Neutrino Masses with Lensing of the Cosmic Microwave Background

Transcription

1 Neutrino Masses with Lensing of the Cosmic Microwave Background (Study of Experimental Probe of Inflationary Cosmology) Asantha Cooray University of California-Irvine

2 (almost) uniform 2.726K blackbody (Penzias & Wilson) Universe at 400kyr: the microwave sky COBE (Mather & Smoot) Dipole (local motion) WMAP O(10-5) perturbations (+galaxy)

3 Anisotropies

4

5 Around 2013 with Planck Hu & Dodelson

6 Amblard

7

8

9 Hu

10 Lensing distributes anisotropies from degree scales to damping tail and smooths acoustic peaks In temperature hard to see because of other secondaries In polarization lensing mixes E & B modes. Polarization secondaries are smaller.

11 Non-Gaussianity of lensing Bad: decreases information content of lensing B-modes from the case of a simple Gaussian mode counting. (Beware of Gaussian Fisher predictions of B-modes) Good: allows a statistical mechanism to reconstruct foreground mass distribution responsible for lensing

12 Non-Gaussianity of lensing Lensing weakly correlates CMB modes with l = l : T (l)t (l ) φ(l l ). Reconstructed field φ is quadratic in CMB temperature: φ(n) = a α(n) a β(n) d 2 l α(n) = (2π) 2 β(n) = d 2 l (2π) 2 C TT C TT 1 + N TT C TT + N TT T (l)e il bn T (l)e il bn Second idea for detecting CMB lensing: look for extra power in φ. Compute C φφ : quadratic in φ, or four-point in CMB. (> 50 publications)

13 Hint of lensing in WMAP? Start (1) Gaussian fields {g m, φ m, a unlensed (2) Lensed CMB a lensed (3) m (4) m } 3.4 detection, as a cross-correlation WMAP data (5) NVSS data (7) Filtered CMB a m (6) Filtered galaxy field g Reconstructed m potential φ m (8) Lensing estimator C φg 2 C φg = (33.2 ± 10.5) 10 7 (20 40, stat.) Smith et al. 07 no detection limits on lensing-isw and lensing-sz Calabrese et al. 09

14 Next steps A detection of the lensing potential power spectrum with WMAP-7? Requires a computation of the 4 point function, work started, results out soon!!! (Joseph Smidt et al. in preparation) Existing estimators (Hu & Okamoto; Seljak & Hirata) are biased, need to properly account for the Gaussian part of the trispectrum and remove noise bias. Fast, optimized estimators for non-gaussianity now developed in a series of papers by Munshi, Smidt et al. (we measured the primordial trispectrum for the first time ever in ) Still requires a large number of Monte-Carlo simulations. Limited by computational resources. Out to ell of 900, ~25,000 CPU hours. Naive estimator scales as l 4. Fast estimators scales as l 3 logl.

15 CMB lensing CMB lensing vs. galaxy lensing Advantages: 1. A precisely known source 2. Linear fluctuations, there is really no need to model nonlinearities down to sub-percent precision. 3. Community experience in analyses of complex CMB datasets Disadvantages: Finite information content!

16 Experimental Probe of Inflationary Cosmology EPIC Selected by NASA in 2003 for a 2 to 3-year study, again in In , EPIC was put forward as a general CMB community-supported mission concept for the CMBpol post-planck mission. In Europe, B-POL study (but not selected; Euclid selected for dark energy as a Cosmic Visions M class mission). Jamie Bock (JPL), PI Bock et al

17 Post-Planck Mission Effort in US The EPIC-IM Study Team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nflation Probe ASMCS,&1/B(8><D,-.G3&%=/<'!B&6='& 3>>*&H 23(4*5+6/?<>==(7>#/%B>6 AE!.,>&66&(7$6D%/H -*+6</=>6(2: L*PHBP=>Q(F>*BD+,-.G3&%=/<'?'&$% 9&6&6H 2:(;+66/B>=& F&*H(9+6B'&M F?A3 L/6=(4*M+6 E4?K!#*+&6(.//( 23(8/*D/%/H 3'&*%/B(.&M*/6</,-.?=/5/(;/H/*((I-4J 2:(3'+<&N>.H1&6(-&N/ -*+6</=>6(2:,>'6(R$'% 3&B/(O/B=/*6 ;+D/(?/+QQ/*=,-. ;&=+&B S&%#&**+&N& 9&*5&*#(2: participants Decadal White Papers The Origin of the Universe as Revealed Through the Polarization of the CMB, Dodelson et al. and 211 Co-signers, ArXiv Observing the Evolution of the Universe, Page et al. and 168 Co-signers, ArXiv A Program of Technology Development and Sub-Orbital Observations of CMB Polarization Leading to and Including a Satellite Mission,, Meyer et al. and 141 Co-signers CMB Community Reports Theory and Foregrounds: 5 Papers with 135 Authors and Co-Authors Probing Inflation with CMB Polarization, Baumann et al. 2008, ArXiv Gravitational Lensing, Smith et al. 2008, ArXiv Reionization Science with the CMB, Zaldarriaga et al. 2008, ArXiv Prospects for Polarized dforeground dremoval, Dunkley et al. 2008, ArXiv Foreground Science Knowledge and Prospects, Fraisse et al. 2008, ArXiv Systematic Error Control: 10 Papers with 68 Authors and Co-Authors CMB Technology Development: 22 Papers with 37 Authors and Co-Authors Path to CMBPol: Conference on CMBPol mission in July with 104 participants Mission Study Reports Study of the EPIC-Intermediate Mission, Bock et al. 2009, ArXiv The Experimental Probe of Inflationary Cosmology, Bock et al. 2008, ArXiv See for a full compilation V

18 Richness of the CMB Polarization Landscape!$%&'($)"*+,#$) &-$./('+)/,).,&+0.) 1%(0%2.$)/,)#%+-023) /%04! 5($.0&0,2).,&+,4,36.,&+,4,36! 8$-%(/'($)9(,+)&.%4$)021:! ;$0,20<%/0,2 =0&/,(6!$%&'($)7*+,#$).,&+0.)&=$%() &-$./('+)/,).,&+0.)) 40+0/&! >$'/(02,)+%&&)=0$(%(.=6! 7*+,#$)&-$./('+)%/) ()I)J:JK)/,)%&/(,-=6&0.%4) 40+0/&!?FG)$2$(36)&.%4$! H%(3$)90$4#)0294%/0,2! 2 / L)().,2&0&/$2.6)/$&/!%-)?%4%./0.) +%32$/0.)90$4#&)10%) #'&/)-,4%(0<%/0,2! DE)%2#)4%(3$*&.%4$)7*90$4#

19 Precision Cosmology

20 Mapping NASA Objectives to EPIC Instrument Requirements NASA Research Objective* What are the origin, evolution, and fate of the universe? NASA Targeted Outcome* Test the Inflation hypothesis of the Big Bang Precisely determine the cosmological parameters governing the evolution of the universe Measurement Criteria Measure inflationary B-mode power spectrum to astrophysical limits for 2 < _ < 200 at r = 0.01 after foreground removal Measure EE to cosmic variance into the Silk damping tail to probe primordial density perturbations Instrument Criteria _ All-sky coverage _ w p -1/2 < 6 µkarcmin _ GHz _ 1 resolution _ Control systematic errors below r = 0.01 _ 10' resolution EPIC-low cost just for this How do planets, stars, galaxies and cosmic structures come into being? Improve our knowledge of dark energy, the mysterious cosmic energy that will determine the fate of the universe Investigate the seeds of cosmic structure in the cosmic microwave background Measure the distribution of dark matter in the universe Determine the mechanism(s) by which most of the matter of the universe became reionized Study the birth of stellar and planetary systems *Taken from NASA 2007 Science Plan Measure lensing-bb to cosmic limits to probe neutrino physics and early (z~2) dark energy density and equation of state Measure EE to cosmic variance to distinguish reionization histories Map Galactic magnetic fields via dust polarization _ w p -1/2 < 2 µkarcmin _ 6' resolution _ Primary mission parameters above _ 500 and 850 GHz bands Primary Objective EPIC-IM optimized for the goal of measuring CMB lensing with deliverables of neutrino masses. Secondary Objective

21 Optimizing an experiment for a science goal

22 Particle physics application of EPIC CMB lensing probes linear fluctuations Source properties known (Both these lead to systematic errors in galaxy lensing) Lensing B-modes and CMB Cosmic Shear Reconstruction A deliverable: neutrino mass (Σm ν < 0.05 ev or better at 95% confidence level) Test SuperK Atmosphere oscillations that suggest Δm ν 2 2x10-3 ev 2 and distinguish between two mass hierarchies EPIC study reports

23 Neutrino mass hierarchy from cosmology For the LCDM cosmological model, EPIC, as currently configured, reaches a sum of the neutrino masses of ev and if the equation of state of dark energy is allowed to vary this constraint is at 0.047eV at the same 95% confidence level. This is not a simple Gaussian Fisher matrix estimate. It accounts for the full covariance, part of which was based on simulations.

24 EPIC-IM Specification Sheet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ass similar to the Planck satellite mission

25 Experimental Probe of Inflationary Cosmology Intermediate Mission (Bock, JPL)!"#$%$&'())*+$,'-.(/* 0*1*)2(3*!"#$%&'()%*+(%+,#-$'"#+&#*$)*.-*/+01,%/#$+(%+2%$,)2+&),)($!3)/#+456+7%"+$#*$)()8)(9!!"#$%"!&'()&*("+$&+,$-(,.!"/.- 4-'.*$5(2-1$61-/*!:).:+$#*$)()8)(9+7%"+;*7&-()%*-"9+<1,%/#$!.01&*.-$*"$2344$5!&+67$8(--("+-9! 3)/#+7"#='#*29+2%8#"-.#+7%"+7%"#."%'*/$ 2%8#"-.# 7%" 7%"#."%'*/$!:).:+7"#='#*2)#$+7%"+>-&-2()2+$2)#*2# 4:$;-1($<'=79! -6&+$-*'&*.:;$<"'$!&':.=-6&!.$%"!&'()&*("+-*'&*.:; -6&!.! $'*$:)#&/+$),)&-"+(%+K&-*2L+-*/+NOPQ! (! *A *!!(* ( (

26 Highly Redundant & Uniform Scan Coverage N-hits (1-day) Angular Uniformity* (6-months) Planck WMAP EPIC 0 1 *<cos 2β> 2 + <sin 2β> 2

27 High Throughput, Multi-Band Focal Plane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z \/[#I/.#@]@L@C#,"P 13/P#@.,"V/0]@9BL

28 Moore s Law for Sensitivity and Mapping Speed BLIP CMB Ground BLIP CMB Space 45$ $%&'#'()*! 6+ +,-./,01" "# 2/'(/"3!" ACT BICEP2 EBEX SCUBA2

29 Neutrino mass hierarchy from cosmology Can we do better? Further optimize EPIC (at a very high cost), factor of 1.2 to 1.3 at most improvement with CMB polarization alone Better, Combine EPIC with Euclid/JDEM-WL for a factor of ~2 to 3 improvement through z-binned lensing + a good model for non-linearities for galaxy lensing. lensing of 21-cm: highly futuristic

30 Summary Planck should do BB lensing, and get down to ~0.2 ev level Post-Planck EPIC satellite for CMB polarization is well developed. US-based CMB community has requested NASA to start a project office after the 2010 Astronomy Decadal Survey, based on recommendations on CMB sciences. If started, EPIC phase-a to begin around 2015, launch around Will Planck provide a hint of tensors and/or primordial non- Gaussianity? motivation for EPIC will be clearer then.