Colloquium by Jonathan Feng - Fermilab Center for Particle ...

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CURRENT STATUS e + + e - PAMELA (2008) ATIC (2008) Solid lines are the astrophysical bkgd from GALPROP (Moskalenko, Strong) 23 Mar 11 Feng 14
ARE THESE DARK MATTER? • Energy spectrum shape consistent with WIMP dark matter candidates • Flux is a factor of 100-1000 too big for a thermal relic; requires – Enhancement from astrophysics (very unlikely) – Enhancement from particle physics – Alternative production mechanism Cirelli, Kadastik, Raidal, Strumia (2008) Arkani-Hamed, Finkbeiner, Slatyer, Weiner (2008) Feldman, Liu, Nath (2008); Ibe, Murayama, Yanagida (2008) Guo, Wu (2009); Arvanitaki et al. (2008) • Pulsars can explain PAMELA Zhang, Cheng (2001); Hooper, Blasi, Serpico (2008) Yuksel, Kistler, Stanev (2008); Profumo (2008) Fermi-LAT Collaboration (2009) KK dark matter with m ~ 600 GeV ATIC (2008) Fermi-LAT Collaboration (2009) 23 Mar 11 Feng 15
Page 1 and 2: WIMP PARADIGM: CURRENT STATUS FNAL
Page 3 and 4: THE COSMIC CONNECTION, c. 1977 “O
Page 5 and 6: DARK MATTER Known DM properties •
Page 7 and 8: 23 Mar 11 THE WEAK MASS SCALE • F
Page 9 and 10: 23 Mar 11 THE WIMP MIRACLE 10-3 σ0
Page 11 and 12: LEP’S COSMOLOGICAL LEGACY Gauge H
Page 13: INDIRECT DETECTION Dark Matter anni
Page 17 and 18: DIRECT DETECTION • Can look for n
Page 19 and 20: LOWER LIMIT ON DIRECT DETECTION •
Page 21 and 22: LOW MASS FRONTIER Collision rate sh
Page 23 and 24: SPIN-DEPENDENT SCATTERING 23 Mar 11
Page 25 and 26: CURRENT BOUNDS FOR SUSY Yellow: pre
Page 27 and 28: 23 Mar 11 THE SIGNIFICANCE OF 10 -4
Page 29 and 30: BEYOND WIMPS • Does the WIMP para
Page 31 and 32: FREEZE OUT WITH SUPERWIMPS WIMPs fr
Page 33 and 34: WARM SUPERWIMPS • SuperWIMPs are
Page 35 and 36: • In SUSY, however, there may be
Page 37: CONCLUSIONS • Particle Dark Matte

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