amanda recent results CRIS04

1
GETTING THERE FROM AMANDA TO ICECUBE
Carlos de los Heros Division of High Energy
Physics Uppsala University EPS2005 Lisbon, July
21-27, 2005
2
THE ICECUBE COLLABORATION
Sweden Uppsala Universitet Stockholm
Universitet Kalmar Universitet
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 AM
College, Baton Rouge
Germany Universität Mainz DESY-Zeuthen
Universität Dortmund Universität Wuppertal
Universität Berlin
UK Imperial College, London Oxford University
Belgium Université Libre de Bruxelles Vrije
Universiteit Brussel Universiteit Gent
Université de Mons-Hainaut
Netherlands Utrecht University
Japan Chiba university
New Zealand University of Canterbury
In March 2005, AMANDA merged into the IceCube
collaboration
3
NEUTRINO ASTRONOMY

• Cosmic rays _at_ gtgtTeV exist
• ? acceleration sites must sit somewhere
• Candidate sources
• SNe remnants, mQuasars
• Active Galactic Nuclei
• Gamma Ray Bursts
• Exotics (decays of topological defects...)

explained by SN?
proton accelerators
?
unexplained

• Guaranteed sources
• atmospheric neutrinos (from p K mesons decay)
• galactic plane
• CR interacting with ISM, concentrated on the
  disk
• CMB (diffuse)
• UHE p g ? D ? n p (p p0)

• Neutrinos not absorbed, not deflected
• ? difficult to detect
• Protons deflected in magnetic fields, GZK
• g-rays propagate straight, however
• reprocessed in sources
• absorbed in IR (100 TeV) and 3K (10 PeV)

4
THE AMANDA DETECTOR
1996 1997
2000
AMANDA-B10 (inner core of AMANDA-II) 10
strings 302 OMs Data years 1997-99
AMANDA-II 19 strings 677 OMs Data years 2000
AMANDA-B4 (first 4-string prototype) 4 strings 80
OMs Data years 1996
Whats up?

Optical Module
PMT noise 1 kHz
5
THE SITE
South Pole
road to work
Station facilities
AMANDA
1500 m
Amundsen-Scott South Pole station
2000 m
not to scale
6
NEUTRINO DETECTION IN POLAR ICE
South Pole ice (most?) transparent natural
condensed material
Event reconstruction by Cherenkov light timing
O(km) long muon tracks
O(10m) Cascades, ne nt Neutral Current
15 m
Longer absorption length ? larger effective volume
7
IN THIS TALK

• Results from
• atmospheric neutrinos
• searches for an extra-terrestrial n 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.
8
AMANDA sensitive in very different energy regimes
Energy range
production site(s)
MeV Supernovae
GeV-TeV Atmosphere Dark matter from Sun/Earth Galactic center
TeV-EeV mQuasars SN remnant AGN GRB
galactic
extra galactic
9
TEST BEAMS ATMOSPHERIC MUONS
cosmic ray muons
Atmospheric muons - AMANDA test beam Im
vs depth, CR composition - Background for
other searches
SPASE (scintillator array _at_ 3000m) e density
_at_ surface shower core resolution 0(m)
shower direction resolution lt 1.5o AMANDA
ms _at_ gt1500m (gt300 GeV _at_ surface) use SPASE
core position for combined fit use expected
lateral photoelectron/event
distribution as estimate of Nm Combined
SPASE-AMANDA detector - Probes hadronic (m)
and EM (e) component of the primary shower - s(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
EHadron ? E-2.7? 0.02
10
TEST BEAMS ATMOSPHERIC NEUTRINOS
Atmospheric neutrinos - Guaranteed test
beam - Background for other searches
First spectrum gt 1 TeV (up to 300 TeV) - matches
lower energy Frejus data
?Neural Network energy reconstruction of
up-going µs ?Regularized unfolding ? n energy
spectrum
horizontal
vertical
Frejus
Set limit on cosmic neutrino flux How much E-2
cosmic ? - signal allowed within uncertainty of
highest energy bins?
Amanda
Limit on diffuse E-2 ?µ flux (100 -300 TeV)
E2??µ(E) lt 2.6107 GeV cm-2 s-1 sr-1
11
ns FROM THE GALACTIC PLANE

• Expected from CRgalactic interstellar medium
• ns follow the primary energy spectrum, E-2.7
• Location of AMANDA ? reach only outer region of
  the galactic plane 33oltdlt213o
• data sample 2000-03 3329 n evts
• Three signal ansatz
• Line source
• Gaussian source
• Diffuse source

()
NO EXCESS OBSERVED
Optimal on-source region on-source events 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 271 283.3 4.8x10-4 (gauss) () (GeV-1 cm-2 s-1 sr-1)
12
SEARCH FOR POINT SOURCES

• 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 ?µ
• 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

13
DIFFUSE SEARCH
Analyses optimized for nm, reduced sensitivity
to ne and nt
All-flavour

• UHE En gt 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

• HE TeV lt En lt PeV
• Use directionality energy-related
• variables to reject atm m background
• Search confined to up-going tracks
• Use high-quality tracks

• Cascades TeV lt E lt PeV
• 4p search
• Background brehmm. from down-going muons

Limit from data sample 1997. 131 d
lifetime Assuming a E-2 flux (1 PeV lt En lt 3
EeV) and nenmnt 111 E2 Falln(E) lt 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 lt En lt 2 EeV) and nenmnt
111 E2 Falln(E) lt 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 lt En lt 3
EeV) and nenmnt 111 E2 Fm(E) lt 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 lt En lt 3.2 PeV) and nenmnt
111 E2 Falln(E) lt 9.5 x 10-8 GeV cm-2 s-1
sr-1
Limit from data sample 1997. 131 d
lifetime Assuming a E-2 flux (50 TeV lt En lt 3
PeV) and nenmnt 111 E2 Falln(E) lt 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 lt En lt 5 PeV) and nenmnt 111
E2 Falln(E) lt 8.6 x 10-7 GeV cm-2 s-1 sr-1

14
DIFFUSE SEARCHES SUMMARY
all-flavor limits
AMANDA 1 B10, 97, ?µ 2 A-II, 2000,
unfold. 3 A-II, 2000, cascade 4 B10, 97, UHE 6
A-II, 2000, UHE sensit. 7 A-II, 2000-03 ?µ
sensit. Baikal 5 98-03, casc.
111 flavor flux ratio
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
15
SEARCH 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 a (i.e. time)
• Sensitivity ? flat up to horizon
• Significant improvement w.r.t. first analysis
  with AMANDA-B10

Average upper limit sensitivity
(dgt0) (integrated above 10 GeV, E-2 signal)
AMANDA-B10
average flux upper limit cm-2s-1
AMANDA-II
sin(d)
Declination averaged sensitivity for a En-2
spectrum and En gt 10 GeV ??lim ? 0.610-8
cm-2s-1
16
SEARCH FOR CLUSTERS OF EVENTS IN THE NORTHERN SKY
Event selection optimized for both dN/dE E-2
and E-3 spectra
Data from 2000-2003 (807 days) 3369 n from
northern hemisphere 3438 n expected from
atmosphere
Maximum significance 3.4 s
Assess statistical significance using random sky
maps Probability of a background Fluctuation
92
17
SEARCH FOR CLUSTERS OF EVENTS FROM KNOWN OBJECTS
Selected objects and full scan of the northern
sky No statistically significant effect observed
Sensitivity Fn/Fg2 for 200 days of high-state
and spectral results from HEGRA
Source Nr. of n events (4 years) Expected backgr. (4 years) Flux Upper Limit F90(Engt10 GeV) 10-8cm-2s-1
Markarian 421 6 5.58 0.68
1ES1959650 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
Crab Nebula The chance probability of such an
excess (or higher) given the number of trials is
64
Preliminary
out of 33 Sources Systematic uncertainties
under investigation
18
POINT SOURCE SEARCH TIME WINDOW EXCESS
Enhance the detection chance by using the time
information Search for neutrino flares without
a-priori hypothesis on their time of occurrence
sliding window
Search for excesses in time-sliding
windows galactic objects 20 days extra-galactic
objects 40 days
events
time
Source Nr. of n events (4 years) Expected BG (4 years) Period duration Nr. of doublets Probability for highest multiplicity
Markarian 421 6 5.58 40 days 0 Close to 1
1ES 1959650 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 Close to 1
GRS 1915105 6 4.76 20 days 1 0.32
GRO J042232 5 5.12 20 days 0 Close to 1
Preliminary
out of 12 Sources ? no statistically
significant effect observed
19
SEARCH FOR ?s CORRELATED WITH GRBs
Low background analysis due to both space and
time coincidence!

• Catalogues BATSEIPN3
• Several search techniques
• coincidence with T90
• precursor (110s before T90)
• cascades (all flavour, 4p)
• -coincident with T90
• -rolling time window
• (no catalogue)
• Bckg. Stability required within 1 hour from
  burst
• Further searches rolling search (without
  temporal/spacial constrains)
• E?2F? lt 6.7x 10-6 GeV cm-2 s-1 sr-1

year GRB from preliminary 90CL upper limit assuming WB spectrum (EB at 100 TeV and G 300)
'97 - '00 312 BATSE triggered bursts E2dFn/dE 4 10-8 GeV cm-2s-1 sr-1
'00 - '03 139 BATSE IPN bursts E2dFn/dE 3 10-8 GeV cm-2 s-1 sr-1
'01 - '03 50 IPN bursts (Assuming the Razzaque model) E2dFn/dE 5 10-8 GeV cm-2 s-1 sr-1
'01 (425) Rolling window E2dFn/dE 2.7 10-6 GeV cm-2s-1sr-1
'00 76 BATSE triggered bursts E2dFn/dE 9.5 10-7 GeV cm-2s-1sr-1


20
SEARCH FOR DM CANDIDATES IN THE SUN/EARTH

• Wm ? 20, Wb ? 5
• ? non-baryonic matter
• ? MSSM c candidate
• accumulating over cosmological time in the
  Sun/Earth. Pair-wise annihilation at its center
• and consider (MCDarkSusy)
• (soft
  channel)
• (hard
  channel)
• for various c masses (50-5000 GeV)

Sun analysis possible due to improved reconstructi
on capability for horizontal tracks in AMANDA-II
compared with B10.
21
SEARCH FOR SNe EXPLOSIONS IN THE GALAXY

• Burst of low-energy
• (MeV) neutrinos from
• core collapse
• supernovae
• increase in
• detector noise rate
• due to
• nee- ? e- X
• Low energy O(ev)
• e- tracks no pointing
• Monitor noise of
• subset of stable OMs
• Special DAQ count
• rates in 10 s

Sun
Crab Nebula
Cassiopeia. A
Cygnus-X1
LMC
Approximate AMANDA horizon
SMC
90 000 light years
22
The IceCube observatory IceCubeIceTop
1200 m

• 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 gt 4 stations in
  coincidence

IceTop
IceCube

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

23
THE SITE
South Pole
road to work
Station facilities
AMANDA
IceCube
1500 m
Amundsen-Scott South Pole station
2000 m
not to scale
24
IceCube an All-Flavor Neutrino Telescope
?m? m
1 year sensitivity a point E2dF/dE flux

• IceCube will be able to identify
• ? tracks from ?? for E? gt 100 GeV
• cascades from ?e for E? gt 10 TeV
• ?? for E? gt 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?m lt 1 PeV focus on the Northern sky E? gt 1
PeV sensitive aperture increases w. energy
? full sky observations possible
25
IceTop Stations with DOMs January 2004
Digitized muon signals from DOMs
signal, freeze control, temperature control cables
Amplitude (ATWD counts) vs time (ns)
power cable
26
IceCube First String January 2005
27.1, 1008 Reached maximum depth of 2517 m,
reversed direction, started to ream up 28.1,
700 drill head and return water pump are out of
the hole, preparations for string installation
start 752 Handover of hole for
deployment 915 Started installation of the
first DOM (DOM 60) 1206 10th DOM
installed 2236 60th DOM installed Typical
time for DOM installation12 min 2248 Start
drop 29.1, 131 String secured at depth of
2450.80 m 2040 First communication to DOM
27
An IceCube-IceTop event
28
Outlook

• 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 n production in AGN.
• Some models already excluded _at_ 90CL
• 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