development of nuclear emulsion for cosmic ray...
TRANSCRIPT
![Page 1: Development of Nuclear Emulsion for Cosmic Ray Radiographyflab.phys.nagoya-u.ac.jp/2011/ICMASS2017/manabe_ICMaSS2017.pdf · Development of Nuclear Emulsion for Cosmic Ray Radiography](https://reader031.vdocuments.us/reader031/viewer/2022040310/5d404f9e88c99391748c0d92/html5/thumbnails/1.jpg)
Development of Nuclear Emulsion for Cosmic Ray Radiography
-Thick supporting base type emulsion-
Yuta Manabe, Kunihiro Morishima, Nobuko Kitagawa, Akira Nishio, Mitsuaki Kuno
Department of Science, Nagoya University
ICMaSS 2017/09/30
![Page 2: Development of Nuclear Emulsion for Cosmic Ray Radiographyflab.phys.nagoya-u.ac.jp/2011/ICMASS2017/manabe_ICMaSS2017.pdf · Development of Nuclear Emulsion for Cosmic Ray Radiography](https://reader031.vdocuments.us/reader031/viewer/2022040310/5d404f9e88c99391748c0d92/html5/thumbnails/2.jpg)
Cosmic-Ray Radiography
muon
Mt.Showahshinzan
Detector
Alfred Tang et al. PHYSICAL REVIEW D 74, 053007
(2006)
Detect particle trajectory
・Archeology remains
・Blast furnace・Nuclear power plant
・Non-destructive inspection for large structure.・Detect CR muon, calculate energy loss.・Estimate target’s material density
![Page 3: Development of Nuclear Emulsion for Cosmic Ray Radiographyflab.phys.nagoya-u.ac.jp/2011/ICMASS2017/manabe_ICMaSS2017.pdf · Development of Nuclear Emulsion for Cosmic Ray Radiography](https://reader031.vdocuments.us/reader031/viewer/2022040310/5d404f9e88c99391748c0d92/html5/thumbnails/3.jpg)
Estimate material density by detected muons
Red:High material density↑Blue:Low material density
We need high angular accuracy
Final imaging resolution is decided by detector’s resolution
・Archeology remains
・Blast furnace・Nuclear power plant
Cosmic-Ray Radiography
Alfred Tang et al. PHYSICAL REVIEW D 74, 053007
(2006)
Detector
![Page 4: Development of Nuclear Emulsion for Cosmic Ray Radiographyflab.phys.nagoya-u.ac.jp/2011/ICMASS2017/manabe_ICMaSS2017.pdf · Development of Nuclear Emulsion for Cosmic Ray Radiography](https://reader031.vdocuments.us/reader031/viewer/2022040310/5d404f9e88c99391748c0d92/html5/thumbnails/4.jpg)
Structure of Nuclear Emulsion
Microscopic view
High spatial resolution ( < 1mm)
100mm
1mm
Development
AgBr crystal
Gelatin
Supporting base(Polystyrene)
70mm
175mm
70mm
Emulsion Layer
Emulsion Layer
Producing in Nagoya University
![Page 5: Development of Nuclear Emulsion for Cosmic Ray Radiographyflab.phys.nagoya-u.ac.jp/2011/ICMASS2017/manabe_ICMaSS2017.pdf · Development of Nuclear Emulsion for Cosmic Ray Radiography](https://reader031.vdocuments.us/reader031/viewer/2022040310/5d404f9e88c99391748c0d92/html5/thumbnails/5.jpg)
Emulsion Cloud Chamber(=ECC)
Estimate momentum by multiple coulomb scattering
𝜃𝑖 = 𝜃𝑠𝑐𝑎𝑡2 + δ𝜃𝑖
2
𝜃𝑠𝑐𝑎𝑡
Momentum estimate to reject back ground(Low energy particles)
We need high angular accuracy
![Page 6: Development of Nuclear Emulsion for Cosmic Ray Radiographyflab.phys.nagoya-u.ac.jp/2011/ICMASS2017/manabe_ICMaSS2017.pdf · Development of Nuclear Emulsion for Cosmic Ray Radiography](https://reader031.vdocuments.us/reader031/viewer/2022040310/5d404f9e88c99391748c0d92/html5/thumbnails/6.jpg)
Detection Principle of Nuclear Emulsion
Supporting Base: 175um
Emulsion Layer: 70um
Charged particle
Taking slice images of emulsion layers→Judge particles tracks by developed grains linearly.
Connecting both side tracks→Reconstruct tracks with corrected distortion of emulsion layer (gelatin).
Emulsion Layer: 70um
![Page 7: Development of Nuclear Emulsion for Cosmic Ray Radiographyflab.phys.nagoya-u.ac.jp/2011/ICMASS2017/manabe_ICMaSS2017.pdf · Development of Nuclear Emulsion for Cosmic Ray Radiography](https://reader031.vdocuments.us/reader031/viewer/2022040310/5d404f9e88c99391748c0d92/html5/thumbnails/7.jpg)
Definition of Angular Accuracy
δ tan 𝜃𝑥 =1
𝑙2𝛿𝑥2 × 2 +
𝑥2 − 𝑥1𝑙2
2
𝛿𝑙2
=2
𝑙𝛿𝑥2 + 𝛿𝑧2 × tan 𝜃𝑥
2
Base
Emulsion
Emulsion
x1
x2
𝜃𝑥 𝑙 𝛿𝑙 = 2𝛿𝑧
z2
z1
tan 𝜃𝑥 =𝑥2 − 𝑥1
𝑙
=𝑥2 − 𝑥1𝑧2 − 𝑧1
We expect to improve angular accuracy by using thick type base.
(From optical design of scanning machine, the limit of all thickness is 1mm.)
![Page 8: Development of Nuclear Emulsion for Cosmic Ray Radiographyflab.phys.nagoya-u.ac.jp/2011/ICMASS2017/manabe_ICMaSS2017.pdf · Development of Nuclear Emulsion for Cosmic Ray Radiography](https://reader031.vdocuments.us/reader031/viewer/2022040310/5d404f9e88c99391748c0d92/html5/thumbnails/8.jpg)
Base CandidatesBase
MaterialsPS TAC PMMA COP PC
BaseThickness
[㎛]
70 175 90 205 200 800 500 300
Water Absorption[Wight%]
0.01~0.03 3.3~3.8 0.1~0.4 <0.01 0.15
Refractive index
1.59 1.49 1.53 1.53 1.59
Birefringence
[nm]- 1.4 3.5 3.6 7.5
Experiments WA75 NowUsing
CHORUS,DONUTS
OPERA CHORUS,DONUTS
CHORUS,DONUTS
UnderInvestigation
UnderInvestigation
Start of Experiments
1983~ 2014~ 1994~,1997~
2006~ 1994~,1997~
1994~,1997~
Emulsionthickness
[㎛]
330 70 350 44 100 100
Water Absorption is literature data
![Page 9: Development of Nuclear Emulsion for Cosmic Ray Radiographyflab.phys.nagoya-u.ac.jp/2011/ICMASS2017/manabe_ICMaSS2017.pdf · Development of Nuclear Emulsion for Cosmic Ray Radiography](https://reader031.vdocuments.us/reader031/viewer/2022040310/5d404f9e88c99391748c0d92/html5/thumbnails/9.jpg)
Improvement of Angular Accuracy Test 1
10000
6000
2000
0
4000
8000
[En
try]
[𝒕𝒂𝒏𝜽𝒙]0.0 0.5 1.0-0.5-1.0
• Beam : π−
• Energy : 5GeV• Density : 103/𝑐𝑚2
• Exposure area : 5 × 12.5𝑐𝑚2
• Emulsion Base Type:175㎛PS, 500㎛COP
Magnet(B=0)
[𝒕𝒂𝒏𝜽𝒚]
0.50 [𝒕𝒂𝒏𝜽𝒙]-0.5-1.0
0.5
0-0
.5-1
.01
.0
2D Histogram of test beams
1D Histogram of test beams
![Page 10: Development of Nuclear Emulsion for Cosmic Ray Radiographyflab.phys.nagoya-u.ac.jp/2011/ICMASS2017/manabe_ICMaSS2017.pdf · Development of Nuclear Emulsion for Cosmic Ray Radiography](https://reader031.vdocuments.us/reader031/viewer/2022040310/5d404f9e88c99391748c0d92/html5/thumbnails/10.jpg)
Angular Accuracy of Vertical Tracks
δ tan𝜃𝑥 =2
𝑙𝛿𝑥2 + 𝛿𝑧2 × tan𝜃𝑥
2
To investigate base thickness dependence of angular accuracy, I use the beam spot of 𝑡𝑎𝑛𝜃 = 0.0 ± 0.02
At the point of 𝑡𝑎𝑛𝜃 = 0.0 , second term of δ tan 𝜃𝑥 = 0→Angular accuracy is expected near to be inversely proportional to the base thickness.
• Calculate angle difference of each tracks
• Define angular accuracy as 1𝜎 of its histogram.
𝜃1
𝜃2
![Page 11: Development of Nuclear Emulsion for Cosmic Ray Radiographyflab.phys.nagoya-u.ac.jp/2011/ICMASS2017/manabe_ICMaSS2017.pdf · Development of Nuclear Emulsion for Cosmic Ray Radiography](https://reader031.vdocuments.us/reader031/viewer/2022040310/5d404f9e88c99391748c0d92/html5/thumbnails/11.jpg)
Angular Accuracy of Vertical Tracks 175㎛PS・500㎛COP Emulsions
Solid Line:500㎛COP Emulsion1σ=0.972 ± 0.006 × 10−3
Dashed line:175㎛PS Emulsion1σ=2.62 ± 0.016 × 10−3
[ 𝟐 ∗ δ𝒕𝒂𝒏𝜽𝒙]
[Entry]
Ratio of base thickness :500𝜇𝑚
175𝜇𝑚= 2.86
Ratio of angular accuracy :2.62 × 10−3
0.972 × 10−3= 2.70
PS COP
Base thickness
175 500
Angular accuracy
2.62 ± 0.016× 10−3
0.972 ± 0.006× 10−3
Not contain base material effects
![Page 12: Development of Nuclear Emulsion for Cosmic Ray Radiographyflab.phys.nagoya-u.ac.jp/2011/ICMASS2017/manabe_ICMaSS2017.pdf · Development of Nuclear Emulsion for Cosmic Ray Radiography](https://reader031.vdocuments.us/reader031/viewer/2022040310/5d404f9e88c99391748c0d92/html5/thumbnails/12.jpg)
Improvement of Angular Accuracy Test 2
Location:Outdoor tentDirection:Horizontal to the groundPeriod:3days
Investigate base dependence of angular accuracy, using same angle as the beam,
−𝟎. 𝟎𝟐 < 𝒕𝒂𝒏𝜽 < 𝟎. 𝟎𝟐
・175㎛ PS base emulsion・300㎛ PC base emulsion
35m
30m
[𝒕𝒂𝒏𝜽𝒚]
0.50
[𝒕𝒂𝒏𝜽𝒙]
-0.5-1.0
0.5
0-0
.5-1
.01
.0
1.0
2D Histogram of Detected Cosmic Ray
![Page 13: Development of Nuclear Emulsion for Cosmic Ray Radiographyflab.phys.nagoya-u.ac.jp/2011/ICMASS2017/manabe_ICMaSS2017.pdf · Development of Nuclear Emulsion for Cosmic Ray Radiography](https://reader031.vdocuments.us/reader031/viewer/2022040310/5d404f9e88c99391748c0d92/html5/thumbnails/13.jpg)
Angular Accuracy of Vertical Tracks 175㎛PS・300㎛PC Emulsions
Solid Line:300㎛PC Emulsion1σ=1.49 ± 0.10 × 10−3
Dashed Line:175㎛PS Emulsion1σ=2.53 ± 0.18 × 10−3
[ 𝟐 ∗ δ𝒕𝒂𝒏𝜽𝒙]
[Entry]
Raito of base thickness :300𝜇𝑚
175𝜇𝑚= 1.71
Raito of angular accuracy :2.53×10−3
1.49×10−3= 1.70
PS PC
Base thickness
175 300
Angular accuracy
2.53 ± 0.18× 10−3
1.49 ± 0.10× 10−3
Not contain base material effects
![Page 14: Development of Nuclear Emulsion for Cosmic Ray Radiographyflab.phys.nagoya-u.ac.jp/2011/ICMASS2017/manabe_ICMaSS2017.pdf · Development of Nuclear Emulsion for Cosmic Ray Radiography](https://reader031.vdocuments.us/reader031/viewer/2022040310/5d404f9e88c99391748c0d92/html5/thumbnails/14.jpg)
Summary of Angular Accuracy of Vertical Tracks
[ 𝟐 ∗ δ𝒕𝒂𝒏𝜽𝒙 × 𝟏𝟎−𝟑]
𝑩𝒂𝒔𝒆 𝒕𝒉𝒊𝒄𝒌[㎛]
δ tan 𝜃𝑥 =2
𝑙𝛿𝑥2 + {𝛿𝑧2 × tan𝜃𝑥
2 = 0}
Power approximation curve is
It is approximately inversely proportional.
And,𝛿𝑥 is calculated ~0.55 ㎛ from this value, which is in agreement with the known value in the order.
0
0.5
1
1.5
2
2.5
3
0 200 400 600
𝑦 = 7.75 × 10−7𝑥−0.936
Red:175㎛PS_CRBlack:175㎛PS_BeamBlue:300㎛PC_CRGreen:500㎛COP_Beam
![Page 15: Development of Nuclear Emulsion for Cosmic Ray Radiographyflab.phys.nagoya-u.ac.jp/2011/ICMASS2017/manabe_ICMaSS2017.pdf · Development of Nuclear Emulsion for Cosmic Ray Radiography](https://reader031.vdocuments.us/reader031/viewer/2022040310/5d404f9e88c99391748c0d92/html5/thumbnails/15.jpg)
Angle Dependence of Angular Accuracy Test
𝑡𝑎𝑛𝜃𝑥 = 0.0, 0.2, 0.4…1.0𝑡𝑎𝑛𝜃𝑦 = 0.0
Each points ±𝑡𝑎𝑛𝜃 = 0.05
𝑡𝑎𝑛𝜃𝑥 = 0.0, 0.1, 0.2…1.0𝑡𝑎𝑛𝜃𝑦 = 0.0
Each points ±𝑡𝑎𝑛𝜃 = 0.05
2D Histogram of Detected Cosmic Ray
[𝒕𝒂𝒏𝜽𝒚]
0.50
[𝒕𝒂𝒏𝜽𝒙]
-0.5-1.0
0.5
0-0
.5-1
.01
.0
1.0
[𝒕𝒂𝒏𝜽𝒚]
0.50
[𝒕𝒂𝒏𝜽𝒙]-0.5-1.0
0.5
0-0
.5-1
.01
.0
1.0
2D Histogram of test beam
![Page 16: Development of Nuclear Emulsion for Cosmic Ray Radiographyflab.phys.nagoya-u.ac.jp/2011/ICMASS2017/manabe_ICMaSS2017.pdf · Development of Nuclear Emulsion for Cosmic Ray Radiography](https://reader031.vdocuments.us/reader031/viewer/2022040310/5d404f9e88c99391748c0d92/html5/thumbnails/16.jpg)
Results1. Thick base type emulsion’s angular accuracy is better than more thin one.
2. Angular accuracy is deferent betweensame base emulsion.
Red:175㎛PS_CRBlack:175㎛PS_BeamBlue:300㎛PC_CRGreen:500㎛COP_Beam
Preliminary
[𝒕𝒂𝒏𝜽𝒙]
[δ𝒕𝒂𝒏𝜽𝒙]
Consideration of Result_2・Deference of angular distribution
・Deference of set up ・Deference of statistics
Angle Dependence of Angular Accuracy TestResult , Consideration
![Page 17: Development of Nuclear Emulsion for Cosmic Ray Radiographyflab.phys.nagoya-u.ac.jp/2011/ICMASS2017/manabe_ICMaSS2017.pdf · Development of Nuclear Emulsion for Cosmic Ray Radiography](https://reader031.vdocuments.us/reader031/viewer/2022040310/5d404f9e88c99391748c0d92/html5/thumbnails/17.jpg)
Base Candidates (New Beam Test Samples)
吸水率、熱膨張率は文献値、屈折率・複屈折率は測定値
ベース素材 PS(Polystyrene)
PMMA(PolyMethylMethAcrylate,
Acryl)
COP(CycloOlefin
Ploymer)
PC(PolyCarbonate)
Glass
Refractive index 1.57 1.48 1.53 1.58 1.52
Birefringence
[nm]- 3.5 3.6 7.5 -
Water Absorption[Wight%]
0.01~0.03 0.1~0.4 <0.01 0.15
Coefficient of thermal expansion
[cm/cm℃]
5.0~8.3 × 10−5 5.0~9.0 × 10−5 7 × 10−5 6.8 × 10−5 7.2 × 10−6
Base Thickness[㎛]
175 500 500 300 300500700
Water Absorption & Coefficient of thermal expansion is literature data,
![Page 18: Development of Nuclear Emulsion for Cosmic Ray Radiographyflab.phys.nagoya-u.ac.jp/2011/ICMASS2017/manabe_ICMaSS2017.pdf · Development of Nuclear Emulsion for Cosmic Ray Radiography](https://reader031.vdocuments.us/reader031/viewer/2022040310/5d404f9e88c99391748c0d92/html5/thumbnails/18.jpg)
Conclusion
• We are developing thick supporting base type nuclear emulsion for improvement of angular accuracy to use cosmic-ray radiography.
• In beam test and observation of cosmic-ray, We confirmed improvement of angular accuracy by using thick type base.
• Next step, using new beam test samples , we’ll evaluate several base type emulsion’s performance inclusive angle dependence of angular accuracy.
JST「原子核乾板を用いた高精度宇宙線ラジオグラフィシステムの開発」
![Page 19: Development of Nuclear Emulsion for Cosmic Ray Radiographyflab.phys.nagoya-u.ac.jp/2011/ICMASS2017/manabe_ICMaSS2017.pdf · Development of Nuclear Emulsion for Cosmic Ray Radiography](https://reader031.vdocuments.us/reader031/viewer/2022040310/5d404f9e88c99391748c0d92/html5/thumbnails/19.jpg)
![Page 20: Development of Nuclear Emulsion for Cosmic Ray Radiographyflab.phys.nagoya-u.ac.jp/2011/ICMASS2017/manabe_ICMaSS2017.pdf · Development of Nuclear Emulsion for Cosmic Ray Radiography](https://reader031.vdocuments.us/reader031/viewer/2022040310/5d404f9e88c99391748c0d92/html5/thumbnails/20.jpg)
角度精度の角度依存性評価
10000
6000
2000
0
4000
8000
[Entry]
[𝒕𝒂𝒏𝜽𝒙] 0.0 0.5 1.0-0.5-1.0
[Entry]
[𝒕𝒂𝒏𝜽𝒙]
1D Histogram of test beam 1D Histogram of Detected Cosmic Ray
𝑡𝑎𝑛𝜃𝑥 = 0.0, 0.2, 0.4…1.0𝑡𝑎𝑛𝜃𝑦 = 0.0
のピーク+-0.05で切り出す
𝑡𝑎𝑛𝜃𝑥 = 0.0, 0.1, 0.2…1.0𝑡𝑎𝑛𝜃𝑦 = 0.0
の点+-0.05で切り出す
![Page 21: Development of Nuclear Emulsion for Cosmic Ray Radiographyflab.phys.nagoya-u.ac.jp/2011/ICMASS2017/manabe_ICMaSS2017.pdf · Development of Nuclear Emulsion for Cosmic Ray Radiography](https://reader031.vdocuments.us/reader031/viewer/2022040310/5d404f9e88c99391748c0d92/html5/thumbnails/21.jpg)
PC(ポリカーボネート) 300㎛屈折率=1.58複屈折率=7.5nm
COP(シクロオレフィンポリマー) 500㎛屈折率=1.53複屈折率=3.6nm
・支持体と乳剤層の屈折率差の効果(乳剤層の屈折率~1.5)
・複屈折率が高いことによる像のボケ
屈折率・副屈折率の違いによる見え方の差
コンプトン電子の飛跡が見える
コンプトン電子の飛跡は殆ど見えない
![Page 22: Development of Nuclear Emulsion for Cosmic Ray Radiographyflab.phys.nagoya-u.ac.jp/2011/ICMASS2017/manabe_ICMaSS2017.pdf · Development of Nuclear Emulsion for Cosmic Ray Radiography](https://reader031.vdocuments.us/reader031/viewer/2022040310/5d404f9e88c99391748c0d92/html5/thumbnails/22.jpg)
散乱効果による画像のボケ
18m
15m
溶鉄耐火レンガ検出器
溶鉄10mを貫通したミューオンの散乱による画像ボケ
[cm]
[GeV]0 10 20 30
185
37
20
300
10m
溶鉄耐火レンガコークス鉄鉱石
18m
50m
散乱されやすい低運動量のミューオンを識別する必要がある
![Page 23: Development of Nuclear Emulsion for Cosmic Ray Radiographyflab.phys.nagoya-u.ac.jp/2011/ICMASS2017/manabe_ICMaSS2017.pdf · Development of Nuclear Emulsion for Cosmic Ray Radiography](https://reader031.vdocuments.us/reader031/viewer/2022040310/5d404f9e88c99391748c0d92/html5/thumbnails/23.jpg)
Glass 500㎛屈折率=1.52複屈折率=未測定
![Page 24: Development of Nuclear Emulsion for Cosmic Ray Radiographyflab.phys.nagoya-u.ac.jp/2011/ICMASS2017/manabe_ICMaSS2017.pdf · Development of Nuclear Emulsion for Cosmic Ray Radiography](https://reader031.vdocuments.us/reader031/viewer/2022040310/5d404f9e88c99391748c0d92/html5/thumbnails/24.jpg)
COP 500㎛屈折率=1.53複屈折率=3.6nm
![Page 25: Development of Nuclear Emulsion for Cosmic Ray Radiographyflab.phys.nagoya-u.ac.jp/2011/ICMASS2017/manabe_ICMaSS2017.pdf · Development of Nuclear Emulsion for Cosmic Ray Radiography](https://reader031.vdocuments.us/reader031/viewer/2022040310/5d404f9e88c99391748c0d92/html5/thumbnails/25.jpg)
PC 300㎛屈折率=1.58複屈折率=7.5nm
![Page 26: Development of Nuclear Emulsion for Cosmic Ray Radiographyflab.phys.nagoya-u.ac.jp/2011/ICMASS2017/manabe_ICMaSS2017.pdf · Development of Nuclear Emulsion for Cosmic Ray Radiography](https://reader031.vdocuments.us/reader031/viewer/2022040310/5d404f9e88c99391748c0d92/html5/thumbnails/26.jpg)
PMMA 500㎛屈折率=1.48複屈折率=3.5nm
![Page 27: Development of Nuclear Emulsion for Cosmic Ray Radiographyflab.phys.nagoya-u.ac.jp/2011/ICMASS2017/manabe_ICMaSS2017.pdf · Development of Nuclear Emulsion for Cosmic Ray Radiography](https://reader031.vdocuments.us/reader031/viewer/2022040310/5d404f9e88c99391748c0d92/html5/thumbnails/27.jpg)
PS 175㎛屈折率=1.57複屈折率=未測定