SMILE2+ SubGeV & MeV WIMPレビュー 1...SMILE2+とSubGeV & MeV WIMPレビュー 1 T. Tanimori on...
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1 SMILE2+とSubGeV & MeV WIMPレビュー T. Tanimori on behalf of SMILE-Project, Cosmic-ray group, Physics Division, Kyoto University, Japan 5th/July/2019@Waseda DM Meeting
Transcript of SMILE2+ SubGeV & MeV WIMPレビュー 1...SMILE2+とSubGeV & MeV WIMPレビュー 1 T. Tanimori on...
1SMILE2+とSubGeV & MeV WIMPレビュー
T. Tanimori on behalf of SMILE-Project, Cosmic-ray group, Physics Division, Kyoto University, Japan
5th/July/2019@Waseda DM Meeting
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Contents
➢ Indirect Search in GeV g
mainly Fermi results➢ MeV Sub-MeV DMとは？➢ MeV g region の特徴➢ SMILE 2+ 紹介➢ SMILE2+ 実験の解析➢ まとめ
6C. Boehm @Wein 2016
Astronomical sources ◼ 1. gammas from pion decays
( ex. Stellar bulge, molecular clounds etc)
◼ millisecond pulsars in bulges
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Normalized spectra of 39 MSPs.
Y.Xing and Z.Wang 2016
GeVからMeVへ◼ GeV
Galactic Center Region
astnophysical sources 多数、Steller-bulge, Sgr A*, Molecular Clouds, Millisecond Pulsars,,,,
◼ MeV region <30MeV
gammas mainly from Inverse Compton and Bremss. from electron, positron
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B. LACKI , S.HORIUCHI J F. BEACOM 2014 arXiv:1206.0772v3
Fermi
EGRET
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MeV ~Sub-GeV DM
Mass limit DM >~3MeV from CMB obs.
XX → gg, π0π0->ggg, γϕ-> ggg, ϕϕ→ gggg
XX →e+e-, π+π-, μ+μ-, ϕϕ-> e+e-e+-e Signal gammas from DM ,direct g& radiative g from decayed e
＋ GEV DM からのe+ e-からのsecondary gammasGeV より拡散が小さい！
それ以外 ●Axion Like Particles (ALPs)10MeV gammas from SN （カットする）
●PBH thermail MeV gamma
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Electron Tracking Compton Camera (SMILE-II)
30cm-cubic Gas Time Projection Chamber+ Scintillator Array for scattered g
--- tracking of recoil electron ---Measuring all parameters of Compton process
1.well-defined 2D-PSF similar to Xray & GeV2. dE/dx + kinematical test using a3. large Field of View (>4str)Micro Pixel
Chamber
electron
is a Half Power Radius (HPR)
Measured data (ARM 5o)
PSF(10o)
PSF(1o)
~1 m
30cmETCC
～60㎝
2006 SMILE-I10cm cubic ETCC
SMILE-II 2010~16
Sub-MeV gamma-ray ImagingLoaded-on-balloon Experiment (SMILE-Project)
Eff
ect
ive A
rea
SMILE-II
0.0
1㎝
2
SMILE-II+
SMILE-I
1㎝
2200㎝
2 Satellite-ETCC
SMILE-Ⅲ
From basic research of nuclear g imaging spectroscopy to Satellite observation with sub-m Crab sensitivity (4orders improvements)
Two orderBG rejectionBy dE/dx cut
SMILE-II+ 30cmETCC2016~2020?
SMILE-I Spectrum
SMILE-2+Aim : certificate imaging spectroscopy of ETCC using celestial objects
Targets : e± annihilation line from the galactic center region / Crab nebula
Flight duration ~29 hourslevel flight ~26 hours
SMILE-2+ balloon, Flight Model, ETCC
gandora
SMILE-II+ Exp. 2018 4/7~8 in Alice Spring
gamma-ray
pixel scintillator arrays
hit pixel
e- track
escaped e- event
gamma-ray
e- track
gas detector
pixel scintillator arrays
hit pixel
fully contained e- event
α
Ratio of obtained events 3 : 2
Detection Area
Time Variation of detection rate of gamma-ray events
• Fly horizontally 26 times
• Height ~39 km
• Galaxy center field ~8 time
• After 7 o’clock 4/8heavy nose in TPCNow we used data before 7
Event selection
Single hit in PSA
Fiducial volume
de/dx cut
Kinematical test
Zenith<60°
Preliminary
Zenith
[degre
e]
Event
rate
aft
er
kin
em
atical
cut
[events
/sec]
4/703:00
4/709:00
4/715:00
4/721:00
4/803:00
4/809:00
0
30
60
90
0
2
4
6
8
10
Sun
Crab
Level flight
GC
Used only in this time window
Preliminary
GC
Enhancement looks consistentwith the observation ratio of the cosmic diffusion and galactic diffusion of about 3:1
Cosmic background MeV gammas
Zenith angle more z>60 degrees => more 105 gamma raysBackgrounds of air diffuse & equipment gamma ray are expected less than a few 10% in total.
DM探査➢ 0.5-5MeVのスペクトル変化➢ 全天の2/3をカバー、今後、
超銀河団、銀河団、矮小銀河等との相関を調べる。
Excess gamma rays from Galactic Center 4/7 9:00-13:00 (ACST)
OFF time
Galactic
coordinates
Analysis of the event rate in the ON and OFF Select the high Declination center of the field of view to OFF zenith angle (only available for 30 °)(Currently, because there is indeterminable in the azimuth direction, only the field information is used)
An excess of ~ 511 keV & diffuse components in G.C. is observed.
4/7 18:00-20:30 (ACST)
ON A
10-6
10-5
10-4
10-3
spectrumON-A
OFF
Residual
keV30050
0
1000100
events/sec/keV
4/7 22:00-24:30 (ACST)
ON B
10-6
10-5
10-4
10-3
spectrum
keV30050
0
1000100
events/sec/keV4/8 4:00-6:30 (ACST)
ON C
10-6
10-5
10-4
10-3
spectrum
keV30050
0
1000100
events/sec/keV
ON-B
OFF
Residual
ON-C
OFF
Residual
Excess gammas from Galactic Center
4/8 4:00-6:30 (ACST)
ONTime zone
4/7 9:00-13:00
(ACST)
OFFTime zoneA4/7 21:00-23:00
(ACST)
OFFTime zoneB
10-6
10-5
10-4
10-3
10-6
10-5
10-4
10-3
Energy SpectrumEnergy Spectrum ON
OFF-A
residual
ON
OFF-B
residual
keV300 50
0
1000 3000100keV300 50
0
1000 3000100
4.90 σ 5.36 σ
Galactic coordinates
Analysis of the event rate in the ON and OFF time zones OFF of the View Center is far from the galactic planeSelect two time zones Ground coordinate zenith angle (only available for 30 °)
events/sec/keV events/sec/ke
V
Excess : 11.5 σ Excess: 10.3 σ
Comparison of significance with other observations
Same time with COSI : ~5 σ ×6.1 ×105sec
6.4 ×103sec= 20~48 σ
511 keV bin over duffuse ~2 σSMILE-2+ 511 keV bin ~5 σ
INTEGRAL/SPI same time: ~5σ ×1.6 × 109 cm2 sec /75cm²
6.4 ×103sec= 140~295 σ
10−6
10−5
10−4
events
/sec/k
e
V
500
10−3
100 1000 keV
keV510500 520
INTEGRAL/SPI
Siegert et al. 2016
SMILE-2+ COSI 2016
Chiu et al. 2017
Balloon46 Days~34 km
BG 1/8
・511 keV line 58 σ
・3-gammas 29 σ
・combined 65 σ
Instum. Eff. Area ΔE/E Normalized Sensitivity to SPI
SPI 75cm2 <1% １ Coded Mask with Veto
COSI ~10cm2 <1% 5 x Conventional CC with Veto
SM2+ 1cm2 13% 100ー200 x ETCC with no-veto
galactic diffuse gamma raysevents
/sec/k
e
V
10-5
10-4
10-3
10-6
差分
1000500100 3000300keV
Energy Spectrum
clarify the radiation mechanism of the
diffuse Mev gamma rays
Strong
+(2011)
All excess : 10～11σ
COMPTEL
INTEGRL
Expected Sensitivity based on well-defined PSF
ETCC-Satellite 50cm-cubic ETCC (CF4 3atm) with >5RL Scinti. x 4 modules Effective Area ~200cm2@1MeV and PSF:HPR-2o
SMILE2 + = > Crab, Galaxy 511keV Galaxy diffuse & cosmic background MeV gamma Detected by the sensitivity as planned = > The world's first in MEV!!we have certificated a high realiability of ETCC
For Continuum g (106 sec)
New MeV gamma Astronomy beynond 1mCrab
６０Ｍｐｃ SN ~20SNe/year
ラインガンマ線はさらに1桁近い感度向上。
PSF by HPR
Summary
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◆SM2＋ in the ETCC technology demonstrated in the Compton area (50kev-30MeV) imaging spectroscopic technique for the first time, as well as x-ray, GEV,
◆GeV 領域 Astrophysical sourcesが多く、DMとの判断が困難。
◆GeV、sub-GeV. MeV のDM信号は30MeV以下の電子の寄与のみの領域が最も判別が確かであり、今後重要となる。
◆GeV-MeV 全天探査が可能、銀河と他の銀河、銀河団などが同時に測定できる。
◆SM2+のデータ DM関係で、Galactic Diffuse gamma（スペクトル、分布）, Cosmic Diffuse gamma（スペクトル、分布）, PBH in Solar system の論文は出す
◆ Balloon SMILE-3 project with NASA long duration balloon ＝＞ 5times better sensitivity than COMPTEL
◆2020年代 sau-MeV, MEV はSMILEの独断場の可能性大！
3
15
103
g10yr 10~~
MM
215
1-20 g10s erg10~
d
d
Mt
E
M
g10MeV100~
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Primordial Black Holes in Solar System
Primordial B.H. still survivingwould emit ~20MeV thermal M~ 1015 g , ~ 1020 erg/s
Density ~104 pc-3 (flat 分布で）104 pc-3 -> ~10 BH <Oort cloud (104AU)
Condensation Factor in Galactic halos x ~106
＝＞ 100AU 球に~10BHs
Satellite-ETCC g線１０個 (1MeV)s-1 @1AU for 1020erg/s
ＢＨが106ｓの間同じ天球位置として、検出限界100g@106sこの場合、300ＡＵのＢＨまで観測可能 数10個のＢＨが見える。さらに太陽系の増幅効果、ディスク（黄道面）分布、太陽近傍集中1桁以上の増加、さらにコメット軌道（数日、明るい）、
Crab (0.2-0.8MeV)
Enhancement of gamma-rays
Obs, time ~104sec, 3s
=>Obs. time~106sec, ~0.1 Crab(3sdetection)
Achieved for the first time that observed sensitivity is consistent with original design in MeV gamma-ray telescopes
10-6
10-5
10-4
[co
un
ts/s
ec/k
eV]
Sensitivity
102103102
Designed sensitivity in SM2+
This results
ON-regionOFF-region
ON –OFF
Expected flux
Crab-ONCrab-OFF
Crab-
Trajectory of FoV of SM2;+
Here pointing is done only for Zenith
Comment
In COSI, 511keV signal from G.C. is obtained by the subtraction of ~70times large 511kev background peak.
In SMILE2+., as shown in light curve of gammas, gamma rate of G.C. region was stronger than the
background region ( side region of Galactic plane),
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