gamma-ray search of dark matter in spatially-extended
TRANSCRIPT
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Nagisa Hiroshima (KEK, ICRR) Masaaki Hayashida (Konan Univ.), Kaz Kohri (KEK, SOKENDAI)
JPS meeting 2019.3.16
Gamma-ray search of dark matter in spatially-extended dwarf spheroidal
galaxies with CTA
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Introduction
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Weakly Interacting Massive Particle (WIMP)
3
•two model parameters
•mass
•annihilation cross-section
𝒪(1) GeV − 𝒪(1) TeV
Gamma-ray observation is powerful 3
Charles et al., 2016
gamma(satellite)
direct detection
collider
gamma(IACT)
dndt
+ 3Hn = ⟨σv⟩ (n2eq − n2)
mDM
⟨σv⟩ ∼ 𝒪(10−26)cm3/s
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Gamma-ray search of WIMP
4
targetobserver
J-factor
Requirements
DM+DM ->??? -> +…γ
•high J-factor •low astrophysical background
dwarf spheroidal galaxies (dSphs)
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dwarf spheroidal galaxies (dSphs)
5
Hayashi et al.,2016
J-factor changes with models.
•satellite galaxy of the Milky Way •
•angular size
•~40 areidentified
M/L
Δθ ≲ 𝒪(1∘)
∼ 103M⊙/L⊙
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CTA for WIMP
6
•great TeV sensitivity •ability to resolve DM distributions in the center of dSphs
previous analyses assuming dSphs as point sources
↔
How the DM distribution in dSphs affect the sensitivity?
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Motivations
7
•Observation of dSph with CTA should enhance our accessibility to WIMP of •dSphs are good targets of low astrophysical background and high J-factor •Previous analyses usually neglect the spatial extension of dSphs •The importance of the profile should increases with the angular resolution of CTA and it must be quantified.
MDM ≳ 𝒪(1) TeV
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Method
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analyses of simulated data
9using ctools
1.Simulate observations of Draco dSph
2.Select and bin the data
3.Derive 95% confidence level upper limits of gamma-ray flux
500-hour, CTA-North full-array
energy: 0.03-180TeV, 5bin/decade space: , bin in4∘ × 4∘ 0.03∘ × 0.03∘
(b̄b, W+W−, τ+τ−)3 channel , 16 profile for Draco
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Flux from DM annihilation
10
DM + DM → W+W−→ π0 + … → 2γ + …
background
Hiroshima, Hayashida, Kohri in prep
W+W−
→ μ + ν̄μ + … → γ + …
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profiles
11
•16 spherical profiles for Draco in the literature •fitted or compared to stellar data
Hiroshima et al., in prep
log10 J = 18.58log10 J = 18.70
log10 J = 19.15
NFW,No.14
PL(core)+cutoff, No.16Burkert,No.9
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Results
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Conclusion
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Conclusion
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•We can probe WIMPs of TeV with CTA. •dSphs are resolved as extended sources. •Analyses assuming a point-like dSph should overly constrain the annihilation cross-section. •We can derive the particle parameter within a factor of ~10 uncertainty in profile models. •We can probe unexplored regions smaller than for WIMPs. •This is sufficient to test some well-motivated models expecting resonant annihilations.
mDM ≳ 𝒪(1)
⟨σv⟩ = 10−23 − 10−24cm3/s mDM ≳ 𝒪(1)TeV