![Page 1: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/1.jpg)
1
with D. Hanson, G. Holder, O. Doré, and M. Kamionkowski
arXiv: 1107.1716 (DG, OD, and MK)- Phys. Rev. Lett. 107 261301 arXiv: 1107.5047 (DG, OD, and MK)- Phys. Rev. D. 84 123003 arXiv: 1306.4319 (DG, DH, GH, OD, and MK)- submitted to Phys. Rev. D
Variation in the cosmic baryon fraction and the CMB
Daniel Grin (KICP/Chicago)Presentation for CAP workshop
09/24/2013
![Page 2: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/2.jpg)
ZOOLOGY OF INITIAL CONDITIONS
2
![Page 3: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/3.jpg)
ZOOLOGY OF INITIAL CONDITIONS
2
![Page 4: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/4.jpg)
ZOOLOGY OF INITIAL CONDITIONS
2
![Page 5: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/5.jpg)
ZOOLOGY OF INITIAL CONDITIONS
2
![Page 6: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/6.jpg)
ZOOLOGY OF INITIAL CONDITIONS
2
All density initial conditions can be expressed in terms of these!These conditions are not conserved under fluid evolution
![Page 7: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/7.jpg)
✴ WMAP 7-year constraints (Komatsu/Larson et al 2010)
OBSERVATIONAL CONSTRAINTS TO ISOCURVATURE
3
Adiabatic
![Page 8: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/8.jpg)
✴ WMAP 7-year constraints (Komatsu/Larson et al 2010)
OBSERVATIONAL CONSTRAINTS TO ISOCURVATURE
3
Adiabatic
✴ Constraints relax if assumptions (scale-invariance, single isocurvature mode) relaxed: Bean et al. 2009
CI NID NIV
nadi = n iso nadi = n iso nadi = n isor iso< 0.13 < 0.08 < 0.14
CI+NID+NIV No BBN/bias
0.44 ± 0.09 0.51 ± 0.09
![Page 9: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/9.jpg)
✴ Planck 1st-year temperature constraints (Et al et al..., 2013)
OBSERVATIONAL CONSTRAINTS TO ISOCURVATURE
3
Adiabatic
✴ Constraints relax if assumptions (scale-invariance, single isocurvature mode) relaxed: Bean et al. 2009
CI NID NIV
nadi = n iso nadi = n iso nadi = n isor iso< 0.13 < 0.08 < 0.14
CI+NID+NIV No BBN/bias
0.44 ± 0.09 0.51 ± 0.09
![Page 10: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/10.jpg)
BARYON-DM ISOCURVATURE
4
Adiabatic
✴ “Nuisance” mode identified (Lewis 2002)
✴ Subdominant fluctuations: Adiabatic modes dominate, but do the relative number densities of DM and baryons fluctuate?
Compensated Isocurvature Perturbation (CIP)
Baryon-dark matter entropy
![Page 11: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/11.jpg)
BARYON-DM ISOCURVATURE
4
Adiabatic
✴ “Nuisance” mode identified (Lewis 2002)
✴ Subdominant fluctuations: Adiabatic modes dominate, but do the relative number densities of DM and baryons fluctuate?
Compensated Isocurvature Perturbation (CIP)
![Page 12: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/12.jpg)
BARYON-DM ISOCURVATURE
4
Adiabatic
✴ “Nuisance” mode identified (Lewis 2002)
✴ Subdominant fluctuations: Adiabatic modes dominate, but do the relative number densities of DM and baryons fluctuate?
Compensated Isocurvature Perturbation (CIP)
![Page 13: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/13.jpg)
✴ Vanishing Sachs-Wolfe effect from CIPs
CIPS AND THE CMB
5
✴ Observationally null in the CMB! (surprising but true)
CIPS AND THE SACHS-WOLFE EFFECT
![Page 14: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/14.jpg)
✴ Vanishing Sachs-Wolfe effect from CIPs
Vanishes for all isocurvature modes
CIPS AND THE CMB
5
✴ Observationally null in the CMB! (surprising but true)
CIPS AND THE SACHS-WOLFE EFFECT
![Page 15: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/15.jpg)
✴ Vanishing Sachs-Wolfe effect from CIPs
Vanishes for all isocurvature modes
Also Vanishes for compensated modes
CIPS AND THE CMB
5
✴ Observationally null in the CMB! (surprising but true)
CIPS AND THE SACHS-WOLFE EFFECT
![Page 16: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/16.jpg)
CIPS AND ACOUSTIC WAVES
6
Adiabatic
✴ Run your favorite Boltzmann code (CAMB/CMBFAST) with a CIP✴Fractional change in anisotropies of less than 0.00001 for angular scales l<10000
DefinitionBaryon conservation
Gravity, pressure, Thomson scattering
DM conservation
Gravity
✴Why?
![Page 17: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/17.jpg)
CIPS AND ACOUSTIC WAVES
6
Adiabatic
✴ Run your favorite Boltzmann code (CAMB/CMBFAST) with a CIP✴Fractional change in anisotropies of less than 0.00001 for angular scales l<10000
✴For CIPs, CMB is only affected on scales where baryonic pressure matters
![Page 18: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/18.jpg)
CIPS AND ACOUSTIC WAVES
6
Adiabatic
✴ Run your favorite Boltzmann code (CAMB/CMBFAST) with a CIP✴Fractional change in anisotropies of less than 0.00001 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!
![Page 19: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/19.jpg)
✴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)
EXISTING MODELS FOR CIPS
7
![Page 20: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/20.jpg)
✴ Curvaton sources entropy fluctuation in CDM
EXISTING MODELS FOR CIPS
8
Adiabatic
✴ After curvaton dominates, adiabatic flucts generated
Gordon and Pritchard, 2009
![Page 21: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/21.jpg)
✴ Curvaton sources entropy fluctuation in CDM
EXISTING MODELS FOR CIPS
8
Adiabatic
✴ After curvaton dominates, adiabatic flucts generated
Gordon and Pritchard, 2009
![Page 22: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/22.jpg)
✴ Curvaton sources entropy fluctuation in CDM
EXISTING MODELS FOR CIPS
8
Adiabatic
✴ After curvaton dominates, adiabatic flucts generated
Gordon and Pritchard, 2009
![Page 23: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/23.jpg)
✴ Curvaton sources entropy fluctuation in CDM
EXISTING MODELS FOR CIPS
8
Adiabatic
✴ After curvaton dominates, adiabatic flucts generated
Gordon and Pritchard, 2009
Fluctuations as high as 8% are allowed by the data
![Page 24: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/24.jpg)
EXISTING CONSTRAINTS TO CIPS- BBN
9
Adiabatic
✴ Primordial abundances of : Blue compact galaxies (He) and QSO Absorption systems (De)
from Holder et al. 2009(from Allen 2008)- 42 ‘relaxed’ galaxy clusters
✴ Baryon fraction measurements in galaxy clusters
![Page 25: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/25.jpg)
EXISTING CONSTRAINTS TO CIPS- BBN
9
Adiabatic
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?
![Page 26: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/26.jpg)
CIPS AND 21-CM FLUCTUATIONS
10
Adiabatic
Gordon and Pritchard, 2009
200 400 600 800 10000.000
0.005
0.010
0.015
0.020
0.025
0.030
1C2!
mK2
z 40 2
3
5
30 40 50 60 70
10
20
30
40
50
60
z
Areakm
2
![Page 27: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/27.jpg)
COMPENSATED ISOCURVATURE AND THE CMB:z~1100 EFFECTS
11
![Page 28: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/28.jpg)
COMPENSATED ISOCURVATURE AND THE CMB:z~1100 EFFECTS
11
![Page 29: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/29.jpg)
ldamp � 1000λD≈N1/2λC
N=η/λC
✴ Damping scale modulated by CIPs
COMPENSATED ISOCURVATURE AND THE CMB:z~1100 EFFECTS
12
![Page 30: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/30.jpg)
✴ Damping scale modulated by CIPs
COMPENSATED ISOCURVATURE AND THE CMB:z~1100 EFFECTS
12
![Page 31: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/31.jpg)
COMPENSATED ISOCURVATURE AND THE CMB:RECOVERING THE REALIZATION
13
✴ Power spec. results were true, averaging over realizations of primordial
I
Q
U
![Page 32: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/32.jpg)
COMPENSATED ISOCURVATURE AND THE CMB:RECOVERING THE REALIZATION
13
✴ Power spec. results were true, averaging over realizations of primordial
I
Q
U
![Page 33: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/33.jpg)
COMPENSATED ISOCURVATURE AND THE CMB:RECOVERING THE REALIZATION
13
✴ Power spec. results were true, averaging over realizations of primordial
I
Q
U
![Page 34: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/34.jpg)
COMPENSATED ISOCURVATURE AND THE CMB:RECOVERING THE REALIZATION
13
✴ 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
![Page 35: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/35.jpg)
COMPENSATED ISOCURVATURE AND THE CMB:RECOVERING THE REALIZATION
13
✴ 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
-++++++
++ + + +
+++++
++++
+
--
---
--- -
---
- --
-- - - - ---
-
-- -
-
-
-
---
�(npatch) < 0
![Page 36: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/36.jpg)
COMPENSATED ISOCURVATURE AND THE CMB:RECOVERING THE REALIZATION
13
✴ 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
-++++++
++ + + +
+++++
++++
+
--
---
--- -
---
- --
-- - - - ---
-
-- -
-
-
-
---
![Page 37: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/37.jpg)
COMPENSATED ISOCURVATURE AND THE CMB:RECOVERING THE REALIZATION
13
✴ 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 all-sky map with patches2. Measure power spec in each patch3. Reconstruct �(n)
-++++++
++ + + +
+++++
++++
+
--
---
--- -
---
- --
-- - - - ---
-
-- -
-
-
-
---
![Page 38: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/38.jpg)
Filtering the map
14
✴ Reconstruct CIP map
![Page 39: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/39.jpg)
Spherical geometry
Estimating CIP power spectrum from data
15
✴ Universe gives us CIP amplitudes as random variables: nonlinear modulation of linear theory CMB Non-Gaussianity at 4-pt function (trispectrum) level
O✓dCl
dnb
◆����2
⌦m
DT~l1
T~l2T~l3
T~l4
E
connected
/ C��
L
h�LM�⇤L0M 0i =CL
X X
C��L /
X
M
1
(2L+ 1)
��LM � �null
LM
�⇤ ⇥��LM � �null
LM
�
✴ CIP power spectrum estimate from Monte Carlos and filtered CMB map
![Page 40: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/40.jpg)
Reconstructed power spectrum from WMAP 9-year data
16
![Page 41: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/41.jpg)
Reconstructed power spectrum from WMAP 9-year data
16
No evidence for CIPs! Cosmic baryon fraction is homogeneous arXiv: 1306.4319 (DG, DH, GH, OD, and MK)- submitted to Phys. Rev. D
![Page 42: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/42.jpg)
Upper limit to CIP spectrum at a variety of scales
17
![Page 43: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/43.jpg)
Upper limit to CIP spectrum at a variety of scales
17Cosmic baryon fraction is homogeneous at 10-20% level at 5-100˚ scales
![Page 44: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/44.jpg)
✴ Combine scales to probe models
✴ Scale-invariant CIP spectrum
✴ Monte Carlo null hypothesis
Limit to amplitude of scale-invariant spectrum
18
CL =A
L(L+ 1)
A . 1.1⇥ 10�2
![Page 45: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/45.jpg)
✴ Combine scales to probe models
✴ Scale-invariant CIP spectrum
✴ Monte Carlo null hypothesis
✴ Observations consistent with null hypothesis
Limit to amplitude of scale-invariant spectrum
18
CL =A
L(L+ 1)
A . 1.1⇥ 10�2
![Page 46: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/46.jpg)
Limit to amplitude of scale-invariant spectrum
18
✴ Proof of technique
✴ First purely primordial test
✴ Great improvement with coming experiments
A . 1.1⇥ 10�2
![Page 47: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/47.jpg)
Possible sources of bias
19
Noise bias
Point sources
Lensing
Secondary CIP
Scale invariant signal
All secondary biases can be neglected for WMAP-9 analysis
![Page 48: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/48.jpg)
COMPENSATED ISOCURVATURE AND THE CMB:PROSPECTS
20
![Page 49: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/49.jpg)
COMPENSATED ISOCURVATURE AND THE CMB:PROSPECTS
20
![Page 50: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/50.jpg)
COMPENSATED ISOCURVATURE AND THE CMB:PROSPECTS
20
Excluded by galaxy cluster measurements
of baryon fraction
![Page 51: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/51.jpg)
COMPENSATED ISOCURVATURE AND THE CMB:PROSPECTS
20
Parameter spaceaccessible with CMB
Two orders of magnitude improvement: conservatively
![Page 52: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/52.jpg)
✴ Primordial, baryons trace DM at ~10-20% 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
CONCLUSIONS
![Page 53: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/53.jpg)
SACHS WOLFE-EFFECT & POWER SPECTRA
22
Adiabatic
![Page 54: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/54.jpg)
SACHS WOLFE-EFFECT & POWER SPECTRA
22
Adiabatic
![Page 55: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/55.jpg)
✴ 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
CIPS AND GALAXIES (IN REALITY)
23
Adiabatic
Pgal = b2T 2matter (k)P� (k)
Might be detectably modulated by CIPs
WORK IN PROGRESS
![Page 56: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/56.jpg)
✴ All perturbations seeded by curvaton
✴ CIPs are correlated with adiabatic flucts
✴ Non-vanishing 3 pt-functions in specific curvaton implementation
24
FUTURE WORK: CORRELATED CIPs AND THE CURVATON MODEL
![Page 57: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/57.jpg)
Errors are strongly signal-dependent
25
![Page 58: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/58.jpg)
✴ From gravitational redshifting
✴ For adiabatic initial condition
✴ For density isocurvature
ISOCURVATURE AND SACHS-WOLFE EFFECT
26
✓�T
T
◆
CMB
= ��SLS +�SLS�
4
![Page 59: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/59.jpg)
OBSERVATIONAL CONSTRAINTS TO ISOCURVATURE
27
Adiabatic
✴ WMAP 7-year constraints (Komatsu/Larson et al 2010)
![Page 60: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/60.jpg)
OBSERVATIONAL CONSTRAINTS TO ISOCURVATURE
27
Adiabatic
✴ WMAP 7-year constraints (Komatsu/Larson et al 2010)
✴ Constraints relax if assumptions (scale-invariance, single isocurvature mode) relaxed: Bean et al. 2009
CI NID NIV
nadi = n iso nadi = n iso nadi = n isor iso< 0.13 < 0.08 < 0.14
CI+NID+NIV No BBN/bias
0.44 ± 0.09 0.51 ± 0.09
![Page 61: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/61.jpg)
OBSERVATIONAL CONSTRAINTS TO ISOCURVATURE
27
Adiabatic
✴ WMAP 7-year constraints (Komatsu/Larson et al 2010)
![Page 62: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/62.jpg)
EXISTING CONSTRAINTS TO CIPS- BBN
28
Adiabatic
✴ Primordial abundances of : Blue compact galaxies (He) and QSO Absorption systems (De)
from Holder et al. 2009(from Allen 2008)- 42 ‘relaxed’ galaxy clusters
✴ Baryon fraction measurements in galaxy clusters
![Page 63: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/63.jpg)
EXISTING CONSTRAINTS TO CIPS- BBN
28
Adiabatic
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?
![Page 64: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/64.jpg)
✴ 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
COMPENSATED ISOCURVATURE AND THE CMB:z~1100 EFFECTS
29
Vastly exceeds reionization signal!!!Second order!
![Page 65: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/65.jpg)
✴ Patchy Screening: (Smith/Dvorkin 2008/2009)
Angular dependence of modulates
✴ Patchy scattering
COMPENSATED ISOCURVATURE AND THE CMB:PATCHY REIONIZATION
30
![Page 66: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/66.jpg)
COMPENSATED ISOCURVATURE AND THE CMB:z~1100 EFFECTS
31
✴ Efficiency of polarization generation is modulated
From Wayne Hu’s website
Isotropic radiation Quadrupole moment
![Page 67: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/67.jpg)
COMPENSATED ISOCURVATURE AND THE CMB:z~1100 EFFECTS
31
✴ a
![Page 68: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/68.jpg)
COMPENSATED ISOCURVATURE AND THE CMB:RECOMBINATION B-MODES
32
![Page 69: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/69.jpg)
✴ ... but at power spectrum level for l>100, all are swamped by lensing!
COMPENSATED ISOCURVATURE AND THE CMB:CIPS VS LENSING
33
(μK2)
![Page 70: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/70.jpg)
✴ ... but at power spectrum level for l>100, all are swamped by lensing!
COMPENSATED ISOCURVATURE AND THE CMB:CIPS VS LENSING
33
✴ ...fortunately, there is life beyond the power spectrum!
(μK2)
![Page 71: Variation in the cosmic baryon fraction and the CMB · Presentation for CAP workshop 09/24/2013. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL CONDITIONS 2. ZOOLOGY OF INITIAL](https://reader034.vdocument.in/reader034/viewer/2022050412/5f88ca3d2d40e571d7526598/html5/thumbnails/71.jpg)
Possible sources of bias
34
✴Weak lensing of CMB ➡Trispectrum (statistical)➡Off-diagonal correlations (in a realization of lensing potential)
✴Unresolved point sources ➡Bispectrum detected in Planck 2013 temp data
✴Secondary CIP/lensing contractions
✴Chance correlations (noise bias)