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CMB 偏光観測と重力波. 服部誠 (東北大学・理・天文). 晴れ上がり期を見通して宇宙創成期を直接観る. 素粒子論. 時間. 4つの力. 137 億年(現在). 加速器. エネルギー(ギガ電子ボルト). 宇宙マイクロ波 背景放射( CMB ). 38 万年 晴れ上がり. 10 4. ?秒. ビッグバン. インフラトン?. 原始重力波?. インフレー ション期: 加速度膨張. 10 16 ?. 10 - 36 秒?. 原始重力波検出. CMB. DECIGO. correlated. 宇宙空間を漂う重力波 =空間の振動. - PowerPoint PPT Presentation
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SIRPOL B
CMB
13710-36 CMB381016104123
CMBDECIGOcorrelated
xy
xy
7CMBCMBLast scattering surface2008/2/20
13710-36 3878Stokes parameters
=0 ,=/2 xy xy
8(V=0)EB
xy
Xz
E
BX
EB
CMB xyXxx
E
EB(X xyE
xyBCMBB
EB
Primordial B
Scalor-tensor ratio r: E_i energy scale of the inflation epoch
Inflationary consistency relation: n_grav power spectrum index of the primordial gravitational waves 14
Pagano-Cooray-Melchiorri-Kamionkowski 2007WMAP5yrs+BAO +SDSSBB15
B-mode: r ~ 0.001 (statistical + instrumental) Figure byYuji ChinoneReionization bumpHorizon size at Simulated Primordial B mode all sky mapby Yuji Chinone
17
Planck18
However, for B-mode, r ~ 0.1 (no big improvement expected)
E-modeup tol ~ 1000Funded CMB Polarization Experiments((near) completed: Bicep1, Boomerang, CBI, DASI, Maxipol, QUaD, WMAP, VSA) NameType/locationInstitutionsNEQ(mKs)Ell rangeFrequencies
#Detectors
Resolution
PlanckBolo-HEMT/SpaceESA, IAS-Orsay, Bologna + many80(@100G)2-200025-100022H+32B(# of pol. ch)8SpiderBolo/BalloonCIT/JPL,CITA, CWRU,Stanford4/3 (@96/145G)2-25040,90,150,220~200040BICEP2Bolo/South PoleCIT/JPL,CITA,Stanford
10-25015051240CloverBolo/ChileCardiff, Oxford, Cambridge, Manchester12(@90G)20-100090,150,225200-40010QUIETHEMT/ChileChicago, CIT, JPL, KEK, Manchester, Miami, MPI, Oxford, Princeton, Stanford12/9 (@40/90G)20-100040,90119x21000x2(P2)10EBEXBolo/BalloonMinn, Berkeley, Brown, Cardiff, Columbia, McGill +85 (@150G)20-1200150,250,42014068PolarBeaRBolo/ChileBerkeley,APC, Cardiff,Colorado, Imperial, KEK, McGill,UCSD10(@150G)20-300090,150,22012743.5SPTPOLBolo/South PoleChicago,Berkeley, Colorado, CWRU, Davis, JPL, McGill,SAO1420-1000090,150,201000-20001.1(Proposed: ACT-POL, SPUD)compiled by Adrian Lee + MHEveryone except Planck claims r=O(0.01) sensitivity and results in 5 yrs.19B20
B-mode: r ~ 0.001 (statistical + instrumental) Figure byYuji ChinoneReionization bumpHorizon size at
WCMBCMB B
CMB:12
A4QUIETCMB
2122
Verde-Peiris-Jimenez 2005QUIET+PolarBearPOLARBeaRCMB
COBE/FIRAS
COBE/DIRBEIRASSchlegel etal. (1998)
Schlegel etal.(1998)PLANCK
Planck26
Provide Unique data for dust components separation
E-modeup tol ~ 1000Goal for future CMB satellite27
LiteBIRD (+Lite (light) Satellite for the studies of B-mode polarization andInflation from cosmic background Radiation DetectionLeader: M.Hazumi (KEK) Small is beautiful ! JAXACryostatEPIC1/3The entire satellite will be in a big cryochamber for testing.
28
20089WGPlanckQUIET+PolarBeaRCMB29
LiteBIRDPlanckQUIET+PolarBeaRBLiteBIRDQUIET+PolarBearPlanck(LiteBIRD)30Foreground removal31
Delensing r=T/S=0.01r=0.001Planckr=0.001 Primordial CMB B mode polarization B
Heiles 9286P0.03-0.4%FWHM=9.2Gaussian windowWMAP
WMAPK
-11Zlogarithmic spiral arm1Anomalous emission
V
0.05%1.5%Archeops143, 217, 343, 545GHzCatalogue Magnitude Full Sky > 24 > 24|b| > 10GGSS 9 < V < 10 216 178 146GGSS 10 < V < 11 2039 1457 1121Tycho 9 < V < 10 61871 36880 28977Tycho 10 < V < 11 141065 82509 625411*QUIET 15
37
2008/02/05 38Input data
30 GHz44 GHz100 GHz70 GHzNoise: 10KNumber of data 200000Number of parameter150000CMB382008/02/05 39
392008/02/05 40Combined Prior
MAPDIFCMBAINDEX4041
Basic: only spectral index prior was used41Histogram2008/02/05 42
123Cl Posterior [combined prior]Our template free methods works at least up to l=50 42