High-redshift 21cm and redshift distortions

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High-redshift 21cm and redshift distortions

• Antony Lewis
• Institute of Astronomy, Cambridge
• http//cosmologist.info/

Work with
Anthony Challinor (IoA, DAMTP)
astro-ph/0702600Richard Shaw (IoA),
arXiv0808.1724
Following work by Scott, Rees, Zaldarriaga, Loeb,
Barkana, Bharadwaj, Naoz, Scoccimarro many more

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Evolution of the universe
Opaque
Easy
Transparent
Dark ages
Hard
30ltzlt1000
Hu White, Sci. Am., 290 44 (2004)
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CMB temperature
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Why the CMB temperature (and polarization) is
great

• Probes scalar, vector and tensor mode
  perturbations
• The earliest possible observation (bar future
  neutrino anisotropy surveys etc)- Includes
  super-horizon scales, probing the largest
  observable perturbations- Observable now

Why it is bad
- Only one sky, so cosmic variance limited on
large scales - Diffusion damping and
line-of-sight averaging all information on
small scales destroyed! (lgt2500)- Only a 2D
surface (reionization), no 3D information
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If only we could observe the CDM perturbations
- not erased by diffusion damping (if cold)
power on all scales - full 3D distribution of
perturbations
What about the baryons?

• fall into CDM potential wells also power on
  small scales
• full 3D distribution
• but baryon pressure non-zero very small scales
  still erased

How does the information content compare with the
CMB?
CMB temperature, 1ltllt2000 - about 106 modes
- can measure Pk to about 0.1 at l2000 (k Mpc
0.1) Dark age baryons at one redshift, 1lt l lt
106 - about 1012 modes - measure Pk to about
0.0001 at l106 (k Mpc 100)
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What about different redshifts?

• About 104 independent redshift shells at l106
• - total of 1016 modes - measure Pk to an
  error of 10-8 at 0.05 Mpc scales

e.g. running of spectral index If ns 0.96
maybe expect running (1-ns)2 10-3Expected
change in Pk 10-3 per log k - measure
running to 5 significant figures!?
So worth thinking about can we observe the
baryons somehow?
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• How can light interact with the baryons (mostly
  neutral H He)?

- after recombination, Hydrogen atoms in ground
state and CMB photons have h? ltlt Lyman-alpha
frequency high-frequency tail of CMB
spectrum exponentially suppressed
essentially no Lyman-alpha interactions
atoms in ground state no higher level
transitions either
- Need transition at much lower energy
Essentially only candidate for hydrogen is the
hyperfine spin-flip transition
triplet
singlet
Credit Sigurdson
Define spin temperature Ts
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What can we observe?
Spontaneous emission n1 A10 photons per unit
volume per unit proper time
1
h v E21
Rate A10 2.869x10-15 /s
0
Stimulated emission net photons (n1 B10 n0
B01)Iv
Total net number of photons
In terms of spin temperature
Net emission or absorption if levels not in
equilibrium with photon distribution - observe
baryons in 21cm emission or absorption if Ts ltgt
TCMB
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What determines the spin temperature?

• Interaction with CMB photons drives Ts towards
  TCMB
• Collisions between atoms drives Ts towards gas
  temperature Tg

TCMB 2.726K/a
At recombination, Compton scattering makes
TgTCMBLater, once few free electrons, gas
cools Tg mv2/kB 1/a2
Spin temperature driven below TCMB by
collisions - atoms have net absorption of 21cm
CMB photons

• (Interaction with Lyman-alpha photons - not
  important during dark ages)

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Whats the power spectrum?
Use Boltzmann equation for change in CMB due to
21cm absorption
Background
Perturbation
l gt1 anisotropies in TCMB
Fluctuation in density of H atoms, fluctuations
in spin temperature
Doppler shiftto gas rest frame
CMB dipole seen by H atomsmore absorption in
direction of gas motion relative to CMB
reionization re-scattering terms
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Solve Boltzmann equation in Newtonian gauge
Redshift distortions
Main monopolesource
Effect of localCMB anisotropy
Sachs-Wolfe, Doppler and ISW change to redshift
Tiny Reionization sources
For k gtgt aH good approximation is
(re-scattering effects)
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21cm does indeed track baryons when Ts lt TCMB
z50
Kleban et al. hep-th/0703215
So can indirectly observe baryon power spectrum
at 30lt z lt 100-1000 via 21cm
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Observable angular power spectrum
Integrate over window in frequency
Small scales
1/vN suppressionwithin window
White noisefrom smaller scales
Baryonpressuresupport
baryon oscillations
z50
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What about large scales (Ha gt k)?
Narrow redshift window
lt 1 effect at llt50
Extra terms largely negligible
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New large scaleinformation?- potentials
etccorrelated with CMB
Dark ages2500Mpc
l 10
14 000 Mpc
z30
Opaque ages 300Mpc
Comoving distance
z1000
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Non-linear evolution
Small scales see build up of power from many
larger scale modes - important
But probably accurately modelled by 3rd order
perturbation theory
On small scales non-linear effects many percent
even at z 50
redshift distortions, see later.
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Also lensing
Modified Bessel function
Unlensed
Lensed
Wigner functions
Lensing potential power spectrum
Lewis, Challinor astro-ph/0601594
c.f. Madel Zaldarriaga astro-ph/0512218
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like convolution with deflection angle power
spectrumgenerally small effect as 21cm spectrum
quite smooth
Cl(z50,z52)
Cl(z50,z50)
Lots of information in 3-D (Zahn Zaldarriaga
2006)
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Observational prospects

• No time soon

- (1z)21cm wavelengths 10 meters for z50-
atmosphere opaque for zgt 70 go to the moon?-
fluctuations in ionosphere phase errors go to
moon?- interferences with terrestrial radio
far side of the moon?- foregrounds large! use
signal decorrelation with frequency
But large wavelength -gt crude reflectors OK
See e.g. Carilli et al astro-ph/0702070,
Peterson et al astro-ph/0606104
Current 21cm
LOFAR, PAST, MWA study reionization at z
lt20SKA still being planned, zlt 25
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Things you could do with precision dark age 21cm

• High-precision on small-scale primordial power
  spectrum(ns, running, features wide range of
  k, etc.)e.g. Loeb Zaldarriaga
  astro-ph/0312134, Kleban et al. hep-th/0703215
• Varying alpha A10 a13 (21cm frequency
  changed different background and
  perturbations)Khatri Wandelt astro-ph/0701752
• Isocurvature modes(direct signature of baryons
  distinguish CDM/baryon isocurvature)Barkana
  Loeb astro-ph/0502083
• CDM particle decays and annihilations(changes
  temperature evolution)Shchekinov Vasiliev
  astro-ph/0604231, Valdes et al astro-ph/0701301
• Primordial non-Gaussianity(measure bispectrum
  etc of 21cm limited by non-linear
  evolution)Cooray astro-ph/0610257, Pillepich et
  al astro-ph/0611126
• Lots of other things e.g. cosmic strings, warm
  dark matter, neutrino masses, early dark
  energy/modified gravity.

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Back to reality after the dark ages?

• First stars and other objects form
• Lyman-alpha and ionizing radiation
  presentWouthuysen-Field (WF) effect -
  Lyman-alpha couples Ts to Tg - Photoheating
  makes gas hot at late times so signal in
  emissionIonizing radiation - ionized regions
  have little hydrogen regions with no 21cm
  signal Both highly non-linear very complicated
  physics
• Lower redshift, so less long wavelengths- much
  easier to observe! GMRT (zlt10), MWA, LOFAR
  (zlt20), SKA (zlt25).
• Discrete sources lensing, galaxy counts (109 in
  SKA), etc.

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How do we get cosmology from this mess?
Would like to measure dark-matter power on
nearly-linear scales. Want to observe potentials
not baryons
1. Do gravitational lensing measure source
shears - probes line-of-sight transverse
potential gradients (independently of what
the sources are)
2. Measure the velocities induced by falling into
potentials - probe line-of-sight velocity,
depends on line-of-sight potential gradients
Redshift distortions
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A closer look at redshift distortions
Real space
Redshift space
y(z)
y
x
x
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Density perturbed too. In redshift-space see

Both linear (higher) effects same order of
magnitude. Note correlated.
More power in line-of-sight direction -gt
distinguish velocity effect
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n
Linear-theory
Redshift-space distance
Actual distance
Define 3D redshift-space co-ordinate
Transform using Jacobian Redshift-space
perturbation
Fourier transformed
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Linear power spectrum
Messy astrophysics
Depends only on velocities -gt potentials
(n.k)4 component can be used for cosmology
Barkana Loeb astro-ph/0409572
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Is linear-theory good enough?
RMS velocity 10-4-10-3
Radial displacement 0.1-1 MPc
Megaparsec scale
Redshift space
Real Space
Looks like big non-linear effect!
M(x dx) ? M(x) M(x) dx
BUT bulk displacements unobservable. Need more
detailed calculation.
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Non-linear redshift distortions
Shaw Lewis, 2008 also Scoccimarro 2004
Assume all fields Gaussian.
Power spectrum from
Exact non-linear result (for Gaussian fields on
flat sky)
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Significant effectDepending on angle
Small scale power boosted by superposition of
lots oflarge-scale modes
z10
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More important at lower redshift.Not negligible
even at high z.
Comparable to non-linear evolution
z10
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Similar effect on angular power spectrum
(A velocity covariance), u (x-z,y-z)
(sharp zz window, z10)
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What does this mean for component separation?
Angular dependence now more complicated all µ
powers, and not clean.
Assuming
gives wrong answer
z10
Need more sophisticated separation methods to
measure small scales.
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Also complicates non-Gaussianity
detectionRedshift-distortion bispectrum

• Mapping redshift space -gt real space nonlinear,
  so non-Gaussian

Linear-theory source
Just lots of Gaussian integrals (approximating
sources as Gaussian)..
Zero if all k orthogonal to line of sight.
Can do exactly, or leading terms are
Also Scoccimarro et al 1998, Hivon et al 1995
Not attempted numerics as yet
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Conclusions

• Huge amount of information in dark age
  perturbation spectrum- could constrain early
  universe parameters to many significant figures
• Dark age baryon perturbations in principle
  observable at 30ltzlt 500 up to llt107 via
  observations of CMB at (1z)21cm wavelengths.
• Dark ages very challenging to observe (e.g. far
  side of the moon)
• Easier to observe at lower z, but complicated
  astrophysics
• Redshift-distortions probe matter density
  ideally measure cosmology separately from
  astrophysics by using angular dependence
• BUT non-linear effects important on small
  scales - more sophisticated non-linear
  separation methods may be required

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Correlation function
z10