ICRR Seminar
2013/June/25

GRAINE project :Cosmic Gamma-ray Observation withBalloon-Borne Emulsion Telescope
Shigeki Aoki for GRAINE collaboration
Shigeki Aoki(1), Kaname Hamada(2), Toshio Hara(1), Katsumi Ishiguro(3), Atsushi Iyono(4), Keiki Kamada(1),Hiroaki Kawahara(3), Nobuko Kitagawa(3), Koichi Kodama(5), Ryousuke Komatani(3), Masahiro Komatsu(3),Motoaki Miyanishi(3), Fukashi Mizutani(1), Saki Mizutani(1), Kunihiro Morishima(3), Naotaka Naganawa(3),Tatsuhiro Naka(3), Ryo Nakagawa(1), Yuji Nakatsuka(3), Mitsuhiro Nakamura(3), Toshiyuki Nakano(3), KimioNiwa(3), Keita Ozaki(1), Hiroki Rokujo(3), Takashi Sako(3), Yoshitaka Saito(5), Osamu Sato(3), YoshihiroSato(6), Atsumu Suzuki(1), Kazuya Suzuki(3), Satoru Takahashi(1), Keisuke Tamura(2), Ikuo Tezuka(6),Junya Yoshida(3) and Tetsuya Yoshida(2)(1)Kobe University, (2)ISAS/JAXA, (3)Nagoya University, (4)Okayama University of science, (5)Aichi
University of education, (6)Utsunomiya University(E>1GeV)SNR W44

CrabAbdo et al., Science, 2010
Color : 2-10GeV gamma-ray (Fermi LAT)
Contour : IR(Spitzer)

A. J. Dean, et al., Science, 2008
INTEGRAL

Unknown
31%

1873 sourcesDetection principle of high energy gamma-ray
PDG

e-pair creation

Arrival direction, timing, energy, polarization

Nuclear emulsion

Microscopic view
10microne+/-Gamma-raye-/+

Cross sectional view of an emulsion film
Powerful tracking device>High spatial resolution : ~1micron>Small radiation length : 0.002Xo

Gamma-ray
Emulsion

Plasticbase

Emulsion

e-e+0.3mm(0.002Xo)
High angular resolution for gamma-ray
Sensitive to gamma-ray polarization

GRAINE

Gamma-Ray Astro-Imager with Nuclear Emulsion
Converter
Convertere- e+Emulsion
Emulsion ++ Copper
Copper foil
foilTimestamper
Timestamper
Multi-stage
Multi-stage shifter
shifter

Calorimeter
Calorimeter
Emulsion
Emulsion ++ metal
metal plate
plate

AttitudeAttitude monitor
monitor* 10m2*trans*conv*detStar
Star camera
cameraGRAINE

Fermi LAT
Angular resolution @100MeV@1GeV

6.0deg (105mrad)

x1/7

0.93deg (16mrad)

0.90deg (16mrad) x1/9 0.10deg (1.7mrad)

Energy range

20MeV - 300GeV

10MeV - 100GeV

Polarization sensitivity

NoYes

Effective area @ 100MeV

0.25m2@ 1GeV
Dead time

0.88m226.5μsec(readout time)

x8x3

2.1m2 *
2.8m2 *
Dead time freeAngular Resolution
Emulsion (data)

Kinematica

0.1GeVl li

Emulsion (MC)1 FilmFermi-LAT(data)
Total

2 FilmsFront

3 FilmsBack

0.13deg(2.2mrad)@1GeV
0.08deg(1.4mrad)@2GeV

mit

1GeV

10GeV

100GeV* http://www.slac.stanford.edu/exp/glast/groups/canda/lat_Performance.htm

High resolution imaging
GRAINE(Simulation)

0.5deg

W44
Abdo et al., Science, 2010
Color : 2-10GeV gamma-ray (Fermi LAT)
Contour : IR(Spitzer)

・3flights (41.7m2days)
・>1GeV
・Smearing IR(Spitzer) distribution
with 0.08deg(1.4mrad)
・Considering atmospheric gamma-ray(>1GeV) as BG

Polarization
measurement

Microscope imageγ

Cross-sectional view of OPERA filmγ

1micronemulsion

293μm
0.002XoTACbaseemulsione-e+Polarization sensitivity
miler
pyr
ani

N(ω)=p2*{1+p0*cos2(ω-p1-90°)}

Consistent with expectedEnergy range

1713mLCS gamma-ray beam
@ UVSOR
Event ID : 221 2314379
E=28+6-4[MeV]
pβ1=13+4-2[MeV/c]pβ2=15+4-3[MeV/c]

Atmospheric gamma-ray@ Mt. Norikura
Event ID : 131 3741965
E=150+38-15[MeV]pβ1=50+12-7[MeV/c]pβ2=100+36-13[MeV/c]

LCS gamma-ray beam
@ SPring-8

Atmospheric gamma-ray@ balloon flight (MSC)

74m

10MeV

100MeV

1GeV

10GeV

100GeVMomentum Measurement by MCS
・・・

Emulsion Metal
Film

Angular Method

0.8 GeV/c 

1.5 GeV/c K. Kodama et al.
NIM A574(2007) pp.192-198

dE/dx measurement (p-id)“OPERA film”  KEK-PS 1.2 GeV/c beam (29 films)

 (  = 0.99,dE/dx = 1.08 MIP )p (  = 0.79,dE/dx = 1.23 MIP )dE/dx (a.u.)

dE/dx measurement (Z-id for nuclei)“desensitized” operation (98% RH 3days)
38C

30C

no “desensitized” operationHeLi

Be

B

Pulse height in sheet-D (counts)

45C

C
B
Be
Li
He

Pulse height in sheet-B (counts)C
pulse height distribution (a.u.)(from 4 plates)

T. Toshito et al.,
NIM A556 (2006) pp.482-489
Phys. Rev. C75 (2007) 054606GRAINE roadmap•

8th/June/2011, TARF, JAXA Scientific Ballooning,
12.5cm x 10cm aperture area, 4.3hours (1.6hours@35km) flight duration– Working test for each element– Connection test between elements– Measurement of atmospheric gamma-rays•

2014(Planned), Alice Springs, JAXA International Scientific Ballooning
2500cm2 aperture area, 1 day flight duration– Overall test by detecting known gamma-ray source– Observation with highest imaging resolution•201510m2 aperture area, 7days flight duration– Starting scientific observation

GRAINE roadmap•

8th/June/2011, TARF, JAXA Scientific Ballooning,
12.5cm x 10cm aperture area, 4.3hours (1.6hours@35km) flight duration– Working test for each element– Connection test between elements– Measurement of atmospheric gamma-rays•

2014(Planned), Alice Springs, JAXA International Scientific Ballooning
2500cm2 aperture area, 1 day flight duration– Overall test by detecting known gamma-ray source– Observation with highest imaging resolution•

201510m2 aperture area, 7days flight duration– Starting scientific observation

H. Fuke et. al, Adv. Space Res., 45 (2010), 490-497

Taiki Aerospace Research Field
Pacific OceanE

Airstrip (L 1,000m)

SNW
Sliding Launcher onRails (L 460m)

MeteorologicalEquipments

Handling Area (140m)

Balloon Operation
BuildingHangar(W30m, H35m, L83m)

Multi-stage shifter( time stamper )S. Takahashi et al.
NIM A620(2010) pp.192-195
dx
Shifter (1)Converter

timedxShifter (1)Shifter (2)))

dx

Shifter (2)))))
time

Shifter (3)SimpleCompactLight
HV freeLow power consumptionDead time free))))))

dx

Shifter (3)timeMulti-stage Shifter (Time Stamper)
Co-developed with
Mitaka Kohki Co., Ltd.
Weight : 5 kg
Power Cons.: 20 W
Reproducibility: 1m
10cm
12.5cmgap of stages=2mm
pulse motor

photo sensor

GPSPressure meter

BatteryStarcamera
Emulsionchamber
1.3m

TARF
8th June 2011
5:05

Flight pathLevel flight
20km

9:36

8:50

7:14

5:05

Duration : 4.3hours
Level :
1.6hours

9:24

Emulsion chamber
Aperture area : 12.5cm x 10cm

Flatness compensation films

Low energy

High energy OPERA film x 2

Converter

102 emulsion films, 91 copper foils (50m)
1.1kg, 35.0mm, 0.54Xo(conv= 34%)

Honeycomb board
Honeycomb boarde+e-e+

OPERA film x 10 (go-ban part)
OPERA film x 88 + Copper foil x 88
New type gel film x 4 + Copper foil x 3-Target & Detector-Precise measurement of incident direction-0.08deg@1-2GeV, 0.93deg@100MeV-Measurement of gamma-rays polarization-Interface of timestamper-Energy measurement of gamma-rays (<~GeV)-Momentum measurement of electron pair with MCSe-Timestamper))))))1st : OPERA film x 2
2nd : OPERA film x 2
3rd : OPERA film x 2
New type gel film x 1

Calorimeter

32 emulsion films, 10 (0.5mm) & 17 (1mm) lead plates
3.2kg, 31.9mm, 4.0Xo (Shower Max.@ a few GeV)OPERA film x 5 (go-ban part)(OPERA film + lead plate(0.5mm))x10(OPERA film + lead plate(1mm))x17

Automated Emulsion Scanning System
Nagoya Univ.
“ S-UTS ”

Number of tracks:8.0×108

10cm

12.5cm|tanproj|<1200micron

Film#67, 1stNumber of tracks

Track reconstruction
RawClustering

Both sides

Between films

BottomTopFilm#Reconstructed tracks (film#1-16) : 8.7x107 (overlap)

Connection accuracy
Low energy

High energy
295micron

Honeycomb board
Honeycomb boarde+e-dr)))295microndEmulsion film)))

Copperfoil

e-50
microne+Emulsion filmConnection accuracy
Pos diff X

dx=0.75micron

Ang diff X

dx=4.2mrad

Film#12-13tan<0.1

Pos diff Ydy=0.76micron

Ang diff Ydy=4.6mrad

Track efficiency
Low energy

High energy

Honeycomb board
Honeycomb boarde+e-e+e))))))Emulsion
Emulsion
Emulsionfilm Copper film Copper filmfoilfoil

Track efficiency

Track efficiency

Y [mm]

Trackefficiency

X [mm]

Film#5Track efficiency

ZY(5mm)2 x10films X
2x104tracks

ZYX

ZYX

10.0cm

12.5cm153events
Reliability 97%

Zoom upOne of gamma-ray events
EventStart
incident(p)left(p)rightE: 71 6923485: #7: 9.748 [deg]: 60 +20 -12 (25%) [MeV/c]: 32 + 9 - 6 (22%) [MeV/c]: 92 +22 -13 (+24% -14%) [MeV]#73.15mm

0.077mm#1

Detection efficiency

Detection efficiency (MC)Normal opening angle (current)
Normal & Large opening angle
High track efficiency film

Geant4.9.5
Normal incident
7 films
Scanning response
Reconstruction programGamma-ray energy [MeV]Integral flux [cm-2・s-1・sr-1]

Atmospheric gamma-ray flux@35km
preliminary

50

Thompson, 1974, 10-5g/cm2
GRAINE2011, 6.6g/cm2

100

Energy [MeV]Establishment of timestamp technique
H.Rokujo, et al., NIM A, 701 (2013) @GRAINE2011“Multi-stage shifter” 1st model

Track rate mesurement@35kmexcess(6.6)Detection ofhadron eventsAperture area: 12.5 x 10 cm2•Correct operation during whole observation time
•Giving time info. to all penetrating tracks•Detection of hadron shower tracks by timing and3-D spatial analysis•Time resolution: 0.15 sec

Ev : 2438038
7:18:34.5 (JST)t=+-0.5s
1.2cm x 1.2cmx 16films

Conversion pointe-pair

YZ

Pointing accuracy
space : 0.65deg (0.0114rad)E : 45+33-10 [MeV] : 46.61 [deg]XPrimary vertex

•Optics filter
cut-on below 610nm

Optics Filter

Schneider Optics B+W091•

Camera Lens

Nikon AF Nikkor 85mm F1.4D– diameter：60.7mm– focal length：85mm•CCD Camera

HAMAMATSU C3077-79(near-IR camera)– pixels：640×480：Daytime sky BG（Dietz et al., 2002）◆：Star spectrum（M-type:3200K）■• CPU board
ADVANTECH PCM-3362- CPU：Intel Atom N450 1.66GHz• Video Capture board
Sensory Frame Grabber Model 311- ADC ：8bit

Field of View：
5.9deg(H)×4.5deg(V)Limiting magnitude：6
Monitoring accuracy：0.16mrad- Frame rate：30FPS• SSD(128GB)TOSHIBA SSDN-ST128H

K.Ozaki, et al., Proc. of Balloon
Sympo., isas12-sbs-022 (in Japanese)Image data on Level Flighttime: 8:11:00.16 (@Altitude 34.6km)

Because of stray light reflected on hood, outer region was saturated.

Image data on Level Flighttime: 8:11:00.16 (@Altitude 34.6km)

6 stars were detected.

Attitude analysis

K. Ozaki et al.,Proc. of Balloon Sympo.,
isas12-sbs-022

8:11:00(JST) @35km

Working rate: 74 %Monitoring
accuracy: < mrad

Daytime star camera view

Star catalog datapattern match

Elevation < 0.25mrad
Azimuth < 0.44mrad

Rotation speed of the balloon
95% time during level flightwas  <0.15deg/sec.

It is important to decide telescope
attitude to celestial coordinate
better than emulsion angularresolution(0.08deg).

We confirmed attitude decisionaccuracy was <t< 0.02deg.

GRAINE
First Light

GRAINE roadmap•

8th/June/2011, TARF, JAXA Scientific Ballooning,
12.5cm x 10cm aperture area, 4.3hours (1.6hours@35km) flight duration– Working test for each element– Connection test between elements– Measurement of atmospheric gamma-rays•

2014(Planned), Alice Springs, JAXA International Scientific Ballooning
2500cm2 aperture area, 1 day flight duration– Overall test by detecting known gamma-ray source– Observation with highest imaging resolution•

201510m2 aperture area, 7days flight duration– Starting scientific observation

Flight model of multi-stage shifter

12.5cm

1st model

Co-developed withMitaka Kohki Co., Ltd.

10cm

2nd model
Aperture area : 2500cm2

Emulsion production
Gelatin1/4, Na type, Fe x 2, MIP (XAA, 20deg, 40min)

New type

GD=86.1+-4.7
FD=2.9+-0.9

OPERA type

GD=34.8+-0.6
FD=3.7+-0.4

Evaluated by K. Kamada (Kobe Univ.)

efficiency [%]Fuji Janet Co., Ltd., Nagoya Univ.

Tracking efficiency
97.7+-0.25 [%]Incident angle

Automated emulsion read-out system (Nagoya Univ.)

Automated emulsion read-out system (Nagoya Univ.)
Hyper-TS: Next Generation Read-out system

Scanning speed
9000cm2/h (design)Flight duration ~1dayVela

Alice Springs 2014/May/15, Culmination 17:09(NT), In FOV 6.5hours (13:53-20:24)
Lat.： -23 40’(-0:30(JST))
Lon.：133 50’ ESignificance Significance vs. Exposure Time
Vela flux : 1.068x10-5cm-2s-1sr-1 (2FGL, >100MeV)
Remaining Air (vertical): 5g/cm2

Taking into account the variation of zenith angle
・transmission efficiency of cosmic gamma-ray
・atmospheric gamma-ray
・detector aperture and effective thickness

4.7 significance from 6.5 hour ovservation[hour]
Come into FOV

Culmination

Leave FOV

Significance Significance vs. Remaining Air Thickness
Vela flux : 1.068x10-5cm-2s-1sr-1 (2FGL, >100MeV)

6.5 hour ovservation

6.4

Taking into account the variation of zenith angle
・transmission efficiency of cosmic gamma-ray
・atmospheric gamma-ray
・detector aperture and effective thickness

The less remaining air shall brings
the higher significance.

5.4
4.7

Remaining Air (vertical) [g/cm2]

2013
JanFebMarAprMayJunJulAug

Sep

Emulsion film : Established 2nd flight model

Oct

Nov

Dec

Film production

Multi-stage shifter : Low T&P test, Assembling, Flight readyStar camera : Design, Test, Assembling, Flight ready2014
JanFebMar

AprMayJunJulAug

Sep

Oct

Nov

Stacking & Assembling•-Sep/2013, emulsion film for 2nd flight model will be established.

•-Sep/2013, multi-stage shifter will be ready for the the flight.

•-Sep/2013, star camera will be ready for the flight.

•Oct/2013-Jan/2014, emulsion film production•Feb-Apr/2014,stacking and assembling•

May/2014,2nd flight model will be ready for the flight.

Dec

Subject• Galactic cosmic-rays origin, acceleration and propagation• Galactic high energy objects– Pulsar, PWN, SNR, Magnetar, X-ray binary, Globular cluster• Extragalactic cosmic-rays origin, acceleration and propagation• Extragalactic high energy objects– AGN, GRB, cluster of galaxy, starburst galaxy• Cosmological research by using gamma-rays from AGNs andGRBs• Search for gamma-rays from annihilation/decay of dark matterfrom galactic center and dwarf galaxy

Summary and Outlook• Promoting GRAINE project• Performed balloon experiment in 2011
• Demonstrated emulsion gamma-ray
telescope with flight data
• Measured atmospheric gamma-ray• Preparing for planned balloon experiment
at Alice Springs in 2014

backupMomentum measurement with multiple coulomb scattering
for gamma-ray energy reconstruction
35MeV electron LINAC@Tokai-mura

35.2+6.5-7.4 [MeV/c]
Absolute:1.8% (34.6MeV/c@incident)
Relative:20% (15films)
14%@E=70MeV (even case)
20%@E=35MeV (uneven case)

SNR W44
放射起源に迫る上で200MeV以下が重要
Emulsion 200MeV
エラーサークル
0.5 deg

シミュレーション結果(150 m2hour)Fermi 200MeV
エラーサークル

M. Ackermann et al.
Science 339, 807 (2013);
DOI: 10.1126/science.1231160