Transcript AMANDA people in Sweden

AMANDA
The Wierdest wonder
• Is it good or is it bad?
2000-06-21
Per Olof Hulth
AMANDA
AMANDA experience
• Bad
 Calibration of the detector very heavy (“perfect” time constants for
AMANDA-B13 ready first May 2000!) The analysis delayed due
to this.
• Good
 Deployment procedure established.
 “Easy” to reconstruct neutrinos
2000-06-21
Per Olof Hulth
AMANDA
AMANDA deployment history
1995/1996
A M A N DA- B4
N umbe r
of
dep loyed
OM
86
1996/1997
A M A N DA- B10
218
10
302
1998/1999
A M A N DA- B13
125
13
428
1999/2000
A M A N DA- II
252
19
680
Y ear
2000-06-21
D et ector
T ot al
numb er o f
st rings
T ot al
numb er o f
OM
4
86
Per Olof Hulth
AMANDA
AMANDA data analysis
• The first neutrino candidates published from AMANDA-B4
(data 1996)
• AMANDA-B10 data 1997 analysis in progress for
 Atmospheric neutrinos
 Search for WIMP annihilation in the Earth
 n point sources
 Diffuse n flux
 Neutrinos from GRB
 and Supernova, magn. monoples, AMANDA-SPASE etc
2000-06-21
Per Olof Hulth
AMANDA
AMANDA data analysis
AMANDA-B10 data is analysed for several different
topics with the following in a “final” stage:
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Atmospheric neutrinos
WIMP search from Earth
Point sources
Diffuse neutrino flux
2000-06-21
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Neutrinos from GRB
Supernova neutrinos
Magnetic monopoles
AMANDA-SPASE
Per Olof Hulth
AMANDA
2000-06-21
AMANDA-II
Feb. 00
Per Olof Hulth
AMANDA
AMANDA n-candidate
• Early photons are red, late
photons are blue. More
photons are larger circles
• Bottom of array is toward
center of Earth
• The muon is clearly
traveling in the upward
direction
2000-06-21
Per Olof Hulth
AMANDA
AMANDA n-candidate
• Early photons are red, late
photons are blue. More
photons are larger circles
• Bottom of array is toward
center of Earth
• The muon is clearly
traveling in the upward
direction
2000-06-21
Per Olof Hulth
AMANDA
Event Rate Predictions
Point Sources
S o ur c e___ _ ___
S N a R e mnant
A GN ( 3 C 273 )
M k 421, M k 501
GR B (  flu ct. m ode l)
2000-06-21
R ate (/k m 2 y r)
E   > 1 T eV
3
1 -100
1 -10 f rom  f lux
~ a fe w
(fr o m a rar e bu rst )
Diffuse Sources
S o ur c e
R ate (/k m 2 y r s r)
E  > 1 T eV_ _ ___
A GN
A GN je ts
GR B
At m n
400 -80 0
45
10
100 0
Per Olof Hulth
AMANDA
Search Strategies for HE n’s
• Diffuse flux are most
difficult to detect, but
largest predicted rates.
• GRBs have least
background due to
time and position
correlations.
2000-06-21
S o ur c e
R e ject ion
met h od____
B a ck gro u nd
D iffuse flu x
1. u p -d ow n
(10 9 /y r)(atm.  )
P o int S ou rce 1. u p -d ow n
(e.g. A GN)
2. d ir ect ion
3. ene rg y ?
(10 9 /y r)(atm.  )
B u rs ts
(e.g. GR B )
(10 9 /y r)(atm.  )
1. u p -d ow n
2. d ir ect ion
3. t ime s tamp
4. ene rg y ?
x (d  /2  )
x (d  /2  )
x (dt/ 3 x10 7 )
Per Olof Hulth
AMANDA
Signal-background Separation
Arb. normalization between signal and BG
2000-06-21
Per Olof Hulth
AMANDA
SPASE-AMANDA
SPASE: South Pole Air Shower Experiment
• Calibration of
absolute pointing
• Calibration of
pointing resolution
• Calibration of
signal efficiency
2000-06-21
Per Olof Hulth
AMANDA
Data Reduction 1997
E.g. one of the atmospheric neutrino analysis, 1997.
O bs er ved numb er
of events
2000-06-21
P re di cted numb er
of n eut rinos
Tr igg ere d
1.2*10
9
4500
R ec onst ructed as
upgoing t rac k
5.1*10
4
570
P assing fin al cuts
193
235
Per Olof Hulth
AMANDA
Atm. n: background rejection
• Satisfactory agreement at
all stages of analysis
103
• Rejection criteria are
progressively improved,
leaving fewer down-going
events
• Initially data agrees with
BG simulation, but then
1
agrees with atm. n signal
2000-06-21
Per Olof Hulth
AMANDA
Angular Distributions
Two distinct analysis techniques, but not independent
(a)
MC
(normalized)
2000-06-21
(b)
Per Olof Hulth
AMANDA
Atmospheric Neutrinos
• Stronger selection
criteria than point
analysis
• Two distinct analysis
methods
• Expected number of
events depends on
analysis efficiency
2000-06-21
Per Olof Hulth
AMANDA
Search for HE n Point Sources
• Concentrate on continuous emission from
sources with hard spectra (~E-2)
• Optimize search on Signal to Noise Ratio
 Aeff depends on rejection requirements
 Iterative procedure defined a priori
• Background for this search
 Poorly reconstructed atmospheric muons
 Atmospheric neutrinos
2000-06-21
Per Olof Hulth
AMANDA
Sky Plot of Events
Equatorial Coordinates
• 1097 events
• No obvious
clustering
• Event sample
consists of
atm. n and
atm. muons.
2000-06-21
Per Olof Hulth
AMANDA
Significance distribution
• Bin sky according to
angular resolution
• Use declination band
to estimate
background
• No statistically
significant excess
2000-06-21
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Per Olof Hulth
AMANDA
Flux Limit (preliminary)
• AMANDA B10
limits are compared
to MACRO limits.
SuperK curve is
estimated!
• AMANDA-II will
complement sky
coverage of SuperK
2000-06-21
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Per Olof Hulth
AMANDA
Point Source Fluxes
Figure adopted from Mannheim & Learned
• Theoretical
predictions
are very
small
• AMANDA
limit assumes
source with
E-2 spectrum
2000-06-21
Per Olof Hulth
AMANDA
Mk 501 Flux Limit
• Recent diffuse IR
measurements imply
strong attenuation of
TeV photons
Figure adapted from Protheroe and Meyer, astro-ph/0005349
AMANDA
• AMANDA can rule
out similar neutrino
spectrum.
2000-06-21
Per Olof Hulth
AMANDA
Search for Diffuse Flux
• OM multiplicity
distribution is
(weakly) related to
energy deposition.
• Distribution is
consistent with atm n
• New energy
estimators will lead to
improved limits
2000-06-21
Per Olof Hulth
AMANDA
Diffuse Flux
• Generally 103 larger
than point fluxes
AMANDA
• Atm.n backgrounds
103 worse
• E2Fn< 1.6x10-6
GeVcm-2s-1sr-1
2000-06-21
Per Olof Hulth
AMANDA
WIMPs from Sun/Earth
2000-06-21
Per Olof Hulth
AMANDA
Angular Spread of WIMP signal
• Angular spread
decreases as WIMP
mass increases,
reducing atm. n
background
2000-06-21
Per Olof Hulth
AMANDA
Cuts for WIMP search
• Optimized cuts for
almost vertical
upward moving
muons.
• The simulated WIMP
signal is reduced to
30% after reducing
background by 108.
2000-06-21
Per Olof Hulth
AMANDA
WIMPs from the Earth
Optimized search for vertical neutrinos (1997 data)
• AMANDA limits
comparable to MACRO
and Baksan
• AMANDA sensitivity
will increase at low
mass due to special
string trigger and better
optimized analyzes
2000-06-21
Per Olof Hulth
AMANDA
WIMP search with
3
Ice
The WIMP search has been tested for two different
geometries and the limits are given for 10 years of running
2000-06-21
Per Olof Hulth
AMANDA
Simulation of WIMPs in
3
Ice
• Signal neutrinos from WIMP annihilations are simulated
with Pythia
• No background simulated, but PMT noise is included
• At least 5 remaining hits after cleaning
• Reconstructed muon angle within 5 degrees of simulated
• This is the best-case limits since since efficiency of future
cuts to remove background has not been included.
2000-06-21
Per Olof Hulth
AMANDA
WIMPs from the Earth with Ice3
Optimized search for vertical neutrinos
• Ice3 will significantly
improve the sensitivity.
2000-06-21
Per Olof Hulth
AMANDA
WIMPs from the Earth with Ice3
Optimized search for vertical neutrinos
• Ice3 will completely
cover the DAMA area
2000-06-21
Per Olof Hulth
AMANDA
WIMPs from the Sun with Ice3
• Ice3 will
significantly
improve the
sensitivity.
2000-06-21
Per Olof Hulth
AMANDA
WIMPs from the SUN with Ice3
2000-06-21
Per Olof Hulth
AMANDA
Search for HE n from GRB
GRB search bin
Off source
GRB Position
GRB burst
1 hour
BKG - off time
2000-06-21
16 s
on time
1 hour
BKG - off time
Per Olof Hulth
AMANDA
GRB Science
• Verify fireball model
• GRBs may be sources of highest energy cosmic
rays
• Test of special relativity
• Search for nt appearance at Dm2> 10-17 eV2(Ice3)
• Search for n emission in coincidence with
Gamma ray detectors
2000-06-21
Per Olof Hulth
AMANDA
HE n emission from GRB’s ?
- Not so far
Fluence (TeVcm-2)
10-1
Combined Limit (90% CL)
10-6
Waxman and Bahcall
1
2000-06-21
100
Burst Duration (s)
Per Olof Hulth
AMANDA
AMANDA Supernova detection
• ne + p
n + e+
• PMT noise increase
due to the positrons
• AMANDA records
noise on the PMTs
over 0.5 sec and
summing up total rate
over 10 sec intervals
2000-06-21
Per Olof Hulth
AMANDA
AMANDA SN sensitivity
• AMANDA-B10 is
monitoring 60% of
the Galaxy with
90% detection
efficiency for a
SN1987 type.
• AMANDA is
going to join
SNEWS in 2001
2000-06-21
Per Olof Hulth
AMANDA
Magnetic Monopole detection
2000-06-21
Per Olof Hulth
AMANDA
AMANDA Effective Area
• AMANDA-II
30,000-50,000 m2
• AMANDA-II has
nearly uniform
response over all
zenith angles
2000-06-21
Per Olof Hulth
AMANDA
Summary and Outlook
• No point sources (AGN, GRB or WIMPS)
detected, but
 more data on tape with bigger array (1998, 1999)
• ~170 atmospheric neutrinos candidates
 Number depends on efficiency of analysis
• Sensitivity and performance confirmed (to within
factor of 2) by atm n, background studies, and
Spase-AMANDA coincidence events
• AMANDA-II is taking data
2000-06-21
Per Olof Hulth
AMANDA
Publications
• Many conference reports and so far X Ph.D. Thesis.
• First neutrino results in Astroparticle Physics 13 (2000) 1,
(AMANDA-B4)
• Eight drafts in preparation for submission in autumn 2000
(AMANDA-B10, 1997 data)
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2000-06-21
Atmospheric neutrinos
WIMP search
Neutrino limits from GRB
Point sources
Diffuse limit
AMANDA-SPASE
Supernova
Magnetic Monoples
Per Olof Hulth
AMANDA
AMANDA Results
• Supermassive Black Holes (AGN)
 E-2 point source: fn (>10 GeV) <10-7 (cm-2s-1)
 E-2 diffuse flux : E2fn< 1.6x10-6 GeV cm-2s-1sr-1
• GRB in coincidence with BATSE
 Cumulative Fluencen< 4x10-4 TeVcm-2
• Atmospheric neutrinos (135 live days)
 ~170 events from 1997, depends on analysis
 Calibration of sensitivity within factor 2
• WIMPs from the earth
2000-06-21
Also, see ICRC99 for limits on relativistic
monopoles, search for SNa, ice properties
Per Olof Hulth