Foex. Pratt. Ferrari. Finoguenov Lanoux. Sartoris. Mazzotta. Bazin. Bourdin.
Colafrancesco Mohr ... Cosmo high-z. N u m b e r. New vision. New approach.
Multi-messenger. Multi-messenger .... Wave-plate polarimeters, FTS-SP.
Systematics.
Moriond Meeting 2010
… some personal conclusions
Sergio Colafrancesco ASI - ASDC Email: Email
[email protected] [email protected]
1
A few numbers … 90 talks 9 posters 45 hours of meeting + 50 min. 27 hours of: ski-gondolas-chairlift-skiliftskilessons-sunbaths-sauna-swimming … or simply email reading, or … Duty Cycle: … demanding ! wakeup
breakfast
talks
lunch
Night setup
Ski setup
bar
dinner
talks
ski
2
… a bit of statistics Moriond Talk Distribution 25
Number
20 15 10 5 0 CMB
Clusters
DM
Leahy Raeth Rozo Dickinson Bonvin Pratt Errard Shaw Finoguenov Kusaka Lewis Charlassier Hinshaw Sartoris Hernandez-M Shanks Bazin Colafrancesco Salatino Piat Democles Gubitosi Pajot Bunn Tristram Fromentau Pointecouteau Amblard Fauvet Lopez-Cruz Delabrouille Rossi Dafni Lanz Girardi
Mod-G
Foex Ferrari Lanoux Mazzotta Bourdin Mohr Borgani
DE
Cosmo sce.
Blanchard Dunlop Beelen Penin Delsart Battye Serra Gawiser Zaroubi Brentjens Peterson Mesinger
Zakharov Serra Serfass Bird Gerbier Nuss Chodorowski Cline Polesello Clerbaux Camera Strahler Viel Kainulainen Vieregg Thomas Desjacques
Santos Koshelev Tartari Kirilova Iliev Tigrak Finke Regos DiPorto Dufaux Badziak Clesse Vikman Caprini Popa Godlowski
Regnault Mortonson Palanque-Del. Sawicki Kronborg Thomas Gangler Taylor Marra Crighton Copeland Abate Garcia-Bellido Busca Pearson Abdalla Quartin Ziaeepour Fourmanoit Baldi Dokuchaev 3
… a bit of statistics 20 18
Number
16 14 12 10 8 6 4 2 0 CMB
CMB Pol SZE cl
X/O cl
NT cl
DM Direct
DM Mod-G Indirect
DE
Cosmo Cosmo Cosmo IR sce. high-z
4
… a bit of statistics Initial conditions
Largest bound structures
Dark Universe Obscure Gravity
Structure formation history
20 18
Number
16 14 12 10 8 6 4 2 0 CMB
CMB Pol SZE cl
X/O cl
NT cl
Multi-messenger New vision
DM Direct
DM Mod-G Indirect
DE
Multi-messenger New approach
Cosmo Cosmo Cosmo IR sce. high-z
Multi-messenger 5
… a bit of statistics Initial conditions 20 18
Number
16 14
Largest bound structures
Dark Universe Obscure Gravity
z~0
z→∞
Structure formation history
z~0
z >> 1
12 10 8 6 4 2 0 CMB
CMB Pol SZE cl
X/O cl
NT cl
Multi-messenger New vision
DM Direct
DM Mod-G Indirect
DE
Multi-messenger New approach
Cosmo Cosmo Cosmo IR sce. high-z
Multi-messenger 6
CMB Established framework COBE Boomerang WMAP PLANCK (… some surprise at the horizon?)
Look for more details Polarization Anomalies Non Gaussianity
7
1992: CMB Anisotropy
THE ASTROPHYSICAL JOURNAL, 396:L1-L5, 1992 “PRELIMINARY SEPARATION OF GALACTIC AND COSMIC MICROWAVE EMISSION…” BENNETT ET AL, THE ASTROPHYSICAL JOURNAL, 396:L1-L5, 1992 “INTERPRETATION OF THE COSMIC MICROWAVE BACKGROUND RADIATION ANISOTROPY…” WRIGHT ET AL, THE ASTROPHYSICAL JOURNAL, 396:L1-L5, 1992 “COBE DIFFERENTIAL MICROWAVE RADIOMETERS – PRELIMINARY SYSTEMATIC ERROR…” KOGUT ET AL, THE ASTROPHYSICAL JOURNAL, 401, 1-18, 1992
First detection of temperature fluctuations (anisotropy): sets the scale of the signal – brighter than the Galactic foreground!
8
1990’s: A Decade of Progress!
QMASK DASI
Boomerang Maxima
9 to name a few…
CMB: intensity WMAP-7yr 23 GHz
33 GHz
41 GHz
61 GHz
94 GHz 10
CMB: power spectrum The imprint of sound waves is visible in the co-added degree-scale hot & cold spots.
Best-fit flat ΛCDM model
The expected radial/tangential polarization pattern around these extrema is clearly seen in the 7-year WMAP data.
This pattern is also imprinted on the baryon gas (baryon acoustic oscillations or BAO) that evolves to form large scale structure.
11
ΛCDM Parameters* Blue curves/contours – 5-year data Grey curves/contours – 3-year data Biggest improvements in: Optical depth, τ Amplitude of fluctuations @ 8 Mpc, σ8 Matter densities, Ωbh2, Ωch2 Age: t0 = 13.69 ± 0.13 Gyr *based on WMAP data only
12
The next step Planck First Light!
13
Planck … expectations
14
Planck … expectations DE equation of state
DE equation of state: evolution
15
… but in the meantime
SPT 16
SPT Survey Field
17
CMB anisotropy @ small scales Astrophysics • point-like • extended sources
No evidence for SZ in power spectrum, nor for a clustered component of point sources! Need to analyses maps @ multi-ν to break degeneracies
mm spectroscopy
SAGACE MILLIMETRON
18
PMN J0419-3010
[ O 12 Blazars in WMAP (3 in Boomerang) ]
PKS 0405-385 PKS 0521-365 PKS 0422-380 PKS 0537-441
PKS 0438-436 PKS 0454-463 PKS 0513-491l
PKS 0539-543 PKS 0252-549
PKS 0549-575
PKS 0506-61
19
1RXS0531-3533 PKS 0548-317 PMN J0419-3010 PKS 0548-322 PKS 0435 -300 PKS 0534-340 PKS 0602-31 1RXS0608-3041 PKS 0439-331 PMN0510-3533 PKS 0610-316 PKS 0426-380
PKS 0613-312
PKS 0448-392 WGA 0428.2-3805
WGA 0624-3230
1RXS0432-3506 PKS 0443-387
PKS 0402-362
PMN J0525-3343 1RXS0606-3447 PKS 0618-37 1RXS0557-3728
PMNJ0529-3555 PKS 0532-378
PKS 0405-385 PMN 0422-3844
PKS 0558-396
PKS 0521-365
PKS 0422-380 1RXS0502-4221
1RXS0543-3956 WGA 0424-3849 PKS 0524-460
PKS 0427-435
PKS 0537-441
Pictor A
PKS 0622-441
PKS 0646-437 RGal PKS 0518-45
PKS 0438-436
PKS 0514-459 PKS 0355-483
PKS 0454-463
PKS 0257-51 PKS 0431-512 PKS 0446-519
PKS 0252-549
RXS J 0606-4730 PKS 0524-485 PKS 0513-491l
PKS 0558-504 WGA 0631-5404
PKS 0452-515
PKS 0539-543 PKS 0549-575 WGA 0533-5817
PKS 0506-61
Multi-frequency analysis
[ O 54 Blazars
with ∆T > 50 µK 20]
CMB: dig into the noise Astrophysical sources from sub-mm to IR
21
CMB: anisotropies of anisotropies Sources: • CMB lensing • Power asymmetries Powerful method to test for a wide class of • Anisotropic primordial power theoretical models anisotropic • Spatially-modulated primordial power & • Primordial B-field (causal) • Non-Gaussianity instrumental systematics - Point-like and extended sources - Source clustering effect Other sources: Interesting physical effects Systematics very large cosmological scales anisotropicon noise beam-effects … 22
CMB: anomalies Large-angle CMB anomalies don’t “prove” that Large-scale power anything nonstandard is going on, but may deficit provide hints of places to look for interesting phenomena on large scales. North-south asymmetry
Important to make predictions and choose statistics in advance for new data sets, to avoid a posteriori statistics. Need a data set that probes other perturbation modes on ultralarge scales: CMB Alignment ofpolarization multipoles structure / 21 cm tomography? (“axis ofLarge-scale evil”) Kamionkowski-Loeb remote quadrupole measurements? 23
CMB polarization WMAP-5yr
24
CMB polarization Scalar quadupole moment
Tensor quadrupole moment
Produced by adiabatic fluctuations at last scattering Large polarization: photons travel significant distance between scatterings (!) Only on causally-connected angular scales (< 1°) A bit smaller-scale than structure in total intensity Polarized brightness up to 10% of total intensity fluctuations Driven by very-large scale gravitational waves, generated at inflation. Tensor-to-scalar power ratio depends on inflationary energy scale: r ≈ (V1/4 / 3.3 × 1017 GeV)4
Nearly negligible on ‘causal’ scales, strongest @ ~2°
25
CMB polarization E-modes: Direct probe of last scattering surface Best constraint on early re-ionization (z ~ 10) Independent check on cosmological model fitted to Temperature data (Nearly) independent of temperature pattern: eventually reduces cosmic variance (needs better SNR) Gravitational lensing B-modes: Sensitive probe of mass distribution: σ8, mass vs light, tests of GR consistency. Primordial B-modes: “Holy Grail of Cosmology” Relic from inflationary epoch: t = 10-37 s, Fixes inflation energy scale: big clue to relevant physics Non-guassian B-modes sensitive test of defects
T
E B
Blens
Quantum effects in CMB: Planck-scale induced birefringence 26
Present & Future Dominated by BICEP at ℓ < 300, QUaD at higher ℓ Best limit: r < 0.72 (95%) (BICEP) 1 more year of BICEP, full year of QUIET data already taken. Expect modest improvement.
Several experimental and technological advances needed → r < 0.1 Space: 3
Ballon: 4
Ground-based: 12 27
Projects ongoing and planned Space Planck CMBPOL/EPIC BPOL
Balloon EBEX PILOT (Dust) SPIDER Boomerang II
Ground-based QUIET1 (40/90 GHz) C-BASS (5 GHz) QUIJOTE1 (10-18, 30 GHz) BICEP2 (150 GHz) GEM-P (5 GHz) ABS (145 GHz) POLARBear (150 GHz) QUIET2 (30/40/90) QUIJOTE2 (30) Keck Array (100/150/220) QUBIC 28
CMB polarization: challenges Sensitivity: 100 nK (E); 10 nK (B) Receivers: bolometers, TES, KIDs, Q-dots Detectors: bolometer arrays Polarimeter on chip Wave-plate polarimeters, FTS-SP Systematics Field description (matrix structure) Experimental artifacts
Signal extraction Polarization signal reconstruction Data analysis techniques 29
CMB polarization: challenges Polarization calibrators (bright, non-variable)
Astronomical “calibrators”
known to ~2° Use physical polarization reference
Intensity Wire-grid Calibrator
Polarization CenA 30
CMB polarization: challenges Foregrounds
• Few, sparse samples • Need larger, deeper catalogues • Large Π variability Cl , Blazar − pol (ν )
ν ∝ GHz Cl , Blazar − pol (1.4GHz ) 1.4
VLA calibrator MG+ Okudaira 93 Aller 92 Lister 01 Nartallo 98 2ζ
ζ = 0.5 ζ = 0.3 ζ = 0.2
31
Galaxy clusters
Planck SZ all sky survey
32
Clusters Clusters are excellent Cosmological probes X-rays Optical SZ
Not completely understood physics (excellent Astro-Particle Physics Labs.) Evolution Potential wells: DM vs. Mod G Atmosphere complexity • • • •
X-ray view and systematics O view and systematics SZ view and systematics GL view and systematics
New data: SZ (mm) needed, especially spectra & polarization X-ray: assesment (hopefully also polarization) O: refinement needed (galaxy population, AGN fraction, …) Radio: new data and not data re-analysis (B-field FR,…) 33
Clusters: cosmological probes Clusters are excellent Cosmo-evolu-meters
• Understand their physics (DM, baryons, Galaxy fedback, CRs, B) • Derive their total gravitational mass
M ~ ρb R3f
• Collect large, unbiased catalogues at various z
N(M,z)
34
Clusters @ X-ray
X-ray observations currently the most efficient and well-tested way to find clusters
LX ~ n2 T1/2 f(E, Z, T)
35
Clusters @ X-rays Non Cool-core
Cool-core Evidence for the presence of non-gravitational phenomena
36
Clusters: non-thermal phenomena AGN feedback CRs B field DM feedback
37
Clusters: non-thermal phenomena AGN feedback Perseus cluster (X,γ) • • • • •
Multi-T Cool Core AGN-dominated core Mini Radio halo Non-thermal plasma
(DM, CRs, WRs, BH,..)
RXJ1347-1145 cluster (µwave-mm) • Multi-T • AGN-dominated core • Non-thermal plasma
(DM, CRs, WRs, BH,..) 38
Clusters: non-thermal phenomena Perseus + NGC1275 1
Fermi-LAT MAGIC
2 3 up
WR Possibility to detect γ-rays from Perseus • in low-states of the central AGN • in the outer parts of the cluster
DM down
39
Clusters: non-thermal phenomena Cosmic Rays Radio halos: LOFAR, SKA X-ray: cavities (Chandra) SZE th+non-th: PLANCK, Millimetron, SAGACE HXRs ICS + Brem.: NuStar, Gamma-rays Brem+ICS+p0 decay: Fermi, CTA, … Origin • Acceleration: shocks, merging • In situ: hadrons + sceondary e+• Injection
Impact on cluster evolution to be determined 40
Clusters: non-thermal phenomena Cosmic Rays
Radio emission ν=37MHz EGev2Bµ
Cavities: hadronic CR support
Merging shocks MS0735.6+7421
RXJ1314.4-2515
A3667 41
Clusters: non-thermal phenomena Acceleration vs. merging Shock acceleration: relativistic covariant formulation
Turbulent acceleration
Power-law
teq ≈ t acc
Maxwellian
teq < < t acc
42
Clusters: non-thermal phenomena B field More and more evidence & constraints Simulations help to check ideas/models
Non-linear evolution in bound structures Origin: open question (primordial or post reconbination ?) • Approach 1: galaxy/AGN outflows + cavities + … • Approach 2: evolving from primordial B-field (10-100 G)
43
B-field in clusters: evidence Synchrotron radiation
Faraday Rotation
Radio Halos
Radio Relics
B ≈ 0.1 − 5µ G
B ≈ 0.2 − 8µ G
A2163
B ≈ 1− 50 µ G A400 3C275
A3667 44
B-field from early ages
Non-linear evolution coupling with DM & baryons
45
B-field in cosmic structures Observable effects X-rays:
scaling-law problem
SZE:
modifies signal power spectrum
Radio halo population
46
Clusters: M determination Mass proxy T, LX, YX, YSZ, RO, fgas: one? M-T
which is the best M-YX
Scatter: under control (!?); extremes due to cool cores & mergers Evolution: less known 47
Cluster mass determination: Lensing From shear to surface density (Kaiser-Squires, 1993): −2 * *
κ + iβ = ∂ ∂ ∂ (γ 1 + iγ 2 )
κ = 12 ∂ 2φ
κ/β (E/B) decomposition:
κ
κ
β
β 48
3-D Dark Matter Mass (φ) Maps 3-D density maps of HST-STAGES A901/2
φ = Ψ + Φ → ρ m
49
Clusters: redshifts z determination: Optical surveys z proxy The location of the red-sequence allows for robust redshift estimates.
50
Clusters: simulations Pearce et al. ‘06 L= 500 h-1 Mpc Ngas+NDM=109 εPl = 50 h-1kpc Non-radiative
QuickTim e™ and a decom pres s or are needed to s ee this picture.
Tornatore et al. ‘10 L= 75 h-1 Mpc Ngas=NDM=5123 εPl = 2.5 h-1kpc SF + SN + enrichment Dolag et al. ‘06 M ~ 2 1015 h-1 M Ngas=NDM~ 107 εPl = 2.5 h-1kpc SF + SN + enrichment 51
Clusters: simulations From single objects to representative parts of the Universe
160h-1Mpc
- Useful to calibrate clusters for cosmology - N-body simulations fail to reproduce inner cluster structure + other detailed features
64h-1Mpc
52
Cluster and cosmology: surveys RASS XMM-COSMOS XMM-LSS SXDF E-ROSITA WFXT … PLANCK SPT ACT SAGACE MILLIMETRON …
+
Optimal Selection Function
DES 53
Cluster & cosmological parameters SPT
DES
DES+SPT
Galaxy clusters probe the physics behind our accelerating universe in a way that is fundamentally different from geometrical probes (e.g. BAO or SN). 54
Clusters and DM Clusters are useful labs for indirect DM search
55
Dark Matter All evidence is astronomical Anomaly in 1933 up to 1970’s Accepted (needed) Anomaly up to today CMB Cosmology + LSS (3D-DM distributions from GL) Cluster + GL + galactic physics
Experimental frustration: anomalies: DAMA, Pamela, ATIC Data-theory tension: go for hidden DM
Big experimental effort: Undeground: direct search Ground: Indirect search: telescopes Above the ground: indirect search: satellites
A multi3 approach: m-freq. + m-mess. + m-exp. Huge data analysis and theoretical effort New directions to go !?
56
The Dark Matter Scenario: timeline
Particle Astro Particle Astronomy Physics PhysicsCosmology
2010
Missing mass Dynamics
Rotation curves
N-body simulations 1977 Thermal relics (Lee & Weinberg)
Lensing
CMB
Today
1984 Indirect DM search idea !? & Srednicki) ν - mass (SIlk Beyond the SM theo. & exp. SUSY 1985 DirectSUSY DM experiments AXION (Goodman & Witten) Sterile ν
2 ∆m ν 57
Hunt for the DM particle DM exists: we feel its (gravitational) presence DM is mostly non-baryonic: we must think of a specific search strategy DM is very elusive: we must consider un-ambiguous evidence
Crucial Probes are required ! 58
Dark Matter probes Under-ground
On-the-ground
Above-the-ground 59
The latest results: CDMS II 2 events in the observed signal region. Based on background estimate, the probability of observing two or more background events is ~23%.
Many direct detection experiment in the (next) future
Ahmed et al. arXiv:0912.3592v1
60
DM - Astrophysical probes INFERENCE
PHYSICAL
+
+
Virial Theorem Hydro Equilibrium Gravitational lensing
Decay
Annihilation
X+ X→ π
0, ±
X → xi + γ
, p,...
X + X → e ± , µ ± ,τ ± ,ν
i 61
DM - Astrophysical search INFERENCE
PHYSICAL
L A CI
NO
C T
U R
+C U R
L A I
C
Vulnerable against: Virial Theorem MOND: Modified Newtonian Dynamics Annihilation Decay Testable against: TeVeS Tensor-Vector-Scalar Hydro :Equilibrium X → xi + γ X + X → π 0, ± , p,... Electromagnetic signals Ordinary matter feels a transformed metric Gravitational lensing X + X → e ± , µ ± ,τ ± ,ν i
62 DM illuminates thru its interaction
DM - Astrophysical search Clean and unbiased location in the sky Best Astrophysical Laboratories
NO
YES
Clear and specific SED in the e.m. spectrum Most specific e.m. signals 63
Multi-wavelength
Multi-messenger
Multi-experiments 64
The Galactic Center
Multi-ν
Galactic center region across the spectrum: red: radio 90 cm (VLA); green: mid-infrared; blue: X-ray (1-8 keV; Chandra ACIS-I) 65
The Galactic Center: a close up
Galactic Center (Survey) Multiwavelength Close-Up A multiwavelength close-up of the recent massive star-forming region near the Galactic center. The color image, plotted also in standard Galactic coordinates, is a composite of 20-cm radio continuum (red); 25-µm mid-infrared (green); and 6.4-keV line emission (blue).
66
Galactic Center demography Crowded, active environment HESS Fermi (1GeV) EGRET source Central Black Hole
X-ray source
SNR
Sgr A East non-thermal filaments (radio) 67
The DM challenge: Fermi GC Cont.
GC line
No evidence of DM signals in Fermi (11 months) data
DSph.G.
Clusters 68
The GC region DM challenge: limits Stronger constraints from radio + γ-rays • Radio: constrain to ~ GeV-TeV mass • γ-rays: constrain to ≤ GeV mass • ν’s : constrain to > 10 TeV mass
Borriello et al. 2008
Radio + EGRET
[Crocker et al. 2010] Radio + HESS
[Regis & Ullio 2008] 69
Pamela and ATIC Charge-dependent solar modulation important below 5-10 GeV
Rapid climb above 10 GeV indicates the presence of a
primary source of cosmic ray positrons!
Pamela
Astrophysical expectation (secondary production)
ATIC
70
Are these signal from DM? ￭ Shape consistent with some generic Dark Matter candidates but with: Very hard spectrum large fraction of annihilation to e+e-, µ+µ- or τ+τ￭ Flux is a factor of 100-1000 too big for a thermal relic; → requires dramatic enhancement Astrophysics
KK dark matter with m ~ 600 GeV
ATIC (2008)
- More small-scale structure than expected (“boost factor” of ~1000) - A narrow diffusion region - A large nearby clump of dark matter
Cheng, Feng, Matchev (2002) 71
Are these signal from DM? ￭ Shape consistent with some generic Dark Matter candidates but with: Very hard spectrum large fraction of annihilation to e+e-, µ+µ- or τ+τ￭ Flux is a factor of 100-1000 too big for a thermal relic; → requires dramatic enhancement Astrophysics Particle physics - non-perturbative effects as the “Sommerfeld Enhancement” important for mφ
