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高感度CMOSカメラシステムによる高速飛翔暗黒物質と流星の探索
DIMS Project for Dark Matter and Interstellar Meteoroid
Study
F. Kajinoa, R. Idea, M. Arahoria, S. Tadaa, K. Nadamotoa, K.
Shinozaki c
M. Bertainab,c, A. Cellinob,d, Y. Tamedag, Y. Iwamig, M.
Casolinoe,f, T. Ebisuzakie
Y. Takizawae, L. W. Piotrowskie, H. Sagawah, J. Matthewsi, S.
Abej, K. Leek, I.H. Parkk
aDepartment of Physics, Konan University, Kobe, Japan
bIstituto Nazionale di Fisica Nucleare - Sezione di Torino,
Italy
cDipartimento di Fisica, Universita' di Torino, Italy
dOsservatorio Astrofisico di Torino, Istituto Nazionale di
Astrofisica, Italy
eRIKEN, Wako, Japan, fIstituto Nazionale di Fisica Nucleare -
Sezione di Roma Tor Vergata, Italy
gDepartment of Engineering Science, Osaka Electro-Communication
University, Neyagawa, Japan
hICRR, University of Tokyo, iDepartment of Physics &
AstronomyUniversity of Utah, USA
jDepartment of Aerospace Engineering, Nihon University,
Funabashi, Japan
kDepartment of Physics, Sungkyunkwan University, Jang-an-gu,
Korea
DIMS Collaboration
令和元年度東京大学宇宙線研究所 共同利用研究成果発表会
東京大学柏キャンパス、2019年12月15日（土）
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研究目的
• 暗黒物質の候補の一つであるNucleariteの探索
• 流星、特に太陽系外起源の流星の観測
• その他の大気発光現象
• EUSO-TAやMini-EUSOなどとの共同観測
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査定額と使途• 査定額 研究費：2万円、旅費：30万円、合計：32万円
• 使途 ユタへの出張旅費
および現地での実験用物品購入費
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What The Universe Is Made Of
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ordinary matter 5%
ordinary matter
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Dark Matter Candidates• Weakly Interacting Massive Particles
(WIMPs)
• Axions
• Primordial Black Holes
• Exotic Candidates
WIMPzillas, gravitinos, gluinos
Q-balls, Q-nuggets, SIMPS
Fermi Balls, EW Balls and GUT Balls
New Class of Dark Matter Objects
Mirror Dark Matter …
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K. Arun et al. arXiv 1704.06155
Glenn Starkman, 2015
Dark matter doesn’t have to interact weakly
if it’s very massive. → Macro Dark Matter
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dd
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udd
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uud u
ud
udd
s
udu du
d
dudd
u
d
dud
dud u
du
udu
udu
u
du
ud s
s
ss
s
ss s
s
s
s
s
ss
s
Strange Quark Matter & Nuclearite
通常の原子核 Strange Quark Matter (SQM)
および Strangelet
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Nuclearite はSQMの周りが電子で覆われた電気的に中性な塊である。
Quark 3個の組み合わせからなる核子の集合体 u, d, s quark がほぼ同数からなる
quark の集合体E. Witten 1984
A. De Rujula & S. L. Glashow, 1984
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R=105 fmR=104 fmR=103 fm
Nuclearites
RH=5*104 fm
H atom
e-
nucleus SQM
Nuclearite
e-
e-
RN=10 km
(Neutron star)
SQM
e-e-
• Nuclearite
の大きさは原子核程度のものから中性子星程度のものまで様々あり、SQMのサイズが大きくなると電子がSQM内部に入ってくる。
• 暗黒物質の一候補。
• 中性子星については理論的に様々な形態が提案されている。
• いくつかの中性子星はquark星の可能性があると指摘されている。
• Nuclearite は宇宙初期や中性子星同士の衝突でできる可能性がある。
• これまでに、加速器による生成実験や、自然界にSQMやNuclearite
が存在しているかどうかの実験が行われてきた。地震計による探索など。 6
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Interstellar Meteoroids
from Outside the Solar System
Meteoroid Mass
Flu
x
1g
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DIMS Observation Concept
Meteor observation
zone
Nuclearite
search zone
〜100km
〜30km
Earth surfaceObservation Instrument 8
TLE’s
(transient luminous events)
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Test of Observation System
Video
Capture
PC
Windows 10
UFO
Capture
USB Cable
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HDMI Cable
UFO Capture:
motion capture
softwareCanon ME20F-SH
Monochrome type
Observation at TA-BRM
Aug. 31, 2019
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Past Observation Periods and Sites
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• Dec. 25th -28th, 2017
• Ishigaki, Okinawa, Japan
• Jan. 1st -4th, 2017
• Okamoto and Miki, Hyogo, Japan
• Aug. 20th -Sept. 1st, 2017
• Telescope Array site Utah, USA
• Sept. 7th -11th, 2018
• Telescope Array site, Utah
TA site @ Utah • Aug. 28th –Sept. 1st, 2019
• Telescope Array site, Utah
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Past Observation Summary（2017-2019）
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Obs. period Feature ISO sensitivityNumber of
meteorsMeteor Type
Jan
2017
Stereo obs.
at Okamoto
and Miki
102,400
~34shower from
Quadrantids
~46 sporadic
13 coincident
Aug – Sept
2017
Single camera
at TA site
51,200 ~
409,600329 sporadic
Dec
2017
3 types of
cameras
at Ishigaki,
Okinawa
204,800 318 sporadic
Sept
2018
Stereo obs.
by 3 cameras
at TA site
204,800 ~2000 sporadic
Sept
2019
Stereo obs.
by 2 cameras
at TA site
204,800 3840 sporadic
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CLF
BRM
HinckleyCLF
Observation and Site Investigation at TA site
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We observed meteors at 3 sites of TA using 2 high
sensitivity
CMOS cameras from Aug. 28 to Sept. 1 for 4 nights in 2019.
Future potential camera positions are also investigated.
BRM
Hinckley
CLF
Candidate camera position
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Composite photo taken at Hinckley, Utah N1 camera, detect size =
2&3, incl. cont. rec., IR = on4th night: 8/31 22:29 - 9/1 5:00
MDT, 2019 (6h 31min)
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Composite photo taken at BRM, Utah N2 camera, detect size = 2,
IR = on4th night: 8/31 22:30 - 9/1 5:00 MDT, 2019 (6h 30min)
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Simultaneous Events4th night: 8/31 22:29 – 9/1 5:00 MDT, 2019
(6h 31min)
N1, Hinckley N2, BRM
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６
1
11
4
7
About 75% of events in N1 are observed simultaneously in N2.
Number of the simultaneous events are estimated to be roughly
400 in this night.
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Observed Number of Meteors
16
0
100
200
300
400
500
600
700
800
900
1000
08/29 08/30 08/31 09/01
Nu
mb
er
of
Me
teo
r E
ven
ts
Date (UTC)
N1
N2
Aug. 29th – Sep. 1 UTC, 2019 (4 nights)
0
100
200
300
400
500
600
08/29 08/30 08/31 09/01O
bse
rva
tio
n T
ime
(m
in)
Date (UTC)
N1
N2
N1: 1733 events
N2: 2107 events
N1+N2: 3840 events
N1: 1129 min = 18.8 h
N2: 1288 min = 21.5 h
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Flux vs. Magnitude of Meteors
CMOS mosaic camera Tomo-e PM (Ohsawaet al.,2019)
Tomo-e PM, Kiso Obs.105cm, 1.98deg2, 2Hz
No.1 System: present result
No.2 System: present result
No.1 System
D=25mm, 1620 deg2, 29.97Hz
No.2 System
D=41mm, 900 deg2, 29.97Hz
Our preliminary results from No.1 System and No.2 System are
consistent with other observational results.
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Camera Station
Camera is mounted on a altazimuth mount and is controlled
remotely.
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。
Conceptual design of the camera station
FoV
56˚x33 ˚
Monitor
DAQ/Control
PC
Battery
Communication
Antenna
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DIMS Observation System
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Central
Control PC
Analysis PC
Data Server
Obs. Station PC
Obs. Station PC
Obs. Station PC
Analysis PC HDDs are sent from Utah to Japan every
1 or 2 month
All data are
stored in HDDs
Obs. Station PC
Japan Utah
HDD
HDD
HDD
HDD
HDDs
Italy, USA, Korea …
Control PC
utdims01
utdims02
utdims03
utdims04
kudims01
kudims02kudims03
kudims04
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まとめ
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高感度CMOSカメラで多くの流星を動画で観測できるシステムを試験してきた。
星は8-9等まで、流星は5-6等程度まで動画で観測できることが分かった。
Macro Dark Matter や太陽系外流星の探索のためのDIMS (Dark Matter and
Interstellar Meteoroid Study)
Project を開始した。
12月7日（土）に、1st DIMS Workshop を理研で開催した。
国際協力体制（日・米・伊・韓）を整備中。
