CMB lensing and delensing. Anthony Challinor and Olivier Doré

Transcription

1 CMB lensing and delensing Anthony Challinor and Olivier Doré

2 Current state of the art Planck Collaboration ,000 resolved modes S/N = 40 (power spectrum)

3 Where we want to be >10 5 resolved modes S/N > 300 (power spectrum)

4 TT/EB dominance in future S/N = 40 S/N > 300 EB particularly helpful for pol. noise < 5 μk arcmin - Polarization reconstructions less susceptible to extragalactic contamintion (e.g., tsz) but more so to Galactic foregrounds

5 Goals for CMB lensing/delensing 4-pt φxφ (neutrino mass etc.) 3-pt φxlss (growth of structure, dark energy, mitigation of systematics/self-calibration) Delensing (improve inflation constraints + Neff etc.) Halo lensing (cluster mass calibration at high redshift)

6 Issues addressed in this session How do we achieve these goals? Survey requirements (resolution, sensitivity, frequency coverage, sky coverage) Space or ground? An ultimate diffuse lensing mission?

7 <latexit sha1_base64="txadzaoqjjjbxdbzfuy8ec6dexw=">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</latexit> <latexit sha1_base64="txadzaoqjjjbxdbzfuy8ec6dexw=">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</latexit> <latexit sha1_base64="txadzaoqjjjbxdbzfuy8ec6dexw=">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</latexit> <latexit sha1_base64="txadzaoqjjjbxdbzfuy8ec6dexw=">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</latexit> Sensitivity and resolution Pol. noise level S N 2 = f sky X L = N modes 2 2L +1 2 C L C L + N (0) L! 2 EB TT

8 Cosmology from φxφ

9 Neutrino masses P m (k) P m =0(k) P m =0(k) k [h Mpc 1 ] Allison m = 0.1 ev m = 0.2 ev m = 0.3 ev C ` appleapple ( m ) C ` appleapple ( m =0) C ` appleapple ( m =0) m = 60 mev m = 120 mev S3-wide S ` Complementary to optical weak lensing - Higher-z, mostly linear regime, no intrinsic-alignment issues Comparable precision on neutrino mass to e.g., Euclid lensing

10 <latexit sha1_base64="skx4pmhgq8jzw8narzqdjoc3vog=">aaacexichvhbahsxenvul0ncs9z2mqretfp3gtltdwkhhash0lekpu4cljfaedywkbqbavrqlv2i/frf8iv5yunkx4xeqgckhc6zgulnsljjh0lyhsw3bt+5u7s80rh3/8hd1eajx4eu8fzatxsqsmczd6ckgr5kvhbcwua6u3cunezn9knvyj0szfecljdqfgxklgxhqa2bz8zjsezmqy5t5rymesimz1aoj/icbr6n3s57rstmgwkhnwwnp56pkep4jtv8l1jt7x/5waennf7blt26ud3ld7v79bdzsjrdzbb0b5b25mfsios4gdz/sfehvaadqnhn+mls4qdifqvqudeyd1bycclh0a/qca1uum2tq+ntwixoxtiwdni5+2tfxbvzu52ftm1x4v7uzus/tl7h/o2gkqb0cezcx5r7rbggsznqkbqgue0d4mlk8fyqjtxygwfajwdcz5/sm0hvdeddj/3cbe1sl9xyjmtkg7rjsrbidvledkipchirrueb0bpomt6i2/gl69q4wtq8ib9f/oykusu+aa==</latexit> <latexit sha1_base64="skx4pmhgq8jzw8narzqdjoc3vog=">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</latexit> <latexit sha1_base64="skx4pmhgq8jzw8narzqdjoc3vog=">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</latexit> <latexit sha1_base64="skx4pmhgq8jzw8narzqdjoc3vog=">aaacexichvhbahsxenvul0ncs9z2mqretfp3gtltdwkhhash0lekpu4cljfaedywkbqbavrqlv2i/frf8iv5yunkx4xeqgckhc6zgulnsljjh0lyhsw3bt+5u7s80rh3/8hd1eajx4eu8fzatxsqsmczd6ckgr5kvhbcwua6u3cunezn9knvyj0szfecljdqfgxklgxhqa2bz8zjsezmqy5t5rymesimz1aoj/icbr6n3s57rstmgwkhnwwnp56pkep4jtv8l1jt7x/5waennf7blt26ud3ld7v79bdzsjrdzbb0b5b25mfsios4gdz/sfehvaadqnhn+mls4qdifqvqudeyd1bycclh0a/qca1uum2tq+ntwixoxtiwdni5+2tfxbvzu52ftm1x4v7uzus/tl7h/o2gkqb0cezcx5r7rbggsznqkbqgue0d4mlk8fyqjtxygwfajwdcz5/sm0hvdeddj/3cbe1sl9xyjmtkg7rjsrbidvledkipchirrueb0bpomt6i2/gl69q4wtq8ib9f/oykusu+aa==</latexit> Parameter degeneracies for m n CORE CORE+BAO 0.20 m [ev] c h H X m X m = 44 mev CORE = 17 mev +BAO A s Constraint on t important: degrades to 30 mev with Planck prior s(t) = 0.01 Cosmic-variance-limited t [s(t) = 0.002] becomes limiting for Nmodes > 10 5

11 Issue I: extragalactic foregrounds Issue in T-based reconstruction tsz and CIB - tszxtszxφ and (tsz) 4 both important (van Engelen+ 2014) Mitigation: - Masking (loss of signal for tsz) - Modelling (e.g., Planck for unclustered sources) - tsz nulling (on gradient leg; Madhavacheril & Hill 2018) 0.06 Standard masking, l max = 3000 Aggressive masking, l max = 2500 Fractional CMB Lensing Bias van Engelen mjy 5x10 14 Msol L 150 GHz tsz 4 pt. CIB 4 pt. tsz 2 κ corr. CIB 2 κ corr. 1 mjy 1x10 14 Msol L

12 Issue 2: Galactic foregrounds Main issue for EB reconstruction Care (mainly) about 4-pt non-gaussianity on intermediate and small scales - Very limited empirical information on these scales Mitigation: - Multi-frequency cleaning - Local analysis with foreground power included in lensing filters to downweight contaminated modes

13 Results on 150 GHz simulations AC+CORE 2017 No dust Worst 600-deg 2 dust field Dust inc. in lensing filters Data-derived simulations (Planck FFP8) but do not capture small-scale NG from small-scale B field

14 Requirements for φxφ Mostly care about Nmodes for power spectrum science - Generally favours large sky coverage at fixed Ndet Neutrino mass requires precise t measurement - Low-l E-mode polarization from space (e.g., LiteBIRD) - Precision on mass (with BAO) saturates around Nmodes~ ksz from patchy reionization (Ferraro & Smith 2018) Multi-frequency at high resolution prudent but less demanding than for low-l B-mode science - Need for Galactic simulations properly capturing small-scale non-gaussianity

15 Cosmology from φxlss

16 Growth of structure h i /b 2 (z)d 2 (z) happle CMB i/b(z)d 2 (z) Giannantonio+ 2016

17 Galaxy lensing-cmb lensing l C κ CMBκgal l ( 10 6 ) Planck WMAP l Hand+2013; see also Liu & Hill 2015 Kirk Current detections around 3s Will improve to >50s with e.g., DES 5-yr x SPT-3G X-correlation more immune to additive systematic effects Full joint analysis can calibrate multiplicative bias effects in shape measurement and intrinsic alignments

18 <latexit sha1_base64="bbmehg89njikxifceu4fgoltnv4=">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</latexit> <latexit sha1_base64="bbmehg89njikxifceu4fgoltnv4=">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</latexit> <latexit sha1_base64="bbmehg89njikxifceu4fgoltnv4=">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</latexit> <latexit sha1_base64="bbmehg89njikxifceu4fgoltnv4=">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</latexit> Issue: extragalactic foregrounds h ˆ(c + f,c + f) LSSi = h ˆ(c, c) LSSi + h ˆ(f,f) LSSi = h LSSi + h ˆ(f,f) LSSi Desired x-correlation Fg-fg-LSS bispectrum tsz and CIB are issues in T-based reconstruction Only, e.g., tszxtszxlss now enters Mitigation: - Masking - Modelling - tsz nulling (on gradient leg; Madhavacheril & Hill 2018)

19 Requirements for φxlss Overlap with optical surveys Generally favours wide survey Galactic foregrounds less of an issue (no bias but can inflate errors) Extragalactic foregrounds in TT require cleaning/ modelling/agressive masking - Gradient-leg cleaning (e.g., with Planck)

20 Delensing

21 Lensing and inflation constraints Lensing relatively more important for recombination signal for non-zero r Factor 6.5 hit by lensing for both scales (no signal c.v.) Lensing limits ability to test these models at high significance No lensing AC+CORE Collaboration 2017

22 Delensing the CMB Remap CMB with Wiener-filtered tracer I of CMB lensing X delens (ˆn) =X obs (ˆn rˆw) ˆW = W I X unlens (ˆn + r( ˆW )) + noise {z } Residual lensing Gradient approximation accurate for large-angle B-modes Residual lensing has power spectrum, delens C l = C l (1 2 l ) 2 l = C I l 2 C II,tot l C l

23 Scales for BB delensing C BB,delens l C BB,lens l X ln C BB,lens ln C L 1 2 L

24 Internal delensing with Planck Scales for lensing B-modes Efficiency rl 2 ` Scales for peak smoothing TT MV P `v TT ` `v EE ` `v BB ` Reconstruction very noisy Carron, Lewis & AC `

25 Improvements from internal delensing Factor by which delensing improves s(r) for r=0 = (r)no delens/ (r)delens µk-arcmin 2 µk-arcmin, it. 3 µk-arcmin 3 µk-arcmin, it. Factor improvement by internal delensing with future satellites; better from ground fwhm [arcmin] AC+CORE Collaboration 2017

26 Bias from dependent recon. noise Consider B-mode template delensing with XY estimator: B delens B ÊW ˆW(X, Y ) Power spectrum after delensing: C BB delens hbbi 2hBÊW ˆW(X, Y )i + hêw ˆW(X, Y )ÊW ˆW(X, Y )i If reconstruction noise were independent of CMB, just gives usual 2hBÊW Wi In practice, reconstruction dependent on CMB giving dominant bias 2BÊW ˆW(X, Y )+2BÊW ˆW(X, Y ) r-dependent bias if X or Y=B and overlapping scales Carron, Lewis & AC 2017; see also Sehgal+ 2017; Teng+ 2011; Namikawa 2017

27 Modelling the bias 6 2 arcmin beam; 7 µkarcmin noise C ` BB [10 6 µk 2 ] Expectation for independent recon. noise Delensed power from sims analytic C BB,res l with ˆ indep. of CMB hc BB,res l i 400sims with ˆEB green + hb temp B temp i c,iv B-mode noise power level 2 Including dominant bias term green + hb temp B temp i G green + hb temp B obs i G green + three corrections ` Baleato-Lizancos+AC in prep.; see also Namikawa 2017 Non-trivial power spectrum covariance also

28 More optimal lens reconstruction Factor by which delensing improves s(r) for r=0 = (r)no delens/ (r)delens Optimal lensing reconstruction 2 µk-arcmin 2 µk-arcmin, it. 3 µk-arcmin 3 µk-arcmin, it. Quadratic estimator for lensing reconstruction fwhm [arcmin] AC+CORE Collaboration 2017

29 External delensing GNILC 353 GHz + WISE co-add CIB+gal. GNILC 353 GHz + WISE + Planck lens co-add -0.1 CMB lensing convergence l (Squared Correlation Coe cient) CIB contribution WISE contribution Planck contribution CIB + WISE + Planck Contribution to the low-l C BB l Remove around 40% of lensing power with signaldominated E-modes Byeonghee CIB+gal.+CMB -0.1 CMB lensing convergence l Need high-z sources (CIB, LSST galaxies etc.) Residual power can be modelled from empirical spectra

30 Requirements for BB delensing Overlap of high-resolution survey with degree-scale B- mode survey (e.g., CMB-S4) Sensitivity better than 5 µkarcmin Bias from non-gaussian Galactic foregrounds not yet quantified - Residual B-mode power involves up to 6-pt function

31 Halo lensing

32 Halo lensing 6.5s detection of cluster lensing Baxter Statistical mass calibration for large samples at high redshift See also Baxter+ 2015; Planck Collaboration 2016; Madhavacheril+ 2015; Geach & Peacock 2017

33 Requirements for halo lensing Fractional mass error on 1000 cluster stack Hu M/M (N/10 3 ) 1/ T = P /2 1/2 (µk ) Arcmin resolution Rejection of tsz and IR emission from cluster galaxies Large area ET EB TT θ FWHM =1 ; l<l beam 10

34 Ultimate diffuse lensing mission? To write Visbal, Trac, Loeb 2011 de Zotti+2016 There is more to extra-galactic galaxies than CIB!

35 Ultimate diffuse lensing mission? Serra, OD, Lagache 2017 Potentially a challenge to measure the primordial distortions

36 Ultimate diffuse lensing mission? To write Serra, OD, Lagache 17 Schaan, Spergel, Ferraro 2018 Foreman But an opportunity to perfectly delense and measure the growth of structures We are at a KISS workshop after all!