Carlos de los Heros, Uppsala University results from neutrino telescopes COSMO05. Bonn, Aug. 28 –...

Carlos de los Heros, Uppsala University

results from neutrino telescopes

COSMO05. Bonn, Aug. 28 – Sep. 1, 2005

Outlook.

as a framework: high energy neutrino astronomy

the world of neutrino telescopes: current projects

recent physics results from AMANDA and Baikal

ICECUBE: status and capabilities

summary

• nature accelerates particles to ~10 7 times the CM energy of LHC!

acceleration sites must sit somewhere

candidate sources:

• SNe remnants, quasars

• active galactic nuclei

• gamma ray bursts

neutrino astronomy

? proton accelerators

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)

T. Gaisser 2005

particle propagation in the Universe

production:neutrino production at source: p+ or p+p collisions give pions: e- + e

neutrino flavors: e : : 1:2:~0 at

source. Expect 1:1:1 at detector

propagation:photons: can be absorbed on intervening matter or radiation;protons: deviated by magnetic fields

at high-enough energies: p and react with the CMB bckgr.

’s will get to you

however: ’s extremely difficult to detect!

your favourite cosmic accelerator

p

your favourite detector

Outlook.





summary

current HE neutrino detection effortscurrent HE neutrino detection efforts

OPTICALOPTICAL

RADIORADIO

ACOUSTICACOUSTIC@ extremely high energies (E>1018 eV)

AMANDA / ICECUBEAMANDA / ICECUBE

NEMONEMONESTORNESTOR

BAIKALBAIKAL

RICE, ANITARICE, ANITA

SALSASALSAKAMCHATKAKAMCHATKA

AUTECAUTECGLUEGLUE

ANTARESANTARES

SADCOSADCO

neutrino detection in ice/water

7.0)TeV/(7.0 E

longer absorption length → larger effective volumelonger scattering length → better pointing resolution

event reconstruction by Cherenkov light timing: need array of PMTs with ~1ns resolution

optical properties of the medium of prime importance

absorption length scattering length

South Pole ice(AMANDA/IceCube)

110 m (@ 400nm) 20 m (@ 400nm)

Lake Baikal 25 m (@ 480nm) 59 m (@ 480nm)

Mediterranean(ANTARES/NESTOR)

~60 m (@ 470nm) 100-300 m (@ 470nm)

neutrino astronomy possible since

O(km) long

muon tracks

O(10m) cascades, e neutral current

signatures

the BAIKAL detectorthe BAIKAL detector

NT-200- - 8 strings with 192 optical modules

- - 72 m height, 1070 m depth

- - effective area >2000 m2 (E>1 TeV)

- - Running since 1998

NT-200+- - commisioned April 9, 2005.- 3 new strings, 200 m height- 1 new bright Laser for time calibration imitation of 20TeV-10PeV cascades, >10^12 photons/pulse w/ diffusor,- new DAQ- 2 new 4km cables to shore

4 Km to shore

NT200+ is tailored to UHE -induced cascades 5 Mton equipped volume; V_eff > 10 Mton at 10 PeV

PMT noise: ~1 kHz

Optical Module

the AMANDA detector

AMANDA-B10- - 10 strings with 302 optical modules

- - 450 m height, 1500 m depth

- - data years: 1997/99

AMANDA-IIAMANDA-II- 19 strings, 677 OMs

- running since 2000

- new DAQ with FADC since 2003

since March 2005 we are called IceCube!

(AMANDA and IceCube collaborations merged)

Amundsen-Scott South Pole station

South Pole

Stationfacilities

AMANDA

your daily commute to work

1500 m

2000 m

the site

[not to scale]

muons:directional error: 1.5° - 2.5°

(log(Ereco/Etrue)): 0.3 – 0.4coverage: 2

cascades: (e±, , neutral current)zenith error: 30° - 40° (log(Ereco/Etrue)): 0.1 – 0.2

(5TeV < E < 5PeV)

coverage: 4

effective area: >10000 m2 for E>1TeV

AMANDA detector performance

Average upper limit = sensitivity (δ>0°)

(integrated above 10 GeV, E-2 signal)

av

era

ge

flu

x u

pp

er

lim

it [

cm

-2s

-1]

sin

AMANDA-B10

AMANDA-II

tim

e

Outlook.





summary

in this talk:

• AMANDA (and Baikal when available) 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

agreed AMANDA collaboration strategy: analyses are done ‘blind’. cuts optimized on a % of data or on a time-scrambled data set.

EHadron E-2.7 0.02

cosmic ray muons

test beams: atmospheric muons

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

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

atmospheric muons: - AMANDA test beam: I vs depth, CR composition

- background for other searches

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

test beams: atmospheric neutrinos

vertical

horizontal

Frejus

AMANDA

► reconstruct energy of up-going μ`s

► obtain energy spectrum from regularized unfolding

atmospheric neutrinos: - guaranteed test beam - background for other searches

on-source region

on-source events

expected background

90% event upper limit

line source limit

GeV-1 cm-2 s-1 rad-1

diffuse limitGeV-1 cm-2 s-1 sr-1

gaussian limit

GeV-1 cm-2 s-1sr-1

2.0º 128 129.4 19.8 6.3 10-5 6.6 10-4 —

4.4º 272 283.3 20.0 — — 4.8 10-4

-

-

-

-

-

-

-

Gaus. limit

model

’s from the galactic plane

• location of AMANDA not optimal reach

only outer region of the galactic plane:

33o<<213o

• three signal ansatz:

line source, Gaussian source, diffuse

source

• limits include systematic uncertainty of 30% on atm. flux

• energy range: 0.2 to 40 TeVdata sample 2000-03: 3369 evts:

strategies in the search for point sources:

•diffuse flux with no time-space correlations. •from high energy tail of atmospheric νμ

• selection with emphasis on background(s) rejection

•spatial correlation with steady objects•search for clusters of events (w. or w.o. catalogue)•stacking of same-type of point source candidates

•space and/or time correlation with transient

phenomena •known active flary periods of TeV gamma sources•coincidence with GRBs

search for HE neutrinos from the cosmos

UHE: E > PeV

•Earth opaque: search in the upper hemisphere and close to the horizon

HE: TeV < E < PeV

•search confined to up-going tracks

analyses optimized for

(reduced sensitivity to e and

)

Cascades: TeV < E < PeV

• 4sensitivity

all-flavour

energy regions:

diffuse flux search

AMANDA

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

Baikal

5: 98-03, cascades8: NT200+ sensitivity to e

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. Proc. HE Neutr. Astrophys. Hawaii 1992. Stecker, Salamon. Space Sc. Rev. 75, 1996 Protheroe. ASP Conf series, 121, 1997

1:1:1 flavor flux ratio

all-flavor limits

67 8

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

search for clusters of events in the northern sky

sourcenr. 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

data from 2000-2003 (807 days)

3369 from northern hemisphere

3438 expected from atmosphere

• search for excesses of events on:

• the full Northern Sky

• a set of selected candidate

sources

significance map

… out of 33 Sources

crab

Mk421Mk501

M87

Cyg-X3

SS433

1ES1959

Cyg-X1

neutrino sky from Baikal

1998-2002 data sample - 372 events - 385 evts expected - no indication of clustering

• catalogues: BATSE+IPN3

• bckg. Stability required within ±1

hour from burst• several search techniques:

• coincidence with T90• precursor (110s before T90)• cascades (all flavour, 4)

-coincident with T90

-rolling time window

(no catalogue)

search for ’s correlated with GRBs

low background analysis due to both

space and time coincidence search!

year#

GRBsfrom

preliminary 90%CL upper limitassuming 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 139BATSE &

IPN burstsE2d/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 73BATSE

triggered bursts

E2d/dE = 9.5 · 10-7 GeV cm-2s-1sr-1

10 min1 hour 1 hour

110 s T90 time

Off-TimePrecursor On Time

Always Blind

• m 20%, b 5%

non-baryonic matter

MSSM candidate: the neutralino,

may exist as relic gas in the galactic halo

gravitational accumulation in Sun/Earth makes ‘indirect’ searches with neutrino telescopes possible

search for DM candidates in the Sun/Earth

neutralino-induced neutrinos:

qq

l+l- W, Z, H

signature: excess from

Sun/Earth’s center direction

A lot of physics (ie. uncertainties) involved:

- relic density calculations

- DM distribution in the halo

- velocity distribution

- properties (MSSM)

- interaction of with matter (capture)

2001

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

search for a neutralino signal from the Earth

search for a neutralino signal from the Sun

results from indirect DM searches

e.g. magnetic monopoles:

Cherenkov-light (n·g/e)2

(1.33*137/2)2

8300 times brighter than ‘s!

signature: ‘slowly‘ moving bright particles

other particle searches

10-16

10-15

10-14

10-18

10-17

= v/c1.000.750.50

up

per

lim

it (

cm-2 s

-1 s

r-1)

KGF

Soudan

Baikal 2005

Amanda-B10

1 km3

electrons

MACRO

Orito

Outlook.





summary

deep ice array: IceCube

digital readout technology (DOMs) 80 strings, 60 DOM’s each 17 m DOM spacing 125 m between strings hexagonal pattern over 1 km2x1 km

1200 m

the IceCube observatory: IceCube+IceTop

IceTop

IceCube

surface array: IceTop

80 stations air shower array(one per IceCube string)

similar station concept as Auger 2 tanks (2 DOMs each) per station 125 m grid, 1 km2 at 690 g/cm2

E=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 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"

Galactic center

IceCube: Aeff and resolution

1 year sensitivity E2·d/dE

diffuse point

8.110-9

[cm-2s-1sr-1GeV]5.510-9

[cm-2s-1GeV]

E< 1 PeV: focus on the Northern sky,

E > 1 PeV: sensitive aperture increases with energy

full sky observations possible

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

dep

loyed

strin

g

AMANDA

4 IceTop stations

timing verification with flashers

Outlook.





summary

• a wealth of physics results from the currently working neutrino telescopes on several topics

• sensitivity reaching the level of current predictions of

production in AGN. Some models already excluded @

90%CL

• first Km3 project (IceCube) started at the South Pole: first events seen

• two projects + R&D efforts for a Km3 detector in the Mediterranean

summary

Absorption

dust

icebubbles

dust

optical properties:data from calibration light sources deployed along the strings and from cosmic ray muons.

absorption length

@ 400 nm

eff. Scattering length

@ 400 nm

110 m 20 m

effective scattering length absorption length

on average:

detector medium: nice icedetector medium: nice ice

AMANDA depthAMANDA depth

Preliminary

source

nr. of events(4 years)

expectedBG

(4 years)

time window

Markarian 421 6 5.58 40 days

1ES 1959+650 5 3.71 40 days

3EG J1227+4302 6 4.37 40 days

QSO 0235+164 6 5.04 40 days

Cygnus X-3 6 5.04 20 days

GRS 1915+105 6 4.76 20 days

GRO J0422+32 5 5.12 20 days

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

… out of 12 Sources → no statistically significant effect observed

timeevents

sliding window

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

search for neutrino flaressearch for neutrino flares

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

•Transient Waveform Recorder system installed between the 2001 and 2004 campaigns

• Increased OM dynamic range x ~100

• Increased 1pe detection efficiency

• Virtually dead-time free

• Manageable trigger rate: ~150 Hz (majority 18)

• Possibility of using software trigger

• Under evaluation

Physics benefits:

• Improved angular resolution

• Improved energy resolution

UHE/EHE physics

TRANSIENT WAVEFORM RECODER UPGRADETRANSIENT WAVEFORM RECODER UPGRADE

Up to 18 holes per season:

Nov.: preparationDec.: constructionJan.: constructionFeb.: commissioning

Deploymentof string N

Drilling of hole N

0h 12h 24h 36h 48h 60h 72h 84h

Time

IceCube: time planIceCube: time plan

Diffuse sensitivity Point source sensitivity

IceCube: sensitivitiesIceCube: sensitivities

1 year sensitivity E2·d/dE

diffuse point

8.110-9

[cm-2s-1sr-1GeV]5.510-9

[cm-2s-1GeV]

IceCube+AMANDA eventIceCube+AMANDA event

• verification of newly deployed string

• off-line synchronization of AMANDA and IceCube data

May '02 July '02June '02

Error bars: off-source background per 40 days

sliding search

window

Preliminary

Example: 1ES1959+650“Orphan flare” (MJD 52429)

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

Preliminary!

... very rare - very high energy events

many proposals for radio and acoustic detectors in ice, water, salt, from moon ..

e.g. ice:>>km attenuation lengthsparse instrumentation100-fold volume increase

... or moon, ice radio emission

>100

< 10 GZK neutrinos/year

RICE AGASA

Amanda, Baikal2002

2007

AUGER Anita

Amanda,Antares, Baikal, Nestor

2012

km3

Auger+ new techn.

2004

RICE GLUE

Carlos de los Heros, Uppsala University results from neutrino telescopes COSMO05. Bonn, Aug. 28 –...

Documents

Transcript of Carlos de los Heros, Uppsala University results from neutrino telescopes COSMO05. Bonn, Aug. 28 –...