Planck. Ken Ganga. APC/CNRS/ University of Paris-Diderot

Transcription

1 Planck Ken Ganga APC/CNRS/ University of Paris-Diderot

2 A Brief History of the Cosmos The CMB was emitted when the Universe was about of its current age. 2

3 Planck/HFI Timeline The HFI builds on the experience of a number of sub-orbital experiments, notably Archeops and BOOMERANG, It represents over 20 years of work and cost roughly one euro per European. 3

4 Launch Launch was May 1, 2009, from Guiana Space Center, Kourou, French Guiana Ariane 5 Launch Vehicle With Herschel (which is also at the Sun-Earth L-2 point) 4

5 Planck's Orbit around L2 Planck orbits around the second Sun-Earth Lagrange point, approximately 1.5 million km further from the Sun than the Earth 5

6 Exterior Temperatures Mirrors: ~ 40 K V-Groove: ~ 50 K V-Groove: ~100 K V-Groove: ~150 K Service Module: ~300 K Solar Array: ~270 K 6

7 Planck Has Two Instruments I will discuss mostly HFI. While the HFI was operating, the HFI detectors were the coldest things in space. The HFI took data until early LFI continues to take data, and will continue at least until the end of 2012, and perhaps to August,

8 Frequency/wavelength coverage Planck fills the SubMM range, so in addition to CMB science, Planck will be able to say a lot about dust emission in our Galaxy and in others. 8

9 Frequency/wavelength coverage IRAS WMAP Planck fills the SubMM range, so in addition to CMB science, Planck will be able to say a lot about dust emission in our Galaxy and in others. 9

10 Frequency/wavelength coverage IRAS Planck WMAP Planck fills the SubMM range, so in addition to CMB science, Planck will be able to say a lot about dust emission in our Galaxy and in others. 10

11 Planck's Scanning Strategy Planck scans the sky in (almost) great circles in a plane defined by the SunEarth axis. The full sky is (almost) covered each six months. 11

12 arxiv.org/ Galactic dust Extragalactic sources Cosmic infrared background 12

13 arxiv.org/ Galactic dust Extragalactic sources Cosmic infrared background 13

14 arxiv.org/ μkcmb Galactic dust Extragalactic sources/cosmic infrared background CMB/SZ 14

15 arxiv.org/ μkcmb Galactic dust Cosmic infrared background/extragalactic sources CMB (little SZ) 15

16 arxiv.org/ μkcmb Galactic Dust Extragalactic radio sources CMB 16

17 arxiv.org/ μkcmb CMB Extragalactic sources and SZ Galactic dust CO and radio emission 17

18 Separated Components Combinations of the 9 Planck channels allow us to separate the signals into CMB, CO, Dust and other astrophysical components Radio CO arxiv.org/ CMB Dust 18

19 Papers: March 2013 I Overview of products & results XVI Cosmological parameters II LFI data processing XVII Gravitational lensing by large-scale structure III LFI systematic uncertainties XVIII The gravitational lensing-infrared background correlation IV LFI beams XIX The integrated Sachs-Wolfe effect V LFI calibration XX Cosmology from Sunyaev-Zeldovich cluster counts VI HFI data processing XXI Compton-parameter map and characterization VII HFI time response & beams XXII Constraints on inflation VIII HFI calibration and mapmaking XXIII Isotropy and statistics of the CMB IX HFI spectral response XXIV Constraints on primordial non-gaussianity X HFI energetic particle effects XXV Searches for cosmic strings and other topological defects XI Consistency of the data XXVI Background geometry and topology of the Universe XII Component separation XXVII Special relativistic effects on the CMB dipole XIII Galactic CO emission XXVIII The Planck Catalogue of Compact Sources XIV Zodiacal emission XXIX The Planck catalogue of Sunyaev-Zeldovich sources XV CMB power spectra & likelihood XXX Explanatory supplement 19

20 Zodiacal Emission Zodiacal emission is detected by Planck It is quite small in the CMB channels Different components have different properties 20

21 Galactic dust emission We expect to make improvements over the FDS dust models and the SFD extinction maps SA/PLANCK/docs/eslab 47/Session04_Astrophy sical_results/47eslab _April_03_14_25_Mivill e-deschenes.pdf 21

22 Sunyaev-Zeldovich Effect arxiv/ Hot electrons in clusters give CMB photons a kick This allows us to detect 1227 clusters and candidates of clusters of galaxies 22

23 Cosmic Infrared Background Far infrared background anisotropies measured from 10' to 2º measured at frequencies between 217 and 857 GHz. Dominates the extragalactic sky in the higher Planck frequencies Has a spectrum similar to Galactic dust Tracer of star formation Represents material at higher redshifts than most catalogs A&A 536, A18 (2011) 23

24 Gravitational Lensing All mass between the last scattering surface and ourselves lenses the CMB We can use the deflections of the CMB to infer the effective potential seen by the CMB arxiv: v1 24

25 Gravitational Lensing All mass between the last scattering surface and ourselves lenses the CMB We can use the deflections of the CMB to infer the effective potential seen by the CMB arxiv: v1 arxiv: v1 25

26 CIB Lensing Potential The CIB is the remnant of star formation, much around z~2 This material lenses the CMB Correlations can also be done with your favorite catalog of sources, or other tracers of mass A cross-correlation shows this 545 GHz Φ arxiv: v1 26

27 Pre-Foreground Removal Spectra Top: Planck spectra at 100, 143 and 217GHz without subtraction of foregrounds. Middle: SPT spectra from R12 at 95, 150 and 220GHz, re-calibrated to Planck. The S12 SPT spectrum at 150 GHz is also shown, but without any calibration correction. Bottom: ACT spectra (weighted averages of the equatorial and southern fi elds) from D13 at 148 and 220 GHz, and the GHz cross-spectrum, with no extragalactic foreground corrections, re-calibrated to the Planck spectra. The solid line in each panel shows the best-fi t base CDM model from the combined Planck+WP+highL fi ts. arxiv: v

28 Planck power spectrum arxiv/ Combination of a number of cross-power spectra Foregrounds removed with help of smaller-scale experiments 28

29 Differences with WMAP The WMAP power spectrum is of order 2% higher than that of Planck over a range of multipoles/angular scales 29

30 Vanilla/Minimal/6-Param Lambda-CDM Lambda-CDM gives a good description of the data Lambda-CDM, parameters are near 1sigma from their WMAP values arxiv: v2 30

31 Non-Gaussianity We don't see any Local: 2.7±5.8 Equilateral: -42±75 Orthogonal: -25±39 Simple Lambda-CDM works We find the expected ISW bispectrum arxiv.org/

32 Masses & effective number of neutrinos Neff= 3.30 ± 0.27 Consistent with the canonical value of Σνmν < 0.23 ev Much of this is from lensing and in conjunction with BAO 32

33 SDSS7/ Padmanabha n Consistency with BAO 6d F SDSS7 / Perciva Baryon Acoustic l Wiggle Z Planc k Oscillations BOSS/DR 9 Measure rs/dv, where rs is comoving sound horizon when baryons become dynamically decoupled from photons Dv is = [(1+z)2DA2(z) cz/h(z)]1/3 33

34 H ± 1.2 km/s/mpc This is low compared to astronomical measurements of H0. Differences with WMAP come from larger matter content preferred by Planck The lower measurement is from Planck SZ measurements 34

35 Consistency w/ SN Magnitude redshift Planck prefers higher values of Ωm than does the Supernova Legacy Survey (SNLS) Apparently (rumor alert!), the SNLS numbers will be moving towards those of Planck soon 35

36 SZ versus CMB cosmology Planck SZ Cluster Counts prefer a lower σ8 and lower Ωm than the CMB anisotropies Or modest tweaks to the bias and a moderate neutrino mass sum Or a large neutrino mass sum arxiv/ (white). 36

37 What's going on? This is a first guess Different spectra --> different matter --> different Hubble constant 37

38 Anomalies Alignment This was seen by WMAP and is reinforced by Planck Planck frequency coverage make foreground causes less likely 38

39 Anomalies High vs. Low Multipoles The parameters determined by small angular scales ( high-ell ) basically set the size of the large angular scale anisotropies expected. The seem to be a bit low. Note also that Planck 143 GHz spectra are 2.5% lower than WMAP V+W 39

40 Anomalies Hemispheric There seems to be more structure over one half of the sky than the other This was seen by WMAP, and seems to persist on many angular scales Planck confirms that this is not an effect specific to WMAP, and improves confidence it is not foregrounds 40

41 Bianchi VIIh Cosmologies A universe with a preferred direction and rotation The Galactic mask is smaller for the Planck analysis Planck data thus do not provide evidence in support of Bianchi VIIh cosmologies. However, neither is it possible to conclusively discount Bianchi VIIh cosmologies in favor of LambdaCDM cosmologies 41

42 Inflation Ns = ± Ns < 1 at > 5σ r < 0.11 With polarization we should be able to reduce this to ~

43 Polarization A couple of papers on Galactic polarization should be released soon The main goal is to limit (or detect) the B-Modes in the CMB, which might be an indication of primordial gravitational waves. 43

44 Polarization A couple of papers on Galactic polarization should be released soon The main goal is to limit (or detect) the B-Modes in the CMB, which might be an indication of primordial gravitational waves. 44

45 Schedule : Planck Early Papers 2012: Planck Intermediate Papers : Science papers; Data release 1 (15 months of data; no timelines; no polarization) 2013: More papers, including Galactic polarization : Second delivery to ESA : Polarization Cosmology papers; Data release 2 (full mission, with timelines and polarization) NEW! 2015 Release (at least some funding has been approved for a number of countries) Archive/Legacy phase 45

46 Thank you! 46