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HiZ-GUNDAMHigh-z Gamma-ray bursts for Unraveling the Dark Ages
and Extreme Space Time Mission
HiZ-GUNDAM working group
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Daisuke YONETOKU (Kanazawa University)
�Mission Concept has been approved by ISAS/JAXA� Target Launch is 2025/26–
Gamma-Ray Bursts in the Gravitational Wave Era (2019/10/28 – 11/1) @ Yokohama, JAPAN
HiZ-GUNDAM� Promotion of Time Domain Astronomy
Key Science 1: Exploration of early universe with GRB
Key Science 2: Multi-Messenger Astronomy
(1) GRB rate at z > 7(2) Cosmic reionization history(3) First heavy metals(4) Survey of Pop-III GRBs
(1) High energy phenomena associated with GW(2) Confirmation of existence of relativistic jet,
and statistical studies(3) Energy transition from
Jet à Cocoon à Kilonova/Macronovafrom X-ray to optical/NIR observation
(4) Diversities of kilonova/macronova
Selection of High-z GRBs,Rapid spectroscopic obs. with large area telescopes
Planck HP
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We timely contribute MM-Astronomyafter achieving design sensitivity of GW facilities.
(1) Detection of GRB/SGRB with the Wide Field X-ray Monitor(2) Automatic Attitude Control, and Follow-up Observation with
Near Infrared Telescope within ~ 100 sec since the trigger(3) Selection of high-z GRBs and kilonovae(4) Spectroscopic Observation with Large Area Telescope
within 1~1.5 hours TAO, Subaru, VLT, Keck, Gemini, GMT, JWST, E-ELT, TMT, etc. 3
HiZ-GUNDAM����� ������� FY 2025/26 –Satellite Orbit Sun Synchronous (twilight)������� 1 deg/sec������ ~ 440 kg������� �� � > 3 years����� ������ Iridium SBD / VHF��� � ������ 81 (JPN, Korea, UK, Italy, etc.)
Mission Overview: Wide Field X-ray Monitor: 136.3 kg (6 units)Near Infrared Telescope : 35.6 kgBase Frame : 15.5 kgSatellite Bus : ~ 250 kg
1m 1m
2m
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Wide Field X-ray Monitor
Items Parameters
Energy band (keV) 0.5 – 4 keV
Telescope type: Lobster Eye Optics
Module aperture size 192 x 192 mm2
Number of module 24
Field of View > 1.0 str (in total)
Focal length 300 mm
Focal plane detectors CMOS array
Number of CMOS 24
Sensitivity ~ 1e-10 (erg/cm2/s)
For 100 sec
Point Spread Function ~ 3 arcmin
Lobster Eye Optics (Micro Pore Optics)
CMOS Imaging Sensor
20μm
6μm
PHOTONIS or Japanese Industry
61.4 mm
61
.4 m
m
Focal Image
Obtained by
Taka Sakamoto’s
Group (AGU)
Jin Li’s poster
GPIXEL CMOSs� Back Side Illuminated type CMOS� Performance Verification � Radiation Tolerance Test
22.5 mm
61.4 mm
GSENSE 400BSI GSENSE 6060BSIActive image size 22.5 x 22.5 mm2 61.4 x 61.4 mm2
Pixel size 11 x 11 um2 10 x 10 um2
# of pixels 2048 x 2048 6144 x 6144
Shutter Rolling Rolling
Frame rate (STD) 48 fps 26.4 fps
Power <0.650 W 5.4 W (full speed)
# of LVDS pairs 8 50
X-ray Performance (400BSI)@ 0 degC, 0.1sec exposure
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multi
Neutral Layer
Depletion Layer
SingleMulti
Al Kα (1.486 keV)Mn Kα/Kβ (5.90 & 6.49 keV)
SingleMulti
� Single pixel event : depletion layerMultiple pixel event : neutral layer
� Single/Multi ratio depends on the resistivity of epitaxial layer
� Successfully measured 1.48 keV line
ΔE ~ 200 eV@ 0 degC
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Radiation Tolerance Test for CMOS (400BSI)Total Irradiation Dose (2018/08/01 – 02)Almost No Damage up to 30 krad
Particle irradiation (2019/05/23 – 24)Proton� 100 MeV, 5 krad (~6 yrs in orbit)� Increase of leakage current
à operation at -20 degC� No Single Event
Low-energy a-particle from 241Am~5 MeV, 24 krad (Over dose test)
à Removing 2.2% of high noise pixels
Ogino & Arimoto‘s poster
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Items ParametersTelescope type Offset GregorianAperture size 30 cmFocal length 183.5 cmF number F6.1Field of view 34 arcmin ×34 arcminFoV per pixel 2 arcsec × 2 arcsecImage size 3 pixel × 3 pixel Integration time 10 minutes (2 minutes x 5 frames)Wavelength Band (μm) 0.5−0.9 0.9−1.5 1.5−2.0 2.0−2.5Band width 0.4 µm 0.6 µm 0.5 µm 0.5 µmLimiting Magnitude AB, 10min, S/N=10 21.4 21.3 20.9 20.7
Focal detector HyViSi HgCdTe HgCdTe HgCdTe
4-band simultaneous photometryOptical & NIR TelescopeHeritages: CIBER-2 Rocket Experiment
28.5 cmLanz et al. (2014)
3 bandimaging
680m
m
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Afterglow spectrum is power-law with 0 < β < 1 ( ~ 95%), and β = 0.5 is used.Red: Input model (power-law with Ly-α drop)Blue: Fitting model (power-law with dust extinction)
Simulations: Photometric Redshift
z=7.019.5 mag(AB)
z=12.019.5 mag(AB)
z=12.020.7 mag(AB)
z=14.019.5mag(AB)
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� Photo-z coverage: 5 < z < 12 for m < 20.5 mag(AB)
� Accuracy of photo-z: Δz ~ +/- 0.1 for 19.5 mag (AB)Δz ~ +/- 1 for 20.7 mag (AB)
�We can observe afterglow candidate up to z < 19.5 even if we can not measure z.
AB M
agni
tude
with
out a
bsor
ptio
n
3s confidence region
Δχ2 mapLy-α drop vs. dust extinction
Redshift (input model)
Redshift (input model)
Reds
hift
(mod
el fi
t)Re
dshi
ft (m
odel
fit)
19.5 mag(AB)
20.7 mag(AB)
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Spacecraft Thermal Modeling
(1) Thermal Model
(2) Thermal Analysis in orbit situationNominal à Follow-up (Worst/HOT case)
à Nominal position Worst (Hot) case
Hot Case (Worst)Tmin [℃] Tmax [℃] ΔT [℃]
Primary M. -80.7 -80.7 < 0.1Secondary -83.6 -82.8 0.6
� Current DesignThe requirement T < 210 K (−63 ℃) isfully satisfied for NIR telescope.
� Thermal strain does not affect the image performance of NIR telescope.
� Temperature of LEO surface may drasticallychange about ΔT ~ 20 degC.
SunShield
We, Nobu KAWAI-san, will establish VHF ground station of SVOM project in Ogasawara island, and are coordinating to use their VHF network.
Real Time Alert (Iridium Short Burst Data/SVOM G-Stations)
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Based on the EGG nano-satellite,Real time communication rate is ~ 49 %(if the satellite attitude is stable)
We performed radiation tolerance test forboth SBD device and control board.We confirmed its tolerance of > 30 krad.
Iridium SBD (SBD 9603)
� X-ray trigger informationTrigger time, direction, lightcurves, etc.� NIR follow-up information� afterglow candidate� 4-band photometric information� bright star catalog for astrometry� trimmed image
After a ground analysis, send GCN Notice.
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12% of all sky
2% of all sky
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(erg
/cm
2 /s)
���$#&% (�) Time Scale of X-ray Transient (sec)
Swift/BAT
HiZ-GUNDAM
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X-ray event/yrGRB (z>9) best model 40GRB (z>9) lower limit > 15
GW/SGRB prompt ~8GW/SGRB E.E. ~8
GRB/SGRB ~700Low-Luminosity GRB > 5
X-Ray Flash 50
X-ray event/yrTidal Disruption 60
SN Shock Breakout > 5Stellar Flare many
Direct collapse BH a fewAccretion induced
collapse~10
Time Since Transient Discovery (sec)
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Sensitivity of Follow-up Obs.
Too lateObservation start
Near Infrared event/yrafterglow (z>9) best model 34afterglow (z>9) lower limit > 13
macronova ~8 + αSupernovae 40afterglow of
GRB/SGRB/XRFmany
Variable stars many
Detection Sensitivity and Expected Event Rate
DiscoverySpace
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Summary� HiZ-GUNDAM will strongly promote
(1) exploration of early universe(2) multi-messenger astronomy
� The mission concept was selected as a candidate of future project of ISAS/JAXA.
�We will have an international review in near future,and a mission definition review (MDR).
� An International follow-up team will effectively work to get ToO time with strong proposal, andto realize early follow-up observation with large area telescopes.
High-z Gamma-ray bursts for Unraveling the Dark Ages Mission
� Detection of high-redshift GRBs (9 < z < 12)
� Probing the reionization history and first metal elements
Mission Aim: Strong Promotion of
“Time Domain” & “Multi-Messenger Astronomy”.
Items ParametersAperture size 30 cmField of view 34 arcmin ×34 arcminIntegration time 10 minutes (2 minutes x 5 frames)Observation Band (μm) 0.5−0.9 0.9−1.5 1.5−2.0 2.0−2.5 Limiting Magnitude (AB)10 min exposure, S/N=10 21.4 21.3 20.9 20.7
Items ParametersEnergy band (keV) 0.4 – 4 keVField of View ~ 1.2 str (6 units)Sensitivity 1e-10 (erg/cm2/s)
For 100 sec exposurePoint Spread Function 3 arcminAngular accuracy ~ 60 arcsec
Wide Field X-ray Monitor Near Infrared Telescope
Observation Strategy(1) Discovery of high-energy transient with Wide Field X-ray Monitor(2) Automatic/Comprehensive follow-up with Near Infrared Telescope(3) Sending Quasi-Realtime Alert Messages(4) Spectroscopy with Large Area Telescopes for selected events
Key Science1: Probing the Early Universe
Key Science2: Progress of Gravitational Wave Astronomy
� Localization of X-ray transient and macronova associated with GW
� Energy transition from jet – cocoon – macronova
Wide Field X-ray Monitor
� Lobster Eye Optics
� CMOS imaging sensor
Near Infrared Telescope
� Offset Gregorian Optics
� simultaneous 4-band photometry
2025/26 –