constraining dark energy from large scale structures

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Constraining Constraining dark energ dark energ y y from large scale from large scale structures structures Yipeng Jing Shanghai Astronomical Observatory

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Constraining dark energy from large scale structures. Yipeng Jing Shanghai Astronomical Observatory. The “Hubble diagram” of Type Ia supernovae tells us that matter is not enough…. log( Distance d L ). a(t). Perlmutter et al. 1999, Riess et al. 1998. Redshift of spectral lines. - PowerPoint PPT Presentation

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Page 1: Constraining  dark energy  from large scale structures

Constraining Constraining dark energydark energy from from large scale structureslarge scale structures

Yipeng Jing

Shanghai Astronomical Observatory

Page 2: Constraining  dark energy  from large scale structures

Perlmutter et al. 1999, Riess et al. 1998

The “Hubble diagram” of Type Ia supernovae tells us that matter is not enough…

log(

Dis

tanc

e d L

)lo

g(D

ista

nce

d L)

dL (1 z)c dz'

H(z',m , )0

z

Redshift of spectral lines Redshift of spectral lines

H Ý a

a

a(t)

Luigi Guzzo

Page 3: Constraining  dark energy  from large scale structures

Cosmic ConcordanceCosmic Concordance

Large-Scale Structure/Clusters

•m =0.25-0.3

Cosmic Microwave Background

• Flat geometry (TOT=1)

• m ~0.25 > 0

Supernovae

Accelerating expansion

• ~ 1

Altogether (any two of them)

• m ~0.25 ~0.75

Page 4: Constraining  dark energy  from large scale structures

1990 Dec Nature, 348,20

Page 5: Constraining  dark energy  from large scale structures
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Matter (m)

Dark energy (

Today

Size=2 Size=4Size=1/2Size=1/4

If w=-1 and the cosmological constant corresponds to some sort of “quantum zero-point”, then its value today is a factor ~10120 too small, plus it is suspiciously fine-tuned: anthropic argument?

time

Fine-tuning and Cosmic Fine-tuning and Cosmic CoincidenceCoincidence

Fine-tuning and Cosmic Fine-tuning and Cosmic CoincidenceCoincidence

Thus could we have w = w(z) ? --> e.g. quintessence, a cosmic scalar field slowly rolling to the minimum of its potential (e.g. Wetterich 1988), inducing an evolving -1 < w(z) < -1/3. Or more complex interactions between DM and DE (e.g. Amendola 2000; Liddle et al. 2008; He et al.) ?

redshift

z=3 z=1

Page 7: Constraining  dark energy  from large scale structures

Observational Probes

• Supernovae M(z)

• Baryonic Acoustic Oscillations (BAO)

• Abundance of rich clusters

• Weak Lensing

• Redshift distortion

Page 8: Constraining  dark energy  from large scale structures

SNe Future experiments: JDEM, DES,

PanSTARRS,LSST

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BAO: SDSS/2dF, WiggleZ, FMOS, BOSS,Bigboss HETDEX, WFMOS,

PAU

Luminous Red Galaxies , LRG) two-point CF

. J. Eisenstein et al., Astrophys. J. 619, 178 (2005).

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But we need to look at both sides of the But we need to look at both sides of the story…story…

R 1

2g R

8G

c2 T

Add dark energyModify gravity theory [e.g. R f(R) ]

R 1

2g R

8G

c2 T g

“…the Force be with you”

Page 11: Constraining  dark energy  from large scale structures

So, the equation of state is not the end of the So, the equation of state is not the end of the story…story…

Cosmic acceleration can also be explained by modifying the theory of gravity [as e.g. in f(R) theories, Capozziello et al. 2005, or in multi-dimensional “braneworld” models, Dvali et al. (DGP) 2000].

The growth equation (and thus the growth rate) depends not only on the expansion history H(t) (and thus on w) but also on the gravitation theory (e.g. Lue et al. 2004)

which has a growing solution:

(x , t) ˆ (x )D(t)

Ý Ý 2H (t) Ý 4G

f d lnD

d lnafrom which we define a growth rate

How to distinguish between these two options, observationally?Growth of linear density fluctuations in the expanding Universe (in GR):

Page 12: Constraining  dark energy  from large scale structures

Observational Probes

• Supernovae M(z)

• Baryonic Acoustic Oscillations (BAO)

• Abundance of rich clusters

• Weak Lensing

• Redshift distortion

Page 13: Constraining  dark energy  from large scale structures

Clusters:SZA, SPT, DES, ACT, 400d, eROSITA

Page 14: Constraining  dark energy  from large scale structures

Weak Lensing: LSST, EUCLID, DES, PanSTARRS

1.1o1.1o simulated shear field by Hamana

()

(+)

Page 15: Constraining  dark energy  from large scale structures

Redshift distortion: Bigboss, Vipers, Euclid etc

Page 16: Constraining  dark energy  from large scale structures

4 个引力模型 : GR ,f(R) , DGP , TeVeS

张鹏杰等提出在宇宙学尺度上检验广义相对论与其

他引力论的新方法

Page 17: Constraining  dark energy  from large scale structures

通过通过 EEGG 方法,广义相对论方法,广义相对论在一亿光年尺度上得到了确认在一亿光年尺度上得到了确认

Reyes et al. (Nature,464, 256-258,11 March 2010) 应用我们的 EG 方法分析了 SDSS 星系巡天的数据。

右图即为其主要结果。测量到的一亿光年尺度上的 EG 与广义相对论的预言相符。

该结果基本排除了 TeVeS 修改引力,并有力限制对 f(R) 引力

Page 18: Constraining  dark energy  from large scale structures

We also consider the dependence on the information used: the full galaxy power spectrum P(k), P(k) marginalized over its shape, or just the Baryon Acoustic Oscillations (BAO). We find that the inclusion of growth rate information (extracted using redshift space distortion and galaxy clustering amplitude measurements) leads to a factor of 3 improvement in the FoM, assuming general relativity is not modified. This inclusion partially compensates for the loss of information when only the BAO are used to give geometrical constraints, rather than using the full P(k) as a standard ruler. We

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BigbossBigboss 简介简介 BigBOSS 项目是美国劳仑斯 - 伯克利实验室 / 国

家天文台发起的第四代暗能量巡天的国际合作项目(目前为第二代 ---- 第三代);已获 DOE预研经费、尚处立项阶段。

通过改造美国国家天文台的 4m 望远镜到直径 3度的视场 , 在焦面上放置 5000 根光纤开展光谱巡天 , 光谱覆盖范围从近红外到光学,分辨率为 5000 ;已经获准;

计划从 2015 年开始正式观测,在 6-10 年时间测量里,把暗能量状态方程的测量精度提高 1-2 个量级;

与其他第四代暗能量项目比较具有系统误差小、投资低、风险低的优点。

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BigbossBigboss 望远镜示意图望远镜示意图

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BigbossBigboss 主要科学指标主要科学指标

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我国参加我国参加 BigbossBigboss 的作用和意的作用和意义义

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特的小规模巡天;从观测能力和观测时间看,正好处在我国

的 LAMOST (三代, 2011 )和南极光学望远镜(五代, 2020 +)之间 。

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欢迎大家推动和参与BIGBOSS 项目,感谢大家的支持!