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MARCH 11 YPM 2015
ray from Galactic Center
Tanmoy Mondal SRF PRL
Dark Matter ?Dark Matter ?
MARCH 11 YPM 2015
Dark Dark MatterMatter
YouLunch**
** Figure is for representative purpose. :-(
MARCH 11 YPM 2015
In this talk
Fermi is not but
Also
Planck is not
MARCH 11 YPM 2015
Study of Galactic cosmic rays and -ray is very active field
Several experiments :PAMELA AMS : mounted on International Space StationLarge Area Telescope (LAT): mounted on Gamma Ray Space Telscope (FermiFermi)
Most detailed map of -ray sky ever
Complementary experiments : Microwave : WMAP, PlanckLow Energy: INTEGRALHigher energy -ray : MAGIC,HESS, VERITASNeutrinos : IceCube
MARCH 11 YPM 2015
Q. What does Fermi-LAT see ?
Galactic Emission
Extra-Galactic (High Altitude) “isotropic” emission
MARCH 11 YPM 2015
Interpretation of Excess
Goodenough, Hooper '09
Hooper, Linden '11
Abazajian, Kaplinghat '12
Yusef-Zadeh et al, '12
Hooper, Slatyer '13
Gordon, Macias '13
Huang, Urbano, Xue '13
Linden et al, '13
Abazajian et al, '14
Daylan et al, '14
Millisecond Pulsers (MSP)
DM
DM
MSP
DM
Nonthermal bremsstrahlung by e- in molecular clouds
DM
DM
Nonthermal bremsstrahlung by e- in molecular clouds
Interactions between the gas and protons accelerated by Sgr A
DM
MARCH 11 YPM 2015
Galactic Diffuse Emission
All the previous analysis has large systematic uncertainties of background emission : GDE
Sources :1)Boosted decayCR scatter inelastically w/ intersteller gas & produce neutral mesons which decays to pairs.2)BremsstrahlungCR electrons scatter w/ intersteller gas 3)Inverse Compton Scattering CR electrons up-scatter low-energy photons via ICS into the gamma-ray energy regime
trace the gas distribution - different in morphology from DMCan potentially mimic DM signal
Depends on : A) CR source distribution and Galactic gas distributionB) Intersteller Radiation Field (ISRF) propertiesC) Galactic magnetic field magnitude, profile etc...
Different assumption on these parameter leads to different GDE models.
MARCH 11 YPM 2015
Calore, Cholis, Weniger (CCW) - 1409.0042
# First study of model systematics coming from the Galactic diffuse emission in the inner part of our Galaxy and their impact on the inferred properties of the excess emission.
What they have done : ~ ROI : 200 X 200 square. Mask inner 20 along Galactic plane.
~ Photon Energy Range : 300 MeV – 500 GeV
~ Studied 60 GDE models to estimate uncertainties due to assumptions.
~ Full ROI has been broken into TEN sections to analyze Fermi-LAT data .
MARCH 11 YPM 2015
Calore, Cholis, Weniger (CCW) - 1409.0042
Conclusion : -- Robust confirmation of a spherically symmetric excess.
-- Centered within 0.05% of GC, hence GCE.
-- Spectrum peaks at 1-3 GeV and extends to 100
-- DM interpretation : hadronic states better than leptonic final states.
-- bb with m45-53 GeV.
v~ 1.78x10-26 cm3s-1
-- MSP ? Not likely
MARCH 11 YPM 2015
CCWM - 1411.4647
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Interpretation depends on GDE
Daylan+ CCW
Fermi Analysis
P6V11
MARCH 11 YPM 2015
What about Fermi collaboration's analysis ?
http://fermi.gsfc.nasa.gov/science/mtgs/symposia/2014/program/08_Murgia.pdf
• Gamma rays in the energy range 1 GeV - 100 GeV
• ROI = 15o x15o square, no masking ( biggest difference from CCW)
• Examine 4 background interstellar emission modelsA) Baseline models: Pulsar or OB star cosmic ray source distributionsB) Tune intensity and spectral indexC) Tune to gamma-rays observed outside ROID) Determine point sources consistently within these models
Excess signal depends strongly on the background model!
Preliminary
MARCH 11 YPM 2015
GCE is confirmed
Astrophysical explanations are less likely
DM Interpretation : hadronic final stated better
A particle physics motivated DM model to explain the excess
Till now
Next
TM and Tanushree Basak, ArXiv:1405.4877
MARCH 11 YPM 2015
U(1)B-L
Extended Standard Model
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Breit-Wigner enhancement
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Summary
Fermi-LAT sees anomalous gamma rays (1-3 GeV energy range) coming from the inner galaxy
Spectrum and morphology prefers annihilating DM to explain the excess
Signal appears to be much harder than previously thought (confirms by Fermi preliminary analysis)
DM annihilating to bb should have mass ~ 50 GeV
U(1)B-L
model can explain the excess
Breit-Wigner enhancement is necessary to boost the annihilation cross-section today near GC.
MARCH 11 YPM 2015
Back Up Slides
MARCH 11 YPM 2015
MilliSecond Pulsar
MARCH 11 YPM 2015