Turning the Cosmos
into
Particle Experiment Laboratory
Festschrift talk in honor of Larry Sulak
October 22, 2005
Tune Kamae (SLAC)
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?
Career Started in Cosmic Ray Laboratory
- Val, Jim, and Pierre were tenants to CRL warehouse where
spark chamber films
were scanned.
machine shop and assembly
space (foreman Fred)
professors offices
small library
students’ bicycles
“Regeneration” “gap”: no generation gap
- Neutral kaons fascinated old and young K1
decay
out
PRD was respected
and well-read.
K2
“gap”
K1 is “regenerated”
K1
K1
K1
K2
K2
Interference
K2
Experiment with man-made accelerators
- Everything was hand-made and reused several times -
“accelerator”
“particles”
“exp setup”
Go underground: cosmic neutrinos
- Crazy idea from Russia turned Larry high -
“Accelerator” and “particle” went cosmic.
IMB 
Super K  Antares  Nova
p
man-mind
underground lab
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
Non-diffractive inelastic
with scaling-violation
(ISR, SPS, CDF, Pythia)
Total g-ray spectrum (via p0 decay)
(power-law proton upto 512TeV)
Non-diff
Resonances
Diffraction dissociation
(ISR, SPS, CDF,
Goulianos)
Resonances
Diffr dissoc
ISR, SPS, CDF Data are making Impact
- Old soldiers are not forgotten Galactic g-ray spctr
by EGRET
New pp data
pp int produces more e+
than e-
e+
proton index 2.0
e-
100 MeV
10 GeV
70’s pp data
1 GeV
10 TeV
Do We Understand Cosmic Accelerators?
So little is known:
• Mechanism? only hand-waving arguments.
• Electron/proton ratio? no clear evidence for proton.
• Max. energy? only guessed
Jets in AGN
Pulsars and
their nebulae
Supernovae and
their remnants
Nature’s Experimental Hall
- CERN, SLAC, Fermi, KEK, Darmstadt, RIKEN on BU Campus Supernova
remnants
Molecular
clouds
200 light year
Molecular
clouds
Super-massive
Black Hole
Galactic Center
Supernova
remnants
Nature’s Experimental Hall in Radio Band
- We only see in a 2D projection l=+1.0 deg
b=+0.5
Galactic
Plane
b=-0.5
+0.5
0
-0.5
-1.0
l=-1.5 deg
Quiet Black Hole at Galactic Center
Many new giant
stars are seen close
to the BH
The BH
at GC
Galactic Center seen in X-ray Band
- We get a quite different image: evidence for old activity? Mild continuum X-ray emission
Strong Fe K X-ray fluorescence
Collisional excitation?
Position of
the Black Hole
No Evidence for “LHC” in X-ray Image
- Black Hole at Galatic Center is dormant now -
DEC
Image taken by Chandra.
RA
The black hole is massive but
almost dormant.
Many young stars are being
born.
1’
Surprise!! HESS found a TeV g-ray Source
HESS image
with radio
contour
SgrA*
Position
of the BM
(SgrA*)
Radio image
Galactic
Plane
l=+1.0 deg
+0.5
0
-0.5
-1.0
l=-1.5 deg
b=+0.5
Galactic
Plane
HESS image
with radio
contour
b=-0.5
Confusion, Confusion, Confusion
- No GeV g-ray found? -
Distribution of g-ray
(E>5GeV) detected
by EGRET
Galactic Center
(Sgr A*)
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. n-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 -
g
Angular Resolution
0.35o @ 1 GeV
0.1o @ 10 GeV
Wide Field of View
(2.4 sr)
> 40 times
EGRET’s
sensitivity
Low dead time:
< 20 ms
e+
Large Effective Area
(20 MeV – 1 TeV)
e–
Good Energy Resolution
(DE/E ~ 10%)
NuSTAR
- First spectral-resolved fine-imaging in hard X-ray SMEX mission in phase A
Launch date 2009+
• Energy range: 6-80keV
• Ang. resolution: 40 arcsec
Science Team:
Fiona Harrison (Caltech; PI)
SLAC/KIPAC, UCSC, JPL, Columbia,
Sonoma State , DSRI
PoGO: Hard X-ray Polarimeter
- X-ray from electrons are likely to be polarized International collaboration:
 SU/KIPAC, Princeton, GSFC, Sweden, Japan
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.
Crab pulsar models and Pol.
Polar Cap Model
AGN/microquasar jets
SNR, GRB, BH binaries
Caustic Model
Outer Cap Model
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/g-ray.
GALPROP
- 3D model of cosmic ray propagation and g-ray emission Andy Strong
Igor Moskalenko
Larry,
your second round of 60 years
will be as exciting as
your first round.
HST image of the core of
NGC 4261
AGN
galaxy
nucleus