Cosmología de precisión, observables cosmológicos.

1. CMBPol
Detectando in
acion con las
Polarizaciones de la RCF
Yohana Bonilla
Profesor:
Cesar A. Valenzuela Toledo
Universidad del Valle
Jun/19/2011
Y. Bonilla (UniValle) CMBPol Jun/19/2011 1 / 14

2. Contenido
1 Cosmologa de precision
Introduccion
Y. Bonilla (UniValle) CMBPol Jun/19/2011 2 / 14

3. Contenido
1 Cosmologa de precision
Introduccion
2 Observables cosmologicos
Cosmologa de concordancia
Y. Bonilla (UniValle) CMBPol Jun/19/2011 2 / 14

4. Contenido
1 Cosmologa de precision
Introduccion
2 Observables cosmologicos
Cosmologa de concordancia
3 Cosmologa in
acionaria
In
acion-Big Bang
La fsica de la in
acion
Observables cosmologicos
Perturbaciones escalares
Perturbaciones vectoriales
Perturbaciones tensoriales
Y. Bonilla (UniValle) CMBPol Jun/19/2011 2 / 14

5. Contenido
1 Cosmologa de precision
Introduccion
2 Observables cosmologicos
Cosmologa de concordancia
3 Cosmologa in
acionaria
In
acion-Big Bang
La fsica de la in
acion
Observables cosmologicos
Perturbaciones escalares
Perturbaciones vectoriales
Perturbaciones tensoriales
4 Polarizaciones de la RCF: Prueba unica del Universo Temprano
Y. Bonilla (UniValle) CMBPol Jun/19/2011 2 / 14

6. Cosmologa de precision Introduccion
Introduccion
Y. Bonilla (UniValle) CMBPol Jun/19/2011 3 / 14

7. Observables cosmologicos Cosmologa de concordancia
Cosmologa de concordancia
Conjunto mnimo de parametros cuyos valores medidos caracterizan el
universo observado.
Y. Bonilla (UniValle) CMBPol Jun/19/2011 4 / 14

8. Observables cosmologicos Cosmologa de concordancia
Cosmologa de concordancia
Conjunto mnimo de parametros cuyos valores medidos caracterizan el
universo observado.
Modelo de seis parametros
? f
b;
CDM; h; g: fondo homogeneo.
Y. Bonilla (UniValle) CMBPol Jun/19/2011 4 / 14

9. Observables cosmologicos Cosmologa de concordancia
Cosmologa de concordancia
Conjunto mnimo de parametros cuyos valores medidos caracterizan el
universo observado.
Modelo de seis parametros
? f
b;
CDM; h; g: fondo homogeneo.
? fAs; nsg:
uctuaciones de densidad primordiales
Y. Bonilla (UniValle) CMBPol Jun/19/2011 4 / 14

10. Observables cosmologicos Cosmologa de concordancia
Figura: Parametros del modelo de la cosmologa de concordancia. Asumimos un universo plano
i.e.
b +
CDM +
1; en caso contrario se incluye la contribucion de curvatura
k. h describe la velocidad de
expansion del universo actual, H0 = 100 h km s1 Mpc1. Espectro se re

11. ere a las perturbaciones de densidad o escalares
primordiales, parametrizadas por As(k=k?)ns1, donde k? = 0;002Mpc1 es una escala espec

12. ca.
Y. Bonilla (UniValle) CMBPol Jun/19/2011 5 / 14

13. Observables cosmologicos Cosmologa de concordancia
Label De

14. nition Physical Origin
k Curvature Initial Conditions
m Neutrino Mass Beyond-SM Physics
w Dark Energy Equation of State Unknown
N Neutrino-like Species Beyond-SM Physics
YHe Helium Fraction Nucleosynthesis
s Scalar Running In
ation
At Tensor Amplitude In
ation
nt Tensor Index In
ation
fNL Non-Gaussianity In
ation (?)
S Isocurvature In
ation
G Topological Defects Phase Transition
Cuadro: Parameters in possible future concordance cosmologies are summarized. At present, these numbers are all either
consistent with zero (or 1 in the case of w), or are

15. xed independently of a

16. t to the global cosmological dataset, in the case
of the helium fraction and the number of neutrino species. The tensor or gravitational wave spectrum is conventionally taken to
be of the form At(k=k?)nt . One could extend the parameterization of the dark energy to include a non-trivial equation of
state (w0), while the parameterization of the scalar spectrum could incorporate more general scale-dependence, such as
features in the spectrum. Likewise, fNL is a placeholder for measurements of generic non-Gaussianity (see x??) and the
parameter S quanti

17. es the amplitude of an isocurvature contribution to the scalar spectrum (see x??).
Y. Bonilla (UniValle) CMBPol Jun/19/2011 6 / 14

18. Observables cosmologicos Cosmologa de concordancia
Label De

19. nition Physical Origin Current Status As Scalar Amplitude V; V 0 (2;445 0;096) 109 ns Scalar Index V 0; V 00 0;960 0;013 s Scalar Running V 0; V 00; V 000 only upper limits At Tensor Amplitude V (Energy Scale) only upper limits nt Tensor Index V 0 only upper limits r Tensor-to-Scalar Ratio V 0 only upper limits
k Curvature Initial Conditions only upper limits fNL Non-Gaussianity Non-Slow-Roll, Multi-Field only upper limits S Isocurvature Multi-Field only upper limits G Topological Defects End of In
ation only upper limits Cuadro: The in
ationary parameter space, i.e. the set of cosmological
observables which are directly associated with in
ation. Under physical originV ,
V 0, etc. refer to the derivative(s) of the potential to which this variable is most
sensitive. A detailed discussion of the connection between in
ationary physics and
the corresponding observable can be found in the listed subsections.
Y. Bonilla (UniValle) CMBPol Jun/19/2011 7 / 14

20. Cosmologa in
acionaria In
acion-Big Bang
In
acion como una solucion a los problemas del
Big-Bang
1 Problema de las reliquias no deseadas.
Y. Bonilla (UniValle) CMBPol Jun/19/2011 8 / 14

21. Cosmologa in
acionaria In
acion-Big Bang
In
acion como una solucion a los problemas del
Big-Bang
1 Problema de las reliquias no deseadas.
2 Problema de planitud.
Y. Bonilla (UniValle) CMBPol Jun/19/2011 8 / 14

22. Cosmologa in
acionaria In
acion-Big Bang
In
acion como una solucion a los problemas del
Big-Bang
1 Problema de las reliquias no deseadas.
2 Problema de planitud.
3 El problema de horizonte.
Y. Bonilla (UniValle) CMBPol Jun/19/2011 8 / 14

23. Cosmologa in
acionaria Fsica de la in
acion
La fsica de la in
acion
Que controla la expansion acelerada del Universo temprano?
1For simplicity, we anticipate the in
ationary solution of the
atness problem and
assume that the spatial geometry is
at. The generalization to curved space is
straightforward.
Y. Bonilla (UniValle) CMBPol Jun/19/2011 9 / 14

24. Cosmologa in
acionaria Fsica de la in
acion
La fsica de la in
acion
Que controla la expansion acelerada del Universo temprano?
Ecuaciones de Friedmann, factor de escala a(t)
1For simplicity, we anticipate the in
ationary solution of the
atness problem and
assume that the spatial geometry is
at. The generalization to curved space is
straightforward.
Y. Bonilla (UniValle) CMBPol Jun/19/2011 9 / 14

25. Cosmologa in
acionaria Fsica de la in
acion
La fsica de la in
acion
Que controla la expansion acelerada del Universo temprano?
Ecuaciones de Friedmann, factor de escala a(t)
H2 =
_a
a
2
=
1
3M2
pl
; (1)
_H
+ H2 =
a
a
=
1
6M2
pl
( + 3p) (2)
of a spatially
at universe with Friedmann-Robertson-Walker (FRW) metric1
1For simplicity, we anticipate the in
ationary solution of the
atness problem and
assume that the spatial geometry is
at. The generalization to curved space is
straightforward.
Y. Bonilla (UniValle) CMBPol Jun/19/2011 9 / 14

26. Cosmologa in
acionaria Fsica de la in
acion
La fsica de la in
acion
Que controla la expansion acelerada del Universo temprano?
Ecuaciones de Friedmann, factor de escala a(t)
H2 =
_a
a
2
=
1
3M2
pl
; (1)
_H
+ H2 =
a
a
=
1
6M2
pl
( + 3p) (2)
of a spatially
at universe with Friedmann-Robertson-Walker (FRW) metric1
ds2 = dt2 + a(t)2dx2 (3)
1For simplicity, we anticipate the in
ationary solution of the
atness problem and
assume that the spatial geometry is
at. The generalization to curved space is
straightforward.
Y. Bonilla (UniValle) CMBPol Jun/19/2011 9 / 14

27. Cosmologa in
acionaria Fsica de la in
acion
reheating
Figura: Examples of In
aton Potentials. Acceleration occurs when the potential energy of the

28. eld V dominates over its
kinetic energy 1
2
_
2. In
ation ends at end when the slow-roll conditions are violated, ! 1. CMB
uctuations are created by
quantum
uctuations about 60 e-folds before the end of in
ation. At reheating, the energy density of the in
aton is
converted into radiation.
Left: A typical small-

29. eld potential. Right: A typical large-

30. eld potential.
Y. Bonilla (UniValle) CMBPol Jun/19/2011 10 / 14

31. Cosmologa in
acionaria Observables cosmologicos
Perturbaciones escalares
Y. Bonilla (UniValle) CMBPol Jun/19/2011 11 / 14

32. Cosmologa in
acionaria Observables cosmologicos
Perturbaciones vectoriales
Y. Bonilla (UniValle) CMBPol Jun/19/2011 12 / 14

33. Cosmologa in
acionaria Observables cosmologicos
Perturbaciones tensoriales (Ondas Gravitacionales)
Y. Bonilla (UniValle) CMBPol Jun/19/2011 13 / 14

34. Polarizaciones de la RCF
Perturbaciones vectoriales
Quadrupole
Anisotropy
Thomson
Scattering
e–
Linear
Polarization
COLD
HOT
Figura: Thomson scattering of radiation with a quadrupole anisotropy generates linear polarization [?]. Red colors (thick
lines) represent hot radiation, and blue colors (thin lines) cold radiation.
Y. Bonilla (UniValle) CMBPol Jun/19/2011 14 / 14