Carlos de los HerosCarlos de los HerosDivision of High Energy Division of High Energy PhysicsPhysicsUppsala UniversityUppsala University

EPS2005EPS2005Lisbon, July 21-27, 2005Lisbon, July 21-27, 2005

GETTING THERE:GETTING THERE:FROM AMANDA TO ICECUBEFROM AMANDA TO ICECUBE

USA: Bartol Research Institute, Delaware Univ. of Alabama Pennsylvania State University UC Berkeley UC Irvine Clark-Atlanta University Univ. of Maryland IAS, Princeton University of Wisconsin-Madison University of Wisconsin-River Falls LBNL, Berkeley University of Kansas Southern University and A&M

College, Baton Rouge

Sweden: Uppsala Universitet Stockholm Universitet Kalmar Universitet

In March 2005, AMANDA merged into the IceCube collaboration

UK: Imperial College, London Oxford University

Netherlands: Utrecht University

Belgium: Université Libre de Bruxelles Vrije Universiteit Brussel Universiteit Gent Université de Mons-Hainaut

Germany: Universität Mainz DESY-Zeuthen Universität Dortmund Universität Wuppertal Universität Berlin

Japan: Chiba university

New Zealand: University of Canterbury

THE ICECUBE COLLABORATIONTHE ICECUBE COLLABORATION

• Cosmic rays @ >>TeV exist

acceleration sites must sit somewhere

Candidate sources:• SNe remnants, Quasars• Active Galactic Nuclei• Gamma Ray Bursts• Exotics (decays of topological defects...)

proton accelerators

Neutrinos : not absorbed, not deflected:

difficult to detect

Protons : deflected in magnetic fields, GZK -rays : propagate straight, however:

– reprocessed in sources– absorbed in IR (100 TeV) and 3K (10 PeV)

?

explained explained by SN?by SN?

unexplainedunexplained

Guaranteed sources:

• atmospheric neutrinos (from & K mesons decay)

• galactic plane: – CR interacting with ISM, concentrated on the disk

• CMB (diffuse):– UHE p + n + (p 0)

NEUTRINO ASTRONOMYNEUTRINO ASTRONOMY

PMT noise: ~1 kHz

AMANDA-B10(inner core of AMANDA-II)

10 strings302 OMs

Data years: 1997-99

Optical Module

“Up-going”(from Northern sky)

“Down-going”(from Southern sky)

AMANDA-II

19 strings677 OMs

Data years: 2000 –

THE AMANDA DETECTORTHE AMANDA DETECTOR

AMANDA-B4(first 4-string prototype)

4 strings80 OMs

Data years: 1996

1996 1997 2000

What’s up?

Amundsen-Scott South Pole station

South Pole

Stationfacilities

AMANDA

road to work

1500 m

2000 m

[not to scale]

THE SITETHE SITE

NEUTRINO DETECTION IN POLAR ICENEUTRINO DETECTION IN POLAR ICE

O(km) long muon tracks

~15 m

7.0)TeV/(7.0 E

South Pole ice: (most?) transparent

natural condensed material

Longer absorption length → larger effective volume

Event reconstruction by Cherenkov light timing

O(10m) Cascades, e Neutral Current

IN THIS TALK:IN THIS TALK:

•Results from:

atmospheric neutrinos

searches for an extra-terrestrial flux: galactic center

diffuse (anytime, anywhere)point source (anytime, somewhere)transient (known ‘flary’ objects & GRBs) (sometime, somewhere)

search for WIMPs: Excess from the center of the Sun/Earth

SN search in the Milky Way

Agreed collaboration strategy: Analyses are done ‘blind’. Cuts optimized on a % of data or on a time-scrambled data set.

AMANDA: sensitive in very different energy regimes

Energy range production site(s)Energy range production site(s)

MeV Supernovae

GeV-TeV

Atmosphere

Dark matter from Sun/Earth

Galactic center

TeV-EeV

Quasars

SN remnant

AGN

GRB

galactic

extragalactic

EHadron E-2.7 0.02

cosmic ray muonsAtmospheric muons: - AMANDA test beam: I vs depth, CR composition - Background for other searches

TEST BEAMS: TEST BEAMS: ATMOSPHERIC ATMOSPHERIC MUONSMUONS

SPASE (scintillator array @ 3000m) e density @ surface shower core resolution: 0(m) shower direction resolution: < 1.5o

AMANDA ‘s @ >1500m (>300 GeV @ surface) use SPASE core position for combined fit use expected lateral photoelectron/event distribution as estimate of N

Combined SPASE-AMANDA ‘detector’:

Probes hadronic () and EM (e) component of the primary shower

(E) ~ 0.07 in log(Eprim)

Results compatible with composition change around the knee

Sources of systematic uncertainties:(~30% in ln(A), not shown in the plot)

-shower generation models -muon propagation

►Neural Network energy

reconstruction of up-going μ`s

►Regularized unfolding

→ energy spectrum

Set limit on cosmic neutrino flux:

How much E-2 cosmic ν - signal

allowed within uncertainty of highest energy bins?

Limit on diffuse E-2 νμ flux (100 -300 TeV):

First spectrum > 1 TeV (up to 300 TeV)- matches lower energy Frejus data

E2μ(E) < 2.6·10–7 GeV cm-2 s-1 sr-1

vertical

horizontal

TEST BEAMS: TEST BEAMS: ATMOSPHERIC NEUTRINOSATMOSPHERIC NEUTRINOS

Frejus

Amanda

Atmospheric neutrinos: - Guaranteed test beam - Background for other searches

’’s s FROM THE GALACTIC PLANEFROM THE GALACTIC PLANE

•Expected from CR+galactic interstellar

medium

• ’s follow the primary energy spectrum, E-

2.7

•Location of AMANDA reach only outer

region of the galactic plane: 33o<<213o

•data sample 2000-03: 3329 evts

•Three signal ansatz:

•Line source

•Gaussian source

•Diffuse sourceNO EXCESS OBSERVED:

Optimal Optimal on-source on-source

regionregion

on-source on-source eventsevents

Expected bckg.Expected bckg.

+-2.0o 128 129.4

6.4x10-5 (line)

(GeV-1 cm-2 s-1 rad-1)

6.6x10-4 (diffuse)

(GeV-1 cm-2 s-1 sr-1)

+-4.4o 271 283.34.8x10-4 (gauss) (*)

(GeV-1 cm-2 s-1 sr-1)

(*)

Several strategies in the search for point sources:

•Diffuse flux of neutrinos with no time-space correlations. Focus on E-2 spectrum

•calculate upper limit on high energy tail of atmospheric νμ

• optimize selection with attention to background(s) rejection

•multi-flavor (muon tracks + cascades)

•Spacial correlation with steady objects•Search for clusters of events (w. or w.o. catalogue)•Stacking of known point source candidates (paper in preparation)

• Space and/or time correlation with transient phenomena •known active flary periods of TeV gamma sources•time window-rolling search of signal excess over background

SEARCH FOR POINT SOURCESSEARCH FOR POINT SOURCES

•UHE: E > P eV:

•Earth opaque

•Search in the upper

hemisphere and close to the

horizon

•Bright events: many hit OMs with several hits/OM Energy -related variables best handle of analysis

DIFFUSE SEARCHDIFFUSE SEARCH

•HE: TeV < E < PeV:

•Use directionality + energy-related

variables to reject atm background

•Search confined to up-going tracks

•Use high-quality tracks

Limit from data sample 1997. 131 d lifetime:

Assuming a E-2 flux (1 PeV < E < 3 EeV) and

e:: = 1:1:1

E2 all(E) < 9.9 x 10-7 GeV cm-2 s-

1 sr-1

Sensitivity from data sample 2000. 174 d lifetime:

Assuming a E-2 flux (0.2 PeV < E < 2 EeV)

and e:: = 1:1:1

E2 all(E) < 4.2 x 10-7 GeV cm-2 s-

1 sr-1

Limit from data sample 1997. 131 d lifetime:

Assuming a E-2 flux (1 PeV < E < 3 EeV) and

e:: = 1:1:1

E2 (E) < 8.4 x 10-7 GeV cm-2 s-1 sr-1

Sensitivity from data sample 2000-03. 807d lifetime:

Assuming a E-2 flux (13 TeV < E < 3.2 PeV) and

e:: = 1:1:1

E2 all(E) < 9.5 x 10-8 GeV cm-2 s-1

sr-1

Analyses optimized for , : reduced sensitivity to e and All-flavour

•Cascades: TeV < E < PeV

•4search

•Background: brehmm.

from down-going muons

Limit from data sample 1997. 131 d lifetime:

Assuming a E-2 flux (50 TeV < E < 3 PeV) and

e:: = 1:1:1

E2 all(E) < 9.8 x 10-6 GeV cm-2 s-1

sr-1

Sensitivity from data sample 2000. 174 d lifetime:

Assuming a E-2 flux (50 TeV < E < 5 PeV) and

e:: = 1:1:1

E2 all(E) < 8.6 x 10-7 GeV cm-2 s-1

sr-1

signal:

background:

AMANDA

1: B10, 97, ↑μ2: A-II, 2000, unfold.3: A-II, 2000, cascade4: B10, 97, UHE6: A-II, 2000, UHE sensit.7: A-II, 2000-03 ↑μ sensit.

Baikal

5: 98-03, casc.

1:1:1 flavor flux ratio

all-flavor limits

DIFFUSE SEARCHES: SUMMARYDIFFUSE SEARCHES: SUMMARY

Limits for other flux predictions: Cuts optimized for each case.

Expected limit from a given model compared with observed limit.

Some AGN models excluded at 90% CL :

Szabo-Protehoe 92

Stecker, Salamon. Space Sc. Rev. 75, 1996

Protehoe. ASP Conf series, 121, 1997

67

SEARCH FOR CLUSTERS OF EVENTS IN THE NORTHERN SKYSEARCH FOR CLUSTERS OF EVENTS IN THE NORTHERN SKY

•Search for excesses of events compared to the background from:

• the full Northern Sky• a set of selected candidate sources

•Cuts optimized in each declination band

•Require good pointing resolution (good quality events)

•Background estimated from exp. data

with randomized α (i.e. time)

•Sensitivity flat up to horizon•Significant improvement w.r.t. first analysis with AMANDA-B10

av

era

ge

flu

x u

pp

er

lim

it [

cm

-2s

-1]

sin

AMANDA-B10

AMANDA-II

Average upper limit = sensitivity (δ>0°)

(integrated above 10 GeV, E-2 signal)

tim

e

declination 0o (horizontal)

90o (vertical)

Declination averaged Declination averaged sensitivity sensitivity

for a Efor a E-2-2 spectrum and E spectrum and E > 10 > 10

GeVGeV

lim 0.6·10-8 cm-2s-1

Maximum significance: 3.4

Assess statistical significance using random sky maps:

Probability of a background

Fluctuation: 92%

Data from 2000-2003 (807 days)

3369 from northern hemisphere

3438 expected from atmosphere

Event selection optimized for both dN/dE ~ E-2 and E-3 spectra

SEARCH FOR CLUSTERS OF EVENTS IN THE NORTHERN SKYSEARCH FOR CLUSTERS OF EVENTS IN THE NORTHERN SKY

Source Nr. of events

(4 years)

Expectedbackgr.

(4 years)

Flux Upper Limit 90%(E>10 GeV)

[10-8cm-2s-1]

Markarian 421 6 5.58 0.68

1ES1959+650 5 3.71 0.38

SS433 2 4.50 0.21

Cygnus X-3 6 5.04 0.77

Cygnus X-1 4 5.21 0.40

Crab Nebula 10 5.36 1.25

Selected objects and full scan of the northern

sky:

No statistically significant effect observed

… out of 33 Sources

Systematic uncertainties under investigation

Sensitivity ~2for 200 days of “high-state” and spectral results from HEGRACrab Nebula: The chance probability of such an excess (or higher) given the number of trials is 64%

Prelim

inary

SEARCH FOR CLUSTERS OF EVENTS FROM KNOWN OBJECTSSEARCH FOR CLUSTERS OF EVENTS FROM KNOWN OBJECTS

On-Source

Off-Source

Source

Nr. of events

(4 years)

ExpectedBG

(4 years)

Period duration

Nr. of doublets

Probability for highest

multiplicity

Markarian 421 6 5.58 40 days 0 Close to 1

1ES 1959+650 5 3.71 40 days 1 0.34

3EG J1227+4302 6 4.37 40 days 1 0.43

QSO 0235+164 6 5.04 40 days 1 0.52

Cygnus X-3 6 5.04 20 days 0 Close to 1

GRS 1915+105 6 4.76 20 days 1 0.32

GRO J0422+32 5 5.12 20 days 0 Close to 1

Search for excesses in time-sliding windows:galactic objects: 20 daysextra-galactic objects: 40 days

Preliminary

… out of 12 Sources → no statistically significant effect observed

eventstime

sliding window

Enhance the detection chance by using the time information:

Search for neutrino flares without a-priori hypothesis on their time of occurrence

POINT SOURCE SEARCH: TIME WINDOW EXCESSPOINT SOURCE SEARCH: TIME WINDOW EXCESS

• Catalogues: BATSE+IPN3

• Several search techniques: • coincidence with T90• precursor (110s before T90)• cascades (all flavour, 4)

-coincident with T90

-rolling time window

(no catalogue)

• Bckg. Stability required within ±1

hour from burst• Further searches: rolling search

(without temporal/spacial constrains) Eν

2Φν < 6.7x 10-6 GeV cm-2 s-1 sr-1

SEARCH FOR SEARCH FOR ’s’s CORRELATED WITH GRBs CORRELATED WITH GRBs

Low background analysis due to both

space and time coincidence!

year#

GRBfrom

preliminary 90%CL upper limit

assuming WB spectrum

(EB at 100 TeV and = 300)

'97 - '00 312BATSE

triggered bursts

E2d/dE = 4 · 10-8 GeV cm-2s-1 sr-1

'00 - '03 139 BATSE & IPN bursts

E2d/dE = 3 · 10-8 GeV cm-2 s-1 sr-1

'01 - '03 50 IPN bursts(Assuming the Razzaque model)

E2d/dE = 5 · 10-8 GeV cm-2 s-1 sr-1

'01 (425) Rolling window

E2d/dE = 2.7 · 10-6 GeV cm-2s-1sr-1

'00 76BATSE

triggered bursts

E2d/dE = 9.5 · 10-7 GeV cm-2s-1sr-1

Sun analysis possible due to improvedreconstruction capability for horizontal tracks in AMANDA-II compared with B10.

• m 20%, b 5%

non-baryonic matter MSSM: candidate

• accumulating over cosmological time in the Sun/Earth. Pair-wise annihilation at its center:

and consider (MC=DarkSusy)• (soft channel)• (hard channel)

for various masses (50-5000 GeV)

HZ,W,,ll,qq -xx

bbxx -WWxx

SEARCH FOR SEARCH FOR DM CANDIDATES IN THE SUN/EARTHDM CANDIDATES IN THE SUN/EARTH

Combined 1997-99 data sets: Searches from the center of the Earth2001 data set: Search from the

Sun

Cygnus-X1

Cassiopeia. ASun

90 000 light years

SMC

LMC

Crab Nebula•Burst of low-energy (MeV) neutrinos from core collapse supernovae

increase indetector noise ratedue to e+e- e- + X

•Low energy O(ev)e- tracks: no pointing

•Monitor noise of subset of stable OMs

•Special DAQ: count rates in 10 s

•92% coverage of theMilky Way

•AMANDA part of SNEWS alert network

SEARCH SEARCH FOR SNe EXPLOSIONS IN THE GALAXYFOR SNe EXPLOSIONS IN THE GALAXY

Approximate AMANDA horizon

Deep ice array: IceCube Digital readout technology (D-OMs) 80 strings / 60 DOM’s each 17 m DOM spacing 125 m between strings hexagonal pattern over 1 km2x1 km

1200 m

IceTop

IceCube

Surface array: IceTop• 80 stations air shower array.

(one per IceCube string)• 2 tanks (2 DOMs each) per station• 125 m grid, 1 km2 at 690 g/cm2

• Ethreshold ~ 300 TeV for > 4 stations in coincidence

The IceCube observatory: IceCube+IceTopThe IceCube observatory: IceCube+IceTop

Amundsen-Scott South Pole station

South Pole

Stationfacilities

AMANDA

road to work

1500 m

2000 m

[not to scale]

IceCube

IceCube

THE SITE

Eµ=6 PeV

IceCube: an All-Flavor Neutrino Telescope

IceCube will be able to identify tracks from for E > 100 GeV cascades from e for E > 10 TeV for E > 1 PeV

Background mainly downgoing cosmic ray (bundles)(+ uncorrelated coincident 's)

- exp. rate at trigger level ~1.7 kHz- atm. rate at trigger level ~300/day

e e “cascade”

E = 375 TeV

~300

m @

E

= 1

PeV

"cascade"

1 year sensitivity a point E2·d/dE flux

IceTop Stations with DOMs – January 2004

Digitized muon signals from DOMs

Am

plit

ude

(AT

WD

cou

nts)

vs

tim

e (n

s)

power cable

signal, freeze control,

temperature controlcables

27.1, 10:08: Reached maximum depth of 2517 m, reversed direction, started to ream up

28.1, 7:00: drill head and return water pump are out of the hole, preparations for string installation start

7:52: Handover of hole for deployment

9:15: Started installation of the first DOM (DOM 60)

12:06: 10th DOM installed

22:36: 60th DOM installed Typical time for DOM installation:12 min

22:48: Start drop

29.1, 1:31: String secured at depth of 2450.80 m

20:40: First communication to DOM

IceCube First String: January 2005

An IceCube-IceTop event

OutlookOutlook

•A wealth of results from AMANDA-B10 and AMANDA-II on several physics

topics

•Results from combined analysis using several years ’00-’03 (more on the way)

•No extraterrestial neutrinos observed yet

•Sensitivity reaching the level of current predictions of production in AGN.

Some models already excluded @ 90%CL

•Digitized readout since 2003: waveform resolution

•First IceTop station deployed on Jan. 2004

•First IceCube string deployed on Jan. 2005

•First IceCube-IceTop and IceCube-AMANDA events seen

•IceCube/IceTop will significantly improve astrophysics and cosmic rays

measurements in energy range and resolution