1. Dark Matter: halo-shape and relic density constraints on dark matter theories with Sommerfeld enhancement Recent observations by PAMELA, etc. have been interpreted as evidence of cold dark matter self annihilation. If these observations and their speculative interpretation are correct, then the dark matter self interaction cross section would need enhancement. In this journal club talk I will discuss the weakly interacting massive particle (WIMP) 'miracle' that results in the dark matter relic density that we see today, I will review recent observations, and I will discuss how proposed interaction enhancement mechanisms are inconsistent with data. Finally, I will discuss signals that dark matter may have on observable halo-shapes. Journal Club. A. B. Fry 4/22/2010

2. Dark Matter: halo-shape and relic density constraints on dark matter theories with Sommerfeld enhancement Journal Club. A. B. Fry 4/22/2010

3. Feng, J., Kaplinghat, M., & Yu, H. (2010) Physical Review Letters, 104 (15) DOI: 10.1103/PhysRevLett.104.15130110.1103/PhysRevLett.104.151301 Nima Arkani-Hamed, Douglas P. Finkbeiner, Tracy R. Slatyer, Neal Weiner http://arxiv.org/abs/0810.0713 http://arxiv.org/abs/0810.0713 Halo-Shape and Relic-Density Exclusions of Sommerfeld-Enhanced Dark Matter Explanations of Cosmic Ray Excesses A Theory of Dark Matter

4. Outline Motivation Relic wimps Observations Constraints The dark sector ○ Sommerfeld enhancement ○ halo shape Conclusions

5. The Question If the particles that make up most of the mass of the universe are not baryons what are they?

6. The Question If the particles that make up most of the mass of the universe are not baryons what are they? They are dark (doesn’t play well with radiation) They are electrically neutral They are highly non-relativistic (cold) Dissipationless

7. The Answer If the particles that make up most of the mass of the universe are not baryons what are they? Can we even understand the information data provides us without tying it to any specific models for DM’s nature? 42

8. Weakly Interacting Massive Particles Massive particles in the Universe decay to lower energetically favored states, however massive particles may survive to the present if they carry some sort of conserved additive or multiplicative number.

9. Weakly Interacting Massive Particles 1.Assume DM particle in equilibrium χχ ↔ff 2.Universe cools χχ → ff 3.Freeze out χχ ↔ff 1 // - - - 2 3

10. Weakly Interacting Massive Particles The WIMP miracle is that parameter space perfectly allows for a CDM WIMP particle that is independently predicted in particle physics and it has the right density to be dark matter.

11. Weakly Interacting Massive Particles In the rest of this talk I will be assuming some sort of supersymmetric dark matter particle.

12. Neutralinos & Supersymmetry Supersymmetry is a theoretical scheme that pairs every known particle with a heavier, undiscovered superpartner. The lightest superpartner, expected to be a few hundred times as massive as a proton (~1 Tev), is the neutralino which could be a WIMP According to supersymmetry WIMPs act as their own antimatter particles!

14. Neutralinos & Supersymmetry Neutralino WIMPs in a galactic halo will collide and annihilate each other to produce high energy gamma ray photons or other ordinary particles like positrons and electrons (consistent because the supersymmetric quantum number is multiplicative)

15. Observations

16. PAMELA: anomalous abundance of positrons in cosmic rays above 10 GeV. ATIC: Excess in total flux of electrons and positrons in cosmic rays WMAP: excess of microwave emission from galactic center “WMAP haze” The time variation of a signal seen by the DAMA-LIBRA collaboration

17. Observations FERMI: despite initial speculation, the 10 month data release seems to be consistent with a single power law distribution of gama-rays as predicted by the cosmic background of AGN.

18. Observations Pulsars can explain PAMELA…

19. Constraints Relic density and Ω DM (Arkani-Hamed 2009 et al.) Late decays would modify nucelosynthesis particularity the 7 Li/H ratio (Feng lecture slides 2007). CMB observations constrain dark matter annihilation energy injection rate during recombination (Zavala 2010 et al.).

20. Constraints The Pamela and Atic signals require a cross section that is of order 100 times greater than what would be expected from thermal relic WIMPs Require a low cross section to hadrons. Require a high cross section into leptons.

21. The Dark Sector

22. From a theoretical viewpoint a new interaction for the dark sector arises naturally in a variety of theories beyond the standard model, and is thus well motivated from a theoretical point of view

23. Sommerfeld Enhancements A plethora of papers propose Sommerfeld enhancement, S, to the DM cross section Sommerfeld enhancement increases the cross section of particles at low velocities similarly to classical gravitational enchantment. The Sommerfeld enhancement is the quantum counterpart to the classical gravitational phenomena.

24. Sommerfeld Enhancements Consider classical gravitational enhancement: for a test particle at velocity ν approaching a massive particle of radius R and mass M it can be shown that the cross section is increased to Where σ 0 =π R 2 and ν esc 2 =2GM/R

25. Sommerfeld Enhancements If you work through the entire derivation the result is that the enhancement leads to a cross section that scales at low energies as S(σν) ∝ 1/ν. It turns out that the velocity of dark matter particles is a factor of 10 - 3 smaller now compared to at. It is a miracle of dark matter that Sommerfeld enhancement therefore provides an elegant mechanism for boosting annihilations now.

26. Halo Shapes Dark matter has an observable effect halo- shapes. Self-interactions can be strong enough to create first order changes in the energies of dark matter particles which will isotropize the velocity dispersion and creative spherical halos (which are not seen)

27. Halo Shapes In Feng et al. 2010 they look at the halo of NGC 720 and consider halo-shape constraints from various DM models

28. Halo Shapes Strong self-interacting DM would cause the formation of constant density cores. Strong self-interacting DM would make subhalos (which have comparable or higher densities than that of the halo and also generally have lower velocity dispersions than the approximately thermal bulk) especially important. Strong self-interacting DM would isotropize the velocity dispersion and creative spherical halos

29. Mass of WIMP Sommerfeld enhancement factor

30. Mass of WIMP Sommerfeld enhancement factor M and S regions which explain PAMELA and Fermi data

31. Mass of WIMP Sommerfeld enhancement factor Halo shape observations set upper limits on the effective mass of the force carrier which mediates interactions in halo

32. Mass of WIMP Sommerfeld enhancement factor Halo shape observations set upper limits on the effective mass of the force carrier which mediates interactions in halo

33. Upper limit from Ω DM Mass of WIMP Sommerfeld enhancement factor

34. Conclusions A satisfactory solution to the dark matter problem must not only have dark matter annihilating at the correct rate, but it must also produce the right density and structure on all cosmological scales which is consistent with observations…

35. We weren’t able to get the cross section high enough to explain ATIC or PAMELA results without invoking Sommerfeld enhancement and even then the enhancement was inconsistent with relic DM density and further it changed the halo shapes. Conclusions Crash and burn?

36. Conclusions (for theorists) WIMPs are motivated from fundamental particle physics! A simple modification of a standard candidate such as a neutralino in the supersymmetric standard model is insufficient. We need a simple theory with a small number of parameters to more quantitatively confront future data.

37. Conclusions (for observers) Hopes for detection of dwarf galaxies through dark matter annihilation Although the cross section is not Sommerfeld enhanced during freeze-out, it keeps pace with the expansion over the cosmic history. This may have significant implications for a variety of early-universe phenomena as well as the cosmic gamma-ray background. Keep analyzing Fermi data. Look for local astrophysical sources of cosmic rays!

38. Questions?

39. Image Credits NGC 720: X-ray: NASA/CXC/UCI/D.Buote et al., Optical: DSS U.K.Schmidt Image/STScI The Thinker: Rodin DM observations square: WMAP, SDSS, Chandra, Hubble Dark matter decay interactions: NASA Pulsar: NASA Observation interactions: Colanfanseco 2010 Dark hallway: http://www.xcravn.com/http://www.xcravn.com/ Slide background: galaxy cluster CL0025+1654 by J.-P. Kneib (Observatoire Midi- Pyrenees, Caltech) et al., ESA, NASACL0025+1654 Observatoire Midi- PyreneesCaltechet al.ESANASA Calvin & Hobbes: Bill Watterson Square peg: Feng

43. Hadrons is a particle made of quarks held together by the strong force. Hadrons are categorized into two families: baryons (made of three quarks), and mesons (made of one quark and one antiquark). Protons and neutrons are hadrons. All hadrons except protons are unstable and undergo particle decay. Particles

44. Fermions include quarks -which are the constituents of protons and neutrons, i.e. nuclear matter- and leptons -the electron and its neutrino, and two pairs of heavier copies of the former. Bosons are the messengers of the forces experienced by fermions; they include the photon, the W and Z bosons, and the gluons. Photons carry electromagnetic forces, W and Z carry the weak forces, and the 8-strong family of gluons keeps quarks bound together. Particles

45. The enhancement is proportional to the coupling of dark matter to the force carrier, and if the coupling is large enough to give the needed enhancement, then it is too large to be consistent with the relic density, so the desired reconciliation cannot be achieved. Moreover, for very light force carriers, self-interactions of the dark matter in models of this type lead to spherical galactic halos of dark matter, inconsistent with observations of elliptical halos. Unless a way around these problems can be found, this approach to explaining the positron excess seems ruled out. – Stanley Brown http://physics.aps.org/synopsis- for/10.1103/PhysRevLett.104.151301 http://physics.aps.org/synopsis- for/10.1103/PhysRevLett.104.151301