1. PROBING THE UNIVERSE AT 20 MINUTES AND 400 THOUSAND YEARS
Gary Steigman
Ohio State University
SUSY 06, Irvine, CA, June 12 – 17, 2006

2. Primordial Nucleosynthesis Relic Photons (CBR) are free
~ 100 s after the Big Bang
Primordial Nucleosynthesis
~ 0.1 s after the Big Bang
Neutrinos Decouple
~ 380 kyr after the Big Bang
Relic Photons (CBR) are free

3. BBN & The CBR Provide Complementary Probes Of The Early Universe
Do the predictions and observations of the
baryon density (10  (nB/nγ)0 = Bh2 )
and the expansion rate (H) of the
Universe agree at 20 minutes (BBN)
and at kyr (CBR) ?

4. D, 3He, 7Li are potential BARYOMETERS
BBN – Predicted Primordial Abundances
BBN Abundances of D, 3He, 7Li
are RATE (Density) LIMITED
7Li
7Be
D, 3He, 7Li are potential BARYOMETERS

5. DEUTERIUM --- The Baryometer Of Choice
As the Universe evolves, D is only DESTROYED 
* Anywhere, Anytime : (D/H) t  (D/H) P
* For Z << Z : (D/H) t  (D/H) P (Deuterium Plateau)
(D/H) P is sensitive to the baryon density (    )
H  and D  are seen in Absorption, BUT …
* H  and D  spectra are identical  H  Interlopers?
* Unresolved velocity structure  Errors in N(H ) ?

6. D/H vs. Metallicity Deuterium Plateau ? Real variations,
systematic differences,
statistical uncertainties ?
LLS
Deuterium Plateau ?
DLA
Low – Z / High – z QSOALS

7. For Primordial D/H adopt dispersion around the mean
D/H vs. Metallicity
For Primordial D/H adopt
the mean and the
dispersion around the mean
105(D/H)P = 2.6 ± 0.4

8. (D/H)P =  0.4 x 10 SBBN  10 =  0.6
BBN

9. CBR

10.   CBR Temperature Anisotropy Spectrum (2003)
(T2 vs. ) Depends On The Baryon Density
 
Barger et al. (2003)
B h2 = , ,
CBR (WMAP) constrains B h2
The CBR is an early - Universe Baryometer

11. CBR (WMAP – ALONE)  10 =  0.3
CBR

12. D/H vs. Metallicity The CBR is a good Deuteronometer ! SBBN/WMAP
105(D/H)P = 2.6 ± 0.2

13. BBN (20 min) & CBR (380 kyr) AGREE !

14.  S (or N) is constrained by YP
The Expansion Rate (H) Provides
A Probe Of Non-Standard Physics
4He production is n/p Limited  YP is
sensitive to the EXPANSION RATE ( H  1/2 )
S  H / H  (/)1/2  (1 + 7N / 43)1/2
where    + N  and N  3 + N
 S (or N) is constrained by YP

15. 4He is an early – Universe Chronometer
Y vs. D / H
N = 2, 3, 4
(S = 0.91, 1.00, 1.08)
Y  N  (S – 1)

16. D & 4He Isoabundance Contours
YP & yD  105 (D/H)
4.0
3.0
2.0
0.25
0.24
0.23
D & 4He Isoabundance Contours
Kneller & Steigman (2004)

17. "2σ" range for YP : 0.228  0.248 (OSW) As O/H  0, Y  0
SBBN Prediction
"2σ" range for YP :  (OSW)

18. BBN (D, 4He)  For N ≈ 2.5 ± 0.3 YP & yD  105 (D/H) 4.0 3.0 2.0 0.25
0.24
0.23

19.  A Non-Standard BBN Example (Neff < 3) Late Decay of a
Massive Particle
Kawasaki, Kohri & Sugiyama
&
Low Reheat Temp.
(TR  MeV)
Neff < 3 
Relic Neutrinos Not
Fully (Re) Populated

20. BBN and Primordial (Pop ) Lithium ? Li/H vs. Fe/H
Li too low ?
SBBN + CBR
log (Li)  2.6 – 2.7
“Spite” Plateau (?)
log (Li)  2.2

21.  log (Li)  2.6  0.1 Or, Late Decay of the NLSP ? Even for N  3
yLi  1010 (Li/H)
4.2
YOSW + D  H 
Li  H   0.8 x 10 10
 log (Li)  2.6  0.1
Li depleted / diluted
in Pop  stars ?
Or, Late Decay of the NLSP ?

22.   CBR Temperature Anisotropy Spectrum (2003)
Depends on the Radiation Density R (S or N)
 
N = 1, 2.75, 5, 7
Barger et al. (2003)
CBR (WMAP) constrains N (S)
The CBR is an early - Universe Chronometer

23. BBN (D & 4He) + CBR (WMAP – 2003)
BBN & CBR
Consistent !
CBR
BBN
Barger et al. (2003)
Barger et al. (2003)

24. Joint BBN (D & 4He) & CBR (WMAP) Fit
Barger et al. (2003)
Barger et al. (2003)

25. Baryon Density Determinations: Consistent ?
Late - Decaying NLSP ? ?
N < 3 ?
Observational Uncertainties Or New Physics?

26. N Determinations (95 % CL Ranges)
(v.1)
WMAP 2006
WMAP 2003

27. Seljak et al. Revised
BUT !
N > 3 !
(v.2)

28. VERY PRELIMINARY ! STAY TUNED ! N & Mh2 Are Correlated
V. Simha & G. S.
N & Mh2 Are Correlated
2 ≤ N ≤ 8 ?
VERY PRELIMINARY !
STAY TUNED !
The CMB Is A Relatively Poor Chronometer

29. BBN (~ 20 min.) And The CBR (~ 400 kyr)
CONCLUSIONS
(Pre – WMAP 2006)
BBN (~ 20 min.) And The CBR (~ 400 kyr)
Are CONSISTENT !
1.9 ≤ N ≤ allowed @ ~ 95%
( Also : 10 = ± 0.2 )