IceCube: Neutrino Messages from GRBs Alexander Kappes Univ. - - PowerPoint PPT Presentation

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IceCube: Neutrino Messages from GRBs Alexander Kappes Univ. - - PowerPoint PPT Presentation

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IceCube: Neutrino Messages from GRBs Alexander Kappes Univ. Erlangen / Univ. Wisconsin-Madison Deciphering the Ancient Universe with GRBs 19. 23. April 2010, Kyoto (Japan) Outline Neutrino detection & the IceCube observatory

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SLIDE 1

Alexander Kappes

  • Univ. Erlangen / Univ. Wisconsin-Madison

Deciphering the Ancient Universe with GRBs

  • 19. – 23. April 2010, Kyoto (Japan)

IceCube: Neutrino Messages from GRBs

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SLIDE 2

Alexander Kappes, GRB’10, Kyoto, 23. April 2010

Outline

  • Neutrino detection & the IceCube observatory
  • Current status of GRB searches with IceCube
  • Prompt neutrinos
  • Precursor neutrinos
  • Model independent searches
  • Future perspectives with IceCube
  • Observational program
  • Optical follow-up

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SLIDE 3

Principle of neutrino detection

muon

νμ

nuclear reaction cascade

time & position of hits µ (~ ν) trajectory energy PMT amplitudes

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SLIDE 4

Alexander Kappes, GRB’10, Kyoto, 23. April 2010

Background: atmospheric muons and neutrinos

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p atmosphere cosmic rays μ νμ νμ cosmic p μ νμ

  • Flux from above dominated by atmospheric muons
  • Neutrino telescopes mainly sensitive to neutrinos from below
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SLIDE 5

Alexander Kappes, GRB’10, Kyoto, 23. April 2010

Sky visibility in neutrinos

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Horizon above below

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SLIDE 6

IceCube at the South Pole

South Pole IceCube surface area

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SLIDE 7

Alexander Kappes, GRB’10, Kyoto, 23. April 2010

The IceCube observatory

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  • IceTop

Air shower detector

  • InIce

86 strings (5160 PMTs) Instrumented volume: 1 km3 Current status: 79 strings deployed

  • 1450 m
  • 2450 m
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SLIDE 8

Alexander Kappes, GRB’10, Kyoto, 23. April 2010 8

Current Status of GRB Searches with IceCube

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SLIDE 9

Alexander Kappes, GRB’10, Kyoto, 23. April 2010

Neutrinos from GRBs

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Fireball model Precursor

~-100 s T0 ~100 s > 1000 s

TeV neutrinos PeV neutrinos EeV neutrinos

Prompt Smoking gun evidence for hadronic acceleration → sources of UHECR

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SLIDE 10

Alexander Kappes, GRB’10, Kyoto, 23. April 2010

Detection channels

Muons:

  • Good angular resolution

(IceCube <1° for E > 1 TeV)

  • Rather poor energy resolution (factor ~3)

Cascades:

  • Sensitive to all flavors
  • Better energy resolution
  • Reduced directional information

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SLIDE 11

Alexander Kappes, GRB’10, Kyoto, 23. April 2010

  • GCN-satellite triggered searches

very low background → 1 event can be significant !

  • Untriggered “rolling window” searches

Analysis methods

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On-time (blind) Off-time Off-time T0 prompt precursor (~100 s) wide window (several hours)

background time

1 evt 2 evt 1 evt

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SLIDE 12

Alexander Kappes, GRB’10, Kyoto, 23. April 2010

Prompt phase: individual GRBs

  • Individual analysis of bright GRBs worthwhile
  • Example “naked-eye” GRB: Expected 0.1 events (9 strings)
  • Expect O(1) event from bright GRBs with 86 strings

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Γ = 300 90% CL upper limit νμ

GRB 080319B

Abassi et al., ApJ 701 (2009)

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SLIDE 13

Alexander Kappes, GRB’10, Kyoto, 23. April 2010

  • Individual modeling of bursts using satellite data

(fireball model á la Guetta et al.)

  • IceCube 40-strings: 117 GCN bursts

(northern hemisphere; mainly Swift + Fermi)

  • Sum expected events = 2.8; no signal found

Prompt phase: stacked searches

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preliminary

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SLIDE 14

Alexander Kappes, GRB’10, Kyoto, 23. April 2010

Waxman-Bahcall spectrum Individual spectra

Prompt phase: stacked searches

  • IceCube starts to constrain fireball model parameters

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90% CL upper limits νμ for 117 bursts

AMANDA final (using 416 bursts)

Achterberg et al., ApJ 674 (2008)

IceCube 40-strings (using 117 bursts) preliminary

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SLIDE 15

Alexander Kappes, GRB’10, Kyoto, 23. April 2010

Precursor phase

  • Jets with low Γ still

inside progenitor star → TeV neutrinos

  • Possibly large fraction
  • f “choked” bursts

→

  • nly detectable with

“rolling window”

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90% CL upper limits νμ

Rolling window AMANDA, cascades

Achterberg et al., ApJ 664 (2007)

Triggered IceCube, 22-strings

Abbasi et al., ApJ 710 (2010)

all SNe have choked jets Razzaque et al., PRD 68 (2003) (H progenitors)

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SLIDE 16

Alexander Kappes, GRB’10, Kyoto, 23. April 2010

SN 2008d: neutrinos from core-collapse supernovae

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90% CL upper limits νμ (IceCube 22-strings) Distance: 27 Mpc

  • First direct observation of

SN shock breakout

  • X-ray flash yields precise SN time
  • “Slow-jet” model

(Razzaque, Meszaros, Waxman, Ando, Beacom)

  • ~0.1 evts expected in IceCube 22-strings

Ando & Beacom, PRL 95 (2005):

  • jet points to Earth
  • Γb=3, Ej=3×1051
  • No signal found

preliminary

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SLIDE 17

Alexander Kappes, GRB’10, Kyoto, 23. April 2010

Model independent

  • Model-independent approaches important

→ choice of time window → energy spectrum

  • Simple approach: fixed (wide) time window
  • IceCube 22 strings (41 GRBs):
  • 1 to +3 h around GRB; No signal found

→ Average νμ upper limit (90% CL) per burst for E-2 flux: 6.6×10−5 erg cm−2 (3 TeV–2.8 PeV)

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Alexander Kappes, GRB’10, Kyoto, 23. April 2010

1 2 3 4 5 6 7 8 9 10 11 12 10 s 100 s 1000 s 10000 s 0.0 ! 100 5.0 ! 10-4 1.0 ! 10-3 1.5 ! 10-3 2.0 ! 10-3 2.5 ! 10-3 3.0 ! 10-3 Muon Neutrino Events Per-Burst Normalization (GeV cm-2) t (s) Icecube 40 E-2 Muon Neutrino Flux Limits 90% Upper Limit 90% Sensitivity

Approach for “arbitrary” time scales:

  • Start with search in small window and

increase it consecutively

  • Trial factor important
  • IceCube 40-strings: No signal found

Model independent

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Sensitivity νμ (90%CL; IceCube 40-strings)

per-burst normalization (GeV cm-2)

GRB Trigger Time Difference

Weighted Entries / bin

  • 40
  • 20

20 40 60

0.000 0.005 0.010 0.015

emission window (s)

preliminary

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SLIDE 19

Alexander Kappes, GRB’10, Kyoto, 23. April 2010 19

Future Perspectives with IceCube

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SLIDE 20

Alexander Kappes, GRB’10, Kyoto, 23. April 2010

Observational program

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Detector sensitivity still increasing significantly during next (analysis) years; operation for at least for 10 years

  • Triggered searches
  • Stacked analysis (model dependent + independent)
  • Individual analyses of exceptional bursts
  • Satellite “coverage”:
  • Present: Swift 2010 + 4 years, Fermi 2013 (+ 5 years)
  • Future:

SVOM (planned 2012 – ?), UFFO (planned 2015 – ?), EXIST (2017?) . . .

  • Rolling-window searches important !
  • All-flavor searches (cascades) underway
  • Optical follow-up
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SLIDE 21

Alexander Kappes, GRB’10, Kyoto, 23. April 2010

  • IceCube coincidence triggers optical follow-up
  • angular window 3.5°
  • time window 100 s
  • Delay neutrino detection → start of optical observations: < 5 min

Optical follow-up

SN/GRB

Institute in the North Optical telescopes

Iridium IceCube

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SLIDE 22

Alexander Kappes, GRB’10, Kyoto, 23. April 2010 22

Observational program

Kahn et al., 2006

t (days after burst) 1E-4 0.01 1 100

Strizinger et al. (2003)

magnitude t (days after burst) 20 40 60

  • Prompt observation (first night):

Search for fast decreasing GRB afterglow

  • 10 short

(5 s obs. time)

  • 10 medium (20 s obs. time)
  • 20 long

(60 s obs. time)

  • Follow-up observations (14 following nights):

Slowly rising supernova light-curve

  • 8 long (60 s obs. time) per night
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SLIDE 23

Alexander Kappes, GRB’10, Kyoto, 23. April 2010

  • Fully robotic
  • 24 hour (almost) all sky coverage
  • Large field of view (1.85˚× 1.85˚)

ROTSE telescope network

H.E.S.S., Namibia McDonald, Texas TUG, Turkey SSO, Australia

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Alexander Kappes, GRB’10, Kyoto, 23. April 2010 24

Image processing

– =

„New“ „Reference“ Subtraction

  • Automatic candidate selection
  • Test of algorithms with simulated

SN light-curve

(SN light-curve model by P. Nugent (SN1999ex))

  • System successfully running

since end of 2008

  • Data analysis underway

Simulated SN light-curve

extracted -mag. TUG, Turkey McDonald, Texas Limiting mag. Measured mag. time [days] T+0 T+10 T+20 T+30

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SLIDE 25

Alexander Kappes, GRB’10, Kyoto, 23. April 2010

Summary

  • With IceCube, the first km3-scale neutrino telescope is

nearing completion

  • GRBs highly interesting targets for neutrino telescope
  • Analyses cover wide range of scenarios;

already starting to constrain models

  • Optical follow-up program extends IceCube’s

physics potential significantly

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SLIDE 26

Alexander Kappes, GRB’10, Kyoto, 23. April 2010

The IceCube collaboration

Alexander Kappes PANIC'08, Eilat 16

  • Univ Alabama, Tuscaloosa
  • Univ Alaska, Anchorage
  • UC Berkeley
  • UC Irvine
  • Clark-Atlanta University
  • U Delaware / Bartol Research Inst
  • Georgia Tech
  • University of Kansas
  • Lawrence Berkeley National Lab
  • University of Maryland
  • The Ohio State University
  • Pennsylvania State University
  • University of Wisconsin-Madison
  • University of Wisconsin-RiverFalls
  • Southern University, Baton Rouge
  • Universität Mainz
  • Humboldt Univ., Berlin
  • DESY, Zeuthen
  • Universität Dortmund
  • Universität Wuppertal
  • MPI Heidelberg
  • RWTH Aachen
  • Universität Bonn
  • Uppsala University
  • Stockholm University

Chiba University

  • Universite Libre de Bruxelles
  • Vrije Universiteit Brussel
  • Université de Mons-Hainaut
  • Universiteit Gent
  • EPFL, Lausanne
  • Univ. of Canterbury, Christchurch

University of Oxford