parameterizing dark energy z. huang, r. j. bond, l. kofman canadian institute of theoretical...
TRANSCRIPT
![Page 1: Parameterizing Dark Energy Z. Huang, R. J. Bond, L. Kofman Canadian Institute of Theoretical Astrophysics](https://reader038.vdocument.in/reader038/viewer/2022110206/56649d1a5503460f949ef190/html5/thumbnails/1.jpg)
Parameterizing Dark Energy Z. Huang, R. J. Bond, L. Kofman
Canadian Institute of Theoretical Astrophysics
![Page 2: Parameterizing Dark Energy Z. Huang, R. J. Bond, L. Kofman Canadian Institute of Theoretical Astrophysics](https://reader038.vdocument.in/reader038/viewer/2022110206/56649d1a5503460f949ef190/html5/thumbnails/2.jpg)
w - Dark Energy Equation of State
Constant w=w0 w(a)=w0+wa(1-a) Principal components
Data: CMB + SN + LSS + WL + Lya Code: modified cosmomc
w0 = -0.98 ± 0.05
s1=0.12 s2=0.32 s3=0.63
![Page 3: Parameterizing Dark Energy Z. Huang, R. J. Bond, L. Kofman Canadian Institute of Theoretical Astrophysics](https://reader038.vdocument.in/reader038/viewer/2022110206/56649d1a5503460f949ef190/html5/thumbnails/3.jpg)
What we know about w
Phenomenologically• w is close to –1 at low redshift• Rich information at z<2, weak information at
2<z<4, almost no information at z>4• Results depend on parametrization. Need
theoretical priors.
What if we start from physics?
![Page 4: Parameterizing Dark Energy Z. Huang, R. J. Bond, L. Kofman Canadian Institute of Theoretical Astrophysics](https://reader038.vdocument.in/reader038/viewer/2022110206/56649d1a5503460f949ef190/html5/thumbnails/4.jpg)
Use physics to solve problems
When Canadian plug does not fit UK socket…
![Page 5: Parameterizing Dark Energy Z. Huang, R. J. Bond, L. Kofman Canadian Institute of Theoretical Astrophysics](https://reader038.vdocument.in/reader038/viewer/2022110206/56649d1a5503460f949ef190/html5/thumbnails/5.jpg)
Dynamics of Quintessence/Phantom
we do need assumptions
simplicity of w(a).
simplicity of V(φ).
![Page 6: Parameterizing Dark Energy Z. Huang, R. J. Bond, L. Kofman Canadian Institute of Theoretical Astrophysics](https://reader038.vdocument.in/reader038/viewer/2022110206/56649d1a5503460f949ef190/html5/thumbnails/6.jpg)
Dynamics of Quintessence/Phantom
define
Field equation + Friedmann Equations
Popular story of quintessence: Fast rolling (large eV) in early universe (scaling regime); Slow rolling (small eV) in late universe.
![Page 7: Parameterizing Dark Energy Z. Huang, R. J. Bond, L. Kofman Canadian Institute of Theoretical Astrophysics](https://reader038.vdocument.in/reader038/viewer/2022110206/56649d1a5503460f949ef190/html5/thumbnails/7.jpg)
Simplicity assumptions
1. V(f) is monotonic. 2. Quintessence rolls down (dV/dt<0). Phantom rolls up
(dV/dt>0).3. w is close to -1 at low redshift. Quantitatively, |1+w|<0.4 at
0<z<1.
4. V(f) is a “simple” function. Quantitatively, |hV| is less than or of the same order of either Planck scale or eV.
examples, V(f) = V0 exp(-lf)V(f) = V0 + V1 fV(f) = V0 fn (n=0,±1, ±2, ±3,…)
In the relevant redshift range (e.g. 0<z<4),
![Page 8: Parameterizing Dark Energy Z. Huang, R. J. Bond, L. Kofman Canadian Institute of Theoretical Astrophysics](https://reader038.vdocument.in/reader038/viewer/2022110206/56649d1a5503460f949ef190/html5/thumbnails/8.jpg)
1-parameter parametrization• Additional assumption: slow-roll at 0<z<10
(initial velocity Hubble-damped at low redshift).
where
es>0, quintessence
es=0, cosmological constant
es<0, phantom
CMB + SN + LSS + WL + Lya
“average slope” es=<ev>
![Page 9: Parameterizing Dark Energy Z. Huang, R. J. Bond, L. Kofman Canadian Institute of Theoretical Astrophysics](https://reader038.vdocument.in/reader038/viewer/2022110206/56649d1a5503460f949ef190/html5/thumbnails/9.jpg)
Initial velocity is damped by Hubble friction
![Page 10: Parameterizing Dark Energy Z. Huang, R. J. Bond, L. Kofman Canadian Institute of Theoretical Astrophysics](https://reader038.vdocument.in/reader038/viewer/2022110206/56649d1a5503460f949ef190/html5/thumbnails/10.jpg)
Time variation of eV is not important
Given solution w(a) and eV(a), define trajectory variables:
• es= eV uniformly averaged at 1/3<a<1.
• ew = (1+w)/f(a/aeq). (remind: 1-param formula is wfit=-1+ es f(a/aeq))
![Page 11: Parameterizing Dark Energy Z. Huang, R. J. Bond, L. Kofman Canadian Institute of Theoretical Astrophysics](https://reader038.vdocument.in/reader038/viewer/2022110206/56649d1a5503460f949ef190/html5/thumbnails/11.jpg)
Constraint Equation
• Define w0=w|
a=1,
wa=-dw/da|a=1
w0 and wa are functions of (es, Ωm).
Numerical fitting yields
![Page 12: Parameterizing Dark Energy Z. Huang, R. J. Bond, L. Kofman Canadian Institute of Theoretical Astrophysics](https://reader038.vdocument.in/reader038/viewer/2022110206/56649d1a5503460f949ef190/html5/thumbnails/12.jpg)
binned SNe samples (192 samples)
Some w0-wa mimic cosmological constant
![Page 13: Parameterizing Dark Energy Z. Huang, R. J. Bond, L. Kofman Canadian Institute of Theoretical Astrophysics](https://reader038.vdocument.in/reader038/viewer/2022110206/56649d1a5503460f949ef190/html5/thumbnails/13.jpg)
2-parameter parametrization• Assumption: slow-roll at 0<z<2 (with possible non-damped
velocity).
Hubble damping termCMB + SN + LSS + WL +
Lya
![Page 14: Parameterizing Dark Energy Z. Huang, R. J. Bond, L. Kofman Canadian Institute of Theoretical Astrophysics](https://reader038.vdocument.in/reader038/viewer/2022110206/56649d1a5503460f949ef190/html5/thumbnails/14.jpg)
2-parameter parametrization - residual velocity at low redshift.
![Page 15: Parameterizing Dark Energy Z. Huang, R. J. Bond, L. Kofman Canadian Institute of Theoretical Astrophysics](https://reader038.vdocument.in/reader038/viewer/2022110206/56649d1a5503460f949ef190/html5/thumbnails/15.jpg)
3-parameter parametrizationIn general eV varies. Assuming no oscillation , we model
Other corrections can only be numerically fitted:
•redefine aeq.
•O(θ3) term numerical fitting.
•as- es power suppression (if es and as are both large, the power of Hubble damping term would be suppressed).
When all smoke clears
![Page 16: Parameterizing Dark Energy Z. Huang, R. J. Bond, L. Kofman Canadian Institute of Theoretical Astrophysics](https://reader038.vdocument.in/reader038/viewer/2022110206/56649d1a5503460f949ef190/html5/thumbnails/16.jpg)
3-parameter parametrization
![Page 17: Parameterizing Dark Energy Z. Huang, R. J. Bond, L. Kofman Canadian Institute of Theoretical Astrophysics](https://reader038.vdocument.in/reader038/viewer/2022110206/56649d1a5503460f949ef190/html5/thumbnails/17.jpg)
3-parameter fitting
• Perfectly fits slow-to-moderate roll.
![Page 18: Parameterizing Dark Energy Z. Huang, R. J. Bond, L. Kofman Canadian Institute of Theoretical Astrophysics](https://reader038.vdocument.in/reader038/viewer/2022110206/56649d1a5503460f949ef190/html5/thumbnails/18.jpg)
Fit wild rising trajectories
![Page 19: Parameterizing Dark Energy Z. Huang, R. J. Bond, L. Kofman Canadian Institute of Theoretical Astrophysics](https://reader038.vdocument.in/reader038/viewer/2022110206/56649d1a5503460f949ef190/html5/thumbnails/19.jpg)
Measuring 3 parameters• Use 3-parameter for 0<z<4. Assume w(z>4)=wh
(free parameter).
![Page 20: Parameterizing Dark Energy Z. Huang, R. J. Bond, L. Kofman Canadian Institute of Theoretical Astrophysics](https://reader038.vdocument.in/reader038/viewer/2022110206/56649d1a5503460f949ef190/html5/thumbnails/20.jpg)
Comparing 1-2-3-parameter1-parameter: use 1-param formula for all redshift.
2-parameter: use 2-param formula for 0<z<2, assuming w(z>2)=wh (free constant).
3-parameter: use 3-param formula for 0<z<4, assuming w(z>4)=wh (free constant).
Conclusion: all the complications are irrelevant, now only can measure es
CMB + SN + WL + LSS +Lya
![Page 21: Parameterizing Dark Energy Z. Huang, R. J. Bond, L. Kofman Canadian Institute of Theoretical Astrophysics](https://reader038.vdocument.in/reader038/viewer/2022110206/56649d1a5503460f949ef190/html5/thumbnails/21.jpg)
Forecast: Planck + JDEM SN + DUNE WL
![Page 22: Parameterizing Dark Energy Z. Huang, R. J. Bond, L. Kofman Canadian Institute of Theoretical Astrophysics](https://reader038.vdocument.in/reader038/viewer/2022110206/56649d1a5503460f949ef190/html5/thumbnails/22.jpg)
Thawing, freezing or non-monotonic?
• Thawing: w monotonically deviate from -1.• Freezing: w monotonically approaches -1.• Our parameterization with flat priors. Roughly 15 percent thawing, 8 percent
freezing, most are non-monotonic.
With freezing prior:
With thawing prior:
![Page 23: Parameterizing Dark Energy Z. Huang, R. J. Bond, L. Kofman Canadian Institute of Theoretical Astrophysics](https://reader038.vdocument.in/reader038/viewer/2022110206/56649d1a5503460f949ef190/html5/thumbnails/23.jpg)
Conclusions
For a wide class of quintessence/phantom models, the functional form V(φ) in the near future is observationally immeasurable. Only a key trajectory parameter es = (1/16πG) <(V’/V)2> can be well measured.
The second parameter as can only be constrained to be less than ~0.3.
For current observational data, even with (physically motivated) dynamic w(a) parametrization, cosmological constant remains to be the best and simplest model.