Searching for High Energy Muonic Searching for High Energy Muonic Neutrinos from Gamma-Ray Bursts Using Neutrinos from Gamma-Ray Bursts Using

AMANDAAMANDA

A.J. Carver

University of Wisconsin – MadisonUniversity of Wisconsin – Madison

Advisors: Prof. Bob Morse & Mike Stamatikos

August 7, 2003

acarver@wisc.edu

Title

NeutrinosNeutrinos - A New Window On Astronomy - A New Window On Astronomy

Telescope User date Intended Use Actual use

Optical Galileo 1608 Navigation Moons of Jupiter

Optical Hubble 1929 Nebulae Expanding Universe

Radio Jansky 1932 Noise Radio galaxies

Micro-wave Penzias, Wilson

1965 Radio-galaxies, noise 3K cosmic

background

X-ray Giacconi … 1965 Sun, moon neutron stars

accreting binaries

Radio Hewish,

Bell 1967 Ionosphere Pulsars

γ- rays military 1960? Thermonuclearexplosions

Gamma raybursts

The 21The 21stst Century will feature Neutrino Astronomy with Century will feature Neutrino Astronomy with AMANDA/IceCube!AMANDA/IceCube!

New Window

Discovering High Energy Muonic Neutrinos Discovering High Energy Muonic Neutrinos from GRBs would be from GRBs would be VERY SIGNIFICANTVERY SIGNIFICANT

• Confirm hadron acceleration in the relativistic GRB wind

• Validate the FIREBALL MODELFIREBALL MODEL phenomenology

• Provide an acceleration mechanism for the highest energy cosmic rays

We hope to make this discoverySignificance

Gamma-Ray Bursts (GRBs) – Gamma-Ray Bursts (GRBs) – The Past 30 The Past 30 yrsyrs

• Discovered in 1969 by Vela nuclear test detection satellites (Klebesadal, et al., 1973)

•Bursts of Gamma-Rays NOTNOT from Sun or Earth

•Little more learned because of little observational data

GRB Discovery

Gamma-Ray Bursts (GRBs) – Gamma-Ray Bursts (GRBs) – QuestionsQuestions

• Where on the sky do GRBs occur?

• Are all GRBs the same?

• How far away are GRBs?

• What causes GRBs?

• More observations needed

• BATSEBATSE - BBurst AAnd TTransient SSource EExperiment

GRB Questions

Gamma-Ray Bursts (GRBs) – Gamma-Ray Bursts (GRBs) – Q&AQ&A• Where on the sky do GRBs occur?

• Everywhere – GRBs Isotropically distributed

Isotropic

Gamma-Ray Bursts (GRBs) – Gamma-Ray Bursts (GRBs) – Q&AQ&A

• NO! Absolutely not.

Unique• Are all GRBs the same?

Gamma-Ray Bursts (GRBs) – Gamma-Ray Bursts (GRBs) – Q&AQ&ACosmological

•GRBs are at cosmological distances

• How far away are GRBs?

GRBs & NeutrinosGRBs & Neutrinos – The Connection – The Connection

μμμ νννμνπγ +++→+→+→Δ→+ +++++eenp

Coincident SearchCoincident Search – Neutrinos Coincident with Photons – Neutrinos Coincident with Photons

Neutrino DetectionNeutrino Detection

• Neutrino Telescope

• Located at South Pole

• Uses PMTsPMTs to detect Cherenkov radiation created by fast moving particles

• We are interested in up-going events

AMANDAAMANDA – AAntarctic MMuon AAnd NNeutrino DDetector AArray

Past Past AnalysisAnalysis

• Searched for neutrinos from GRBs detected by BATSE between 1997 and 2000 data

• Used generic neutrino spectrum

Past

Past Past AnalysisAnalysis• Produced a framework and tools for future GRB analyses

• Detector stability & data integrity

• Background minimization (cuts)

Past

Blinded (10) minute window

- (5) minutes

+ (5) minutes

(120-10 = 110) Minute background used to set cuts and check for data quality & stability

- (60) minutes

+ (60) minutes

NONO GRB neutrinos coincidence detected – results in 2003 International Cosmic Ray Conference (ICRC) proceedings

PresentPresent Analysis Analysis• Models the neutrino spectrum on a per burst per burst basis basis (based on Guetta et al. 2003 astro-ph0302524)(based on Guetta et al. 2003 astro-ph0302524)

• Determines per burst neutrino event rates

• Extends analysis to 2003Extends analysis to 2003

• Creating user-friendly and flexible infrastructure

BATSEBATSE Kommers et al. Stern et al.Stern et al. GUSBADGUSBAD

Duration of Search (TJD)

~8360-~8360-1169011690

8600– 10800 8369-116908369-11690 8365-8365-1169011690

Energy Range (KeV) 50-30050-300

50-300 7 combos of

energy analyzed50-30050-300 50-30050-300

Sigma above background for trigger

σσ11>=5.5>=5.5

σσ22>=5.5>=5.5

σ1>=σ2>=2.5 & σ1+σ2>8

σσ11>=4 >=4 σσ22>=2.5>=2.5

σσ11>5>5

σσ22>5>5

Data Used

4 Energy 4 Energy Channels Channels over three over three

time time resolutionsresolutions

DISCLA DISCLADISCLA DISCLADISCLA

Time Resolution

(msec)

64, 256, 64, 256, 10241024

1024 10241024 10241024

The Stern catalog overlaps ~96%~96% of Kommers and ~94%~94% of Schmidt (GUSBAD) catalogs.

GRB Catalog Comparisons GRB Catalog Comparisons

T90 Distribution

-90°

+90°

360°0°

Sky plot of GRBs comprising Master List for Sky plot of GRBs comprising Master List for New UW Analysis:New UW Analysis:

96 BATSE (triggered)96 BATSE (triggered) bursts and 9 Stern (non-triggered)9 Stern (non-triggered) bursts passed the selection criteria

Dec Distribution

• BATSE trigger 7644 – solar flare, NOT A GRBNOT A GRB

• BATSE triggers 2463 and 2464 – SGRs, NOT NOT GRBsGRBs

• 8 more triggers will be reclassified for the upcoming 5B catalog

• Many order problems in 4B & Current Cmax/Cmin Catalog

• Being corrected by BATSE teamBeing corrected by BATSE team

• Demonstration of thoroughness

Discovery of Discovery of ErrorsErrors in current in current BATSE CatalogBATSE Catalog

K. Hurley, http://ssl.berkeley.edu/ipn3/

• Group of satellites capable on Gamma ray detection

• BridgeBridge between BATSE & Swift

• 24 member instruments as of 5/22/03

• Major endeavor

• 16 eliminated16 eliminated

• 3 still under investigation

• 5 accepted

• Comparisons have begun

IPN3

FutureFuture Analysis Analysis

• Methods developed now will allow for speedier analysis of future data

• A dedicated GRB satellite ~200 bursts/yr

Future

ICECUBEICECUBE – Kilometer cubed neutrino telescope

ConclusionsConclusions• Neutrino AstronomyNeutrino Astronomy – New Window on the Universe

• Neutrino ProductionNeutrino Production - Consequence of Fireball Phenomenology of GRBs

• GRB Neutrino CoincidenceGRB Neutrino Coincidence – Significant Discovery

• Comprehensive ComparisonsComprehensive Comparisons - BATSE & 3 non-triggered catalogs

• Generating IPN3 catalogGenerating IPN3 catalog – Welcomed by GRB community

• Analysis EvolutionAnalysis Evolution

EXCITING FUTUREEXCITING FUTURE

Thank YouThank You

Without each of your influences, assistance, confidence, guidance, patience, empathy, support, and humor this

research and my summer would not have been nearly as great. I am deeply grateful. Thank you!Thank you!

Mike Stamatikos, Bob Morse, Rellen Hardtke, Francis Halzen, Cary Forest, Paolo Desiati, Kath

Rawlins, Brennan Hughey, Jodi Cooley, Bill Santner, Anupam Singh, Newt Ganugapati, Gary Hill,

Albrecht Karle, Annie Malkus, more “AMANDROIDS” (Chris, Jessica, Dave, Kael), Bob Benjamin, Greg

Madsen, Ron Reynolds, Aaron Steffen, Ken Nordsieck, Tony

Weitenbeck, the REU students: Eric, Stephanie, Kiwi, Jeremy, Amanda, Karl, Tommy, Sam, Luis,

Kimb, Quennie, Kelen, Luisa, and Marleen

My apologies if I overlooked someone in preparing this slide

To learn more about “To learn more about “Searching for High Energy Searching for High Energy Muonic Neutrinos from Gamma-Ray Bursts Using Muonic Neutrinos from Gamma-Ray Bursts Using

AMANDAAMANDA” contact:” contact:

A.J. Carver - acarver@wisc.edu

Or visit online at:

http://wisp.physics.wisc.edu/~reu2003/carver

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