hiz-gundamyokohamagrb2019.wdfiles.com/local--files/program:files-day2/43_hiz-gundam_yonetoku.pdfhiz-gundam...

15
HiZ-GUNDAM High-zGamma-ray bursts for Unraveling the Dark Ages and Extreme Space Time Mission HiZ-GUNDAM working group 1 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

Upload: others

Post on 20-Jan-2020

4 views

Category:

Documents


0 download

TRANSCRIPT

HiZ-GUNDAMHigh-z Gamma-ray bursts for Unraveling the Dark Ages

and Extreme Space Time Mission

HiZ-GUNDAM working group

1

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

2

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

4

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

����� �����

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

7

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

8

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

9

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)

10

� 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)

11

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)

12

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.

�����

!��

������

���!����

���

12% of all sky

2% of all sky

��

��

(erg

/cm

2 /s)

���$#&% (�) Time Scale of X-ray Transient (sec)

Swift/BAT

HiZ-GUNDAM

13

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)

���

�!������

��!"��

����

����!"��

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

14

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 –