The Extreme Universe - Brown Universitygaitskell.brown.edu/.../Ong_Brown04_GammaRayAstro.pdf · The...

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The Extreme Universe The Extreme Universe Rene A. Ong Brown University Colloquium University of California, Los Angeles 1 March 2004 (The Limits of Particle Physics and Astronomy) (The Limits of Particle Physics and Astronomy)

Transcript of The Extreme Universe - Brown Universitygaitskell.brown.edu/.../Ong_Brown04_GammaRayAstro.pdf · The...

Page 1: The Extreme Universe - Brown Universitygaitskell.brown.edu/.../Ong_Brown04_GammaRayAstro.pdf · The Extreme Universe Rene A. Ong Brown University Colloquium University of California,

The Extreme UniverseThe Extreme Universe

Rene A. Ong Brown University ColloquiumUniversity of California, Los Angeles 1 March 2004

(The Limits of Particle Physics and Astronomy)(The Limits of Particle Physics and Astronomy)

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OUTLINEOUTLINE

• IntroductionMessengers, energy scales, & questions.Messengers, energy scales, & questions.

• Detecting Very High Energy (VHE) particles

• Physics: Origin of VHE particlesPower sources & particle acceleration.Power sources & particle acceleration.Probing particle physics and cosmologyProbing particle physics and cosmology

• Astrophysics: Sources and what not γγ--ray and ray and νν skies at skies at TeV TeV energies.energies.Active galaxies and dark matter.Active galaxies and dark matter.

• Future

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Cosmic MessengersCosmic Messengers

We know about the Universe primarily from:

Particles charge status

1. Photons neutral crucial

2. Cosmic Rays charged v. important

3. Neutrinos neutral developing

4. Grav. Waves neutral infancy

5. (New stable particle)

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Energy ScalesEnergy Scales

Planck

EW

Now

GUT

10-45

109 yr

10-40

10-35

10-30

10-25

10-20

10-15

10-10

10-5

105

1

103 yr

Time (sec)

Photons

CMBR

optical

X-raysG

amm

a ra

ys

CR

’s

CosmicRays

Temp.(oK)

1027

1024

1021 (ZeV)

1018 (EeV)

1015 (PeV)

1012 (TeV)

109 (GeV)

106 (MeV)

103 (keV)

1

1030

1025

1020

1015

1010

105

1

Energy (eV)

10-3

Hig

h-E

ner

gy

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Cosmic Ray SpectrumCosmic Ray Spectrum

• Total,diffuse spectrum individual species notresolved.

• Power-law spectrumE-3 differential.

• E > 1020 eV.

• Energy density~ 1 eV / cm3.

• What about gammas and neutrinos ?

TeV PeV EeV

γ ν ?

γCR

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At the Highest EnergiesAt the Highest Energies

Particles E > 1020 eVare not expected:

1. Very hard to accelerateto these energies.

2. Nuclei cannot travelbeyond 100 Mpc

p γcmbr ∆+ π’s

What are these particles and where do they come from ??

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HE ImplicationsHE Implications

Phenomenological

Energy scale is reached by either:Energy scale is reached by either:

1. Non1. Non--thermal & thermal & radiativeradiative processesprocesses ((AstrophysicsAstrophysics).).

2. Decays, interactions from higher mass scale2. Decays, interactions from higher mass scale((Particle PhysicsParticle Physics).).

Experimental

1. Particles are detected by total absorption.1. Particles are detected by total absorption.

2. We are required to measure tiny fluxes. 2. We are required to measure tiny fluxes. (< 1 /km(< 1 /km22/century at highest energies)./century at highest energies).

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Magnetic FieldsMagnetic Fields B

1. Galaxies have magnetic fields.• Protons and nuclei will be deflected by

the B ~ 3 µG galactic field.

M51

Larmor radius r = R/cB

R r _

1015 eV 0.3 pc

1020 eV 30 kpc size of galaxy

2. Intergalactic fields may also be significant• Clusters (e.g. Coma) have field strengths B ~ 0.1 – 2 µG,

perhaps extending out along sheets and filaments.

Charged CR directions will be scrambled by B fields.

We need neutral particles to do astronomy γ, ν

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Questions Questions

1. What is the origin of this diffuse flux of cosmic-ray particles?

• Abundant, extremely energetic particles. Sources must be both powerful and renewable.

• At highest energies – we have no understanding of how they can be produced.

2. Do these particles provide clues about the early Universe or about the physics at higher mass scales?

3. What can we learn from Astronomy at very high energies?

• Gamma-rays, ν’s point directly back to sites of extreme particle acceleration or unexpected phenomena.

• VHE particles can be used to probe radiation fields and the fabric of space-time.

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DETECTION OFDETECTION OFVHE/UHE PARTICLESVHE/UHE PARTICLES

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Experimental TechniquesExperimental Techniques

Balloon

Air shower arrayCherenkov Telescopes

Satellite

Ice/WaterCherenkov

ν

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EGRET (CGRO)EGRET (CGRO)

CGRO

• Flew 1991-2000.• Very successful mission.

EGRET

• Energy range 30 MeV – 20 GeV.• Small collection area.• Detected ~ 300 sources..

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Cherenkov Cherenkov Telescopes Telescopes

Area = 104 – 105 m2

~60 optical photons/m2/TeV

Whipple 10m (Arizona)

PMT camera

ns electronicsCherenkov image

γ−ray

θ ~ 1.5o

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Isolating Isolating γγ--raysrays

Shower profile in atmosphere

Mrk 421 2001

γ-rays

cosmic rays

Orientation angle (α)

RejectionFactor ~ 300(single tel)

P

γ

Proton shower movie

γ-ray shower movie

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ORIGIN OF ORIGIN OF HE PARTICLESHE PARTICLES

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Astrophysical OriginsAstrophysical Origins

To build a HE cosmic accelerator, we need the following parts:

1. Injection

2. Power Source

3. Acceleration

Emission

4. Propagation

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Power SourcesPower Sources

Broadly speaking, there are two types of sources:

1. ElectromagneticRotating highly magnetized objectRotating highly magnetized object (Pulsar)(Pulsar)

2. GravitationalCore collapse of a massive star Core collapse of a massive star –– SN and its remnantSN and its remnant

–– GammaGamma--ray Bursts ray Bursts Accretion onto a compact object (BH, NS, etc.)Accretion onto a compact object (BH, NS, etc.)other…other…

Somewhat intertwined – eventually acceleration is doneelectromagnetically, and often both are involved.

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Power Source: PulsarPower Source: Pulsar

Crab Nebula

Pulsar

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Supernova RemnantSupernova Remnant

SNR E102

radio x-ray • Collapse of massive star.

• Outer layers ejected with v ~ 1-2 x 104 km/s.

• Shell expands and shock frontforms as it sweeps up material from ISM.

• In ~ 104 yrs, blast wave begins to deccelerate (Sedov phase) and slowly dissipate.

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Active Galactic Nuclei (AGN)Active Galactic Nuclei (AGN)

• AGN are likely powered by accretion onto BH’s of 106 – 109 solar masses.

• Matter falling in piles up in rotating accretion disk. Released energy powers jets of relativistic outflow.

• Leading candidate as a source of UHE cosmic rays and neutrinos.

AGN model

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AGN MovieAGN Movie

Movie

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FermiFermi Acceleration Acceleration

A variety of mechanisms have been proposed to explain how HEparticles are accelerated in astrophysical environments.

Leading contender: Fermi acceleration.

Shock moves rapidly through ISM.HE particles move back and forth acrossshock, gaining energy. First-order Fermi acceleration ~(V/c).Naturally get power-law spectrum.

Applied to SN remnants, acceleration time ~ 104 yrs, we reach a limiting energy:

E max < Z x 1014 eV Very hard to go higher !

V

shock

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Beyond the Standard ModelsBeyond the Standard Models

Selected topics:

• SUSY & Dark Matter.• Probing space-time at high energies.

• (“GZK Neutrinos”.)• (“Top-down” sources of E > 1020 eV particles.)• (Primordial black holes).• (Cosmic IR radiation).

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Dark Matter & SUSYDark Matter & SUSY

γ

γ

X

X

Galactic Center

Neutralino Annihilation

• Neutralinos can have enhanced density in GC.• Annihilate to give γ-rays at GeV and TeV energies.• Prospects depend strongly on the actual density.

Flux ~ ( ρ / Mx )2 σ v

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Probing Intergalactic SpaceProbing Intergalactic Space--TimeTime

Quantum gravity:

• Discrete space-time “foam”• Effects propagation of light

• Flares from AGN and GRB’s.• Violation of Lorentz invariance.

Low E High E

AGN FlareWhipple 1996

• Probe to Mplank / 100.

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VHE VHE γγ--ray ASTRONOMYray ASTRONOMY

(A new window)(A new window)

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GeV GeV γγ--ray Skyray Sky

Pulsar

GRB

AGN

SNR

Radio Galaxy

Cosmic Rays !

• ~ 250 HE point sources, most unidentified.

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TeV TeV γγ--ray Skyray Sky

• Pulsars, SNR’s, AGN, Starburst galaxy …• All detected by Cherenkov telescopes.

1st UnknownSource ! Standard

Candle

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HE HE νν SkySky

• No sources yet !

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GeV GeV and and TeV TeV AGN: AGN: BlazarsBlazarsMrk 421 Whipple

Blazars:• Powerful, radio-loud objects.• Highly variable at all

wavelengths. • Jets – superluminal motion.• Produce GeV/TeV beams.

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AGN VariabilityAGN Variability

• Shortest variations probe to within factor of 10 of the Schwarzchild radius !

Whipple

• R < cTδ / (1+z) ~ 10-4 pc

• For M = 108 Msun, Rs ~ 10-5 pc.

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Correlation with XCorrelation with X--raysrays

• VHE Flares are generally well correlated with X-ray flares.

• But not in this case !

1ES1959+650 2002

Whipple

RXTE

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Broadband SpectrumBroadband Spectrum

Correlation in γ-ray and X-ray variability is mosteasily explained in ICscenarios.

Same e- population.

Additional constraints on electron energies, time scales, etc.

Starting to get adetailed understanding of these sources.

Mrk 501 Same epoch

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Has DM Already Been Detected?Has DM Already Been Detected?

Probably not !

CANGAROO-II(S. Australia)

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More on Dark MatterMore on Dark Matter

• Other good candidates include nearby galaxies with high mass/light: Draco, Ursa Minor, M32, M33.

• These are being pursued.

Core of Draco Dwarf

• Whipple result on GC• Excess γ-ray map from

2000-2003 data (16 hrs).

STAY TUNED !

SGR A*

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FUTUREFUTURE

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Future HE TelescopesFuture HE Telescopesγ-ray telescopesNeutrino telescopesGLAST, SWIFTIn space

VERITAS

HESS

ANTARES/NESTOR

IceCube

CANGAROO

MAGIC

ANITA

4 Telescope Arrays

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VERITASVERITAS

Collaboration: 50 scientistsU.S, Canada, U.K., Ireland

Detector Design:• Seven 12m telescopes• 500 pixel cameras (3.5o)• Site in southern Az (1700m)• Phase 1 operational in 2006.

Some characteristics:• Energy threshold ~ 100 GeV• Ang. Resolution ~ 4 arc-min • Crab rate ~ 35 γ/min

(45s detection!)VERITAS CONCEPT

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VERITAS VERITAS –– Well UnderwayWell Underway

Telescope 1:• All major systems tested.• Operational in fall 2004.

Electronics trailer

500 MHzFADC

Mt. HopkinsArizona

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VERITAS VERITAS ––11stst Cherenkov Cherenkov ImagesImages

• End-to-end test of system.• Looks very good.

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VERITAS Event Movie (Dec 03)VERITAS Event Movie (Dec 03)

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Variability PerformanceVariability Performance

30 min @ 1.5 Crab

6 min @ 4 Crab

6 min @ 1 Crab

• has hour-scale sensitivity for time-resolved spectralmeasurements.

• can probe intrinsic variability timescales.

VERITAS:

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The Competition: HESSThe Competition: HESS

H.E.S.S. Phase I4 x 12m Telescopes

Namibia Site (1700 m)

Jan 2004

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GLAST GLAST –– Satellite TelescopeSatellite Telescope

GLAST LAT Instrument:• Si tracker• CsI calorimeter• Anti-coincidence veto Sky map from 1 year survey

Launch in 2007.

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SummarySummary

• Very HE particles provide unique tests of the limits of physicallaws. Probe astrophysics in regimes not well understood.

• We have made a survey of the sky at GeV energies. At TeV energies, we have detected some remarkable phenomena, but most of the sky remains unexplored New Instruments.

• Great potential for discovery of physics beyond our standard models. (But, this physics is not yet required).

“The real voyage of discovery consists, not in seeking new landscapes, but in having new eyes.”

Marcel Proust (1871-1922)