HiZ-GUNDAM
High-z Gamma-ray bursts for Unraveling the Dark Ages Mission

Daisuke YONETOKU (Kanazawa University)
HiZ-GUNDAM working group
9月末にアナウンスされる予定の公募型小型計画への提案を検討しています2015年度 光学赤外線天文連絡会シンポジウム ＠ 国立天文台 (2015/09/14 – 16) 1

HiZ-GUNDAM Working Group Members (since 2012)◆ X-ray & Gamma-Ray part
D.Yonetoku(Kanazawa), T.Mihara(RIKEN), T.Sawano(Kanazawa), N.Kawai, M.Arimoto(TITech),
H.Ikeda(ISAS), T.Enoto(Kyoto), M.Ohno(Hiroshima), S. Kurosawa(Tohoku), T.Sakamoto(Aoyama),
M.Serino(RIKEN), M.Tashiro(Saitama), T.Tanimori(Kyoto), Y.Nakagawa(ISAS),
T.Murakami(Kanazawa),
Y.Yatsu(TITech), K.Yamaoka(Nagoya), T.Yuasa(RIKEN), A.Yoshida(Aoyama), N.Gherels(NASA/GSFC)◆ Near Infrared part
K.Kawabata, M.Yoshida(Hiroshima), S.Matsuura(ISAS), K.Tsumura(Tohoku),
T.Matsumoto(Taiwan), M.Shirahata, K.Yanagisawa, H.Okita, M.Tanaka(NAOJ),
Y.Urata(Taiwan), K.Motohara(Tokyo)
Advisor: H.Kaneda(Nagoya), T.Wada(ISAS)◆ Theoretical part
K.Asano(ICRR), K.Ioka(KEK), H.Itoh(RIKEN), S.Inoue(RIKEN), N.Kawanaka(Tokyo),Y.Suwa(Kyoto), K.Takahashi(Kumamoto), Y.Teraki(RIKEN), K.Toma(Tohoku),
T.Totani(Tokyo), H.Nagakura(Kyoto), S.Nagataki(RIKEN), T.Nakamura(Kyoto),
Y.Niino(NAOJ), J.Matsumoto(RIKEN), A.Mizuta(RIKEN), K.Murase(Penn.s),
R.Yamazaki(Aoyama), J.Yokoyama(Tokyo),
M.G.Dainotti(Stanford), M.Barkov(RIKEN), J.Mao(Kyushu), A.Tolstov(IPMU)◆ Satellite system
S.Sakai, K.Yamada(ISAS)

59 members／22 Univ. & Institutes

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3 key issues for X-ray transient observations(1) Counterpart of gravitational wave source
・Tests of the theory of general relativity in strong gravitational field(2) Probing the early universe with high-z gamma-ray bursts
・First stars and First black hole formation in the universe
・History of cosmic reionization and its origin
・Chemical evolution of heavy elements(3) Multi-wavelength/messenger astronomy
・From radio to TeV gamma-ray, and neutrino, cosmic ray, and GW・Understanding the extreme universe with transient phenomena
Main purpose of HiZ-GUNDAM is (2) to probe the early universe with GRBs,
but also strongly contribute to (1) and (3).
NASA’s Decadal Survey 2010 (Science Frontier Discovery)(1) Habitable Exoplanet(2) Gravitational wave astronomy(3) Time Domain Astronomy
HiZ-GUNDAM will be able to(4) Astrometry
contribute to 3 of 5 themes.
(5) Epoch of cosmic reionization

3Evolution of the universe
BigBang

End of the dark age
Beginning of the star formation
CMBLarson & Bromm (2001)

Dark AgeFirst StarFirst SNeBlack HoleHigh redshift universe (z > 7)

PrimordialGalaxy

Massive stars■ Formation of first stars (Pop-III stars)■ Cosmic reionization
UV radiation■ First metal production
Nucleosynthesis■ First black hole formation

Present AgeGRBs

explosion

Evolution to super massive BH? GRBs as a cosmological probing tool.
4

HiZ-GUNDAM observation strategy(1) GRB discovery in X-ray band, and send 1st alert of the localization.
(2) Automatically start follow-up obs. with near infrared telescope.
(3) 2nd alert of fine localization (~ 1”) and rough redshift (z>5 or z>7).
after that,

High-z GRB rate = 5 – 10 event/yr(4) Spectroscopic observation with large area telescopes.

Combination with X-ray and NIR for high-z GRB observation
X-ray imaging detector
1 steradian FOV
5~10 arcmin position accuracy
Si + coded aperture mask
(1 < E < 10 keV)
30cm NIR telescope
34 arcmin FOV
Photometric observation in optical & NIR
5(0.5 – 1.7 um)

Cosmic Reionization
GRB 050904 @ z = 6.295

Kawai et al. (2006)
Totani et al. (2006)

3.4 days

GRB 130606A @ z = 5.913

Subaru/FOCAS
10.4 – 13.2 hrs~ 20 mag(AB)Subaru/FOCASxHI < 0 .17 and 0.60, at 68 and 95%
The existence of neutral hydrogen was foundmore than 3 s statistical level for GRB130606A.
The neutral fraction of IGM is measured as
xHI = 0.1 – 0.5.

Totani et al. (2014)

6Expected lightcurve of GRB afterglow @ z=7
TAO, Subaru

Based onKann et al. 2011

JWST, TMT

Spectroscopic
sensitivity
Subaru MOIRCS (1hr, 5s)
TAO SWIMS (1 hr, 5s)
Subaru FOCAS (1hr, 5s)

2nd alert t < 15 min
High-z GRB (z>7)?
Brighter than 20mag(AB)?

090423@z=8.26

Requirement
Sensistivity: 20 mag (AB) in NIR
2nd alert earlier than 15min

1st alert
Localization in X-ray
1min

JWST NIRISS (104s, 10s)
TMT IRIS (5hrs, 10s)
JWST NIRspec (104s, 10s)

15min
7

Silicon Strip Detectors for coded aperture mask system
Strip pitch
300 mmElectrode widthof strip

1-dimensional random mask

Angular resolution
θ = tan-1(d/D)= 5 arcmin
1str FOV

500 cm2X

1str FOVY

500 cm2

D = 30cm

Si stripd = 0.3mm pitch8

Wide Field X-ray Imaging Detector

ΔE ~ 1 keV (FWHM) @ 5.9 keV
55Fe

LD = 2.0 keV
pedestal

100 mm8s detection sensitivity

RadioIsotope

4 – 150 keV~ 1000 cm2

1 – 20 keV・ Silicon Strip Detector with Coded Aperture Mask
1000 cm2, 1 steradian・ X-ray Spectroscopy from 2 keV (Goal 1 keV)・ Tungsten Coded Aperture Mask with 0.5 mm thickness
・ Verification of X-ray Imaging
・ Final sensitivity will be ~ one order of magnitude
higher than Swift/BAT and SVOM/ÉCLAIR for soft X-ray transients & high-z GRBs.

15 – 150 keV~ 5400 cm29

1/10 Proto-Type Model of FPGA/CPU・ FPGA for ASIC control and data handling, CPU for data handling and user interface
・ This Digital boards are developed for micro-satellite Kanazawa-SAT3.

10Radiation tolerance Test for readout ASICs and SSDs

Wakasa-wan energy research centerTITech

2013/10/03 – 04 : Proton irradiation test for SSD (200 MeV monochromatic)
No change of breakdown voltage for the proton for 10 yrs fluence in orbit
Leakage current increased by factor of 4
2014/06/12 – 13 : Proton irradiation test for ASIC (200 MeV)
Maintain the operation function for 10 yrs irradiation
No single event (SEU/SEL)
2015/02/04 – 06 : Carbon irradiation for ASIC ( ~ 10 MeV)
Loss the capability of analog electronics for 10,000 yrs irradiation
SEU occure for 100,000 yrs irradiation
Completely destroyed for 1,000,000 yrs irradiation
2015/07/24: Gamma-ray irradiation for ASIC （60Co）
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Maintain the operation function for 40 krad, 100 krad, 200 krad

Offset Gregorian Optics

NIR telescope

30 cm in diameter

Similar to the optics ofCIBER-2 rocket experiment

34 x 34 arcmin2

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CIBER-2 Rocket Experiment

Lanz et al. (2014)• NASA’s rocket experiment for the near infrared background light• Telescope Size : 28.5cm cooled telescope ⇒ 30 cm• 3 band photometric observation in optical and NIR Verification for the NIR telescope aboard HiZ-GUNDAM
Flight Configuration

Flight Primary Mirror

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HiZ-GUNDAM (1.0-1.7 mm)
Exposure Time per Field (min)Limiting Magnitude (AB)Calculated byTsumura (2014)24

Confusion
Limit

HiZ-GUNDAM

Survey Area (deg2)

Monitoring observations and Transients
NIR telescope■ monitor of variable objects■ fluctuation of NIR background■ NIR catalogue(deeper than 2MASS catalogue)■ high-z QSO survey■ transit of exoplanet
2.4 um

3.2 um

4.1 umWide field X-ray imaging detector■ Normal GRBs (~100 events/yr) ■ shock break-out of SN explosion■ Tidal disruption events■ X-ray flash & X-ray rich GRBs
■ short GRB & Gravitational Wave ■ Supergiant fast X-ray transientbinaries of High-mass + NS
■ optically dark GRBs
■ X-ray monitor for bright sources■ ultra long GRBs, pop-III GRBs
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Summaries◆ Japanese GRB community considers the future GRB mission “HiZ-GUNDAM”.
◆ We are developing the 1/10 proto-type model of the X-ray instrument,
and the flight model of NIR telescope for CIBER-2 rocket experiment.
◆ We need a world wide collaboration
especially for the NIR telescope system, satellite operation, alert system,
and also the driving powers of scientific outputs.

・ 初代星、初代銀河、宇宙再電離、化学進化に興味のある方々
・ 80 – 90 % 程度の自由な時間に近赤外線望遠鏡を有効利用していただける方々
・ 2030年代に向けて、地上からスペースへの技術移行に興味のある方々
懇親会で議論させてください & ミッション提案の際にご協力ください

分野横断型プロジェクト合同検討委員会の皆様へ
心より感謝申しあげます
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17

1050

Short GRBLong GRB

Ultra-Long GRB

XRF/XRR
Tidal
Disruption

SGR Flare1040

SN Ia
Breakout

ULXs

X-ray Binaries

1030

Flare Stars

Schedue1415161718192021

MAXIg-ray

Fermi

OpticalNIRRadionG-Wave232425ALMA
IceCube272829303132

HiZ-GUNDAM
iWF-MAXI

将来の突発天体観測

CTA
JWSTSubaru

26

AthenaASTRO-H
X-ray
GRB Swift
Wide Field

22

TAO

SPICA
LSSTTMTSKA
KAGRA, A-LIGO, A-VIRGO・ We will propose the HiZ-GUNDAM to the next AO of Competitive M-Class Mission.
・ Collaboration with TAO, Subaru, Keck, VLT, JWST and TMT・ Multi-Messenger/Multi-Wavelength observatory

Weight Specifications (Estimations)
Wide Field X-ray Imaging Detector

Near Infrared Telescope System

Weight [kg]1.2
SSD sensor＋electric board
FPGA board
1.2
Chassis (sensor box)
5.0
Tungsten coded mask
1.5
Shield (Pb sheet)
4.6
CPU box
2.0
MLI
0.5

Weight [kg]Telescope Tube
5.4
Primary Mirror (PM)
4.0
Secondary Mirror (SM)0.5
Support board of PM
7.7
Telescope Support
1.4
0.6
Support of SM
Cassegrain Baffle
0.6
Bend Mirror Box
3.2
Lens
2.9
Beam Splitter Holder
0.6
Dichroic Mirror & optics
1.9
Optical base plate
9.1
Detector (Hawaii x2,HyViSi x 2)
0.9
MLI
0.8radiation shield
1.0

Subtotal
MarginTotal

16.0
2.0
18.0

2 instruments for each X-/Y-direction.
36.0 kg in total

Mission Payload Total 80.7 kg
Satellite Bus ~ 200 kg

Subtotal
Margin
Total

40.6
4.1
44.7
20

Sun synchronous orbit (Twilight)

Sun synchronous orbit (Local time 9/21 h)

Visible region

Visible region

Impossible toPossible tocover the midnight

cover the midnight

SUNSUN

Visible region

Visible region

ElV. >30 degree is needed forSpec. observation by Large area telescope

We need tradeoff study for satellite orbit(Low earth orbit with 31deg inclination,Sun Synchronous orbit, L2 and Geostationary orbit)

SVOM衛星との対比（中国・フランス、2020年以降の打ち上げ目標）■ Ｘ線検出器の感度
SVOM/ÉCLAIR の感度は、Epeak < 10 keV の GRB に対してあってもSwift よりも、若干、良い程度である。
(CdTe を使うことで 250 keV まで感度があるが高エネルギー側は感度の改善に寄与しない)
可能な限り低エネルギーからの観測が重要
HiZ-GUNDAM は 1 keV からの観測を目指し、Swift よりも 1 桁高い感度を実現する。

■ 望遠鏡の観測波長帯
赤方偏移 z>7 は、波長 λ > 980 nm の近赤外線で観測しなくては原理的に検出できない。
SVOM VT は 45cm 望遠鏡, 400 – 950 nm なので高赤方偏移に対応できない
HiZ-GUNDAM は 1.7μm までカバーし、z < 13 をターゲットとする。
※ SVOM は地上に 1.2m 近赤外線望遠鏡を設置する計画も含まれるが、近赤外線帯での感度は不十分であることと、全GRBの追観測に対応できない。
スペースにおける 30cm 望遠鏡の方が格段に感度が高い

22

地上近赤外線観測の例
以前の補足資料より
GROND (Greiner et al. 2008)

15min

1 day

2.2m MPI/ESO 望遠鏡
La Silla Observatory (チリ)2009 – 2013 年
GRB の報告数

573

GROND の観測数 152 (全体の26.5%)
15分以内の観測

GROND

24 (全体の4.2%)

リアルタイム追観測の割合：
夜時間1/3, 北/南半球1/2, 他の観測, 天候 < 1/6 (16.7 %)20mag(AB)/3分露光 ＝ 3～4メートル級の近赤外線望遠鏡 ＠ 海抜2000 m程度の高地

人工衛星に近赤外線望遠鏡を搭載し、High-z GRB を見逃さないよう系統的に (～100%) 追観測する意義は高い (予算・観測効率・マンパワーの面でも)23

Focus of Large Projects in late 2010’s and 2020’s
TMT
Primordial galaxies(z > 10)
Reionization (z～10)
Gamma-Ray Bursts

z=1000SPICA

Gamma-Ray Bursts

ALMA

Pop-III stars:
H2 molecular (z<7)
H2 excitation (z～20)
Obscured AGN (z<1)
Evolution of dust

z=12
Galaxy formation(z～10)
Massive BH evol.(2<z<10)

SKA
High-z HI 21cm-line

Astro-H

JWST

Optical/NIR/Sub-mm Obs.
z=7
Athena

z=6
2028～

z=0.5
2015～
Cluster of gal. (z～0.3)
Obscured AGN(z＜1)
Cosmic web, CXB

z=0

High energy Obs.
X-ray and Gamma-Ray

Evolution of cosmic web
WHIM (z<2)
Massive BH (z<6)
Cluster of gal. (z<2)
Accretion disk 24
Iron emission line

Readout ASICs (ASICs for Low Energy X-ray ver. 01)
Electrons (RMS)

Noise characteristics for input capacitance∝ 3 electron/pF

Readout from 1.7 keVusing SSDs
Input capacitance (pF)

Thanks to
K. Ikeda
T. Takahashi(ISAS/JAXA)
And
M. Arimoto(TITech)(1.3 keV for 4s significance)

25

Aperture Shade
30 degrees
Toward the SUNSUN

Pointingdirection

56 degrees toward the earth.
(horizon is under 26 degrees)

68cm

opticalinfrared

1353 W/m2

Aluminum mirror
Opt emissivity ～0.11
IR emissivity ～0.02

NOT USEFor radiator

EARTH
thermal＋albedo of sun rad.
1.3W + 2.12W

Thermal isolation

GFRP thermal
conductance
0.785 mW/(mm.K)

MLI 30 layers, and sun shirlds

Teflon with Ag
Opt emissivity ～0.11
IR emissivity ～0.82

Radiator
For aperture shade26

Real Time Alert

Sendable area fraction of real time alert (400 km otbit)

3.2 cm

3.0 cmIridium Short-Burst-Data(SBD 9603)
Packet Communication
Send： 340 byte
Receive： 270 byte
Delay： 1～3 min

FromNagata-san (Okayama U.)
Yamada-san (ISAS/JAXA)Special thanks
Yamada-san (TMU)

・ Duration of non-contact time isless than 15 minutes : 50 ~ 60 %,but the longest case is 5 hours
・ Almost perfectly covered around
Arctic/Antarctic regions.
・ We need an additional UHF antenna.

Distribution of non-contact time
15min27

0.18 Gyr (z=20)0.5(1) Estimation from lumi-func. (Niino 2012)
2.5 ～50 event/yr/str for z > 7

GRB090423 (z=8.2：spec.)
GRB090429 (z=9.2: phot.)

0.49 Gyr (z=10)

Redshift

Time since big bang (billion years)

Transition of the highest redshift record

1

1.5QSOsGRBs

2(2) Evolution from Dark matter halo(Mao 2012)~ 16 events/yr/str for z > 7(3) Star Formation Rate
(Wanderman & Piran 2010)~ 10 events/yr/str for z > 7~ 3 events/yr/str for z > 10High-z GRBs: ~10 events/yr/str

galaxiesYear

Swift observation:~ 0.5 event/yr/str for z > 6 (lower limit)

Expected high-z GRB rate is ~ 5 event/yr/strif we realize one order of better sensitivity than Swift-BAT in soft X-ray band28

1 – 1000 keV peak flux (photon/cm2/s)

GRB
090429B
090423080913140515A
050904120521C
130606A
060927

redshift
9.4
8.26
6.695
6.32
6.29
6.0
5.913
5.47

T90 (sec)
5.5 ± 1.0
10.3 ± 1.1
8±130
225 ± 1026.7 ± 4.4276 ± 19.31
22.6 ± 0.3

8s detection

Epeak (keV)
42.1 ± 5.6
54 ± 22121 (-39/+232)
71.7 ± 17.6

Redshift
CXB+GRCXB

100cm2CXB+GR
1000cm2

Time duration (sec)Properties of high-z GRBs

CXB■ Time duration of prompt emission ismuch shorter than expected one.
■ Typical energy of high-z GRBs are lower
than ones of nearby GRBs (Epeak ~ 200 keV).
We must observe E < 10 keVwith better sensitivity in soft X-ray band.
The goal is 1 < E < 20 keV.
Effective area of 1000 cm2 @ a few keV
will realize better sensitivity than Swift-BAT.
29