CMB Cosmological Parameter Extraction

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Trajectories 05.11.16
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Bond, Contaldi, Frolov, Kofman, Souradeep,
Vaudrevange 05
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Potential of the Hybrid D3/D7 Inflation Model
String Theory Landscape Inflation
Phenomenology for CMBLSS
running index as simplest breaking, radically
broken scale invariance, 2-field inflation,
isocurvatures, Cosmic strings/defects,
compactification topology, other baroque
add-ons. subdominant String/Mtheory-motivated,
extra dimensions, brane-ology, reflowering of
inflaton/isocon models (includes curvaton),
modified kinetic energies, k-essence,
Dirac-Born-Infeld sqrt(1-momentum2), DBI in
the Sky Silverstein etal 2004, etc.
KKLT, KKLMMT
any acceleration trajectory will do?? q (ln
Ha) H(ln a,) V(phi,) Measure?? anti-baroque
prior
14 std inflation parameters
many many more e.g. blind search for patterns
in the primordial power spectrum
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Beyond P(k) Inflationary trajectories
Peiris et al. 2003
Bond, Contaldi, Frolov, Kofman, Souradeep,
Vaudrevange 05
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HJ expand about uniform acceleration, 1q, V
and power spectra are derived
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Trajectories cf. WMAP1B03CBIDASIVSAAcbarMaxi
ma SDSS 2dF Chebyshev 7 10 H(N) and RG Flow
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10
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H (ln Ha) / (10-5 mP) inflation trajectory
reconstructed from CMBLSS data using Chebyshev
expansion (order 10) MCMC.
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Ps,t (ln k) / (10-10) reconstructed from CMBLSS
data using dual Chebyshev expansions (order 15
scalar 5 tensor) and Markov Chain Monte Carlo
methods. best-fit mean-fit. No S/T generalized
consistency relation is imposed. Probe of
CMBLSS window only 10 e-folds.
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H (ln a) / (10-5 mP) inflation trajectory
reconstructed from CMBLSS data using Chebyshev
expansion (order 10) MCMC. Derived scalar and
tensor power spectra Ps,t (ln k) / (10-10)
(generalized consistency relation built in) and
derived potential V
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H (ln a) / (10-5 mP) vs ln H (ln a) / (10-5 mP)
inflation trajectory reconstructed from CMBLSS
data using Chebyshev expansion (order 10) MCMC.
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H (ln a) / (10-5 mP) inflation trajectory
reconstructed from CMBLSS data using Chebyshev
expansion (order 10 cf. order 5) MCMC.
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Forecasts of how ln H(ln Ha) Chebyshev expansions
will do with Planck 2.5 year and other CMB
datasets using order 10 as an example
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CL for H (ln Ha) best-fit inflation trajectory
reconstructed from CMBLSS data using Chebyshev
expansion (order 10) MCMC cf. dual Chebyshev
expansion of scalar (15) tensor (5) power
spectra, unconstrained by T/S consistency /
inflation
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Forecasts of how ln H(ln Ha) Chebyshev expansions
will do with Planck 2.5 year datasets using order
10 as an example cheb used instead of A_s, r_ts,
alpha_s, n_s to describe the inflation dynamics
for planck2.5yr 100 and 143 GHz data, With a
chebyshev expansion of lnH to order 10, with
other cosmic parameters fixed of 10 cheb coeffs,
10 determined to 10, 5 to 1 accuracy cheb 5
cosmic params (4 abundances and the Compton
depth) of 15 all to 10, 10 to 1 (includes one
fixed) 9 cosmic params, A_s, r_ts, alpha_s, n_s
in place of the Chebyshev coefficients of 9 all
to 10, 7 to 1 result of this limited study
omb, omc, omv omnu errors are similar, tauC a
little higher. one reason is that there is not
much complexity in the cheb in the high L region
where omega_b etc are concentrated. Polarization
information helps to break degeneracies as well.
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Forecasts of how ln H(ln Ha) Chebyshev expansions
will do with Planck 2.5 year datasets using order
10 as an example a series of Delta C_L /C_L figs,
comparing simulated data with perturbed chebyshev
templates and eigentemplates for TT Fig
ch1_Planck25_jan04_cosmicvar magenta error bars
are for planck. act and spt will improve the high
L end as well. dashed blue - curves, the higher
shows the cosmic variance limit for each
multipole, using fsky0.9, as was used for
planck. the lower one shows cosmic variance if
the data is banded into log spacings with Delta
ln L 0.1. black error bars are jan04 data, so
not including boomerang03, new acbar or combined
CBI TT. dashed black line best fit to jan04
data relative to lnH10g best fit (which does not
have as much freedom at the high L end because
thecosmic params were fixed)
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Forecasts of how ln H(ln Ha) Chebyshev expansions
will do with Planck 2.5 year datasets using order
10 as an example a series of Delta C_L /C_L figs,
comparing simulated data with perturbed chebyshev
templates and eigentemplates for TT Fig
ch1_Planck25_cl5chmodes CL first 5 templates for
the 10 chebyshevs shows that there is not that
much complexity in 1 to 5, more for 6 to 10.
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Forecasts of how ln H(ln Ha) Chebyshev expansions
will do with Planck 2.5 year datasets using order
10 as an example a series of Delta C_L /C_L figs,
comparing simulated data with perturbed chebyshev
templates and eigentemplates for TT Fig
ch1_Planck25_cl10chemodes CL top 5 eigentemplates
for the lnH10 expansion for chebyshev only, with
other cosmic parameters fixed top 5 eigenmodes in
CL. the sign of the template patterns is
arbitrary. the value of the eigenmode would be
determined by shifting the amplitude of the curve
until it fits the data. the templates have been
scaled so as to be visible on the figure. some CL
modes have been scaled more than others.
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Forecasts of how ln H(ln Ha) Chebyshev expansions
will do with Planck 2.5 year datasets using order
10 as an example a series of Delta C_L /C_L figs,
comparing simulated data with perturbed chebyshev
templates and eigentemplates for
TT Figch1_Planck25_cl10ch6paremodes top 5
eigentemplates for the lnH10 expansion for
chebyshev 6 parameters, one of which (omega_k)
is frozen (to zero) Baryonic acoustic
oscillations appear in some of the modes
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Forecasts of how ln H(ln Ha) Chebyshev expansions
will do with Planck 2.5 year datasets using order
10 as an example a series of Delta C_L /C_L figs,
comparing simulated data with perturbed chebyshev
templates and eigentemplates for TT Fig
ch1_Planck25_cl16paremodes CL top 5
eigentemplates for 10 std cosmo parameters, the
usual 6 plus A_s, n_s, alpha_s, r_ts (omega_k is
frozen to zero)
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Degeneracy of the Potential Reconstruction