Variation in the cosmic baryon fraction and the CMB

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1 Variation in the cosmic baryon fraction and the CMB with D. Hanson, G. Holder, O. Doré, and M. Kamionkowski Daniel Grin (KICP/Chicago) Presentation for CAP workshop 09/24/2013 arxiv: (DG, OD, and MK) Phys. Rev. Lett arxiv: (DG, OD, and MK) Phys. Rev. D arxiv: (DG, DH, GH, OD, and MK) submitted to Phys. Rev. D 1

2 ZOOLOGY OF INITIAL CONDITIONS 2

3 ZOOLOGY OF INITIAL CONDITIONS 2

4 ZOOLOGY OF INITIAL CONDITIONS 2

5 ZOOLOGY OF INITIAL CONDITIONS 2

6 ZOOLOGY OF INITIAL CONDITIONS All density initial conditions can be expressed in terms of these! These conditions are not conserved under fluid evolution 2

7 OBSERVATIONAL CONSTRAINTS TO ISOCURVATURE WMAP 7year constraints (Komatsu/Larson et al 2010) 3

8 OBSERVATIONAL CONSTRAINTS TO ISOCURVATURE WMAP 7year constraints (Komatsu/Larson et al 2010) Constraints relax if assumptions (scaleinvariance, single isocurvature mode) relaxed: Bean et al CI NID NIV n adi = n iso n adi = n iso n adi = n iso r iso < 0.13 < 0.08 < 0.14 CINIDNIV No BBN/bias 0.44 ± ±

9 OBSERVATIONAL CONSTRAINTS TO ISOCURVATURE Planck 1styear temperature constraints (Et al et al..., 2013) Constraints relax if assumptions (scaleinvariance, single isocurvature mode) relaxed: Bean et al CI NID NIV n adi = n iso n adi = n iso n adi = n iso r iso < 0.13 < 0.08 < 0.14 CINIDNIV No BBN/bias 0.44 ± ±

10 BARYONDM ISOCURVATURE Nuisance mode identified (Lewis 2002) Compensated Isocurvature Perturbation (CIP) Baryondark matter entropy Subdominant fluctuations: Adiabatic modes dominate, but do the relative number densities of DM and baryons fluctuate? 4

11 BARYONDM ISOCURVATURE Nuisance mode identified (Lewis 2002) Compensated Isocurvature Perturbation (CIP) Subdominant fluctuations: Adiabatic modes dominate, but do the relative number densities of DM and baryons fluctuate? 4

12 BARYONDM ISOCURVATURE Nuisance mode identified (Lewis 2002) Compensated Isocurvature Perturbation (CIP) Subdominant fluctuations: Adiabatic modes dominate, but do the relative number densities of DM and baryons fluctuate? 4

13 CIPS AND THE SACHSWOLFE EFFECT CIPS AND THE CMB Observationally null in the CMB! (surprising but true) Vanishing SachsWolfe effect from CIPs 5

14 CIPS AND THE SACHSWOLFE EFFECT CIPS AND THE CMB Observationally null in the CMB! (surprising but true) Vanishing SachsWolfe effect from CIPs Vanishes for all isocurvature modes 5

15 CIPS AND THE SACHSWOLFE EFFECT CIPS AND THE CMB Observationally null in the CMB! (surprising but true) Vanishing SachsWolfe effect from CIPs Vanishes for all isocurvature modes Also Vanishes for compensated modes 5

16 CIPS AND ACOUSTIC WAVES Run your favorite Boltzmann code (CAMB/CMBFAST) with a CIP Fractional change in anisotropies of less than for angular scales l<10000 Why? Definition Baryon conservation Gravity, pressure, Thomson scattering Gravity DM conservation 6

17 CIPS AND ACOUSTIC WAVES Run your favorite Boltzmann code (CAMB/CMBFAST) with a CIP Fractional change in anisotropies of less than for angular scales l<10000 For CIPs, CMB is only affected on scales where baryonic pressure matters 6

18 CIPS AND ACOUSTIC WAVES Run your favorite Boltzmann code (CAMB/CMBFAST) with a CIP Fractional change in anisotropies of less than for angular scales l<10000 There seems to be no affect on the CMB! No way to observationally disentangle (using CMB) CDM and baryon isocurvature models! 6

19 EXISTING MODELS FOR CIPS If heavy CDM produced before curvaton domination Direct branching from inflaton Gravitational particle production during inflation WIMPzilla (Kolb et al. 1998) Curvatons dominate, decay to baryons (Lyth et al. 2002) 7

20 EXISTING MODELS FOR CIPS Gordon and Pritchard, 2009 Curvaton sources entropy fluctuation in CDM After curvaton dominates, adiabatic flucts generated 8

21 EXISTING MODELS FOR CIPS Gordon and Pritchard, 2009 Curvaton sources entropy fluctuation in CDM After curvaton dominates, adiabatic flucts generated 8

22 EXISTING MODELS FOR CIPS Gordon and Pritchard, 2009 Curvaton sources entropy fluctuation in CDM After curvaton dominates, adiabatic flucts generated 8

23 EXISTING MODELS FOR CIPS Gordon and Pritchard, 2009 Curvaton sources entropy fluctuation in CDM After curvaton dominates, adiabatic flucts generated Fluctuations as high as 8% are allowed by the data 8

24 EXISTING CONSTRAINTS TO CIPS BBN Primordial abundances of (He) and QSO Absorption systems (De) Baryon fraction measurements in galaxy clusters from Holder et al (from Allen 2008) 42 relaxed galaxy clusters : Blue compact galaxies 9

25 EXISTING CONSTRAINTS TO CIPS BBN Fluctuations as high as 8% are allowed by the data Can we empirically show, rather than simply assume, that baryon trace DM in the early universe? 9

26 CIPS AND 21CM FLUCTUATIONS Gordon and Pritchard, Area km z 10

27 COMPENSATED ISOCURVATURE AND THE CMB: z~1100 EFFECTS 11

28 COMPENSATED ISOCURVATURE AND THE CMB: z~1100 EFFECTS 11

29 COMPENSATED ISOCURVATURE AND THE CMB: z~1100 EFFECTS Damping scale modulated by CIPs N=η/λ C λ D N 1/2 λ C l damp

30 COMPENSATED ISOCURVATURE AND THE CMB: z~1100 EFFECTS Damping scale modulated by CIPs 12

31 COMPENSATED ISOCURVATURE AND THE CMB: RECOVERING THE REALIZATION Power spec. results were true, averaging over realizations of primordial I Q U 13

32 COMPENSATED ISOCURVATURE AND THE CMB: RECOVERING THE REALIZATION Power spec. results were true, averaging over realizations of primordial I Q U 13

33 COMPENSATED ISOCURVATURE AND THE CMB: RECOVERING THE REALIZATION Power spec. results were true, averaging over realizations of primordial I Q U 13

34 COMPENSATED ISOCURVATURE AND THE CMB: RECOVERING THE REALIZATION Power spec. results were true, averaging over realizations of primordial In single realization of CIP spec., a long wavelength CIP w/ amp affafafmodulates the power spectrum across the sky 13

35 COMPENSATED ISOCURVATURE AND THE CMB: RECOVERING THE REALIZATION Power spec. results were true, averaging over realizations of primordial In single realization of CIP spec., a long wavelength CIP w/ amp affafafmodulates the power spectrum across the sky (ˆn patch ) < 0 13

36 COMPENSATED ISOCURVATURE AND THE CMB: RECOVERING THE REALIZATION Power spec. results were true, averaging over realizations of primordial In single realization of CIP spec., a long wavelength CIP w/ amp affafafmodulates the power spectrum across the sky 13

37 COMPENSATED ISOCURVATURE AND THE CMB: RECOVERING THE REALIZATION Power spec. results were true, averaging over realizations of primordial In single realization of CIP spec., a long wavelength CIP w/ amp affafafmodulates the power spectrum across the sky Heuristically: 1. Tile allsky map with patches 2. Measure power spec in each patch 3. Reconstruct (ˆn) 13

38 Filtering the map Reconstruct CIP map 14

39 Estimating CIP power spectrum from data Universe gives us CIP amplitudes as random variables: nonlinear modulation of linear theory CMB NonGaussianity at 4pt function (trispectrum) level E 2 DT dcl ~l1 T ~l2 T ~l3 T ~l4 / C L X O X connected dn b m h LM L 0 M i =C 0 L Spherical geometry CIP power spectrum estimate from Monte Carlos and filtered CMB map Ĉ L / X M 1 (2L 1) LM null LM LM null LM 15

40 Reconstructed power spectrum from WMAP 9year data 16

41 Reconstructed power spectrum from WMAP 9year data No evidence for CIPs! Cosmic baryon fraction is homogeneous arxiv: (DG, DH, GH, OD, and MK) submitted to Phys. Rev. D 16

42 Upper limit to CIP spectrum at a variety of scales 17

43 Upper limit to CIP spectrum at a variety of scales Cosmic baryon fraction is homogeneous at 1020% level at 5100 scales 17

44 Limit to amplitude of scaleinvariant spectrum Combine scales to probe models Scaleinvariant CIP spectrum C L = A L(L 1) Monte Carlo null hypothesis A

45 Limit to amplitude of scaleinvariant spectrum Combine scales to probe models Scaleinvariant CIP spectrum C L = A L(L 1) Monte Carlo null hypothesis Observations consistent with null hypothesis A

46 Limit to amplitude of scaleinvariant spectrum Proof of technique First purely primordial test Great improvement with coming experiments A

47 Scale invariant signal Possible sources of bias Noise bias Point sources Lensing Secondary CIP All secondary biases can be neglected for WMAP9 analysis 19

48 COMPENSATED ISOCURVATURE AND THE CMB: PROSPECTS 20

49 COMPENSATED ISOCURVATURE AND THE CMB: PROSPECTS 20

50 COMPENSATED ISOCURVATURE AND THE CMB: PROSPECTS Excluded by galaxy cluster measurements of baryon fraction 20

51 COMPENSATED ISOCURVATURE AND THE CMB: Parameter space accessible with CMB PROSPECTS Two orders of magnitude improvement: conservatively 20

52 CONCLUSIONS Primordial, baryons trace DM at ~1020% level A new test of curvaton models is at hand Degeneracy between baryon and CDM isocurvature can be broken with CMB data In progress: Correlated case, effect on galaxies Future work: (use SPT/Planck data) 21

53 SACHS WOLFEEFFECT & POWER SPECTRA 22

54 SACHS WOLFEEFFECT & POWER SPECTRA 22

55 CIPS AND GALAXIES (IN REALITY) WORK IN PROGRESS CIPs would change baryon fraction of halos: affect properties of galaxies in different patches of sky (detectable in SDSS? vs. astrophysical confusion) Baryonic part of halo collapses late CIPs would change transfer function for LSS power spectrum, induce couplings between scales P gal = b 2 T 2 matter (k) P (k) Might be detectably modulated by CIPs 23

56 FUTURE WORK: CORRELATED CIPs AND THE CURVATON MODEL All perturbations seeded by curvaton CIPs are correlated with adiabatic flucts Nonvanishing 3 ptfunctions in specific curvaton implementation 24

57 Errors are strongly signaldependent 25

58 ISOCURVATURE AND SACHSWOLFE EFFECT From gravitational redshifting T T CMB = SLS SLS 4 For adiabatic initial condition For density isocurvature 26

59 OBSERVATIONAL CONSTRAINTS TO ISOCURVATURE WMAP 7year constraints (Komatsu/Larson et al 2010) 27

60 OBSERVATIONAL CONSTRAINTS TO ISOCURVATURE WMAP 7year constraints (Komatsu/Larson et al 2010) Constraints relax if assumptions (scaleinvariance, single isocurvature mode) relaxed: Bean et al CI NID NIV n adi = n iso n adi = n iso n adi = n iso r iso < 0.13 < 0.08 < 0.14 CINIDNIV No BBN/bias 0.44 ± ±

61 OBSERVATIONAL CONSTRAINTS TO ISOCURVATURE WMAP 7year constraints (Komatsu/Larson et al 2010) 27

$EXISTING CONSTRAINTS TO CIPS BBN Primordial abundances of (He) and QSO Absorption systems (De) Baryon fraction$

62 EXISTING CONSTRAINTS TO CIPS BBN Primordial abundances of (He) and QSO Absorption systems (De) Baryon fraction measurements in galaxy clusters from Holder et al (from Allen 2008) 42 relaxed galaxy clusters : Blue compact galaxies 28

63 EXISTING CONSTRAINTS TO CIPS BBN Fluctuations as high as 8% are allowed by the data Can we empirically show, rather than simply assume, that baryon trace DM in the early universe? 28

64 COMPENSATED ISOCURVATURE AND THE CMB: z~1100 EFFECTS 90% of CMB photons last scatter at decoupling (z~1100) CIPs are primordial: induced anisotropies at z~1100 >> reionization terms Prior work neglected effects at z~1100 Vastly exceeds reionization signal!!! Second order! 29

65 COMPENSATED ISOCURVATURE AND THE CMB: PATCHY REIONIZATION Patchy Screening: (Smith/Dvorkin 2008/2009) Angular dependence of modulates Patchy scattering 30

66 COMPENSATED ISOCURVATURE AND THE CMB: z~1100 EFFECTS Efficiency of polarization generation is modulated Isotropic radiation Quadrupole moment From Wayne Hu s website 31

67 COMPENSATED ISOCURVATURE AND THE CMB: z~1100 EFFECTS a 31

68 COMPENSATED ISOCURVATURE AND THE CMB: RECOMBINATION BMODES 32

69 COMPENSATED ISOCURVATURE AND THE CMB: CIPS VS LENSING... but at power spectrum level for l>100, all are swamped by lensing! (μk 2 ) 33

70 COMPENSATED ISOCURVATURE AND THE CMB: CIPS VS LENSING... but at power spectrum level for l>100, all are swamped by lensing!...fortunately, there is life beyond the power spectrum! (μk 2 ) 33

71 Possible sources of bias Chance correlations (noise bias) Weak lensing of CMB Trispectrum (statistical) Offdiagonal correlations (in a realization of lensing potential) Unresolved point sources Bispectrum detected in Planck 2013 temp data Secondary CIP/lensing contractions 34

The Once and Future CMB

The Once and Future CMB DOE, Jan. 2002 Wayne Hu The On(c)e Ring Original Power Spectra of Maps 64º Band Filtered Ringing in the New Cosmology Gravitational Ringing Potential wells = inflationary seeds