Turning the Cosmos into

Particle Experiment Laboratory

In his first round of 60 years ( 還暦 ), Larry has dominated over us, with foresight and enthusiasm, in connecting cosmos to particle physics.In his second round of 60 years, don’t we want to tell him what to do?

Festschrift talk in honor of Larry SulakOctober 22, 2005

Tune Kamae (SLAC)

Career Started in Cosmic Ray Laboratory- Val, Jim, and Pierre were tenants to CRL -

machine shop and assembly space (foreman Fred)

warehouse where spark chamber filmswere scanned.

small library students’ bicycles

professors offices

“Regeneration” “gap”: no generation gap- Neutral kaons fascinated old and young -

K1 is “regenerated”

K2

K1

K1

K2

decay out

K2 K2

K1

K1

Interference

“gap”

PR

D w

as r

esp

ecte

dan

d w

ell-

read

.

Experiment with man-made accelerators- Everything was hand-made and reused several times -

“particles”“exp setup”

“accelerator”

Go underground: cosmic neutrinos- Crazy idea from Russia turned Larry high -

man-mindunderground lab

p

“Accelerator” and “particle” went cosmic.

IMB Super K Antares Nova

cosmic neutrinos

Can We Use Cosmic Setup too?- Challenge in borrowing the cosmic experimental setup -

Setup not well known: for example our Galactic Center

Cartoon made on radio and IR obs. by Charles Towns’ group at Berkeley

Super-massive black hole

Yes, but if…

Particle physicists with Larry’s• energy, • enthusiasm, • confidence, and • organization skill can turn the Cosmos into Particle Exp. Laboratory.

I am only 10 milli-Larry, so I need your help!

Parameterized Model of pp Interaction

Diffraction dissociation(ISR, SPS, CDF, Goulianos)

Non-diffractive inelastic with scaling-violation(ISR, SPS, CDF, Pythia)

Total -ray spectrum (via 0 decay)(power-law proton upto 512TeV)

Resonances

Diffr dissoc

Resonances

Non-diff

ISR, SPS, CDF Data are making Impact- Old soldiers are not forgotten -

New pp data

70’s pp data

Galactic -ray spctrby EGRET

pp int produces more e+

than e

e+

e

10 GeV100 MeV 1 GeV 10 TeV

proton index 2.0

Do We Understand Cosmic Accelerators?

Jets in AGN Pulsars and their nebulae

Supernovae and their remnants

So little is known:• Mechanism? only hand-waving arguments.• Electron/proton ratio? no clear evidence for proton.• Max. energy? only guessed

Nature’s Experimental Hall- CERN, SLAC, Fermi, KEK, Darmstadt, RIKEN on BU Campus -

200 light year

Supernova remnants

Supernova remnants

Molecular clouds

Molecular clouds

Galactic Center

Super-massiveBlack Hole

Nature’s Experimental Hall in Radio Band- We only see in a 2D projection -

Galactic Plane

l=+1.0 deg +0.5 0 -0.5 -1.0 l=-1.5 deg

b=+0.5

b=-0.5

Quiet Black Hole at Galactic Center

Many new giant stars are seen close to the BH

The BHat GC

Galactic Center seen in X-ray Band- We get a quite different image: evidence for old activity? -

Position of the Black Hole

Strong Fe K X-ray fluorescenceCollisional excitation?

Mild continuum X-ray emission

No Evidence for “LHC” in X-ray Image - Black Hole at Galatic Center is dormant now -

DEC

RA

1’

Image taken by Chandra.

The black hole is massive but almost dormant.

Many young stars are being born.

Positionof the BM(SgrA*)

SgrA*

GalacticPlane

Radio image

HESS imagewith radio contour

Galactic Plane

l=+1.0 deg +0.5 0 -0.5 -1.0 l=-1.5 deg

b=+0.5

b=-0.5

HESS imagewith radio contour

Surprise!! HESS found a TeV -ray Source

Galactic Center(Sgr A*)

Confusion, Confusion, Confusion - No GeV -ray found? -

Distribution of -ray (E>5GeV) detected by EGRET

New Idea for Instruments and Analyses Needed- Work for Larry’s second round of 60 years -

Particle physicists have been migrating to astrophysics with • new detector technology (ie. -detectors, GLAST)• new analysis methods (ie. SDSS, SN search, Macho search) • new physics emphasis (ie. dark matter, dark energy)motivated by exciting theories and big prizes.

We need the support team for “primary beam”,“secondary beams”, “magnets”, “floor survey”, “DAQ”.• All objects need to be modeled in 3D.• All wavelength must come out to be consistent.• Lots of models to be tried and eliminated.just like particle physics was in early 1960’s.

Why? Finding dark matter, cosmic ray sources, structure evolution,

as well as serendipitous discoveries require higher-quality analyses.

GLAST- Large Area Telescope- Daily survey in sub-GeV to 300GeV band -

e+ e–

> 40 times EGRET’s sensitivity

Angular Resolution0.35o @ 1 GeV0.1o @ 10 GeV

Large Effective Area (20 MeV – 1 TeV)

Wide Field of View(2.4 sr)

Good Energy Resolution(E/E ~ 10%)

Low dead time:< 20 s

NuSTAR- First spectral-resolved fine-imaging in hard X-ray -

SMEX mission in phase ALaunch date 2009+

Science Team:Fiona Harrison (Caltech; PI)SLAC/KIPAC, UCSC, JPL, Columbia, Sonoma State , DSRI

•Energy range: 6-80keV•Ang. resolution: 40 arcsec

PoGO: Hard X-ray Polarimeter- X-ray from electrons are likely to be polarized -

Main feature: Energy band: 25-80 keV FOV: ~5 deg2

Background: ~10mCrab Sensitivity = 6-10% in 100 mCrab sources in

a 6-hr balloon flight.

International collaboration: SU/KIPAC, Princeton, GSFC, Sweden, Japan

Polar Cap Model

Outer Cap ModelCaustic Model

Crab pulsar models and Pol.

AGN/microquasar jetsSNR, GRB, BH binaries

Higher Precision CO/HN Survey- 3D reconstruction -

Example: CO map around RXJ1713 by Nagoya Group:

Matching the size of SNR cavity observed by CO survey and X-ray/-ray.

GALPROP- 3D model of cosmic ray propagation and -ray emission

-

Andy StrongIgor Moskalenko

Larry, your second round of 60 years

will be as exciting as your first round.

HST image of the core of NGC 4261

galaxy nucleus

AGN