lead!!

4
Some neutrino numbers

• The Sun sends every second out 200.000.000.000.000
  .000.000.000.000.000.000.000.000 (21038)
  neutrinos
• At Earth we receive about 40.000.000.000
  neutrinos/cm2/second
• From Big Bang we have 330 000 000 neutrinos/m3
  (Energi 0.0004 eV) but only half a proton
• 340 000 000 neutrinos are creataed in our body
  every day (40K)

5
Neutrinos from Supernova

• When a star explodes 99 of the energy is emitted
  in neutrinos
• A star exploded 1054. Today the Crab nebula

6
Gamma astronomy
Space is not transparent for High Energy Photons!
R. Svensson Zdziarski AA.Ap.J.349415-28(1990) Kne
iski TM, Mannerheim K, Hartmann D.Ap.J. Submitted
2000)
7
Three open questions in Astrophysics

• What is the missing dark matter in the Universe?
• What is the origin of the Highest Energy Cosmic
  rays?
• What is powering the Gamma Ray Bursts (GRB)?

8
You need 20 times more matter to keep the system
together than what is observed DARK MATTER !!!!

9
Most popular model

• New type of matter (WIMPs)
• Supersymmetric particles from Big Bang
• Neutralinos.

10
WIMPs from Sun/Earth
Dark Matter search
Look for excess of neutrinos from centre of the
Earth and the Sun!!
11
Cosmic rays
proton
mesoner
muons
About 100 muons/m2sek
12
Cosmic rays
Energies up to 50 Joules! What is the process
creating these particles???
13
A possible candidate for a source for cosmic rays
14
Gamma Ray Bursts
Source 9 Billion light years away!
The sources of GRBs on cosmologic distances! The
most violent objects in the Universe
15
Gamma Ray Bursts

• Could be danger to be too close

16
Messengers of Astronomy
Only neutrinos cover the whole energy range
17
Neutrino production
If protons are accelerated we expect about equal
amount of gammas and neutrino!!
18
Classes of Models
log(E2 ? Flux)
pp core AGN
p? blazar jet
Top-Bottom model
Various recent models for transient sources
GRB (WB)
3 6
9
log(E/GeV)
TeV PeV EeV
19
Neutrino astronomy so far

• Only two neutrino sources in space has been
  observed.
• The solar neutrinos (Nobel price 2002)
• Neutrinos from SN1987 in the Large Magellanic
  Cloud (180 000 light years)
• Energy of neutrinos only 1-30 MeV

20
Neutrino physics (again)
We have three types of neutrinos Electron
neutrino ne Muon neutrino nm Tau
neutrinon nt
E.g. Neutron decay neutron -gt proton e-
ne
21
Neutrino interaction
??
??
lt 1 degree
The muon can travel several km in e.g. ice
22
Cherenkov radiation
A charged particle moving with the speed of light
in the medium will generate a shock wave of light
q
cosq 1/(nb) b v/c, n refraction index
23
The AMANDA telescope at the South Pole
Why the South Pole? A 3000 meter thick glaciar
A scientific base with all infra structure No
fishes and no 40K
24
AMANDA
25
South Pole
26
(No Transcript)
27
Joakim Edsjö SU
28
Joakim Edsjö SU
29

myon
neutrino
30

106 muons from cosmic rays/muon from
neutrinos !!!!
myon
Select only muons from below!!!!
neutrino
31
Hot water heaters

-50 m
-55 C
-25 C
-2400 m
32
Joakim Edsjö SU
33
(No Transcript)
34
-840 m
35
AMANDA
36
(No Transcript)
37
AMANDA Event SignaturesMuons
DATA
CC muon neutrino interactions ? Muon tracks
nm N ? m X
38
Point Sources Amanda II (2000)
Skyplot is scrambled in event time for blind
analysis, Plot has been released, and results
will be available soon. Examples for a few
candidates will be given.

Equatorial coordinates declination vs. right
ascension.
39
Point Sources Amanda II (2000)
Results for three examples of possible sources
PRELIMINARY
Source candidate looked at Mrk421 Mrk501 SS433
Declination 38.2 39.8 5.0
Right ascension 11.1 16.9 19.2
Fm(Egt10GeV,90 c.l.)/10-15 cm-2 s-1 2.05 1.71 10.52
Fn(Egt10GeV,90 c.l.)/10-8 cm-2 s-1 1.28 1.06 3.49
Number of events (observed) 2 1 7
Number of events (background) 1.5 1.1 4.1
Muon sensitivity (as Fm) 1.72 1.80 6.05
Neutrino sensitivity (as Fn) 1.07 1.12 2.01
Fm Limit on integrated E-2 muon flux above 10
GeV 10-15 cm-2 s-1 Fn Limit on integrated E-2
neutrino flux 10-8 cm-2 s-1
40
AMANDA B10 and A-II some limits and projected
sensitivity
10-13
m ? cm-2 s-1
AMANDA B10 average Sensitivity for sel. soruces
Super-Kamiokande
To appear in ApJ astro-ph/0208006
10-14
A-II, limit on SS433
A-II, sensitivity on SS433
MACRO
10-15
SS433
A-II, limit on Mrk 501
A-II projected sensitivity Combined 97-02
Mrk501 (HEGRA 97, n/g1)
Declination (deg)
41
AMANDA-II Online analysis
4.5 atmospheric ??candidates / day
The Stockholm model
42
Amanda Analysis activities

• AMANDA-B10 1997 analysis at the end
• AMANDA-B10 1999 analysis started
• AMANDA-II 2000 filtering done, first analyses
  started
• AMANDA-II 2001 online filtering continuously done

In order to do a blind analysis only 20 of the
data is used for tuning cuts
43
IceCube!!
IceCube has been designed as a discovery
instrument with improved
telescope area detection volume energy
measurement of secondary muons and
electromagnetic showers identification of
neutrino flavor angular resolution
44
The IceCube Collaboration
Institutions 11 US and 8 European institutions
Bartol Research Institute, University of
Delaware BUGH Wuppertal, Germany Universite Libre
de Bruxelles, Brussels, Belgium CTSPS,
Clark-Atlanta University, Atlanta
USA DESY-Zeuthen, Zeuthen, Germany Institute for
Advanced Study, Princeton, USA Lawrence Berkeley
National Laboratory, Berkeley, USA Department of
Physics, Southern University and A\M College,
Baton Rouge, LA, USA Dept. of Physics, UC
Berkeley, USA Institute of Physics, University
of Mainz, Mainz, Germany Dept. of Physics,
University of Maryland, USA University of
Mons-Hainaut, Mons, Belgium Dept. of Physics and
Astronomy, University of Pennsylvania,
Philadelphia, USA Dept. of Astronomy, Dept. of
Physics, SSEC, University of Wisconsin, Madison,
USA Physics Department, University of Wisconsin,
River Falls, USA Division of High Energy Physics,
Uppsala University, Uppsala, Sweden Dept. of
Physics, SCFAB, Stockholm University, Stockholm,
Sweden University of Alabama Vrije Universiteit
Brussel, Brussel, Belgium
Also AMANDA only IceCube
Spokesperson P.O.Hulth Stockholm
University Co-spokesperson F.Halzen University
of Wisconsin
45
The IceCube Collaboration

• 11 European, 1 Japanese, 1 South American and 11
  US Institutions
• (many of them are also AMANDA member
  institutions)
• Bartol Research Institute, University of
  Delaware, Newark, USA
• BUGH Wuppertal, Germany
• Universite Libre de Bruxelles, Brussels, Belgium
• Dept. of Physics, Chiba University, Japan
• CTSPS, Clark-Atlanta University, Atlanta USA
• DESY-Zeuthen, Zeuthen, Germany
• Imperial College, London, UK
• Institute for Advanced Study, Princeton, USA
• Dept. of Technology, Kalmar University, Kalmar,
  Sweden
• Lawrence Berkeley National Laboratory, Berkeley,
  USA
• Dept. of Physics, Southern University and A\M
  College, Baton Rouge, LA, USA
• Dept. of Physics, UC Berkeley, USA
• Institute of Physics, University of Mainz,
  Mainz, Germany
• Dept. of Physics, University of Maryland, USA
• University of Mons-Hainaut, Mons, Belgium
• Dept. of Physics, Pennsylvania State University,
  University Park, PA, USA

46
IceCubeTop View
80 strings 60 modules/string Volume 1 km3 Depth
1400-2400 m
Counting House
47
IceTop
AMANDA
South Pole
IceCube
Skiway
80 Strings 4800 PMT
1400 m
2400 m
48
??- flavors and energy ranges
Filled area particle id, angle, energy Shaded
area energy and angle.
49
µ-events in IceCube
Eµ6 PeV
Eµ10 TeV
AMANDA-II
1 km
Measure energy by counting the number of fired
PMT. (This is a very simple but robust method)
50
Sensitivity to diffuse n?-fluxes
Atmospheric neutrino flux (after quality cuts)
130.000 / year Signal hard spectrum (E-2) Apply
energy cut 200 PMT signals (5 background
events left) Sensitivity (3 yr) dN/dEn 4.8 x
10-9 E-2/(cm2 sec GeV)
51
Diffuse Fluxes Predictions and Limits
Mannheim Learned, 2000
Macro
Baikal
Amanda
IceCube
52
Point source sensitivity
53
Compare to Mrk 501 gamma rays
Field of view Continuous 2 p sr (northern sky)
AMANDA B10 prelim. limit
Sensitivity of 3 years of IceCube
54
Neutrinos from Gamma Ray Bursts
Test signal 1000 GRB a la Waxman/Bahcall 1999
Expected no. of events 11 upgoing muon
events Expected background 0.05
events Sensitivity (1000 bursts)


0.2
? dN/dE (Waxman/Bahcall 99)
Only 200 GRB needed to detect/rule out WB99
flux
55
Cascade event
ne N --gt e- X
The length of the actual cascade, 10 m, is
small compared to the spacing of sensors 1 PeV
500 m diameter Fully active calorimeter with
linear energy resolution
Sensitivity for diffused flux about the same as
for muons
E 375 TeV
56
Double Bang
?t N --gt t- X
?t X

• E ltlt 1 PeV Single cascade
• (2 cascades coincide)
• E 1 PeV Double bang
• E gtgt 1 PeV Second cascade tau
  track

57
Tau neutrinos and oscillations
Enhanced role of tau neutrinos because of
neutrino oscillation!?
Cosmic beam ne nµ nt because of
oscillations nt not absorbed by the Earth
(regeneration) Pile-Up near 1 PeV where ideal
sensitivity IceCube sensitive to ?m2gt10-17 eV2
58
Dark matter detection with IceCube
WIMPS from Earth
WIMPS from Sun
Ice3 will significantly improve the
sensitivity!
59
Supernova detection

• ne p n e (10-40 MeV)
• PMT noise increase due to the positrons
• AMANDA/IceCube records the noise of the PMTs
  over 0.5 sec and summing up total rate over 10
  sec intervals.
• Detectors to be connected to Supernova Early
  Warning System

AMANDA
IceCube
In addition to the MeV ?e neutrinos, 10-100 muon
neutrinos are expected after a few hours in the
TeV energy range.
60
IceCube deployment schedule
61
Summary

• IceCube will open a significant new window on the
  Universe.
• Hopefully we will observe something which has not
  been discussed in this presentation.

62
Hotwater Drilling
Experience with AMANDA 19 holes Upgradefrom 2
to?5 MW Projected time to 2450 m depth 40
h Diameter 50 cm Drill 2 holes per week 16
holes per season
63
Optical sensor
Installation of one sensor 10 min
64
(No Transcript)
65
Mats Pettersson Gymnasielärare från Angereds
gymnasium Göteborg vid sydpolen 14 november 2001
66
(No Transcript)
67
Joakim Edsjö SU
68
Joakim Edsjö SU
69
Joakim Edsjö SU
70
(No Transcript)