Dark Matter in the Left Right Twin Higgs Model
description
Transcript of Dark Matter in the Left Right Twin Higgs Model
![Page 1: Dark Matter in the Left Right Twin Higgs Model](https://reader034.fdocuments.us/reader034/viewer/2022051316/5681553e550346895dc314a0/html5/thumbnails/1.jpg)
Dark Matter in theDark Matter in theLeft Right Twin Higgs ModelLeft Right Twin Higgs Model
Ethan DolleEthan Dolle
University of ArizonaUniversity of Arizona
Work done withWork done with
Shufang Su and Jessica GoodmanShufang Su and Jessica Goodman
![Page 2: Dark Matter in the Left Right Twin Higgs Model](https://reader034.fdocuments.us/reader034/viewer/2022051316/5681553e550346895dc314a0/html5/thumbnails/2.jpg)
OutlineOutline
• Left Right Twin Higgs ModelLeft Right Twin Higgs Model
• Relic Density AnalysisRelic Density Analysis
• Direct and Indirect DetectionDirect and Indirect Detection
• ConclusionConclusion
![Page 3: Dark Matter in the Left Right Twin Higgs Model](https://reader034.fdocuments.us/reader034/viewer/2022051316/5681553e550346895dc314a0/html5/thumbnails/3.jpg)
Left Right Twin Higgs ModelLeft Right Twin Higgs Model
•Chacko, Goh, and Harnik: Chacko, Goh, and Harnik: arXiv:hep-ph/0506256v1arXiv:hep-ph/0506256v1
•solution to Little Hierarchy Problem
•To avoid EW precision constraints, add a second Higgs Ĥ that couple to gauge boson only
![Page 4: Dark Matter in the Left Right Twin Higgs Model](https://reader034.fdocuments.us/reader034/viewer/2022051316/5681553e550346895dc314a0/html5/thumbnails/4.jpg)
Left Right Twin Higgs ModelLeft Right Twin Higgs Model
SU(2)SU(2)LL Higg doublet Higg doublet
SM Higgs doubletSM Higgs doublet
Couples only toCouples only to
gauge bosonsgauge bosons
DM candidateDM candidate
EWSBEWSB
![Page 5: Dark Matter in the Left Right Twin Higgs Model](https://reader034.fdocuments.us/reader034/viewer/2022051316/5681553e550346895dc314a0/html5/thumbnails/5.jpg)
Left Right Twin Higgs ModelLeft Right Twin Higgs Model
• Ĥ couples only to gauge bosonsĤ couples only to gauge bosons could be achieved by impose a discrete symmetry could be achieved by impose a discrete symmetry
• the lighter one of S, and A are stable, weakly the lighter one of S, and A are stable, weakly interactinginteracting
GoodGood
BadBad
⇒⇒Natural WIMP candidatesNatural WIMP candidates
![Page 6: Dark Matter in the Left Right Twin Higgs Model](https://reader034.fdocuments.us/reader034/viewer/2022051316/5681553e550346895dc314a0/html5/thumbnails/6.jpg)
Left Right Twin Higgs ModelLeft Right Twin Higgs Model
• h1 and h2 mass splittingh1 and h2 mass splitting
• Need to impose mass splitting between ANeed to impose mass splitting between A and S: Constraints from direct detection and S: Constraints from direct detection
![Page 7: Dark Matter in the Left Right Twin Higgs Model](https://reader034.fdocuments.us/reader034/viewer/2022051316/5681553e550346895dc314a0/html5/thumbnails/7.jpg)
Left Right Twin Higgs ModelLeft Right Twin Higgs Model
• Similar to Inert Higgs Doublet ModelSimilar to Inert Higgs Doublet Model
•Proposed by Barbieri, et al.•arXiv:hep-ph/0603188v2
•Dark matter analyzed by Honorez, et al.•arXiv:hep-ph/0612275
•Indirect detection analyzed by Gustafsson, et al.•arXiv:astro-ph/0703512
![Page 8: Dark Matter in the Left Right Twin Higgs Model](https://reader034.fdocuments.us/reader034/viewer/2022051316/5681553e550346895dc314a0/html5/thumbnails/8.jpg)
Model ComparisonModel Comparison
Inert Higgs Doublet Inert Higgs Doublet ModelModel
Left Right Twin Higgs ModelLeft Right Twin Higgs Model
MMhsm hsm ~ 500 GeV~ 500 GeV MMhsmhsm ~ 170 GeV ~ 170 GeV
New particlesNew particles New particlesNew particles
extra extra scalarsscalars extra scalarsextra scalars
Heavy gauge bosonsHeavy gauge bosons
Heavy top, heavy neutrinosHeavy top, heavy neutrinos
![Page 9: Dark Matter in the Left Right Twin Higgs Model](https://reader034.fdocuments.us/reader034/viewer/2022051316/5681553e550346895dc314a0/html5/thumbnails/9.jpg)
Relic Density AnalysisRelic Density Analysis
• WMAP: 0.093<ΩhWMAP: 0.093<Ωh22<0.128 at 2σ level<0.128 at 2σ level
•Must consider co-annihilations when mass splittings are small
•Used program micrOMEGAS_2.0•Solves Boltzmann equation exactly
•Need to solve Boltzmann equationNeed to solve Boltzmann equation
![Page 10: Dark Matter in the Left Right Twin Higgs Model](https://reader034.fdocuments.us/reader034/viewer/2022051316/5681553e550346895dc314a0/html5/thumbnails/10.jpg)
Relic Density AnalysisRelic Density Analysis
• Modest choice of parameters yields Modest choice of parameters yields
• High mass: MHigh mass: MSS ~ 500 GeV ~ 500 GeV
• Low mass: MLow mass: MSS<M<MWW ( in progress) ( in progress)
![Page 11: Dark Matter in the Left Right Twin Higgs Model](https://reader034.fdocuments.us/reader034/viewer/2022051316/5681553e550346895dc314a0/html5/thumbnails/11.jpg)
•Two regions:•Bulk•Pole•Due to heavy gauge bosons
Omg hOmg h22 vs M vs MSS
•Can change regions by changing:•f•mass splittings
![Page 12: Dark Matter in the Left Right Twin Higgs Model](https://reader034.fdocuments.us/reader034/viewer/2022051316/5681553e550346895dc314a0/html5/thumbnails/12.jpg)
Contour plot of Omg hContour plot of Omg h22
•MS in bulk region consistent
•Can change regions by changing mass splittings
![Page 13: Dark Matter in the Left Right Twin Higgs Model](https://reader034.fdocuments.us/reader034/viewer/2022051316/5681553e550346895dc314a0/html5/thumbnails/13.jpg)
Direct DetectionDirect Detection
• General idea: observe recoil of detector General idea: observe recoil of detector nuclei from dark matter collisionsnuclei from dark matter collisions
• Contributions from spin independent (SI) Contributions from spin independent (SI) and spin dependent (SD) cross sectionsand spin dependent (SD) cross sections
• Spin independent contribution dominatesSpin independent contribution dominates
![Page 14: Dark Matter in the Left Right Twin Higgs Model](https://reader034.fdocuments.us/reader034/viewer/2022051316/5681553e550346895dc314a0/html5/thumbnails/14.jpg)
Contributing ProcessesContributing Processes• First 2 are First 2 are
difficult to see difficult to see due to small due to small CW couplingsCW couplings• ~(gv)~(gv)22 instead instead
of usual ~(λv)of usual ~(λv)22
•Third process too big Third process too big (~10(~10-31-31 cm cm22))•Current CDMS limit: Current CDMS limit: ~10~10-43-43 cm cm22
•Impose A-S mass Impose A-S mass splitting to avoid splitting to avoid constraint constraint
![Page 15: Dark Matter in the Left Right Twin Higgs Model](https://reader034.fdocuments.us/reader034/viewer/2022051316/5681553e550346895dc314a0/html5/thumbnails/15.jpg)
• SI beats SD SI beats SD by 8 orders by 8 orders of magnitudeof magnitude
• THM THM predicts predicts values below values below future CDMS future CDMS limitslimits
• Difficult!Difficult!
Direct Direct Detection Detection
ExperimentsExperiments
![Page 16: Dark Matter in the Left Right Twin Higgs Model](https://reader034.fdocuments.us/reader034/viewer/2022051316/5681553e550346895dc314a0/html5/thumbnails/16.jpg)
Indirect DetectionIndirect Detection•General idea: dark matter annihilates into General idea: dark matter annihilates into photons, positrons, and neutrinosphotons, positrons, and neutrinos
•Looked at photonsLooked at photons
•Monochromatic photonsMonochromatic photons
•Hadronization and fragmentationHadronization and fragmentation
•Final state charged particle Final state charged particle radiationradiation
![Page 17: Dark Matter in the Left Right Twin Higgs Model](https://reader034.fdocuments.us/reader034/viewer/2022051316/5681553e550346895dc314a0/html5/thumbnails/17.jpg)
Indirect DetectionIndirect Detection
• Γ~(ρ)Γ~(ρ)22
• Increased events for areas of high densityIncreased events for areas of high density• Galactic HaloGalactic Halo• SunSun• EarthEarth
• High dependence on halo dark matter High dependence on halo dark matter density distributiondensity distribution
![Page 18: Dark Matter in the Left Right Twin Higgs Model](https://reader034.fdocuments.us/reader034/viewer/2022051316/5681553e550346895dc314a0/html5/thumbnails/18.jpg)
Monochromatic PhotonsMonochromatic Photons• Photon flux as a function of density:Photon flux as a function of density:
•Parameterize density with J:Parameterize density with J:
•Photon flux as a function of JΔΩ:Photon flux as a function of JΔΩ:
![Page 19: Dark Matter in the Left Right Twin Higgs Model](https://reader034.fdocuments.us/reader034/viewer/2022051316/5681553e550346895dc314a0/html5/thumbnails/19.jpg)
Monochromatic PhotonsMonochromatic Photons
• J gives the clumping of DM near galactic J gives the clumping of DM near galactic centercenter• Highly model dependentHighly model dependent
• 101033 for NFW profile for NFW profile• 101055 for Moore et al profile for Moore et al profile
• ΔΩ indicates field of view of telescopeΔΩ indicates field of view of telescope• 1010-3 -3 sr for ground based ACTs (typical)sr for ground based ACTs (typical)
• JΔΩ~1-100JΔΩ~1-100• Flux scales linearlyFlux scales linearly
![Page 20: Dark Matter in the Left Right Twin Higgs Model](https://reader034.fdocuments.us/reader034/viewer/2022051316/5681553e550346895dc314a0/html5/thumbnails/20.jpg)
Monochromatic PhotonsMonochromatic Photons
•Contributing processesContributing processes•Through loop processes onlyThrough loop processes only
•Difficult to observe due to Difficult to observe due to small couplingssmall couplings•Same problem as with direct Same problem as with direct detection!detection!
![Page 21: Dark Matter in the Left Right Twin Higgs Model](https://reader034.fdocuments.us/reader034/viewer/2022051316/5681553e550346895dc314a0/html5/thumbnails/21.jpg)
Hadronization and FragmentationHadronization and Fragmentation•Number as a function of Number as a function of EEγγ
•Spectra depends only on Spectra depends only on W/Z initial energiesW/Z initial energies
• Contributing processesContributing processes
![Page 22: Dark Matter in the Left Right Twin Higgs Model](https://reader034.fdocuments.us/reader034/viewer/2022051316/5681553e550346895dc314a0/html5/thumbnails/22.jpg)
Hadronization and FragmentationHadronization and Fragmentation•THM predictions THM predictions for 2 regionsfor 2 regions•Detector limits:Detector limits:•GLASTGLAST•ACTsACTs
•Difficult, unless Difficult, unless J is largeJ is large•DM strongly DM strongly clumped at clumped at galactic centergalactic center
GLAST
ACT
BULK
POLE
J ΔΩ = 1J ΔΩ = 1
![Page 23: Dark Matter in the Left Right Twin Higgs Model](https://reader034.fdocuments.us/reader034/viewer/2022051316/5681553e550346895dc314a0/html5/thumbnails/23.jpg)
Final state radiationFinal state radiation
Contributing ProcessesContributing Processes
![Page 24: Dark Matter in the Left Right Twin Higgs Model](https://reader034.fdocuments.us/reader034/viewer/2022051316/5681553e550346895dc314a0/html5/thumbnails/24.jpg)
Final State RadiationFinal State Radiation
•Predictions for Predictions for THMTHM•2 processes2 processes•Unique knee Unique knee signaturesignature•2 orders of 2 orders of magnitude magnitude below detector below detector limitslimits•Difficult!Difficult!
J ΔΩ = 1J ΔΩ = 1
BULK
POLE
![Page 25: Dark Matter in the Left Right Twin Higgs Model](https://reader034.fdocuments.us/reader034/viewer/2022051316/5681553e550346895dc314a0/html5/thumbnails/25.jpg)
ConclusionConclusion• Left Right Twin Higgs Model provides a Left Right Twin Higgs Model provides a
natural dark matter candidatenatural dark matter candidate
• Can explain 100% of dark matter observed Can explain 100% of dark matter observed by WMAPby WMAP
• Direct detection difficultDirect detection difficult
• Indirect detection: hadronization possible, Indirect detection: hadronization possible, other 2 are difficultother 2 are difficult
• Thank you!Thank you!