mario e. gómez universidad de huelva,...
TRANSCRIPT
![Page 1: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/1.jpg)
Gamma Flux from SUSYDark Matter Annihilation
Mario E. GómezUniversidad de Huelva, Spain
Sanchez-Conde, Prada, Lokas , Wojtak, Moles, Cannoni, MEG,PRD77(2007)+work in progress
GALEON
![Page 2: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/2.jpg)
The DM gamma signal
€
Fγ E > Eth( ) =14π
fsusy ⋅U(Ψo) photons cm-2 s-1
Particle physics Astrophysics
(Sánchez-Conde, Prada, Lokas, Gómez et al. 2007)
SUSY Model: ∫ ΩΩΨ=Ψ dBJU o )()()(
€
J(Ψ) = ρdm2
l .o.s∫ (r)dl
φθθσθ dddBtsinexp)( 2
2
−=ΩΩ
2
€
fsusy =nγ σ ⋅ v2mχ
2
Integral along the l.o.s.:
Telescope PSF:
Where to search?
• Our galaxy (Galactic Center, substructure…)• Dwarf spheroidal galaxies (e.g. Draco, Willman-1…)• Andromeda• Galaxy clusters (e.g. Virgo, Coma)
nγ: Number of photons<σ·v>: cross section
mχ: neutralino mass
Very large uncertainties!
(No evidence as y e t)
![Page 3: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/3.jpg)
SuperSymmetric Extension of the SM
![Page 4: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/4.jpg)
THE OTERS…..
![Page 5: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/5.jpg)
Unification of the Interactions
![Page 6: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/6.jpg)
Why SUSY?
![Page 7: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/7.jpg)
Soft SUSY Breaking Terms
![Page 8: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/8.jpg)
SUSY spectrum
![Page 9: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/9.jpg)
LSP, WIMP candidate
Goldberg 83, Ellis et al 84
![Page 10: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/10.jpg)
The LSP on the CMSSM
![Page 11: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/11.jpg)
![Page 12: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/12.jpg)
Relic Density Channels
Gondolo,Edsjo 1997, Lazarides, Pallis , M.E.G.
Very good public codes MICROMEGAS (Belanger et al), DarkSusy (Gondolo et al.)
![Page 13: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/13.jpg)
Neutralino Direct Detection
Neutralino-Matter interaction is very weak
![Page 14: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/14.jpg)
Experimental Prostpects
Ruiz de Austri, Roszkowski, Trotta
Baudis 0902.4253
![Page 15: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/15.jpg)
Indirect Dark Matter Searches* Detectability of gamma rays coming from the annihilation of SUSY DM particles.* IACTs and satellites: MAGIC, HESS, VERITAS, CANGAROO, Fermi, AGILE…
IACT example: MAGIC
![Page 16: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/16.jpg)
LSP Anihilation into GammasSubdominant channels because:
Loop Supressed Monoenergetic Channels:
Bresstralung
![Page 17: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/17.jpg)
Continuum Spectrum
Secondary Gamma’s from annihilation’s:
Computation of the number of Gammas/Annihilation requiresone event simulator (DarkSusy uses PHYTIA).
![Page 18: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/18.jpg)
Internal BremsstrahlungFrom annihilation channels with charged particles on the final state:
Bringmann, Bergstrom, Edsjo 2008and references there in.
![Page 19: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/19.jpg)
Example
T. Bringmann, L. Bergstrom and J. Edsjo, JHEP 01 (2008) 049
![Page 20: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/20.jpg)
mSUGRA Parameter Space, Large tanβ
![Page 21: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/21.jpg)
Parameter Space Low tanβ
![Page 22: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/22.jpg)
THE GAMMA-RAY FLUX IN IACTʼS
Flux above a certain Eth:
AstrophysicalParticle Physics
![Page 23: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/23.jpg)
M0 <2000 GeV
![Page 24: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/24.jpg)
M0 >2000 GeV
![Page 25: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/25.jpg)
mSUGRA
![Page 26: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/26.jpg)
Gammas from dSph galaxies
![Page 27: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/27.jpg)
Observations of Draco with MAGIC
• Draco is probably the dSph with more observational constraints.
• Near (80 kpc from the GC).
• M/L ~ 300
• High in the Northern Sky --> suitable for MAGIC
MAGICobservationsand analysis
Total Observation Time of 7.8 HOURS (may 2007) Zenith Angle ranges between 29º and 42º
Calibration of the data and Hillas parameterization of the shower images
Hadronic background supression and energy estimation by Random Forest method
![Page 28: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/28.jpg)
Results from MAGIC
![Page 29: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/29.jpg)
Result from GLAST
![Page 30: Mario E. Gómez Universidad de Huelva, Spainweb.mit.edu/cygnus2009/talks/SessionVIII/mgomez_cygnus.pdf · Mario E. Gómez Universidad de Huelva, Spain Sanchez-Conde, Prada, Lokas](https://reader033.vdocumento.com/reader033/viewer/2022051608/603d339b76c116036833c3e1/html5/thumbnails/30.jpg)
Conclusion
Neutralinos are the most “admired/studied” candidates to explain the DM problem.
Their annihilation rates are small enough to account for WMAP data. However, the annihilation channels with Gammas in the final states are subdominant: Ether loop supressed or produce a continuum of secondary gammas.
dSph galaxies can be studied as good sources of Gamma rays.For the analysed case of Draco (and also Willman) the predicted upper bounds are more than 3 orders of magnitude above the detection limits.