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SIST Final Presentation August 5, 2008
August 5, 2008
Dark Matter Dark Matter
Galactic Scale:
halo bulge disk You Are Here!
Rotational Curves
show that galaxies rotate faster than what is expected from the luminous
- mass. This also
Dark Matter, Dark Matter, Supersymmetry, Supersymmetry, and - - PowerPoint PPT Presentation
Dark Matter, Dark Matter, Supersymmetry, Supersymmetry, and - - PowerPoint PPT Presentation
Dark Matter, Dark Matter, Supersymmetry, Supersymmetry, and Accounting for the and Accounting for the WMAP Haze WMAP Haze Gabriel Caceres Gabriel Caceres Advisor: Dr. Dan Hooper Advisor: Dr. Dan Hooper Theoretical Astrophysics
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August 5, 2008
Dark Matter Dark Matter
Cluster Scale:
http://chandra.harvard.edu/photo/2003/apm08279/more.html
Gravitational
lensing shows that there’s more mass than what can be observed
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August 5, 2008
Dark Matter Dark Matter
Cosmological Scale:
From the Cosmic Microwave Background (CMB)
we can tell that the universe is made up of ~23% DM (compared to ~5% baryonic matter)
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August 5, 2008
Dark Matter Dark Matter
Main Focus:
Main Focus: Weakly Interacting Weakly Interacting Massive Particle Massive Particle (WIMP) (WIMP)
Many Proposed Many Proposed Explanations: Explanations:
Axions
Axions
Massive Compact Halo
Massive Compact Halo Object (MACHOs) Object (MACHOs)
Modified Gravity
Modified Gravity
And More!
And More!
Candidates and Detection
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August 5, 2008
Dark Matter Dark Matter
Main Focus:
Main Focus: Weakly Interacting Weakly Interacting Massive Particle Massive Particle (WIMP) (WIMP)
Many Proposed Many Proposed Explanations: Explanations:
Axions
Axions
Massive Compact Halo
Massive Compact Halo Object (MACHOs) Object (MACHOs)
Modified Gravity
Modified Gravity
And More!
And More!
Candidates and Detection
Non-baryonic matter
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August 5, 2008
Dark Matter Dark Matter
Main Focus:
Main Focus: Weakly Interacting Weakly Interacting Massive Particle Massive Particle (WIMP) (WIMP)
Many Proposed Many Proposed Explanations: Explanations:
Axions
Axions
Massive Compact Halo
Massive Compact Halo Object (MACHOs) Object (MACHOs)
Modified Gravity
Modified Gravity
And More!
And More!
Candidates and Detection
Non-baryonic matter Doesn’t interact
through the electromagnetic or the strong force
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August 5, 2008
Supersymmetry Supersymmetry
Broken symmetry
between Fermions (spin ½) and Bosons (integer spin)
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August 5, 2008
Supersymmetry Supersymmetry
Broken symmetry
between Fermions (spin ½) and Bosons (integer spin)
New particles
introduced
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August 5, 2008
Supersymmetry Supersymmetry
Broken symmetry
between Fermions (spin ½) and Bosons (integer spin)
New particles
introduced
Neutralino LSP, Dark
Matter candidate
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August 5, 2008
Supersymmetry Supersymmetry
Broken symmetry
between Fermions (spin ½) and Bosons (integer spin)
New particles
introduced
Neutralino LSP, Dark
Matter candidate
~120 free parameters
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August 5, 2008
CMSSM CMSSM
Constrained Minimal Supersymmetry
Standard Model (CMSSM) reduces free parameters through theoretically
- riented assumptions
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August 5, 2008
CMSSM CMSSM
Constrained Minimal Supersymmetry
Standard Model (CMSSM) reduces free parameters through theoretically
- riented assumptions
Through 5 parameters, the entire particle
spectrum can be calculated (here using the DarkSUSY package):
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August 5, 2008
CMSSM CMSSM
Constrained Minimal Supersymmetry
Standard Model (CMSSM) reduces free parameters through theoretically
- riented assumptions
Through 5 parameters, the entire particle
spectrum can be calculated (here using the DarkSUSY package):
- Universal gaugino mass: m½
- Universal scalar mass: m0
- Universal tri-linear scalar coupling: A0
- Ratio of v.e.v. of the two Higgs doublets: tan β
- Sign of the Higgsino mass parameter: μ
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CMSSM CMSSM
(Done for μ>0, tanβ 3,10,35,50 and μ<0, tanβ 35,50)
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CMSSM CMSSM
Bulk (Done for μ>0, tanβ 3,10,35,50 and μ<0, tanβ 35,50)
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CMSSM CMSSM
Bulk Coannihilation (Done for μ>0, tanβ 3,10,35,50 and μ<0, tanβ 35,50)
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CMSSM CMSSM
Bulk A-funnel Coannihilation (Done for μ>0, tanβ 3,10,35,50 and μ<0, tanβ 35,50)
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CMSSM CMSSM
Bulk A-funnel Focus Point Coannihilation (Done for μ>0, tanβ 3,10,35,50 and μ<0, tanβ 35,50)
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WMAP Haze WMAP Haze
Cosmic Microwave Background
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August 5, 2008
WMAP Haze WMAP Haze
Cosmic Microwave Background
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August 5, 2008
WMAP Haze WMAP Haze
Cosmic Microwave Background
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August 5, 2008
WMAP Haze WMAP Haze
WMAP
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August 5, 2008
WMAP Haze WMAP Haze
WMAP: CMB & Galactic Foregrounds...
- Synchrotron
Free-free T & S Dust
WMAP
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WMAP Haze WMAP Haze
22 GHz
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WMAP Haze WMAP Haze
22 GHz 22 GHz After known foregrounds are subtracted, an excess appears in the residual maps within the inner ~20° around the Galactic Center
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WMAP Haze WMAP Haze
Dark Matter requirements to produce Haze:
Hooper, Finkbeiner, Dobler 2007
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CMSSM Analysis CMSSM Analysis
Take CMSSM data and calculate cross-section
and annihilation modes
Sample:
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CMSSM Analysis CMSSM Analysis
Compare with Haze requirements Sample:
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Detection Prospects Detection Prospects
Direct Detection Neutrino Detection
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Conclusions Conclusions
Much of the CMSSM parameter space provides us with a
WIMP which is capable of producing the WMAP Haze
In particular:
- Most of the Focus Point and A-funnel regions
provide a viable candidate
- At high tanβ, a fraction of the Bulk region can
accommodate a WIMP of the desired properties
- The stau coannihilation region does not give a
WIMP that satisfies the requirements of the WMAP Haze
Very positive detection prospects for models in the Focus
Point region
For more information see arXiv:0808.0508v1 [hep-ph]
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August 5, 2008
Questions?
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August 5, 2008
Dark Matter Dark Matter
Gravitational lensing
Gravitational lensing shows that there’s shows that there’s more mass than more mass than visible stars. visible stars.
Bullet Cluster shows
Bullet Cluster shows two clusters colliding two clusters colliding leaving the leaving the intergalactic gas intergalactic gas behind as the dark behind as the dark matter and galaxies matter and galaxies continue forward. continue forward.
(Sample of) Current Evidence
http://chandra.harvard.edu/photo/2003/apm0827 9/more.html http://chandra.harvard.edu/photo/2006/1e0657/index.html
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Detection Prospects Detection Prospects
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Direct Detection Direct Detection
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Indirect Detection Indirect Detection
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WMAP Haze WMAP Haze
WMAP: CMB & Galactic Foregrounds...
+ + +
Synchrotron Free-free T & S Dust CMB