??????: SU(3) C

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??????? ??????
??? 2006.6.5
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?????? (????)

• ???????
• ?????? SU(3) CSU(2)LU(1)Y
• Higgs ??????

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WMAP The Biggest
Surprise Nothing Particular
Surprising ?Inflation ? ?
?
Important ???????

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• ??
• ???????
• ????????????
• ?????????

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?????

• ??????????,???????????????
• ?????????????,???????-????????
• ??????????????????,???,??????
• Inflation???inflaton?

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• ???????
• ?????????
• II. ??????????

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Application showcase neutrino mass
neutrino mass and abundance
O. Elgaroy et al (2dFGRS) PRL 89, 061301 (2002)
hot dark matter suppress power at small scale
current cosmological bound (95 CL) m?lt1.7/3
eV (weak prior) m? lt0.6/3 eV (strong prior)
vs.
tritium decay m?e lt 2.2 eV
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hep-ph/0503257
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Weighing neutrinos in the presence of a running
primordial spectral indexastro-ph/0605742

• Bo Feng, Jun-Qing Xia, Jun'ichi Yokoyama, Xinmin
  Zhang, Gong-Bo ZhaoThe three-year WMAP(WMAP3),
  combined with other cosmological observations
  from galaxy clustering and Type Ia Supernova
  (SNIa), prefers a non-vanishing running of the
  primordial spectral index independent of the low
  CMB multipoles. Motivated by this feature we
  study cosmological constraint on the neutrino
  mass, which severely depends on what prior we
  adopt for the spectral shape of primordial
  fluctuations, taking possible running into
  account. As a result we find a more stringent
  constraint on the sum of the three neutrino
  masses, m_\nu lt 0.76 eV (2 \sigma), compared with
  the case where power-law prior is adopted to the
  primordial spectral shape.

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?????????? ??(Axion)
?????(Neutralino)
??,???????? Interacting Dark
Matter Non-thermal produced
Neutralino Steril Neutrino
Gravitino Quintessino
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• ??(Axion)
• ????CP??????? (Peccei Quinn)
• ?? ????
• ??
• ?????

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Cosmic rays from the halo of the MWsome weak
hints on DM
Baltz et al. 2002

• Some astrophysics observations can not be
  explained by the canonical physics. They may
  indicate the signal of DM, however, no conclusion
  can be drawn now.
• One of such experiments is the HEAT. (The HEAT
  signal may indicate the non-thermal production or
  the subhalo nearby)

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ASg and ARGO (High Duty cycle,Large F.O.V)
TeV
100GeV
???? ARGO ??RPC??
???? AS ? ???????????
Here comes the two experiments hosted by YBJ
observatory. One is call ASg, a sampling detector
covering 1 of the area and have been operated
for 15 years. The other full coverage one is
called ARGO, still under installation. ASg use
scintillation counter and ARGO use RPC to
detector the arrival time and the number of
secondary particles, with which the original
direction and energy of CR particle can be
restored. ASg has a threshold energy at a few TeV
while ARGO down to about 100GeV. Both experiment
have the advantages in high duty cycle and large
field of view. Because for both of the
experiments there is only one layer of detector,
it is very difficult to separate the g ray shower
from CR nuclei showers. Working in the similar
energy range on mountain Jemez near Los Alamos,
by using water cherenkov technique, MILAGRO has
two layer of PMT, which enable it a rather good
capability to separate g ray from background.
Though it locates in a low altitude, has a
smaller effective area, it has similar
sensitivity to ASg experiment. To combine this
technique with high altitude would greatly
improve the sensitivity of our current EAS
experiments.
ARGO hall, floored by RPC. Half installed.
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???
???? ????
?
???? w1/3, ?? w0
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??????? 1,???(?????) ??
???????! ???w-1?
???

Fine Tuning
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2,????(Quintessence)
?
??
A.
????????
Within 2 s, the cosmological constant fits well
the data
Data mildly favors a running of the W across -1
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Constraints on EOS from SN Ia

• ??????
• I. ???? w
• II. ??????
• a. b.
• ?? SN Ia ?????

Astro-ph/0510447
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Feng, Wang Zhang Astro-ph/0404224 Huterer
Cooray Astro-ph/0404062
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Within 2 s, the cosmological constant fits well
the data
Data mildly favors a running of the W across -1
Feng, Wang Zhang Astro-ph/0404224
??1, ??? w-1 2,
Quintessence -1w1 3, Phantom
-1w 4, Quintom w transit
from below 1 to above -1
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astro-ph/0407259, Steen Hannestad, Edvard
Mortsell
Probing Dark Energy with Supernovae a
concordant or a convergent model? Authors J.-M.
Virey, A. Ealet, C. Tao, A. Tilquin, A.
Bonissent, D. Fouchez, P. Taxil,astro-ph/0407452
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Constraints on dark energy with SN Ia (Riess)
SDSS WMAP-1
????? W0-1.30 W11.25
Observing dark energy dynamics with supernova,
microwave background and galaxy clustering
Jun-Qing Xia, Gong-Bo Zhao, Bo Feng, Hong Li and
Xinmin Zhang Phys.Rev.D73, 063521,
2006
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Global fitting with SN Ia, galaxy clustering and
WMAP3

• Quintom is also mildly favored
• The standard ?CDM model is
• still a good fit to the current data

Probing dynamics of DE with supernova, galaxy
clustering and the three-year Wilkinson
Microwave Anisotropy Probe (WMAP) observations
G.-B. Zhao, J.-Q. Xia, B. Feng and X. Zhang,
astro-ph/0603621
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Riess et al, astro-ph/0402512
SNAP Collaboration astro-ph/0405232
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?????????

• ??????????????
• ??????(Quintessence, Phantom, Quintom)?????
• Quintom is mildly favored

?????? ???????????--???????
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Quintessence ? ????????
?????????
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Quintessence ? ????????

• ???????????
• ?CDM
• QCDM

????
???,???,???,PRD68, 087301 (2003)
??????????
GRB Delay of flight time? ?????? NEUTRINO
OSCILLATIONS AS A PROBE OF DARK ENERGY D.
Kaplan, A. Nelson, N. Weiner
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Cosmological evolution of Interacting Dark
Energy models with massvarying
neutrinos hep/ph/0412002
-Xiaojun Bi, Bo Feng, Hong Li, Xinmin Zhang

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??????????
????
?? ?????? ??,
???????

• D.B. Kaplan et al., PRL 93,091801 (2003)
• V. Barger et al., PRL 95 (2005) 211802
• M. Cirelli et al., NPB 719 219 (2005).

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??????????
????????????

• ????? ??
• ?????????

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Oscillating Quintom and the Recurrent Universe
astro-ph/0407432 Bo
Feng, Minzhe Li, Yunsong Piao, Xinmin Zhang
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Astro-ph / 0605366
Parameterization
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?????
??
BBN
CMB
Sakharov????

• ???B???(??)
• C?CP??( C???????, P????? )(CKM??)
• ?????(??????)

?????????????????,??,?????????, ???????
? ???CPT????
Spontaneous baryo(lepto)genesis ??
CPT?? ?????
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?????? Baryogenesis ??????? Leptogenesis
???????? ?? (???) ??????CP??
(?????2100????????????)

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Leptogenesis ??
M. Tegmark et al, Phys.Rev. D 69, 103501 (2004).
???????
Sakharov ??? A.D. Sakharov, JETP Lett. 5,
24 (1967).
1. ????? 2. C ? CP ?? 3. ?????
Leptogenesis M. Fukugita and T.
Yanagida, Phys. Lett. B 174, 45 (1986).
1. ?????? Majorana ???????? 2. ?????? Yukawa
????? C ? CP 3. ??????????
Sphaleron ??????????????
V.A. Kuzmin, V.A. Rubakov and M.E. Shaposhnikov,
Phys. Lett. B 155, 36 (1985).
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Seesaw ??
M. Gell-Mann, P. Ramond and, R. Slansky T.
Yanagida R.N. Mohapatra and G. Senjanovic S.L.
Glashow.
For a review, see S.M. Bilenky, C. Giunti, and
W. Grimus, Prog.Part. Nucl. Phys. 43, 1 (1999).
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Type-I Seesaw ???? Leptogenesis ??
M. Fukugita and T. Yanagida, Phys. Lett. B 174,
45 (1986) M.A. Luty, Phys. Rev. D 45, 455
(1992) R.N. Mohapatra and X. Zhang, Phys. Rev.
D 45, 2688 (1992).
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????
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W. Buchmuller, P. Di Bari, and M. Plumacher,
Nucl. Phys. B 665, 445 (2003) Annals. Phys.
315, 305 (2005).
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?????? ? ???
????? Dirac ?? ???
?----?Baryogenesis ???? ?----? Dark
Energy ??
?? Any connections?
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????????
??? ?
?????
???
??
Solution
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????
Bo Feng, Hong Li, Minzhe Li and
Xinmin Zhang Phys. Lett. B620(2005)27
??
???? in the future CMB polarization
experiments will be
Tested.
????
?baryogenesis
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Searching For CPT Violation With WMAP And
BOOMERANGastro-ph/0601095

• Bo Feng, Mingzhe Li, Jun-Qing Xia, Xuelei Chen,
  Xinmin ZhangVersion accepted by PRL
• We search for signatures of Lorentz and CPT
  violations in the cosmic microwave background
  (CMB) temperature and polarization anisotropies
  by using the WMAP and the 2003 flight of
  BOOMERANG (B03) data. We note that if the Lorentz
  and CPT symmetries are broken by a Chern-Simons
  term in the effective lagrangian, which couples
  the dual electromagnetic field strength tensor to
  an external four-vector, the polarization vectors
  of propagating CMB photons will get rotated.
  Using the WMAP data alone, one could put an
  interesting constraint on the size of such a
  term. Combined with the B03 data, we found that a
  nonzero rotation angle of the photons is mildly
  favored \Delta \alpha -6.04.0_-4.0
  3.9_-3.7 deg (1, 2 \sigma).

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Cosmology and collider physics

• Baryogenesis two Higgs models, left-right
  symmetric SUSY anomalous top,Higgs
  couplings------tested by LHC
• Dark matter Neutralino --------tested by LHC
• Dark energy inflation (scalar fields
  quintessence, quintom inflaton) Higgs tested at
  LHC

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Thanks !