# Presentation: 861674

## Dark Matter Annihilations and the “WMAP Haze”

***Particle Astrophysics Center***
***Fermi National Accelerator Laboratory***
***dhooper@fnal.gov***

**Dark Matter Annihilations and the “WMAP Haze”**

*Fermilab*
*September 10, 2007*

## Dark Matter

- Evidence from a wide range of astrophysical observations including rotation curves, CMB, lensing, clusters, BBN, SN1a, large scale structure
- Each observes dark matter through its gravitational influence
- Still no observations of dark matter’s electroweak interactions (or other non-gravitational interactions)

**Dan Hooper**** - ***Dark Matter Annihilations **	**          and the WMAP Haze*

## Dark Matter

- Evidence from a wide range of astrophysical observations including rotation curves, CMB, lensing, clusters, BBN, SN1a, large scale structure
- Each observes dark matter through its gravitational influence
- Still no observations of dark matter’s electroweak interactions (or other non-gravitational interactions)
***The particle identity of dark matter remains unknown***

**Dan Hooper**** - ***Dark Matter Annihilations **	**          and the WMAP Haze*

## The Thermal Abundance of Weakly Interacting Massive Particles

- T >> m, ’s in thermal equilibrium
-  T < m, number density of ’s become Boltzmann suppressed
- T ~ m/20, Hubble expansion dominates over annihilations, freeze-out occurs
- Precise temperature at which freeze-out occurs, and the density which results depends on the WIMP’s annihilation cross section

**Dan Hooper**** - ***Dark Matter Annihilations **	**          and the WMAP Haze*

## The Weak Scale and Weakly Interacting Massive Particles

- As a result of the thermal freeze-out process, a relic density of WIMPs is left behind:   h2 ~ xF / <v>
- For a particle with a GeV-TeV mass, to obtain a thermal abundance equal to the observed dark matter density, we need an annihilation cross section of <v> ~ pb
- Generic weak interaction yields:
- <v> ~ 2 (100 GeV)-2 ~ pb

**Dan Hooper**** - ***Dark Matter Annihilations **	**          and the WMAP Haze*

## The Weak Scale and Weakly Interacting Massive Particles

- As a result of the thermal freeze-out process, a relic density of WIMPs is left behind:   h2 ~ xF / <v>
- For a particle with a GeV-TeV mass, to obtain a thermal abundance equal to the observed dark matter density, we need an annihilation cross section of <v> ~ pb
- Generic weak interaction yields:
- <v> ~ 2 (100 GeV)-2 ~ pb

**Dan Hooper**** - ***Dark Matter Annihilations **	**          and the WMAP Haze*

- Numerical coincidence?  Or an indication that dark matter originates from EW physics?

## Astrophysical Probes of Particle Dark Matter

**Direct Detection** 			-Momentum transfer to detector   	    through elastic scattering
**Indirect Detection** 			-Observation of annihilation 	    products (, , e+, p, etc.)

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

## Indirect Detection of Dark Matter

**WIMP Annihilation** 		        Typical final states include heavy fermions, gauge or Higgs bosons

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

- 

- 

- W+

- W-

## Indirect Detection of Dark Matter

**WIMP Annihilation** 		        Typical final states include heavy fermions, gauge or Higgs bosons
**2) Fragmentation/Decay  ** 		        Annihilation products decay and/or fragment into some combination of   electrons, protons, deuterium, neutrinos and gamma rays

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

- 

- 

- W+

- W-

- e+

- 

- q

- q

- p

- 0

- 

- 

## Indirect Detection of Dark Matter

**WIMP Annihilation** 		        Typical final states include heavy fermions, gauge or Higgs bosons
**2) Fragmentation/Decay  ** 		        Annihilation products decay and/or fragment into some combination of   electrons, protons, deuterium, neutrinos and gamma rays
**3) Synchrotron and Inverse Compton **Relativistic electrons up-scatter starlight to MeV-GeV energies, and emit synchrotron photons via interactions with magnetic fields

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

- 

- 

- W+

- W-

- e+

- 

- q

- q

- p

- 0

- 

- 

- e+

- 

## Indirect Detection of Dark Matter

**Neutrinos **from annihilations     	               in the core of the Sun
**Gamma Rays** from annihilations 	               in the galactic halo, near the 		galactic center, in dwarf galaxies, etc.
**Positrons/Antiprotons** from annihilations throughout the galactic halo
**Synchrotron Radiation** from electron/positron interactions 		 with the magnetic fields of the 	          inner galaxy

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

## Indirect Detection With Synchtrotron

- Electrons/positrons produced in 				      dark matter annihilations inverse 				Compton scatter with starlight and 			      emit synchrotron photons as they 			propagate through the galactic 				magnetic fields
- For electroweak-scale dark matter, the resulting synchrotron radiation falls within the frequency range of WMAP

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

## WMAP As A Synchrotron Telescope

- In addition to CMB photons, WMAP data is “contaminated” by a number of galactic foregrounds that must be accurately subtracted
- The WMAP frequency range is well suited to minimize the 	impact of foregrounds
- Substantial challenges are 					involved in identifying and 						   removing foregrounds

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

**Thermal Dust**

**Soft Synchrotron**

**Free-Free**

**WMAP**

## WMAP Foregrounds

**Soft Synchrotron** - From SN shocks; morphology traced by the     408 MHz Haslam map
**Free-Free** - Hot gas electron/ion thermal Bremsstrahlung; morphology traced by the H recombination line map (Finkbeiner, 2003)
**Thermal/Spinning Dust** 	 				         -Emission from vibrating and 						spinning dust grains; morphology 					traced by the SFD98 dust map 					(Schlegel et al.) and the 						      94 GHz Finkbeiner map

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

**Thermal Dust**

**Soft Synchrotron**

**Free-Free**

**WMAP**

## =

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

**=**

**+**

**+**

**+**

- Synchrotron

- Free-free

- T & S Dust

- CMB

- WMAP

## =

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

**=**

**+**

**+**

**+**

- Synchrotron

- Free-free

- T & S Dust

- CMB

- WMAP

**Well, actually... No**

## = ...

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

**_**

**+**

**+**

**+**

- Synchrotron

- Free-free

- T & S Dust

- CMB

- WMAP

**= ...**

## The “WMAP Haze”

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

- 22 GHz

## The “WMAP Haze”

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

- 22 GHz

- After known foregrounds are subtracted, an excess appears in the residual maps within the inner ~20 around the Galactic Center

## The “WMAP Haze”

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

- 22 GHz

- Initially interpreted as likely 					thermal bremsstrahlung        					(free-free emission) from hot gas 					(104-106 K)
- This interpretation has since 					been ruled out by the lack of a 				corresponding H recombination (X-ray) line
- Appears to be hard synchrotron emission from a new population of energetic electrons/positrons in the inner galaxy
-    	-Too hard to be supernovae shocks
-    	-Too extended to be a singular event (GRB, etc.)
- Very Difficult to explain astrophysically

## Dark Matter and the WMAP Haze

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

- 22 GHz

- In 2004, Doug Finkbeiner 					suggested that the WMAP Haze 					could be synchtrotron from 			electrons/positrons produced in 					dark matter annihilations in the 					inner galaxy (astro-ph/0409027)
- In particular, he noted that:
- 1) Assuming an NFW profile, a WIMP mass of 100 GeV and an annihilation cross section of 3x10-26 cm3/s, the total power in dark matter annihilations in the inner 3 kpc of the Milky Way is 	~1.2x1039 GeV/sec
- 2) The total power of the WMAP Haze is between 		    	0.7x1039 and 3x1039 GeV/sec

## Dark Matter and the WMAP Haze

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

- 22 GHz

- In 2004, Doug Finkbeiner 					suggested that the WMAP Haze 					could be synchtrotron from 			electrons/positrons produced in 					dark matter annihilations in the 					inner galaxy (astro-ph/0409027)
- In particular, he noted that:
- 1) Assuming an NFW profile, a WIMP mass of 100 GeV and an annihilation cross section of 3x10-26 cm3/s, the total power in dark matter annihilations in the inner 2 kpc of the Milky Way is 	~1.2x1039 GeV/sec
- 2) The total power of the WMAP Haze is between 		    	0.7x1039 and 3x1039 GeV/sec

**Coincidence?**

## Electron-Positron Diffusion

- When electrons/positrons are produced in dark matter annihilations, they travel through the galaxy’s tangled magnetic fields, losing energy via synchtrotron and inverse Compton
- Resulting spectrum can be calculated by solving the diffusion-loss equation:
- For 10-50 GeV e+/- in					   	   the inner galaxy, leads to 						~0.1-1 kpc diffusion (~1-10)

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

- Diffusion Constant

- Energy   Loss Rate

- Source  Term

## Fitting The Haze To The Dark Matter Halo Profile

**Fitting The Haze To The Dark Matter Halo Profile**

- When the effects of diffusion   			      	          are accounted for, we find that 			       		 an NFW halo profile (  R-1) 			  		under produces the WMAP  			   		haze at small angles
- Angular distribution of the haze matches that found for a cusped halo profile, with   R-1.2
- Although the precise result of this fit depends on the diffusion parameters adopted (magnetic fields, starlight density, etc.), the approximate result (slope of -1.1 to -1.3) is fairly robust

**Hooper, G. Dobler and D. Finkbeiner, arXiv:0705.3655**

- (R)  R-1.2

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

- (R)  R-1    (NFW)

- Significant systematic errors

## Dark Matter Annihilation Radiation and the Spectrum of the WMAP Haze

- By comparing the ratio of the intensities at 22 and 33 GHz from the inner galaxy, the responsible electron/positron spectrum can be constrained, and along with it the dark matter mass and annihilation modes

**Dark Matter Annihilation Radiation and the Spectrum of the WMAP Haze**

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

- (Caution: statistical errors only)

## Dark Matter Annihilation Radiation and the Spectrum of the WMAP Haze

- For WIMPs annihilating to 					gauge bosons or leptons, a 					WIMP with a mass in the 						range of ~50 GeV to        						multi-TeV is acceptable
- For a WIMP annihilating to b quarks, 				200 GeV to multi-TeV is favored

**Dark Matter Annihilation Radiation and the Spectrum of the WMAP Haze**

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

**Hooper, G. Dobler and D. Finkbeiner, arXiv:0705.3655**

- bb

- WW, ZZ

- ee

- 

- 

## The Dark Matter Annihilation Cross Section

**The Dark Matter Annihilation Cross Section**

**Hooper, G. Dobler and D. Finkbeiner, arXiv:0705.3655**

- For a given annihilation mode, diffusion parameters and halo profile, we can calculate the 							annihilation cross 	 						section needed to 							normalize the 							   observed intensity 	          						   of the WMAP Haze
- For a typical 100-1000 GeV WIMP, the annihilation cross section needed is within a factor of 2-3 of the value needed to generate the density of dark matter thermally (3x10-26 cm3/s);  			 No boost factors are required!

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

- bb

- WW, ZZ

- ee

- 

- 

## Testing the Haze-Dark Matter Connection With Gamma-Rays

- _Advantages of Gamma-Rays_:
- Propagate undeflected (point sources possible, angular information)
- Propagate without energy loss (spectral information)
- Rapid development in 		both space (GLAST) 		and ground-based 			(HESS, MAGIC, VERITAS) technologies

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

## Gamma-Rays From The Galactic Center

- Simulations predict that the GC contains very high densities of dark matter (and high annihilation rates)
- Long considered likely to be the brightest dark matter annihilation region in the sky
- HESS, MAGIC, WHIPPLE and CANGAROO each claim positive detection of ~TeV gamma-rays
- Evidence for dark matter, or other astrophysics?

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

## Gamma-Rays From The Galactic Center

**Gamma-Rays From The Galactic Center**

- Spectrum as measured  by HESS extends to at least ~10TeV
- Consistent with a constant power-law spectrum
- To fit with dark matter would require a very heavy particle   (15-30 TeV) - Far too heavy for a neutralino
- A very heavy dark 						     matter candidate also fails 						  to match the spectral 						shape reported by HESS

**Power-Law Fit**

**Heavy DM**

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

**HESS Collaboration, PRL, astro-ph/0610509**** **

## Gamma-Rays From The Galactic Center

- The GC is a region rich in extreme astrophysical objects
- Particle acceleration associated with supermassive black hole?
**Aharonian and Neronov (astro-ph/0408303), **
**Atoyan and Dermer (astro-ph/0410243)**
- This astrophysical source 					represents a very daunting 				background for future dark matter 				searches to compete with

**Hooper, Perez, Silk, Ferrer and Sarkar, JCAP, astro-ph/0404205**** **

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

## Gamma-Rays From The Galactic Center

- Prospects for GLAST and other future gamma-ray experiments are reduced as a result of this new background
- Range of annihilation rates 				observable with GLAST is 						reduced considerably
- Other potential sources of dark 					matter annihilation radiation 					become more interesting 						(dwarf spheroidal galaxies, 					the diffuse background, etc.)

**Hooper and G. Zaharijas, PRD, hep-ph/0603540**

**Excluded by EGRET**

**Excluded       by HESS**

**GLAST Reach**

**GLAST Reach (neglecting BG)**

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

## Gamma-Ray Signals of The Dark Matter-WMAP Haze Connection

- The observed properties of the Haze can be used to calculate the intensity and angular distribution of gamma rays from dark matter annihilations from the inner galaxy
- An angular distribution and intensity similar to this prediction would provide an important confirmation of the dark matter origin of the haze; Conversely the absence of such a signal would refute the hypothesis (highly falsifiable!)

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

## Gamma-Ray Signals of The WMAP Haze

**Dobler, Finkbeiner, Hooper, Zaharijas, in preparation **

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

- Inner 0.1

- 0.3-0.5

- background

- Projected GLAST Error Bars

- Annihilations to heavy fermions or gauge bosons
- and easily identifiable by GLAST; annihilations
- to muons/electrons are unlikley to be observable

## The WMAP Haze In Light Of Planck

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

- Planck (launch in 2008) will represent a 				major step forward from WMAP:
- Improved frequency coverage
- Much greater polarization information 			(synchrotron emission is highly polarized)
- Improved angular resolution
- At frequencies above ~100 GHz, all 			foregrounds other than emission from 				thermal dust are negligible; subtracting 			           one foreground rather than the several 			              (3 or 4) required at WMAP frequencies 				 will enable for a much more robust confirmation of the synchrotron origin of the Haze
- Systematic uncertainties are expected to be reduced by more than an order of magnitude relative to WMAP

## What About Other Claims of Evidence For Dark Matter Annihilation?

- The HEAT positron excess
- 511 keV emission from the 			galactic bulge
- EGRET’s galactic gamma ray 		spectrum
- EGRET’s extragalactic 				gamma ray spectrum

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

## The HEAT Positron Excess

- In its 1994-95, 2000 flights, the HEAT balloon-based cosmic ray detector observed an excess of positrons relative to electrons in   the 7-30 GeV range
- Measurements from AMS-01     add some support
- Combined statistical significance  of several (4-5) sigma, neglecting (likely important, but difficult to evaluate) systematic uncertainties

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

- E. Baltz and J. Edsjo, PRD, astro-ph/9808243

## The HEAT Positron Excess

_**Strengths:**_
- Fit to data can be easily improved  if dark matter component is included
_**Weaknesses**__***:***_
- Messy astrophysics
- Requires annihilation boost of ~50 or more (possible, but unlikely), or non-thermal dark matter production
_**Prospects:**_
- PAMELA data (August?) should clearly confirm or refute this signal, and measure the spectrum up to much higher energies

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

- PAMELA

## 511 keV Emission from the Galactic Bulge

- INTEGRAL/SPI observed bright 511 keV emission from the bulge of the Milky Way  (1.3 x 1043 positrons injected per second)
- Gaussian, spherically symmetric morphology   (FWHM of 8 ̊)
- The source of these positrons remains unknown

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

## 511 keV Emission from the Galactic Bulge

- Type Ia supernovae are unable to generate the observed injection rate (too few escape)
- Hypernovae (type Ic SNe) or gamma ray bursts could potentially generate enough positrons if high estimates for rates are considered
- Even if the injection rate is sufficient, a mechanism is required to transport from disk to bulge - appears to be somewhat difficult

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

## 511 keV Emission and MeV Dark Matter

- The INTEGRAL morphology matches well that which would    be generated through the annihilation (or decay) of dark matter
- 1-10 MeV dark matter particles annihilating to e+e- could simultaneously generate the measured dark matter relic abundance, and the observed 511 keV emission
- (Boehm, Hooper, Silk, Casse, Paul, PRL, astro-ph/0309686)

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

## 511 keV Emission and MeV Dark Matter

_**Strengths:**_
- Challenging to explain 511 signal with non-exotic astrophysics
_**Weaknesses**__***:***_
- Somewhat difficult to construct a viable particle physics model with an MeV WIMP
_**Prospects:**_
- No clear path to confirmation or exclusion of the MeV dark matter hypothesis (perhaps 511 emission from dwarf galaxies?)

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

## EGRET’s Galactic Gamma Ray Spectrum

- EGRET observed an excess of gamma rays above 1 GeV, compared to the the most simple galactic cosmic ray models
- Coud be the product of a 	     ~50-100 GeV WIMP 	        (W. de Boer et al, PLB, hep-ph/0511154; Astron.Astrophys, astro-ph/0508617; astro-ph/0408272)

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

## EGRET’s Galactic Gamma Ray Spectrum

- The same dark matter annihilation spectrum can fit the shape of the GeV excess in all regions of the sky
- To normalize the intensity 	     of each region, however, 		requires a departure from 		      a simple halo profile
- De Boer, et al. introduce 		   two rings of dark matter 		 near the galactic plane at 	                 4 and 14 kpc from galactic 		center (8x1010 M tidally 		disrupted dwarf galaxy? 		 motivated by rotation curves)

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

- (W. de Boer et al, A.A., astro-ph/0508617)

## EGRET’s Galactic Gamma Ray Spectrum

- With a standard treatment of cosmic ray diffusion, far too many antiprotons are produced in this scenario
- To reconcile, anisotropic diffusion, strong 	convection away from (and outside of) the disk and local spatial variations are required

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

- (Bergstrom, Edsjo, Gustafsson and Salati, 	JCAP, astro-ph/0602632)

- Prediced  in de Boer model

- Prediction from standard secondary
- cosmic ray production

## EGRET’s Galactic Gamma Ray Spectrum

_**Strengths:**_
- Consistent with a neutralino or 					other EW-scale WIMP
- Similar spectral shape over sky
_**Weaknesses**__***:***_
- Non-standard dark matter 				distribution is needed (two rings)
- Conflict with antiprotons unless 					non-standard comic ray diffusion is invoked
- The GeV excess can plausbily be reduced or eliminated without dark matter by modifying the diffusion model
_**Prospects:**_  GLAST will clear up these questions considerably

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

## EGRET’s Extragalactic Gamma Ray Spectrum

- EGRET has also detected a diffuse, extragalactic gamma ray signal, which becomes more intense above 1 GeV
- Integrated signal from dark matter annihilations throughout the universe could produce a potentially observable signal 	  (Ullio, Bergstrom,Edsjo 2002)
- Intensity depends critically on 					   dark matter distribution - 						 cuspy halos and substructure 					     are required
- The EGRET extragalactic 						diffuse spectrum can be fit by 					annihilations from a ~500 GeV 				     neutralino (or other WIMP)

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

- Elsasser and Mannheim, PRL, astro-ph/0405235

## EGRET’s Extragalactic Gamma Ray Spectrum

_**Strengths:**_
- Consistent with a (somewhat heavy) neutralino or other WIMP
_**Weaknesses**__***:***_
- Not a particularly distinctive signal, 				          could easily be astrophysical
- High annihilation rate needed; 					 either large degree of very cusped 			substructure, or a non-thermal WIMP
- Signal from our galactic center 					 would have been seen, unless cusp 				       is removed by tidal effects (S. Ando, PRL, astro-ph/0503006)
_**Prospects:**_ GLAST will clearly resolve

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

## Dan Hooper - Dark Matter Annihilations       		          and the WMAP Haze

| Signal | Required Particle Physics | Required Astrophysics |
| --- | --- | --- |
| WMAP Haze | 100 GeV to multi-TeV WIMP, ~3x10-26 cm3/s annihilation cross section | Cusped halo profile, standard diffusion, no boost factors |
| HEAT Positron Excess | 50-1000 GeV WIMP; Either large (non-thermal) annihilation cross section OR ... | Large boost factor            (50 or more) |
| INTEGRAL 511 keV Emission | ~MeV particle, p-wave annihilator with ~3x10-26 cm3/s annihilation cross section | Mildly cusped halo profile |
| EGRET Diffuse Galactic | ~50-300 GeV WIMP; Either large (non-thermal) annihilation cross section OR ...
 | Large boost factors; two massive rings of dark matter in the galactic plane; non-standard, highly convective diffusion model  |
| EGRET Diffuse Extragalactic | ~500 GeV WIMP; Either large (non-thermal) annihilation cross section OR ... | Large boost factors/highly cusped profiles; Conflict with Milky Way unless Galactic Center is exceptional |

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

## Dan Hooper - Dark Matter Annihilations       		          and the WMAP Haze

| Signal | Required Particle Physics | Required Astrophysics |
| --- | --- | --- |
| WMAP Haze | 100 GeV to multi-TeV WIMP, ~3x10-26 cm3/s annihilation cross section | Cusped halo profile, standard diffusion, no boost factors |
| HEAT Positron Excess | 50-1000 GeV WIMP; Either large (non-thermal) annihilation cross section OR ... | Large boost factor            (50 or more) |
| INTEGRAL 511 keV Emission | ~MeV particle, p-wave annihilator with ~3x10-26 cm3/s annihilation cross section | Mildly cusped halo profile |
| EGRET Diffuse Galactic | ~50-300 GeV WIMP; Either large (non-thermal) annihilation cross section OR ...
 | Large boost factors; two massive rings of dark matter in the galactic plane; non-standard, highly convective diffusion model  |
| EGRET Diffuse Extragalactic | ~500 GeV WIMP; Either large (non-thermal) annihilation cross section OR ... | Large boost factors/highly cusped profiles; Conflict with Milky Way unless Galactic Center is exceptional |

**Dan Hooper**** - ***Dark Matter Annihilations       **	**	**          and the WMAP Haze*

## Conclusions

**WMAP data, after the subtraction of known foregrounds, contains an excess from the region around the center of the  Milky Way - The “WMAP Haze”**
**Consistent with synchrotron ****	****	****	****	****	****emission from energetic  ****	****	****	****	**** ****	****electrons/positrons from ****	****	****	****	****	**** dark matter annihilations with:**
**  ****-A cusped halo profile **
**  ****-A 100 GeV to multi-TeV WIMP**
**  ****-An annihilation cross section within a factor of 2-3 of the value required of a thermal relic (~3x10****-26**** cm****3****/s)**

## Conclusions

**We may very well be looking at the first detection of supersymmetry or other TeV scale physics beyond the Standard Model**
**Future measurements by GLAST and PLANCK will clarify the nature of the WMAP Haze **
** ****The dark matter - WMAP Haze connection is a clearly falsifiable/verifiable hypothesis**
**With GLAST and Planck, in a ****	****	****	****	****	****couple of years, we will know ****	****	****	****	****	****  one way or the other**