粒子宇宙学简介

Probing Dark Energy with Supernovae : a concordant or a convergent model?
J.-M. Virey, A. Ealet, C. Tao, A. Tilquin, A. Bonissent, D. Fouchez, P. Taxil,astro-ph/0407452
Q
Q V (Q )


1 2
Q
2
V
, p

1 2
Q
2
V
1 wQ 1
Q
2
V
→
wQ
1
检验：
A. w Q 0
ห้องสมุดไป่ตู้
状态方程的参数化：
1 .w ( z ) w 0 w1 z 2 . w ( z ) w 0 w a z /( 1 z )
* Within 2 σ, the cosmological constant fits well the data
ASg and ARGO： (High Duty cycle,Large
F.O.V)
~100GeV
中意合作 ARGO 实验RPC大厅
~TeV
中日合作 AS γ 实验区闪烁体探测器阵列
ARGO hall, floored by RPC. Half installed.
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.
( 2 10
3
eV )
4
w p / 1
m ~ 10
-3
eV
但是：
th
/
ob
~ 10
3
1 20
宇宙学常数问题！
3
为什么w=-1?
d ( a ) pda
const
w -1
物理？
Fine Tuning
2，动力学场(Quintessence)
L 1 2

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)
Authors:
Constraints on dark energy with SN Ia (Riess) + SDSS + WMAP-1
w w 0 w 1 * z /( 1 z )
最佳拟合值: W0=-1.30 W1=1.25
Observing dark energy dynamics with supernova, microwave background and galaxy clustering
为解决强CP破坏问题而引进 (Peccei & Quinn)

g 32
2 s

~a a G
a
(
10
9
?)
轴子: 标量粒子
m
a
2 QCD
~
~ 10
3
eV
f PQ
探测:
至今未发现
Cosmic rays from the halo of the MW— Baltz et al. 2002 some weak hints on DM

中微子与暗物质
I.
中微子是暗物质粒子
II. 热暗物质不起主导作用
Application showcase: neutrino mass
neutrino mass and abundance:
O. Elgaroy et al (2dFGRS) PRL 89, 061301 (2002)
hot dark matter suppress
暗物质粒子最佳候选者： 轴子(Axion) 中性伴随子（Neutralino）
近年，较多研究“温暗物质”： Interacting Dark Matter Non-thermal produced Neutralino Steril Neutrino Gravitino Quintessino
轴子(Axion)

利用 SN Ia 数据限模型
Astro-ph/0510447
Feng, Wang & Zhang Astro-ph/0404224 Huterer & Cooray Astro-ph/0404062
* Within 2 σ, the cosmological constant fits well the data * Data mildly favors a running of the W across -1
Jun-Qing Xia, Gong-Bo Zhao, Bo Feng, Hong Li and Xinmin Zhang Phys.Rev.D73, 063521, 2006
Global fitting with SN Ia, galaxy clustering and WMAP3
Feng, Wang & Zhang Astro-ph/0404224
注意：1， 真空能：
w=-1
2， Quintessence: -1≤w≤1
3， Phantom: -1≥w
4,
Quintom: w transit from below –1 to above -1
astro-ph/0407259, Steen Hannestad, Edvard Mortsell
Important: 精确宇宙学时代
问题:
•什么是暗物质？
•暗能量的物理本质是什么？
•为什么没有反物质？
需要新物理
暗物质：中微子是暗物质，但不是冷暗 物质；什么是冷暗物质？ 暗能量：势能和真空能是暗能量，但理 论预言太大－宇宙学常数问题？ 反物质：标准模型可以产生正反物质不 对称，但太小，需要新物理？ Inflation：什么是inflaton？
Weighing neutrinos in the presence of a running primordial spectral index
astro-ph/0605742

Bo Feng, Jun-Qing Xia, Jun'ichi Yokoyama, Xinmin Zhang, Gong-Bo Zhao The 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 < 0.76 eV (2 \sigma), compared with the case where power-law prior is adopted to the primordial spectral shape.
power at small scale
current cosmological bound: (95% CL) m<1.7/3 eV (weak prior) m <0.6/3 eV (strong prior) vs. tritium decay: me < 2.2 eV
hep-ph/0503257
粒子宇宙学简介
中科院高能所 张新民
2006.6.5
物质基本结构
• 三代夸克和轻子
(粒子物理)
• 规范相互作用: SU(3) ×SU(2) ×U(1)
C L
Y
• Higgs 粒子仍未发现
真空自发破缺机制???
WMAP:
The Biggest Surprise Nothing Particular Surprising Inflation DE ( 73 %) DM ( 23 %) B ( 4 %)
暗能量
实验证据： 基本特征：
a /a 4 G 3 ( 3 p)
a 0
3p 0
w p / 1 / 3
注意：辐射 w=1/3,
物质 w=0
暗能量的候选者：
1，真空能（宇宙学常数）
T 8 G g

p
8 G
* Data mildly favors a running of the W across -1
Constraints on EOS from SN Ia

暗能量参数化： I. 一个常数 w II. 动力学参数化 a.
w w 0 w1 z
b. w w 0 w 1 z /( 1 z )