Experimental Astroparticle Physics

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1 Experimental Astroparticle Physics WIMP Lecture UZH / ETH Zurich Spring Semester 2013

2 Organization Lectures: Fridays, 11:15 13:00 (this room) Exercises: Fridays, 14:00 15:45 (every 2nd Friday!) Slides, Information etc:

3 Lecturers Laura Baudis (044 63) UZH Y36-J-50 Adrian Biland: (044 63) ETH HPK-E24 Marc Schumann AEC Universität Bern ( ) 3837 Olaf Steinkamp: UZH Y36-J-22 (044 63)

4 Experimental Astroparticle Physics Overview and Introduction to Cosmology Experimental Astroparticle Physics, FS 2013 Marc Schumann (AEC Universität Bern)

5 What will we learn today? What is Astroparticle Physics? Cosmology in a Nutshell - the expanding Universe - the Friedmann equation relates expansion with the energy density and curvature - dark energy and high-z supernovae - the critical density and m, - analyzing the cosmic microwave background precision cosmology Literature Perkins, Particle Astrophysics, Oxford University Press, 2003 WMAP webpage:

6 Astrophysics Astrophysics deals with the physical foundations of planets, stars, galaxies, etc. and the Universe itself. It is a branch of classical Astronomy.

7 + Particle Physics Particle physics studies the elementary sub-atomic constituents of matter and Radiation and their interactions. Simulation of Higgs Detection in CMS

8 The Standard Model

9 = Astroparticle Physics Connects largest and smallest scales Idenfify the building blocks of the Universe sometimes: Particle physics without accelerator??!! sometimes: Rare event searches??!!

10 neutralino dark matter supernovae: the death of stars neutrino Poperties how do cosmic accelerators work? air shower propagation Examples taken from G. Drexlin (KIT)

11 Astroparticle Physics: Research Topics

12

13

14 Proton Stability? Baryon Number Violation? Gravitational Waves High Energy Gamma-Astronomy (charged) cosmic rays Dark Matter direct neutrino mass measurements neutrinoless double beta decay high energy neutrinos, neutrino astrophysics

15 Topics covered in this Lecture Charged cosmic rays (3) phenomenology sources detection: satellites and ground-based detectors Dark Matter (5) evidence candidates detection: direct, indirect and collider searches Neutrinos (4) phenomenology oscillations and neutrino mass experiments: solar, reactor, atmospheric, accelerator neutrinos neutrinoless double-beta decay

16 Summary: Astroparticle Physics What is the role of high-energetic processes for the development of the observed cosmic structures? study all accessible observables: gamma rays, cosmic rays, neutrinos, gravitational waves identification of dark matter, distribution? are the laws of nature valid everywhere in the Universe? What is the Universe made of? What is dark matter? Dark energy? Study matter and its interactions at smallest scales (=highest energies) Rare Decays: Proton lifetime, neutrinoless double-beta decay Studies at the highest energies ( GUT scale )

17 Bullet Cluster M. Schumann (U Zürich) Dark Matter & XENON100 17

18 The expanding Universe Hubble's original data

19 some numbers: =0.10 nm vr= 6.7 km/s =0.78 nm vr=13.6 km/s H line at 656 nm (brightest line of Balmer series, n=3 m=2, in ionized H)

20

21 SN high z

22

23 Find the Supernova...

24 Find the Supernova...

25 normalized distance modulus µ= (m-m) µ = 5 log10(r) 5 Nobel Price 2011

26 SN1997ff One of the oldest supernovae in the Universe ever found farthest distance found by HST wide-field camera (seen already by accident by IR instrument of HST before) 1 GLy away, z= Universe had only 1/3 of size as today, and less than ¼ of the present age

27 Fine tuning to the critical density

28

29 Discovery of the CMB Nobel prize 1978

30 What is the CMB?

31 CMB: The surface of last scatter

32 The WMAP Satellite Instrument: a set of passively cooled microwave WMAP is a differential experiment: radiometers with 1.4 x 1.6 m diameter primary it measures the temperature difference reflectors provide the desired angular between two points in the sky rather resolution. than measuring absolute temperatures. Temperature measurements with T/T=10--6 WMAP orbits about the Sun-Earth L2 point. very stable thermal environment 5 frequency bands from 22 to 90 GHz to near 100% observing efficiency; Sun, Earth, separate the of galactic foreground signals and Moon are always behind the from the cosmic background radiation. instrument's field of view.

33 CMB is remarkably isotropic perfect black body spectrum T/T = large dipole visible from Doppler effect since Earth is moving wrt the CMB T/T = primoridial fluctuations become visible strong signal from Milky Way

34 1996 Nobel Price J. Mather, G. Smoot Cosmology becomes a precision science

35 Analyzing the CMB n m Average sky temperature T Correlation between pairs of points of the CMB: The Pℓ(cos ) are the Legendre polynomials, running over all ℓ ℓ = ~90 ℓ = ~1 ℓ = ~

36 st CMB 1 peak and curvature Red: straight light paths to us from opposite sides of a typical hot spot in the CMB, as would be the case in a "flat" universe; Gray: curved light paths as they would appear in a universe with "negative curvature". The apparent (angular) size of the spots gives access to the information which sets of lines the light followed. The location of the main peak in the spectrum determines the average spot size: flat universe main peak at ℓ~220 negatively curved Universe ( open ) shifted to right positively curved Universe ( closed ) shifted to left

37

38 CMB Baryon/Photon ratio The properties of sound waves in the baryon-photon fluid are given by the density of photons, atoms, and dark matter dark matter defines the potential wells baryons respond to the gravitational pull a higher baryon density leads to enhancement of the 1st and 3rd acoustic peak (these are due to the baryon fluid falling into the dense regions of dark matter) suppression of the 2nd (and 4th) peaks (from the fluid moving outward) The relative heights of the even and odd peaks gives access to the relative density of baryons and dark matter The sound speed in the bayron-photon fluid is decreased by an increased ratio of baryons (ne) to photons. If the fluid moves more slowly, successive oscillations occur at smaller linear and angular scales. spacing between the peaks gets larger; smaller peaks are shifted to the right

39 CMB Matter Content the observed CMB is also affected by gravitational fluctuations along its path to the observer. photos falling into the potential wells of clusters gain energy. photons lose this energy when climbing out of the wells. The effects cancel in a flat and matter dominated universe (as opposed to dark energy) no net gravitational effect of the matter along the path The vertical position of low ℓ peak height determines the content of the Universe If >0, the depth of potential wells decays with time. A photon falls into a deep potential well but escapes out of a slightly shallower one, leading to a slight increase in photon energy along this path. A photon which travels through a low density region ( a potential hill") loses energy Models with a cosmological constant have additional fluctuations on large angular scales (at low z). At high z~ , photons and neutrinos contribute significantly to the total energy density, which also leads to decaying gravitational potentials enhancement of fluctuations < ~2 The larger photon energy density compared to the matter density, the more important is radiation in this epoch, leading to higher T fluctuations. since the photon energy density is known (from the measurement of the CMB spectrum), the amplitude of fluctuations around 2 can be used to determine the matter energy density. gains E time loses E

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