Fundamental Physics in the Planck era

Transcription

1 Fundamental Physics in the Planck era Nazzareno Mandolesi INAF/IASF Bologna Planck LFI PI On behalf of the Planck collaboration J. Tauber: Bogotá, 6 Aug.2009

2 OPERA neutrino velocity 1/3 First of all CONGRATULATIONS to the team at CERN and LNGS for the excellent experiment Their detection accuracy on the neutrino (E=17GeV) velocity is (v-c)/c = 2.8+/-(0.28 stat.)+/- (0.30 syst.))x 10-5 against similar experiments on ground which had accuracies on deviation from c <10-5 (E>30GeV) and 5.1+/-2.9x10-5 (E peak =3 GeV) At E of the order of 15 MeV the observation of anti neutrinos from the explosion of the SN 1987A (LMC at 170,000 l.y.) from three sites found no anomalies from c with a relative accuracy < 2x10-9 (four order of magnitudes better!)

3 SN 1987A (Hubble Telescope)

4 OPERA neutrino velocity 2/3 Authors write: "the potentially great impact of the result motivates the continuation of our studies in order to investigate possible still unknown systematic effects that could explain the observed anomaly. We deliberately do not attempt any theoretical or phenomenological interpretation of the results Systematic effects have different origin but all are simply diabolic: - known knowns - unknown knowns - known unknowns - unknown unknowns

5 Caution! OPERA neutrino velocity 3/3 But if the result is confirmed the consequences on the particle physics, cosmology and fundamental physics will be simply dramatic. For the time being let s think that particle physics and cosmology are complementary in determining neutrino properties (e.g. the CMB anisotropy spectrum and the power spectrum of the galaxies distribution are both sensible the total mass and number of neutrinos)

6 The Standard Big Bang Model: The Basic Framework Isotropy + Homogeneity General Relativity Big Bang Model Hubble Expansion CMB Perfect Fluids Made of several Constituents p w Nucleosynthesis Euclid: measuring w DE (t) Large Scale Structure

7 Energy budget of the Universe

8 Create particles & antiparticles that existed ~ ns after Big Bang. One Force Four Forces Particle physicists look at the properties of particles produced by accelerator. Astrophysicists look at the CMB, galaxies, etc. in the space. 8

9 The explosive expansion of space during inflation would have created ripples in the fabric of space. As explained later, these gravity waves should have left a signature in the polarization of the lastscattered photons (CMB). The amplitude of the gravity wave is proportional to the expansion rate H during inflation, which in turn is proportional to the inflation energy scale squared: GW amplitude H Einf(exp2), where Einf~<1016GeV

10 Fluctuation and GW generator Fluctuation amplifier But GW dissipator

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12 Cosmic Microwave Background Radiation Overview The oldest light or the first light of the Universe Discovered the remnant afterglow from the Big Bang. 2.7 K Blackbody radiation, Discovered the patterns (anisotropy) in the afterglow. angular scale ~ 7 at a level ΔT/T of 10-5 (Wilkinson Microwave Anisotropy Probe): angular scale ~ Planck angular scale ~ 5, ΔT/T ~ 2x10-6, 30~867 Hz

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14 Science with Planck Determining cosmological parameters to high accuracy Geometry, Contents, Dynamics of Universe epoch of reionisation: birth of the first stars Constraining dark energy, neutrino mass, Testing inflation: constraining the inflaton potential Finding signatures of primordial gravitational waves Finding primordial non-gaussianity in primordial perturbations: Testing different inflationary scenario Evolution of structure and nature of dark matter Testing fundamental symmetries: P, CPT Galactic and extra galactic Astrophysics

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21 Planck-LFI: the Instrument Sensitivity, stability & low systematics Sensitivity ( T/T /pix) - State-of-the-art InP LNA technology - Cryo operation 20K Sorption Cooler - 22-element array 70 GHz MMIC HEMT 20K (Sorption cooler) 30 GHz GHz 44 GHz K 26 (MB et al 2010, Mandolesi et al 2010)

22 First light Data from 14 Jun 09 (2 months before start of survey, NO tuning) Sky Preliminary Dipole Calibration Ref Diff In-flight tuning LFI cooldown (Jun-Jul 09) (Cuttaia et al 2009, Gregorio et al 2011) Functionality tests all 44 LFI detectors OK! Optimisation of bias for LNAs, Phase switches Exploit cool-down of HFI 4K stage (LFI loads) Tuning of electronics and compression parameters

23 Planck-LFI: Data Processing (Zacchei, Maino, et al. 2011) Beginning of Nominal Survey: 13/08/2009 Till now, LFI acquired about 760 days of data No significant problems detected, no missed OD s Percentage of missed data Real gaps Data flagged as not suitable for science - Occasional Idrain steps - DAE gain changes Total of 39 events in 1 year Science data acquired during re-pointing - Currently not usable by pipeline - In principle recoverable with full pointing information Cosmic ray hits on DAE The stability of the pipeline contributed to the creation of ERCSC (first public product from Planck) with high quality

24 LFI Beams (Sandri, Villa et al. 2010, 2011) Jupiter is by far best beam calibrator for LFI (in LFI beams: 24 Oct 1 Nov, 2009) Use calibrated, differenced TOD s Measure M and S radiometers independently 1/f fluctuations removed by destriping (Madam) χ2 fit of beam model (bivariate Gaussian) (Burigana et al. 2001) - Uncertainty on FWHM ~ Ellipticity ~1.3, as expected Good match with model predictions

25 Planck-LFI eyes in the sky Modele Measurement Measurements Model Contours: 3, 10, 15, 20 db Nazzareno Mandolesi ASI, SIF Roma, L Aquila 11 Gennaio 26 th September M.Bersanelli Planck in volo

26 Noise properties Noise spectra well described by 2-component (3-parameter) model (of all 22 LFI radiometers) P( f) 1 2 WN fknee Fit to noise power spectra (Natoli et al. 2001) (de Gasperis et al. 2005) with slope: 1 f WN level LFI 19M OD s 100 to Sigma Map from Jack-knife timelines: 1 st 2 nd half of each pointing period - Structure-less map - Small residuals on galactic plane due to beam ellipticity Contribution of residual 1/f to white noise: 4.0% at 30 GHz 1.6% at 44 GHz 0.2% at 70 GHz Requirement: < 12%

27 Planck-LFI: rough data 10min of flight data 1/44 LFI detectors Sky Signal Reference Signal Difference

28 Planck-HFI: rough data 3min of flight data 1/54 HFI detectors

29 Current Status 864 days since launch. Satellite and instruments working nominally and continuously since start of sky surveys (mid August 2009) Sky coverage is 100% All the sky has been surveyed four times. Fifth survey already ongoing. The currently approved mission operation (to end Nov 2011) will do over > four sky surveys, until the end of the cold phase (end January 2012) with two instruments: HFI + LFI A further 12 months extension has been approved with LFI only

30 COBE years data Why Planck? M. Maris - 09

31 COBE years data Why Planck? WMAP years data

32 COBE years data Why Planck? WMAP years data PLANCK months data

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34 Expected results from simulations 30, 44, 70, 100, 143, 217, 353, 545, 857 GHz I, Q, U at all channels Except 545 & 857 GHz Cosmic Microwave Background Sunyaev-Zeldovich The Milky Way Point & Compact sources

35 The Planck view of the sky after alm ost one year of operations (CMB rem oved) 3 0 GHz 4 4 GHz 7 0 GHz GHz GHz GHz GHz GHz GHz

36 1st public delivery from Planck Early Release Compact Source Catalogue ERCSC It contains more than 10,000 sources at 9 frequency band fro 70 to 857 GHz It is the most complete full sky Source catalogue It s alreaddy triggering a huge number of follow up (from ground based and space borne observatory)

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42 The Planck ERCSC in brief

43 Sunyaev-Zeldovich effect: basics It is a secondary anisotropy predicted in 1972 due to inverse Compton Scattering between CMB photons (~0.3 mev) and free electrons (~ few KeV) of the hot Intra-Cluster Medium. CMB photons acquire energy! CMB photons blue shifted CMB photons hot ICM Planck Thermal SZ : CMB photons are scattered by random motion of thermal electrons Kinetic SZ : CMB photons are scattered by bulk motion of electrons

44 Sunyaev-Zeldovich effect: properties y-compton parameter provides the frequency dependence SZ effect does not depend on z; Carlstrom, Holder and Reese 2002 y-compton gives the amplitude of the effect (~ 1 mk) SZ vanishes for ~217 GHz (signature of the effect; one of the Planck channels is 217 GHz specifically to identify the zero transition of TSZ); Y is the integrated Compton that is proportional to the temperature-weighted mass of the cluster divided by the angular diameter distance which is the only term depending on z (weakly). This is an useful relation for extracting cosmological information (that are in ) when combined with other observations (X-ray typically).

45 The Early SZ (ESZ) cluster sample from Planck Abell 2319 newly discovered supercluster, PLCK G , Planck (left) and XMM-Newton (right panel) At the end of the mission it will be delivered the Planck SZ cluster catalogue containing many hundreds of clusters at z~1. The previous all-sky catalogue is RASS (Rosat All Sky Survey) but at much lower depth (i.e. z~0.1)

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47 COMA CLUSTER The Coma cluster is most formidable SZ source of the Planck sky. It is a low redshift (z=0.023) massive (M_500=9.9E14 M_sun) hot clusters (T=8.7 kev, r_500=1.86mpc). For this reason its angular size is so extended that Planck can resolve it spatially (R_500=1.86Mpc=47.8arcmin.) So Far the best profile SZ measured for coma cames for the 7years WMAP data (e.g. Komatsu et al 2011) WMAP S/N of coma = 3.6 Planck S/N=22 4/12/11

48 Detection by Planck and confirmation by XMM-Newton of PLCK G , an exceptionally X ray luminous and massive galaxy cluster at z = 1

49 Detection by Planck and confirmation by XMM-Newton of PLCK G , an exceptionally X ray luminous and massive galaxy cluster at z = 1

50 XMM-Newton follow-up for validation of Planck discovered clusters 25 Planck candidates analyzed 21 are confirmed 17 are single clusters 4 are double or triple systems XMM-Newton images (0.3-2 KeV) of the confirmed cluster candidates, except for two triple systems

51 The Early SZ (ESZ) cluster sample from Planck Validation consistency check (simulation, but based on data): Integrated Compton parameters of ESZ are used to extract the Hubble parameter reference used h = 0.7 recovered parameter h = 0.71

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54 The case of NGC 205

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57 15 days of rough Planck data Detailed Views of the Recombination Epoch (z=1088, 13.7 Gyrs ago)

58 LFI 70 GHz vs WMAP V-band

59 HFI 100 GHz vs WMAP W-band

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61 WMAP 7 CMB map Courtesy WMAP Science Team

62 10/5/ point correlation function depends only on a single angle: statistical isotropy ) ( ) ( T T T T ) ( ) ( ) ( T T T T T T ) ( ) ( ) ( ) ( T T T T T T T T Two-point Three-point Four-point For a Gaussian field (CMB is VERY Gaussian), only two-point counts Analyze the field through correlation functions (CF)

63 Typical model prediction for CMB anisotropy APS Pre recombination (acoustic) oscillations of photon-baryon fluid SW plateau: l(l+1)cl ~ cost Photon diffusion damping a m ( x) = òy 4p * m DT ( g ) T ( x, g )

64 POLARIZATION 2X2 SYMMETRIC TRACE-FREE POLARIZATION TENSOR EXPRESSED IN TERMS OF THE STOKES PARAMETERS Q AND U, CAN BE EXPANDED IN SPIN SPH: E-MODES EVEN UNDER PARITY B-MODES ODD UNDER PARITY CANNOT BE GENERATED BY DENSITY FLUCTUATIONS, WE NEED TENSOR PERTURBATIONS (GRAVITY WAVES)! 6 SPECTRA: DUE TO PARITY

65 Planck: Predicted Power Spectrum Planck error boxes Note: polarization peaks out of phase w.r.t. intensity peaks due to flow velocities at z =1100 Goal for Beyond Einstein Inflation Probe depends on energy scale of inflation Predicted from large- scale structure Hu & Dodelson ARAA 2002

66 CMB Angular Power Spectrum WMAP+ 7yr TT power spectrum (Komatsu et al. 2010) Courtesy WMAP Science Team

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68 Blue: current data Red: Planck

69 New Measurements, More Parameters! Neutrino masses m Neutrino effective number eff N Primordial Helium Y P

70 Small scale CMB can probe Helium abundance at recombination.

71 WMAP constraints Komatsu et al, 2010,

72 Forecasts on Helium Abundance Blue: Planck Yp=0.01 Red: Planck+ACTpol Yp=0.006 Green: COrE Yp=0.003

73 Current constraints on neutrino mass from Cosmology Blue: WMAP-7 Red: w7+sn+bao+h0 Green: w7+cmbsuborb+sn+lrg+h0 Current constraints (assuming LCDM) m <1.2 [ev] CMB m < [ev] CMB+other m <0.3 [ev] CMB+LSS (extreme) [ev]

74 Forecasts on Neutrino Mass Blue: Planck m 0.16 Red: Planck+ACTpol m 0.08 Green: COrE m 0.05

75 Forecasts on Neutrino Number Blue: Planck N =0.18 Red: Planck+ACTpol N =0.11 Green: CMBPol N =0.044

76 What is the Parity Transformation? It is the transformation that is applied when we look at the world in a mirror. In math it is the flip of sign of one spatial coordinate. In three dimensions it is equivalent to the flips of all the 3 spatial dimensions (note that the flip of signs of 2 axes in 3 dimensions is equivalent to a rotation). The determinant of a Parity transformation is -1 (whereas a Rotation has determinant =1) If Physics equations are invariant under Parity then we say that Parity is conserved. Specifically Parity is conserved in electromagnetic interactions (as well as in gravity and strong interactions) whereas is broken in weak interactions. CMB physics is purely electromagnetic. Therefore through CMB anisotropies we can study whether the Lagrangian of the photon is Parity conserved as we expect. This analysis might help in constraining Parity-violating terms that can be introduced.

77 Algebraic Properties for Testing Parity in CMB Temperature Map spherical harmonics expansion for T anisotropies Parity Property behavior of T coefficients of spherical harmonics under parity symmetry (i.e. even multipoles are invariant under parity whereas odd multipoles acquire a -1 ) CMB physics does not distinguish between even and odd multipoles. For example at low ell the TT power spectrum is given by the so called Sachs - Wolfe plateau that reads: Therefore it is possible to divide each T map in two subsets corresponding to even and odd multipoles, satisfying two different transformation under P symmetry. Considering the angular power spectrum contained in the two subsets it is possible to study the consistency with P symmetry

78 Algebraic Properties for Testing Parity in CMB Polarization Maps spherical harmonics expansion for Pol anisotropies Parity Property Similar consideration previously expressed for T can be applied to the E mode and (potentially) to the B mode Moreover the opposite behavior of B w.r.t. T or E, forces the cross-correlations <T B> and <E B> to be vanishing in order to be consistent with Parity symmetry!

79 Testing parity (P) symmetry: definition of estimators For X = TT, TE, EE and BB: For X = TB and EB: (Kim & Naselsky, 2010) these estimators have been computed at large angular scale considering an optimal APS estimator. A MC of realizations with realistic noise (both for WMAP 7 and Planck) has been performed (Gruppuso et al., MNRAS, 2010)

80 TT results (WMAP 7) R D

81 Percentage vs angular scale solid line: R estimator dashed line: D estimator % l max this plot suggests the existence of a characteristic scale lying in the range between 15 and 24 for which the estimators might be considered anomalous (<1%)

82 Considerations on this Parity analysis TT anomaly large angular scale with a confidence level of 99.5% in the WMAP 7 data. 1.matter of taste if such percentage is to be considered anomalous 2.It is still unknown whether such a result comes from fundamental physics or if it is due to some not perfectly removed astrophysical foreground or systematic effect Polarization analysis of the WMAP 7 data does not show any deviation from Parity symmetry but: 1.This might be due to the large WMAP 7 noise level that make the signal sinking 2.If ell_max is too large the considered estimators are testing the Parity of the WMAP noise Planck data are awaited with great interest in this respect because: 1.Planck is observing the sky with a totally different scanning strategy wrt WMAP (benefit from the point of view of systematic effects analysis) 2.Confirm TT anomaly and extend the Polarization analysis

83 Planck forecasts (e.g. 143 GHz channel) Standard deviations for D Planck is much more sensitive to polarization estimators Standard deviations for C R on EE

84 COSMIC BIREFRINGENCE We call birefringence angle (BA) the rotation angle of the polarization direction of each photon traveling in the universe. If the Maxwell theory of electromagnetism is valid than the BA is zero. If terms (like Chern-Simons) have to be added to the standard electrodynamics than the BA is different from zero (and Lorentz, CPT symmetries will be violated). Considering CMB photons the APS of CMB anisotropies will be modified as follows: where is the birefringence angle From these equations it is possible to build estimators for alpha. Measuring alpha it is then possible to test the fundamental theory of electromagnetism and constraining the amplitude of the terms that violate CPT symmetries. this analysis is divided in high and low ell

85 Small Angular Scale QUAD EXPERIMENT Wu et al. PRL 102 (2009) alpha = / (statistical) +/- 0.5 (systematic) [deg]

86 WMAP EXPERIMENT Small Angular Scale using a pixel based likelihood code Komatsu et al. ApJSS 192 (2011) alpha = /- 1.2 (statistical) +/- 1.5 (systematic) (WMAP 7YR) [deg] using a wavelet analysis: Cabella, Natoli and Silk PRD76 (2007) alpha = /- 3 [deg] (WMAP 3YR)

87 WMAP EXPERIMENT Large Angular Scale using a pixel based likelihood code Komatsu et al. ApJSS 192 (2011) alpha = /- 5.2 [deg] (WMAP 7YR) using the following estimators (as Wu et al.) not taking into account a systematic error of ~1.5 [deg] Gruppuso et al. (2011) arxiv: alpha = /- 3.5 [deg] (WMAP 7YR)

88 WMAP EXPERIMENT Large Angular Scale using a pixel based likelihood code Komatsu et al. ApJSS 192 (2011) alpha = /- 5.2 [deg] (WMAP 7YR) using the following estimators (as Wu et al.) not taking into account a systematic error of ~1.5 [deg] Gruppuso et al. (2011) arxiv: alpha = /- 1.7 [deg] (WMAP 7YR)

89 WMAP EXPERIMENT Large Angular Scale Varying l_min and l_max, the D estimators allow to build the spectrum of the birefringence angle at large angular scale. This provides a scale dependent information on the birefringence angle. For example considering the DTB estimator: Joint Likelihood slices for different Delta ell (WMAP 7YR) [2,16] [17,31] [32,46] Gruppuso et al. (2011) arxiv:

90 Planck and CMBPol forecast Small Angular Scale Xia et al. (2009), IJMPD Planck CMBPol

91 Planck forecast Large Angular Scale Red = WMAP 7 year Blue = Planck forecast For example considering the joint estimator for the ell range [2,23] Planck should outnumber WMAP by a factor above 16 in terms of standard deviations

92 But there is also another well known consequence of GR: gravitational fields can propagate as waves!

93 Gravitational wave searches across the spectrum

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96 Inflation models S-dimensional assisted inflation assisted brane inflation anomoly-induced inflation assisted inflation assisted chaotic inflation boundary inflation brane inflation brane-assisted inflation brane gas inflation brane-antibrane inflation braneworld inflation Brans-Dicke chaotic inflation Brans-Dicke inflation bulky brane inflation chaotic inflation chaotic hybrid inflation chaotic new inflation D-brane inflation D-term inflation dilaton-driven inflation dilaton-driven brane inflation double inflation double D-term inflation dual inflation dynamical inflation dynamical SUSY inflation eternal inflation extended inflation extended open inflation extended warm inflation extra dimensional inflation F-term inflation F-term hybrid inflation false-vacuum inflation false-vacuum chaotic inflation fast-roll inflation first-order inflation gauged inflation Hagedorn inflation higher-curvature inflation hybrid inflation hyperextended inflation induced gravity inflation intermediate inflation inverted hybrid inflation isocurvature inflation... And last but not least: Higgs and Dilaton Cosmology (J. Garcìa- Bellido et al.)

97 Universi a bolle (o multiversi) Extra dimensioni (oltre 4)

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99 Planck: Understanding the Big Bang George Efstathiou 19/3/2009

100 Conclusions Planck is the ESA most unbitious scientific mission in Astrophysics, Cosmology, Particle and Fundamental Physics The first results have already been published or are in process to be published. The First Cosmological release is expected to be delivered by January 2013 and more and more refined results will come out thereafter (polarized maps and spectra etc.) The improvement of the knowledge of the cosmological parameters is expected to be substantial Fundamental Physics is the final goal

101 Acknowledgments It is difficult to thank individually every single person (ESA, Industries, Funding Agencies, scientists, engineers, managers, technical staff in our Institutes and Universities; all over more than 1000 people) who has been deepley involved in Planck in the past 19 years, but we should always remember everyone with deep gratitude.

102 The scientific results that have been presented yesteray are a product of the Planck Collaboration, including individuals from more than 100 scientific institutes in Europe, the USA and Canada Planck is a project of the European Space Agency -- ESA -- with instruments provided by two scientific Consortia funded by ESA member states (in particular the lead countries: France and Italy) with contributions from NASA (USA), and telescope reflectors provided in a collaboration between ESA and a scientific Consortium led and funded by Denmark.

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