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The CMB and the SZ Effect Current Topics 2008 Dr. Katy Lancaster.

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Presentation on theme: "The CMB and the SZ Effect Current Topics 2008 Dr. Katy Lancaster."— Presentation transcript:

1 The CMB and the SZ Effect Current Topics 2008 Dr. Katy Lancaster

2 Course Content Introduction - The Cosmic Microwave Background - The Sunyaev Zeldovich Effect Science from the SZ effect - The Hubble constant - Gas fractions - Number counts Practicalities - Telescopes - Issues

3 Lecture 1 A brief history Production of the CMB Production of primary anisotropies The Sunyaev Zeldovich effect

4 Brief history lesson 1950s, two conflicting cosmological theories Steady State theory Universe always has been and always will be in a static, homogenous state. Expanding Universe Hubbles observations, 1929 Gamov - realised that the Universe was once extremely dense and hot, thus must have since expanded and cooled

5 Penzias and Wilson 1965, were making sensitive observations of microwave emission from the galaxy Detect annoying level of static in all directions At the same time, Dicke at Princeton predicted the existence of relic radiation from the Big Bang Nobel Prize, 1978

6 COBE NASA satellite launched late 80s Cosmic Microwave Background radiation was found to have a perfect blackbody spectrum Implies Universe was once isothermal. Only Big Bang models predict this. For this (and other reasons), the COBE scientists won the Nobel prize in 2007

7 Primordial Universe Early Universe: Devoid of structure. T > 4000K, entirely ionised - sea of electrons, protons, helium nuclei and photons Too hot for atoms to form Photons repeatedly Thomson scatter from electrons, unable to propagate freely Almost perfect thermal equilibrium due to the coupling of matter and radiation Predicted and required by Big Bang models Universe is opaque

8 Thermalisation As COBE discovered, the CMB has a perfect blackbody spectrum. Two contributory processes during the first year after the Big Bang, each creates/destroys photons: At very early times, thermal Bremstrahlung radiation / absorption: e+p e+p+. This ceased as the Universe cooled. Produces thermal spectrum Later, double Compton scattering: e+ e+2. Only effective while collision rate > expansion rate Since then there has been no process capable of destroying the spectrum (although there may be tiny distortions)

9 Recombination Early Universe filled with free electrons, photon mean- free path small (Universe in thermal equilbrium, opaque) Impossible for any information about this time to be communicated to us via radiation Temperature of Universe falls to ~4000K, very few photons with energy > Hydrogen binding energy, 13.6eV Electrons and protons combine: e+p H+ Vast majority of free electrons disappear. Universe now neutral, photons can free-stream In fact recombination happens over a time or redshift slice (1500 > z > 1200 ) rather than instantaneously.

10 Surface of last scattering The CMB photons were emitted at the same time, and thus underwent their final scattering event at the same time All CMB photons move at the speed of light, have travelled the same distance since this time We can think of the CMB as being emitted from a fictitious spherical surface, of which we are at the centre Like observing the surface of the sun, although it is the outer reaches (or rather, the very early Universe) that we can not observe, rather than the inner workings Strictly speaking, recombination is not instantaneous, so we sometimes talk about the thickness of the surface

11 Surface of last scattering

12 The CMB today The CMB photons have been significantly redshifted by the Hubble expansion. Photon wavelengths have increased by R(t)=1/(1+z) CMB temperature falls as 1/R(t): a specific prediction of the Big Bang model Temperature of the CMB today T 0 = T/(1+z) = 2.73K Can test the relation at other redshifts by observing stellar line emission from CN molecules Actually first measured in circa 1940 but not identified as the CMB until much later!

13 Observing the CMB Uniform high energy glow - the sky is not dark at radio frequencies

14 The Dipole Doppler shift introduces hot and cold regions The Local group is moving at 400km/s relative to the CMB! Also see annual modulation due to Earths orbit

15 Primary Fluctuations The CMB appears isotropic (same temperature everywhere) unless we look very carefully Initial isotropy actually slightly distorted during / before recombination We observe temperature variations, referred to as primordial anisotropies or fluctuations (see pic) We measure the temperature difference in two directions separated by some angle. Take many measurements and find the mean value for a particular angular scale All CMB anisotropies are characterised in this way

16 WMAP, monopole, dipole and galactic emission removed K in the presence of 3K background

17 Primary Fluctuations The CMB appears isotropic (same temperature everywhere) unless we look very carefully Initial isotropy actually slightly distorted during / before recombination We observe temperature variations, referred to as primordial anisotropies or fluctuations (see pic) We measure the temperature difference in two directions separated by some angle. Take many measurements and find the mean value for a particular angular scale All CMB anisotropies are characterised in this way

18 Measure size of temperature difference for a range of Plot against : Power Spectrum


20 Sources of anisotropy Sachs Wolfe Effect Acoustic Oscillations Doppler Shift Silk Damping Secondary processes

21 Sachs Wolfe Effect Quantum fluctuations in the dark matter distribution led to density inhomogeneities These developed under gravity A CMB photon released from a region with a non-zero gravitational potential will experience an additional redshift It has to climb out of the potential well This creates power on the scales > 1

22 Acoustic Oscillations Over-dense regions in dark matter amplified during inflation, collapse under gravity Baryons falls into the resulting potential wells Radiation pressure increases as the material collapses Eventually the pressure overcomes gravity and causes an expansion…. …..expansion continues until gravity wins again

23 Acoustic Oscillations This was taking place at recombination Oscillations were happening on all scales. Largest scale: sound horizon. Other scales were not causally connected. Modes which had reached their extrema by recombination produced enhanced features in the CMB Compressions - hot spots. (Recombined slightly later, thus suffered less cosmological redshifting) Rarefactions - cold spots. (Recombined slightly earlier)

24 Acoustic Oscillations Oscillating modes form harmonic sequence: Largest regions had diameter of the sound horizon, next largest were half this size etc Oscillation frequencies corresponded to this: largest region oscillates at half the speed of the next largest etc First peak: region which had time to compress exactly once before recombination Second peak: region which had time to compress and rarefy, ie one full oscillation before recombining Third peak, fourth peak….

25 Doppler shifts Also related to the acoustic oscillations At times inbetween the extrema of expansion for each oscillation region, the motion of the fluid reached its maximum velocity This resulted in a Doppler shift of the photons released when the plasma recombined This contriubutes power inbetween the locations of the acoustic peaks: the power spectrum does not go to zero

26 Silk Damping On the smallest scales, the effect of photons escaping from the oscillating region becomes important The loss of these photons damps the power on the smallest angular scales

27 What can we learn? The power spectrum is a complicated function which depends on the values of the various cosmological parameters: H 0, M, b,, k, z re, t 0 ….and many more. We observe the CMB and then try fitting the powere spectrum to the data. We tweak the parameters to find the best fit. And hey presto, we have our very own measurement of the cosmological model

28 What can we learn?

29 Galaxy formation The anisotropies in the CMB are widely regarded as imprints of the seeds of structure formation That is, those oscillating regions from the early Universe grew and developed under gravity into the stars and galaxies we see today If we take the CMB and compare it to observations of large scale structure, we can constrain structure formation scenarios


31 Secondary Anisotropies Majority of CMB photons have travelled through the unimpeded since last scattering - Hence observed power spectrum Some have interacted with ionised matter on their path towards us This imprints structures on the observable CMB - Secondary Anisotropies - Also contribute to the power spectrum

32 Sources of anisotropy Integrated Sachs-Wolfe effect Gravitational lensing Rees-Sciama effect Ostriker-Vishniac effect Cosmic strings Sunyaev Zeldovich effect - by far the largest Many more postulated…..


34 Rich Clusters - congregations of hundreds or even thousands of galaxies See cluster galaxies and lensing arcs in the optical But only around 5% of a clusters mass is in galaxies Most of the mass is in Dark Matter But a sizable fraction is found in baryonic gas Galaxy Clusters

35 X-rays - see hot gas via Bremstrahlung emission 10-30% of total mass Chandra Image of the Coma cluster

36 Cluster Gas Clusters of galaxies have masses ~ 3x10 14 M Deep potential wells, gas temperatures ~7keV Ionised and energetic Constitutes ~30% of the cluster mass Gas characteristics may reflect those of the Universe as a whole - interesting to study

37 Compton Scattering Compton scattering: Photon loses energy on interacting with matter Inverse Comptin scattering: Photon gains energy on interacting with matter In the SZ effect: low energy CMB photon scatters from high energy cluster electron Photon energy is boosted

38 SZ Effect basics CMB photons incident on a galaxy cluster Scattering probability is small Those which do collide receive energy boost due to inverse Compton scattering Spectrum shifted to higher frequency Decrement - null - increment

39 Optical Depth For a cluster atmosphere with electron density n e (r), the optical depth for scattering along a particular line of sight is: Where T is the Thomson cross section The cluster gas is optically thin e <<1, ie the probability of scattering is small

40 Comptonisation The degree to which the CMB is affected by inverse Compton scattering is described by the Comptonisation parameter: Or for the isothermal approximation (often employed in the past):

41 Brightness Temperature Often used in Radio / CMB astronomy Defined as: The temperature of a blackbody that would be observed with the same intensity as the observed source, at a particular frequency From the Planck law: For the low frequency Rayleigh-Jeans region:

42 Temperature Decrement The change in the brightness temperature of the CMB due to the thermal SZ effect is given by: Where the frequency dependence is given by: For the Rayleigh Jeans region:

43 Intensity Change In units of specific intensity: With frequency dependence given by:


45 Kinematic SZ Effect Additional spectral distortion caused by cluster velocity component along line of sight, z Collective motion of cluster gas modifies CMB spectrum via Doppler shift Observe decrement: Frequency dependence:

46 SZ Intensity Spectra g(x), h(x) Thermal: decrement, null, increment Kinematic: Near maximum at the thermal null

47 Thermal vs Kinematic Specific intensity changes: Spectral dependence similar at low freq. i.e for a typical cluster: The KSZ effect is < 10% of the thermal effect at low freq.

48 Decrement - Null - Increment ACBAR produced these nice images of a galaxy cluster at 150, 220 and 275 GHz Multi-frequency observations useful for eliminating primordial CMB contamination (as well as detecting the kinematic effect)

49 Summary 1 CMB - blackbody spectrum, primordial features Fit power spectrum to deduce values of the cosmological parameters CMB photons incident on a galaxy cluster may be inverse Compton scattered by hot gas This Sunyaev Zeldovich Effect manifests itself as a decrement - null - increment depending on observing frequency Cluster peculiar velocity also modifies the radiation via the smaller Kinematic effect

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