Download - Dark Matter Detection in Space Jonathan Feng UC Irvine SpacePart 03, Washington, DC 10 December 2003
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Dark Matter Detection in Space
Jonathan Feng
UC Irvine
SpacePart 03, Washington, DC
10 December 2003
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10 December 2003 SpacePart 03 Feng 2
Dark Matter
• We live in interesting times:– We know there is dark matter, and how much– We have no idea what it is
• This talk: Recent developments with a focus on implications for space-based experiments
• The Wild, Wild West of particle physics:– Neutralinos, axions, Kaluza-Klein DM, Q balls,
wimpzillas, superWIMPs, self-interacting DM, warm and fuzzy DM,…
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10 December 2003 SpacePart 03 Feng 3
A Selection Rule: DM and the Weak Scale
• Universe cools, leaves a residue of dark matter with DM ~ 0.1 (Weak/) – remarkable!
• 13 Gyr later, Martha Stewart sells ImClone stock – the next day, stock plummets
Coincidence? Maybe, but worth investigating!
time
Freeze outSto
ck p
rice
($)
ExponentialdropExponential
drop
Freeze out
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10 December 2003 SpacePart 03 Feng 4
Neutralino Dark MatterGoldberg (1983) Ellis et al. (1983)
• Predicted by supersymmetry, motivated by particle physics considerations
• One of many new supersymmetric particles
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10 December 2003 SpacePart 03 Feng 5
Spin
U(1) SU(2) Up-type Down-type
2 G
graviton
3/2
1 B W 0
1/2
0 Hd
SUSY Particles
Neutralinos:
Spin
U(1)
M1
SU(2)
M2
Up-type
Down-type
m m3/2
2 G
graviton
3/2 G
gravitino
1 B W 0
1/2 B
Bino
W 0
Wino
Hu
Higgsino
HdHiggsino
0 Hu Hd
sneutrino
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10 December 2003 SpacePart 03 Feng 6
Neutralino Properties
Mass: ~ 100 GeV
Interactions: weak (neutrino-like)
The “typical” WIMP (but note: neutralinos are Majorana fermions – they are their own anti-particle)
• Direct detection: see Matchev’s talk
• Indirect detection: annihilationin the halo to e’s: AMS-02, PAMELA…
in the center of the galaxy to ’s: GLAST, AMS/, telescopes,…
in the center of the Sun to ’s: AMANDA, NESTOR, ANTARES,…
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10 December 2003 SpacePart 03 Feng 7
PositronsTurner, Wilczek (1990)
Kamionkowski, Turner (1991)
• The signal: hard positrons
• Best hope: e+e
• Problem: are Majorana-like, so Pauli Jinit = 0
e e
This process is highly suppressed
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10 December 2003 SpacePart 03 Feng 8
• Next best hope: WW, ZZ e+…
• Problem: conventional wisdom in simple models, ≈ Bino, does not couple to SU(2) gauge bosons
We are left with soft e+: bb ce+…
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10 December 2003 SpacePart 03 Feng 9
Photons
• ≈ Bino also suppresses the photon signal
• Best hope: – highly suppressed
• Next best hope: W+W, ZZ – also suppressed
[Both e+ and signals are sensitive to cuspiness, clumpiness in the halo.]
Urban et al. (1992)Berezinsky, Gurevich, Zybin (1992)
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10 December 2003 SpacePart 03 Feng 10
Example: Minimal Supergravity
Relic density regions and Bino-ness (%)• A simple model incorporating unification
≈ Bino in the
0.1 < DM < 0.3 region
• But not always!
= Bino-Higgsino mixture in “focus point region”
Feng, Matchev, Wilczek (2000)
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10 December 2003 SpacePart 03 Feng 11
SUSY WIMP DetectionSynergy: Particle probesDark matter detection
Recent data:• mh > 115 GeV• B(bs) ~ SM• (g2) ~ SM (maybe)• DM low (red region)
Conclusion: indirect detection favored
(valid beyond mSUGRA)
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10 December 2003 SpacePart 03 Feng 12
Extra Dimensional Dark Matter
• Extra dimensions generically predict Kaluza-Klein particles with mass n/R. What are they good for?
• If R ~ TeV-1, the lightest KK particle may be a WIMP
• Consider B1, the first partner of the hypercharge gauge boson
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10 December 2003 SpacePart 03 Feng 13
Positrons
• Here fi(E0) ~ (E0mB1). Is the peak is erased by propagation?
Moskalenko, Strong (1999)
• Recall in SUSY:
e+e suppressed by angular momentum
• But B1 has spin 1
• B1B1 ee is large, ~20% of all annihilations
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10 December 2003 SpacePart 03 Feng 14
Positrons from KK Dark MatterCheng, Feng, Matchev (2002)
Precision data dark matter discovery and mass measurement
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10 December 2003 SpacePart 03 Feng 15
SuperWIMP Dark Matter
• Both SUSY and extra dimensions predict partner particles for all known particles. What about the gravitino G or the 1st graviton excitation G1?
• G and G1 interact only gravitationally, but that’s sufficient for dark matter
• Consider G; the G1 case is identical up to O(1) factors
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10 December 2003 SpacePart 03 Feng 16
• G LSP
• Qualitatively new cosmology
Gravitinos from Late Decay• Assume gravitinos are diluted by inflation, and the universe
reheats to low temperature.
• G not LSP
• No impact – implicit assumption of most of literature
SM
LSPG
SM
NLSP
G
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10 December 2003 SpacePart 03 Feng 17
• Early universe behaves as usual, WIMP freezes out with desired thermal relic density
• A year passes…then all WIMPs decay to gravitinos
Gravitinos from Late Decay
WIMP≈G
Gravitinos naturally inherit WIMP density,but are superweakly-interacting – “superWIMPs”
MPl2/MW
3 ~ year
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10 December 2003 SpacePart 03 Feng 18
SuperWIMP Detection
• SuperWIMPs evade all conventional dark matter searches
• The only possible signal: WIMP superWIMP decays in the early universe
• Decay time is sensitive to
m = mWIMP – msWIMP
Feng, Rajaraman, Takayama (2003)
gravitino graviton
msWIMP = 0.1, 0.3, 1 TeV (from below)
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10 December 2003 SpacePart 03 Feng 19
Gravitino Cosmology: Detection• For m ~ O(100 GeV), WIMP superWIMP decays
occur before CMB and after BBN. This can be tested.
Cyburt, Fields, Olive (2003)Fields, Sarkar, PDG (2002)
WMAP
D = CMB
[7Li low]
Baryometry
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10 December 2003 SpacePart 03 Feng 20
• Signals are determined by WIMP: e.g., B → G ,…
• mWIMP , mG determine
Decay time: X
Energy release: EM = m nG / n
(G = DM)
• Large energy release destroys successes of BBN
• But G DM is allowed and low 7Li may even be superWIMP signal
G Signals: BBN
Cyburt, Ellis, Fields, Olive (2002)
Feng, Rajaraman, Takayama (2003)
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10 December 2003 SpacePart 03 Feng 21
• Late decays may also distort the CMB spectrum
• For 105 s < < 107 s, get
“ distortions”:
=0: Planckian spectrum
0: Bose-Einstein spectrum
• Current bound: || < 9 x 10-5
Future (DIMES): || ~ 2 x 10-6
G Signals: CMB
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10 December 2003 SpacePart 03 Feng 22
G Signals: Diffuse Photon Flux• For small m, decays may
be very late
• Photons produced at later times have smaller initial
E ~ m
but also redshift less; in the end, they are harder
• SuperWIMPs may produce excesses in keV-MeV photon spectrum (INTEGRAL) Feng, Rajaraman, Takayama (2003)
mSWIMP = 1 TeV
m = 1 GeV
m = 10 GeV
HEAO OSSE
COMPTEL
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10 December 2003 SpacePart 03 Feng 23
Summary and Outlook
• New dark matter possibilities (all satisfying the selection rule):– Bino-Higgsino dark matter– Kaluza-Klein dark matter– superWIMP dark matter
• New theoretical possibilities new signals for dark matter in space
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10 December 2003 SpacePart 03 Feng 24
Collider Inputs
Weak-scale Parameters
Annihilation N Interaction
Relic Density Indirect Detection Direct Detection
Astrophysical and Cosmological Inputs
What’s in our Future?