Filling the gap between
MeV and GeV~ eASTROGAM and CAST ~Kazuhiro Nakazawa（U.Tokyo）	 

15-­‐16	  Dec.	  2016	  	  “The	  extreme	  Universe	  viewed	  in	  very-­‐high-­‐energy	  gamma	  rays	  2016”	  @	  ICRR  This talk is supported by…
eASTRAOGAM Collaboration (for ESA-M5)
Alessandro De Angelis, Vincent Tatischeff, Marco Tavani, Uwe Oberlack, Isabelle Grenier,Lorraine Hanlon, Roland Walter, Andrea Argan, Peter von Ballmoos, Andrea Bulgarelli,
Immacolata Donnarumma, Margarita Hernanz, Irfan Kuvvetli, Mark Pierce, Alessio Aboudan,Giovanni Ambrosi, Denis Bernard, Elisa Bernardini, Andrea Borgna, Marica Branchesi, Andrei
Bykov, Martina Cardillo, Paolo Coppi, Domitilla De Martino, Roland Diehl, Michele Doro,
Valentina Fioretti, Stefan Funk, Gabriele Ghisellini, Eric Grove, Clarisse Hamadache, DieterHartmann, Masaaki Hayashida, Gottfried Kanbach, Jurgen Kiener , Jurgen Knodlseder, Philippe
Laurent, Olivier Limousin, Karl Mannheim, Mario Nicola Mazziotta, Julie McEnery, Sandro
Mereghetti, Gabriele Minervini, Alexander Moiseev, Aldo Morselli, Kazuhiro Nakazawa, Piotr
Orleanski, Josep Maria Paredes, Barbara Patricelli, Jean Peyre, Giovann Piano, Martin Pohl,
Harald Ramarijaona, Riccardo Rando, Ignasi Reichardt, Marco Roncadelli, Fabrizio Tavecchio,David Thomson, Alexei Ulyanov, Xin Wu, Andrei Zdziarski, Andreas Zoglauer
AND

CAST ex-WG à to reform as RG (ISAS/JAXA)
Tadayuki Takahashi, Shin Watanabe, Motohide Kokubun, Yuto Ichinohe, Takeshi Takashima,Takefumi Mitani (ISAS/JAXA), Makoto Tashiro, Yukikatsu Terada (Saitama U), Toru Tamagawa(RIKEN), Masaharu Nomachi (Osaka U), Yasushi Fukazawa, Tsunefumi Mizuno (HiroshimaU), Yasunobu Uchiyama (Rikkyo Univ.) and Teruaki Enoto (RIKEN) et al.

1-1: A New era in high-E astro-physics
X-ray to GeV, TeV, new all-sky surveys
and high-sens. probes came about.
GeV：Fermi (US+:2008-)

examples …
TeV HESS (Int.: 2004-)

100 keV Swift(US+: 2004-)… but not yet in MeV
MeVCOMPTEL(1990-2000)“Existing best” MeV survey
X-ray

MAXI(Jp: 2009-)

1-1: A New era in high-E astro-physics
With GW, neutrino, as well as radio,
optical, X-ray, GeV, a time domain
astronomy is also coming (soon)
Opt.

examples …
GW LIGO (US+:200X-)

SDSS (US+:1999-)

Pan-STARRS (US: 2008-)… but far away in MeV
MeVCOMPTEL(1990-2000)

Abbot+ 2016

Neutrino
Kamiokande(JP+:1986-)

NASA

ICRR

Hirata+ 1987

1-2: Sciences left around MeV to sub-GeV
Motivation： Non-thermal energy in the Universe
Extream physics/Unknown phenomena
SN and metal synthesis etc …
Many science, “Only MeV to sub-GeV can access”- Many “left-over” from Suzaku, Swift (HXR), Fermi, HESS (Gev, TeV) etc.
à MeV to sub-GeV is needed to resolve the issue (AGN, jet, NS, BHB..)- Many science only MeV can do à Nuclear gamma-ray lines related
NASA

NASA/CXC/Rutgers/J.Warren & J.Hughes+

NASA/ESA/Arizona U.

DM
SNeAGN, Jet : nonthermal E

Extream

SNe+GRB

CRmolecular clouds

Explore
the Frontier
1-3: eASTROGAM = Fillthe sensitivity
gap

Sensitivity (erg cm

The next stepforward• 0.2-1000 MeVband with• 10 mCrab sens.
• with wide-FoVis needed!
à eASTROGAM-2-1s )• Clear Sensitivity Gap exists around 0.1-100 MeV• Swift, Fermi, with ~1000 sources à for “Astronomy” ~10 mCrab sens. needed• Fermi à “need low-GeV sensitivity with better Δθ”• New-gen. Compton telescopes with good Δθ for MeV is emerging(Hitomi-SGD (Si-CdTe), COSI (Ge-strip balloon), etc.),
can also adopt pair telecopemode, in principle
-8
1010
10
10
1010
10

IBIS-PICsIT-9SPICOMPTEL

-10

EGRET

-11 Swift/BAT-12-13

e-ASTROGAM
Fermi-LAT

IBIS-ISGRI
JEM-X

-2

CTA North

VERITASHiSCOREMAGICCTA SouthMeVsensitivity10 mCrab
gap-1410HAWC

10-111010210310410LHAASO510610710810910Energy (MeV)

10Explorethe Frontier
1-3: eASTROGAM = Fillthe sensitivity
gap
3 DAQ modes

Angular resolution
ARM σ

68% conf for
30 deg src.

DSSDs

x3
CsIs
Comptone-track Comptonpair• Combination of DSSD + CsI arrays• new-gen. Compton Telescope• converter-free pair Telescope
BOTH for better angular-resolutionà better sensitivity on 0.2 MeV – 10 GeV

x3

1-4: eASTROGAM proposed for ESA-M5• 550-600 km LEO,incl. 2.5 deg• Ariane 6.2, aimed at2029 launch• 550 MEuro (ESA)Cap
payload 1000 kg,1340 W (+bus)	 

~1m

2. MeV – sub-GeV all-sky sciencefrom proposal document	 2-1 AGN jet and flare-ups
BL Lac and FSRQ: the strongest
accelerator in the universe
Swift J1644+57

ERC

Sync.

SSC

電波

100 keV flares

IR/可視keV

MeV

GeV

GeV flares
Sync.

ERC

Burrows+2011 NatureeASTROGAM will see > 100 of MeV-blazers
up to z ~ 4.5 à radio-laud vs quiet evolution

SSCe.g. Ghisellini+2011

Hz2-1 AGN jet and flare-ups
SED of 3C279 flares

3C279 light curve > 100 MeV
Fermi LAT obs.
5 min
5 min
3 min bin3 min

Ackerman+2016	 

0.5 &50 ks
sens	 hours

• Origin (SSC or ERC of what ?) à SED and polarimetry• very short time-variability à search for megnetic recconection-like feature?
• hadronic or electron? à SED (and polarimetry?)2-2 Cosmic-ray accelarations
GeV SNR SED

CR - molecular cloud interaction

1 yr onplane
sens.

hours
• GeV SNRs à SED, evenspace resolved (Δθ 0.1deg) + nuclear lines• Better Δθ at sub-GeV for
M-cloud CR study

4 yr Fermi vs 1 yr eASTROGAM

2-2 Cosmic-ray accelarations-2 -1

dN/dE (erg cm s )1010-6-80˚ < l < 80˚ ; -8˚ < b < 8˚

nuclearnuclear + leptons+ sources + BG

-8Fermi-LAT-10e-ASTROGAM

E2On-plane
MeV survey
for LE-CRs

10On-plane 1yr sens.

Benhabiles-Mezhoud+ 2013

10-12

10-1

110

10

210

310

410

5E (MeV)can alsoFig.
detect,prompt
MeV lines
fromdue
low-energyCR,
9: Predictedgamma-rayemission
to nuclear interactionsof CRsinteractingwithM-Clouds.
à MClineionization,
CR propagation…to L
innerGalaxy.
The gamma-rayemission below
10 MeV is due

whose properties in the ISM have been adjusted such that the mean+observations and the Fermi-LAT data (magization rate deduced from H

2-3 Time domain: Pulsar Wind & Magnetors
Crab GeV flare	 

Magnetors	 
Giant flares(3 histrorical)

Striani+2013
1010

Fermi 4-yr
light-curve
E >100 MeV

keV2 (Photons cm-2 s-1 keV-1)

SGR Initial Spike

Weisskopf+2013

SED
spec.

.

100 MCrabe+/e- Fire Ball
511 keV ！

SGR 1806-20
SOPA

104

Intermediate Flare
1E 1547.0-5408
Suzaku/HXD-WAM

Burst
102 Short
1E 1547.0-5408

Enigmatic HXR
10 Crab
MeV peak?

Suzaku/XIS-HXD

1Persistent

50 ks sens

10-2

4U 0142+65
Suzaku1 mCrab

Beloborodov
2013

Kuiper+06, Enoto+10

How to acc. Electrons up to PeV
in ~day. Reconnection ? 	 

1

10100Energy (keV)103

MeV all-sky needed	 2-4 Multi-messenger Astronomy
eASTROGAM has “wide-filed of view” à Good synergy withGW and Neutrino detectors.
Fermi-GBM : 240 GRBs/yr	 • GRBs: CsI array trigger. ~200 GRBs/yr
If bright, with Δθ = 0.1-1 deg withCompton/Pair reconstruction.
Abbot+ 2016

• ~40 (16) GRBs/yr with polarimetry, if 20(10)% polarized• Binary NS merger : synery with GW andeASTROGAM- up to 1.4/yr detection “GW && ShortGRB” (Patriceli+2016) could be 1 per 3-4year?
Pelassa+Ohno 2009

2-5: Time domain: SN-Ia + SN II
SNIa 56Ni synthesis amount

1E-5

SNIa @ 10 (3) 	 Mpc

847 keV light curve

1e6 slinesens.	 

1E-6

INTEGRAL/SPIdata

1E-7

Sim.

1E-5

1E-6

1E-7

Maeda+2013

à eASTROGAM will detect
10+/-3 SNIa in 3 years

SNIa senario has diversity. 56Ni is “key” to see models
SN II also will be observed, also 26Al, as well as Nova

2-7：solar flares
Obs (RHESSI)

Models

2.2 MeV
Ishikawa+
2013

NTBremss• 2.2 MeV lines from flares à proton acc.
• 12C, 16O prompt lines also appear à proton energy• polarimetry in rim-flares à acceleration axis?

3. Mission designfrom proposal document	 3-1 e-ASTROGAM requirements
enegy range : 0.3 MeV – 3 GeV (Compton + pair)(30 keV – 200 MeV (GRB with CsI array))Δθ
: 1.5 deg @ 1 MeV (ARM FWHM),
1.5 deg @ 100 MeV (68% contaminant)
0.2 deg at 1 GeV (68% contaminant)Sensitivity : 2—5 x10-5 MeV/cm2/s
1 MeV – 500 MeV (106 s expo.)
Line sens. : 5x10-6 ph/cm2/s @ 511 keV (106 s expo.): 5x10-6 ph/cm2/s @ 847 keV: 3x10-6 ph/cm2/s @ 4.44 MeV

3-2 e-ASTROGAM designPair production(0.01-3 GeV)

~1.2 mCompton(0.3-2 MeV)

e-tracking Compton(2-10 MeV)
• 9.5x9.5 cm2 DSSD in 10x10 tiling, with 0.5 mmt, 240um pitch x
56 layers à 2.8 cm Si• 8500 cm2 of 8cm long CsI in 5x5 mmà 8 cm CsI	 
• with anti-co. plastic

3-3 Si-Tracker• 9.5x9.5 cm2 DSSD in 10x10 tiling, with 0.5 mmt, 240um pitch x
56 layers (“Silicon Radiation Sensors” or “HPK”)• 2.8 cm total thickness à 0.3 ratiation length• dE < 6 keV (FWHM)• Ileak = 96 pA/strip at T = 0 C (or 36 pA/strip at T = -10 C). 85 pF/strip.
• 860,160 DSSD signals are read by a total of 26,880 IDeF-X HD ASICs

8 cm = 4.3 radiation length

3-4 Caloriemeter• 33,856 bars of CsI(Tl) of 8 cm thich and 5x5 mm2 cross section,
read out by silicon drift detectors (SDDs) at both ends,• array of 529 (= 23x23) modules comprising each 64 crystalsI(4.3 radiation length), read-out with VEGA ASIC
• FWHM of 4.5% at 662 keV, dZ ~ 5mm FWHM

3-5 Anti-Coincidence Detector• total active area of about 4.7 m2.
• silicon photomultipliers (SiPM) by optical fibers• detection inefficiency < 1e-4

3-6 Performance

BGD inputs

Basic ΔθBasic ΔE

3-6 Performance… A few new idea

90 cm distance

3+2 year operation

10-2

Sensitivity (erg cm101010101010

Line: 1 Ms 1 σ(not 1 year operation)

Comtinuum: 1 year exposure-8 (not 1 year operation)
IBIS-PICsITs-1)

3-4 Sensitivity estimation-9SPIvs SPICOMPTEL-10

EGRET-11-12-13

HAWC
Fermi-LAT

IBIS-ISGRI

e-ASTROGAM

JEM-XCTA North

VERITASHiSCOREMAGICCTA South

10 mCrab

LHAASO-1410-210-111010210310410510610710810910Energy (MeV)

104. Other Missions

4-1 CAST mission concept (Japan)
Basic concept• Si-CdTe Compton Camera à goodΔE, good Δθ. Good at sub-MeV• More photon à smaller mission(~50 cm) to cover 0.1– a few MeV.

γγ
Mod-SGDSCT x9

CC support+heat pipe

ARM of Compton Telescopes

BGO x36
50 kgx63 degWatanabe+ 2007	 Experimental results (not sim.)radiator

BGO support
CFRP

radiatordegree

5 deg

220180main elec.
500500

4-1 CAST mission concept (Japan)
Based on heritage from “Hitomi”
Soft Gamma-ray Detectorγγ
Mod-SGDSCT x9

CC support+heat pipe
BGO x36
50 kg
Si-CdTe Compton
Cameraradiator* there is also a u-TPC based etracking MeV Compton camera,by Tanimori-group

BGO support
CFRP

radiatornext step will be- ballooning (for low BGD)
- e-tracking (with new Si-device)

220

180

main elec.
500

500

4-2 COMPAIR (US, for MIDEX?)
Concept
Add CZT layer between DSSDs and CsI calorimeter
Both, Compton mode and Pari-mode (0.5-100 MeV)

Moiseev+ 2016

5 Summary• MeV – GeV is a frontier in high-energy astronomy• eASTROGAM (for ESA-M5 2029 launch) uses, DSSD-tracker+ segmented-CsI calorimeter. Operates with combined• (orthodox) Compton telescope• electron-tracking Compton telescope• converter-less pair telescope• Desinged for “better than 10 mCrab” sensitivity, and with lowE Δθ improvements over Fermi-LAT, at 0.3 MeV— 30 MeV• CAST is another plan, focussed on sub-MeV to make it smallà we will renew it, incoporating electron-trcking new Si-device• COMPAIR is similar to eASTROGAM, with CZT middle layer.

For MeV, we will hold a small WS at Kyoto on 2019/2/27-28