Dark Matter、Dark Energy
and Baryo/Leptogenesis
Xinmin Zhang
Institute of high energy physics
Chinese Academy of Sciences, Beijing
Talk given at the 1st IAS-CERN Workshop
on Particle Physics and Cosmology
NanYang Technological University
25-27 March, 2013
One of the Biggest Achievements
in Physics and Astronomy
for the past 10 years=
Precision Cosmology
* Helpful to the Nobel Prizes in 2011 and 2006
* Important questions:
Dark Matter Particles? (Axion、WIMPs…)
Nature of Dark Energy ? (Cosmological constant, Dynamical fields )
Mechanism of Baryogenesis ? (Electroweak baryogenesis, Leptogenesis,
Quintessential Baryo/leptogenesis with CPT violation …)
Dynamics、Models of Inflation ?
(WMAP9 claims scale invariant spectrum ruled out at 5 sigma,
Planck new results )
Singularity of the Big-Bang cosmology (Ekpyrotic Model,
Quintom bounce ….)
……..
Outline of the Talk (I)
1) Current status on cosmological parameters:
*WMAP9 results: H-Z spectrum ruled out at 5 sigma
*Constraints on scalar spectrum Index from Latest
Observational measurements, arXiv:1303.3428
Hong Li, Junqing Xia and Xinmin Zhang
* Planck results:
2) WIMP Dark Matter:
Thermal WIMP --- cold dark matter
Non-thermal WIMP -- cold or warm dark matter
* “Gamma-rays from warm WIMP dark matter annihilation” Qiang Yuan et al, PRD (2012)
* “CosRayMC: a global fitting method in studying the properties
Of the new sources of cosmic e+- excesses” Jie Liu et al, PRD (2012)
current status on the WIMP detection
direct detection
indirect detection
AMS results ( see talk by Shih-Chang Lee)
Outline of the Talk (II)
3) Dark Energy
Very brief review on models
Current constraints on EoS (WMAP, Planck results)
* “Examining the evidence for dynamical dark energy”
Gongbo Zhao et al , PRL (2012)
4) Baryo/Leptogenesis
Electroweak baryogenesis in effective theory （Xinmin Zhang et al)
Leptogenesis ( see talk by Petkov)
Baryo/leptogenesis with cosmological CPT violation
CPT test with CMB polarization
Junqing Xia et al
WMAP9 new result
5) Summary
Final WMAP 9-year DataBennett et al. (2012)
• Wilkinson Microwave
Anisotropy Probe
(WMAP) group has
released the final 9year CMB data last
year.
Constraints on ΛCDM
Hinshaw et al. (2012)
• Combining the WMAP9, BAO, small-scale
CMB data and the prior on H0, the current
data give tight constraints on cosmological
parameters.
Spectral Index ns
Hinshaw et al. (2012)
• The current data strongly disfavor a pure HarrisonZel'dovich (HZ) spectrum at about 5 sigma C.L., even if
tensor modes are allowed in the model fits.
Degeneracy: ns & Neff
Li et al. (2013)
• Due to the strong degeneracy between ns and
Neff, the constraint on ns becomes weak. The
HZ spectrum now is consistent with the current
data at 2 sigma confidence level.
Spectral Index (Planck paper)
• The HZ spectrum is ruled out by the Planck data at
~8 sigma even if the tensor mode is included.
Including Neff (Planck paper)
• When Neff is free, the error bar of ns becomes
larger
Hinshaw et al. (2012)
Other Constraints (WMAP9)
• The 2sigma upper limit of total neutrino mass:
• The number of Neutrino species, Neff:
• The curvature of the Universe, Ωk:
• The primordial Non-Gaussianity, fNL:
Other Constraints (Planck paper)
WIMP Dark Matter
Why WIMPs？
？
i) Well motivated in particle
physics (SUSY…)
ii) Weak Interaction (detectable)
iii)Thermal WIMP miracle
Why thermal production?
relic photon, hot Big-Bang
Non-thermal Processes
Topological defects (cosmic string) decays
Reheating
Heavy particles decays
Free neutron decay in BBN
==
non-thermal WIMP miracle ( G. Kane et al )
Difficulties with thermal WIMPs
1）
）Strong constraints on the model parameters
2) Cross section too small to account for the anomalous data
observed by Pamela, ATIC, Fermi, HESS, AMS ……
• Non-thermal production of neutralino cold dark matter from
cosmic string decays
R. Jeannerot, (ICTP, Trieste) , X. Zhang, (CCAST World Lab, Beijing & Beijing, Inst. High Energy
Phys. & ICTP, Trieste) , Robert H. Brandenberger, (Brown U.) .
BROWN-HET-1160, IC-98-236, Jan 1999. 4pp.
Published in JHEP 9912:003,1999.
e-Print: hep-ph/9901357
•
Nonthermal production of WIMPs and the subgalactic structure of the universe
W.B. Lin, (Beijing, Inst. High Energy Phys.) , D.H. Huang, (Peking U. & Beijing, Inst. High Energy
Phys.) , X. Zhang, (Beijing, Inst. High Energy Phys.) , Robert H. Brandenberger, (Brown U.) .
Sep 2000. 6pp.
Published in Phys.Rev.Lett.86:954,2001.
e-Print: astro-ph/0009003
There is increasing evidence that conventional cold dark matter
(CDM) models lead to conflicts between observations and numerical
simulations of dark matter halos on sub-galactic scales. Spergel and
Steinhardt showed that if the CDM is strongly self-interacting, then the
conflicts disappear. However, the assumption of strong self-interaction
would rule out the favored candidates for CDM, namely weakly interacting
massive particles (WIMPs), such as the neutralino. In this paper we propose
a mechanism of non-thermal production of WIMPs and study its implications
on the power spectrum. We find that the non-vanishing velocity of the WIMPs
suppresses the power spectrum on small scales compared to what it obtained in the conventional CDM model. Our results
show that, in this context, WIMPs as candidates for dark matter can work well both on large scales and on sub-galactic
scales.
=======〉Warm WIMPs model
张新民SUSY04大会报告
大会报告
张新民
Thermal WIMPs
Non-thermal WIMPs
1
i) Distribution: :
ii) Model parameter space
a)Enlarging the parameter space;
constrained by relic density b)Explaining the Boost factor
required for Pamela ….
iii) Cold dark matter
Cold or Warm dark matter
X. Zhang et al
JHEP 9912:003,1999.
arXiv: hep-ph/9901357
Phys.Rev.Lett.86:954,2001.
arXiv: astro-ph/0009003
Phys Rev. D (2012)
Constraint on the spin-independent interaction
(来自
来自XENON100
共225天的观测
天的观测，
来自
天的观测，
排除DAMA和
和CoGeNT的信号区间
的信号区间)
排除
的信号区间
来自XENON100观测
观测225天最新的
天最新的spin-dependent的限制
的限制
来自
观测
天最新的
限制与中子的耦合
限制与质子的耦合
PAMELA Results （Positron Excess）
The total electron+positron spectrum
ATIC bump
Chang et al. Nature456, 362 2008
Fermi excess
Phys.Rev.Lett.102:181101,2009
Leptonic dark matter annihilation/decay
Liu, YQ, et al., 2011,
arXiv:1106.3882
Negative pressure: Brief Introduction to Dark Energy
a&& / a = −
4π G
(ρ + 3 p)
3
a&& > 0 → ρ + 3 p < 0 w = p / ρ < −1 / 3
* Smoothly distributed, (almost ) not clustering
Candidates:
I Cosmological constant (or vacuum Energy)
T
=
µν
Λ
8π G
g
ρ = − p =
µν
Λ
8π G
th
/ ρ
ob
~ 10
eV ) 4
↓
w = p / ρ = −1
ρ
−3
≈ ( 2 × 10
m
ν
~ 10
-3
Neutrino
eV Dark Energy?!
cosmological constant problem!
120
II Dynamical Field: Quintessence, Phantom, Quintom….
L =
1
∂ µ Q ∂ µ Q − V (Q )
2
ρ
Q
=
1 &
Q
2
2
+ V , pQ =
− 1 ≤ wQ ≤ 1
1 &
Q
2
2
− V
Equation of state w=p/ρ: characterize the properties of the dark energy models
* Vacuum :
* Quintessence:
* Phantom:
* Quintom:
w=-1
w ≥ −1
w<-1
w across -1
Important determining the equation of state
of dark energy with cosmological observations
I) Parameterization of equation of state:
(very much like S.T.U parameters for the particle
physics precision measurements)
A)
w=w_0+w_1 z / (1+z) (used mostly in the literature)
For Example: BOSS results in 2012
Gongbo Zhao et al, arXiv:1211.3741
B) Model independent method { w_1…w_i…}
Cosmological
Parameters:
II) Global analysis with
II)
astronomical
observational data:
SN (Union2.1, SNLS3)
LSS (SDSS),
CMB(WMAP9, …)
And code used
CAMB/CosmoMC
However, difficulty with the dark energy perturbation
when w across -1 ========== divergent
(like the infinity in massive W, Z
boson model)
1 + w → 0, w& ≠ 0 ⇒ δ&,θ&, δ ,θ → ∞
Perturbation with Quintom dark energy
(introducing an extra degree of freedom
like the Higgs ….)
Here δ and θ are the density perturbation and the divergence of the
fluid velocity respectively
Perturbation of DE is continuous during crossing!
Feng, Wang, Zhang, Phys. Lett. B607, 35 (2005)
Zhao et.al., Phys.Rev.D 72,123515, (2005)
Y. Cai et. al., Phys Rept. 493:1-60, (2010)
similarly, Fang, Hu, Lewis, Phys.Rev. D78, 087303 (2008)
Constraints on dark energy with SN Ia + SDSS + WMAP-1
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
Current status in determining the EoS of dark energy
G. Zhao and X. Zhang
Phys.Rev.D81:043518,2010
WMAP7 E. Komatsu et al. SNLS3，
SNLS3，
e-Print: arXiv:1001.4538
e-Print: arXiv:1104.1444
Results:
1) Current data has constrained
a lot of the theoretical models;
2) Cosmological constant is
consistent with the data;
G. Zhao,
Zhao, H. Li,
Li, E. Linder,
Linder,
K. Koyama,
Koyama, D. Bacon,
Bacon, XZhang
arXiV:: 1109.1846 Sep
arXiV
2011
with WMAP7+Union2.1+BAO+…
3）dynamical models are not
ruled out; quintom scenario
mildly favored；
favored；
WMAP9
Li et al. (2013)
Planck
2.5 sigma for dynamical dark energy with w crossing -1
the Quintom scenario !
More on Quintom Cosmology
for a review, see:
“Quintom cosmology: theoretical implications and observations”
Cai et al, Phys Rept. 439 (2110) 1-60
Quintom scenario:
w crosses over w=-1 during the evolution
Why interested these years?
1)Challenges to the model buildings
theoretically interesting!
(no-go theorem)
and data favoring
2) Quintom bouncing cosmology
standard cosmology-singular
quintom cosmology-non-singular
NO-GO Theorem
• For theory of dark energy in the 4D Friedmann-RoberstonWalker universe described by a single perfect fluid(1) or a
single scalar field with a lagrangian of
(2), which
minimally (3) couples to Einstein Gravity (4), its equation of
state cannot cross over the cosmological constant boundary.
Feng, Wang & Zhang, Phys. Lett. B 607:35, 2005, astro-ph/0404224 ;
Vikman, Phys. Rev. D 71:023515, 2005, astro-ph/0407107 ;
Waye Hu， Phys. Rev. D 71:047301, 2005;
Caldwell & Doran, Phys. Rev. D 72:043527, 2005;
Zhao, Xia, Li, Feng & Zhang, Phys. Rev. D 72:123515, 2005;
Kunz & Sapone, Phys. Rev. D 74:123503, 2006;
……
Xia, Cai, Qiu, Zhao, & Zhang, Int.J.Mod.Phys.D17:1229,2008
To realize Quintom, one of the conditions should be violated
Ekpyrotic Model
The collision of two M branes in 5D gives rise to a nonsingular cyclic
universe, and the description of effective field theory in 4D is
1 DE domination
2 decelerated expansion
3 turn around
4 ekpyrotic contracting phase
5 before big crunch
6 a singular bounce in 4D
???
7 after big bang
8 radiation domination
9 matter domination
Quintom Bounce
The expanding of the universe is transited from a contracting
phase; during the transition the scale factor of the universe a is at
its minimum but non-vanishing, thus the singularity problem can be
avoided.
20
Contracting
phase：
H < 0；
Expanding
Phase:
H > 0.
18
16
14
At the bouncing point:
H =0
Around it:
•
H > 0.
•
H = − 4π G ( ρ + p ) ⇒ w < − 1
Transition to the observable universe w > −1.
(radiation dominant, matter dominant,…)
So w needs to cross -1, and Quintom
matter is required！
12
a108
6
4
2
a=1
0
-10 -8
-6
-4
-2
0
2
4
6
8
t
Yifu Cai et al., JCAP 0803:013(2008).
Yifu Cai et al., JHEP 0710:071(2007).
10
Oscillating universe with Quintom matter
Xiong et al., arXiv:0805.0413
Solution:
Matter Antimatter Asymmetry
and New Physics
1) Our universe is matter antimatter asymmetric
2）
）Initial condition?
In the framework of inflation, all of the matter created during or after
reheating processes
dynamical generation of baryon number
asymmetry
3）
）Dynamical generated =
Baryogenesis
i) Electroweak baryogenesis Generating matter asymmetry at the
TeV scale =
new physics tested by LHC
ii) Leptogenesis =
Neutrino physics (see talk by Petkov)
iii) (Dark energy + Baryogenesis)
Quintessential Electro/Leptogenesis
====
CMB polarization
Baryogenesis
by Andrei Sakharov （1967)
i) B violation
ii) C and CP violation
iii)Out of thermo-equilibrium (CPT conserved)
Freezing out of the heavy particles
If CPT is broken, can be generated in thermo-equilibrium
Electroweak baryogenesis
i) B violation ----anomaly, non-trivial vacuum, sphaleron
ii) C and CP violation -----CKM mechanism
(however, too small-new physics)
iii) First order phase transition
Need Higgs mass
< 35 GeV!
Need
New physics
Electroweak Baryogenesis
and TeV scale Physics
i) New Physics Models:
2- Higgs，SUSY ……
L-R model (Mohapatra and Zhang, 1992)
ii) Effective Lagrangian Method
Xinmin Zhang, Phys. Rev. D47, (1993)3065
Bing-Lin Young and Xinmin Zhang, PRD49 (1994) 563
Anomalous couplings from higher dimensional operators
esspecially for Higgs and top quark
i
Operator relevant to Higgs mass limit
Effective potential:
potential:
Xinmin Zhang PRD47,
3065 (1993)
Cedric Delaunay,
Delaunay,
Christophe Grojean
Grojean,,
James D. Wells
JHEP 0804:029,2008
Operator relevant to baryon number generation
(top quark, large Yukawa coupling, interacts with bubble wall
strongly, plays essential role for baryon number generation)
===
===
=====
=====
Anomalous toptop-Higgs
couplings::
couplings
X. Zhang et al,
PRD 50, 7042
(1994)
Lars Fromme
Fromme,,
Stephan J. Huber,
Huber,
JHEP 0703:049,2007
Interacting Dark Energy
----non-gravitational method
• Coupling constant vary：
QFµν F µν
• Mass varying neutrino：P.Gu, X.Wang and X.Zhang PRD68,
ρ = − p =
Λ
8π G
Qν ν
−3
≈ ( 2 × 10
eV ) 4
↓
m
ν
~ 10
-3
eV
087301 (2003)
Rob Fardon, Ann E. Nelson, Neal Weiner JCAP 2004.
G.Dvali, Nature
432:567-568,2004
• Quintessential Baryo/Leptogenesis，
Baryo/Leptogenesis
反常方程
M.Li, X.Wang，
，
B.Feng, X.Zhang,
PRD65,103511(2002)；
；
B. Feng, H. Li, M. Li and XZ,
PLB602, 27 (2005)
CMB Pol
B.Feng ,et.al
PRL.96:221302,2006.
Quintessential Baryo/Leptogenesis
M.Li, X.Wang, B.Feng, X. Zhang PRD65,103511 (2002)
De Felice, Nasri, Trodden, PRD67:043509(2003)
M.Li & X. Zhang, PLB573,20 (2003)
Lint = c
∂ µQ
M
J Bµ
In thermo equilibrium⇒
⇒
Cohen & Kaplan
1/ 2
gb ∞
2
2
1
n B =  b − n b =
E
(
E
−
m
)
dE
×
[
1 + exp[( E − µ b ) / T ] −
2 ∫m
2π
µb 3
g bT 3 µ b
g b Q& T 2
=
[
+ O( ) ] ≈ c
6
T
T
6M
2π 2
s≈
g ∗T
45
3
1
1 + exp[( E + µ b ) / T ]
15 c g b Q&
η = nB / s ≈
4 π 2 g ∗ MT
depends on the model of Quintessence
Cosmological CPT violation!
]
Leptogenesis
Anomaly for CMB
Cosmological CPT violation: predicting <TB> and <EB>
∂µQ → ∂ µ f (R)
Hong Li et al
Bo Feng, Hong Li, Mingzhe Li and Xinmin Zhang
Phys. Lett. B 620, 27 (2005);
Bo Feng, Mingzhe Li , Jun-Qing Xia, Xuelei Chen and Xinmin Zhang
Phys. Rev. Lett. 96, 221302 (2006)
Current status on the
measurements of the
rotation angle
===
===
WMAP9
PLANCK : σ = 0.057 deg
（Xia et al ）
Interacting DE, Cosmological CPT violation
Baryo/Leptogenesis and CMB test
Baryo/Leptogenesis
Anomaly
Equation
CMB polarization and CPT test
Features:
1) Derivative couplings: no long range force limit;
No large radiative correction
2) Cosmological CPT violation:
Many speculation theoretically on CPT violation:
Evidence: expanding universe, matter-antimatter asymmetry
strength ~ O( H ), unobservable in the laborary experiments
CMB: travelling around O(1/H),
so accumulated effect ~ O(1) observable !
Summary
1) Strong motivations for new physics
beyond standard model from cosmology
2) Dark matter: (cold and warm WIMPs…)
Dark energy:
Cosmological constant still consistent with data
Quintom scenario favored at 2.5 sigma
Baryogenesis:
=== new physics
Leptogenesis -Neutrino physics
Electroweak scale --New particles
- Anomalous Higgs and top couplings
detected at LHC and LC……
Baryo/leptogenesis with cosmological CPT violation
==need Colliders and Astronomical Observations together!!!
Thank You !