power point file

MAXI STATUS
全天X線監視装置
M.Matsuoka
NASDA-SURP
松岡勝
2002.7.17
Introduction
• X-ray ASM: one of the most important fields in the
space astronomy.
• MAXI mission: to scan the entire sky every 90
minutes with X-ray slit cameras in order to record
patterns of X-ray emission from thousands of
astronomical objects.
• MAXI sensitivity: the best of so far realized X-ray
ASM.
• MAXI enables us to monitor a short-term and longterm activities of weak extra-galactic objects as
well as Galactic objects accompanying BH & NS.
History of X-ray All Sky Monitor
-- ASM progress every Decade -• Vela 5 a&b (USA)
late 1960 era
g-ray bursts, X-ray novae
> 100 mC
• Ariel 5 (UK)
late 1970 era
Systematic obs. of X-ray novae
> 50 mC
• Ginga (Japan)
late 1980 era
Spectral obs. of X-ray novae
> 30 mC
• RXTE (USA)
late 1990 and now
Systematic obs. of Galactic X-ray targets > 10 mC
• MAXI (Japan)
~ 2006 AGN
• Lobster-ISS (UK &) ~ 2010 Syst. AGN
> 1 mC
~ 0.1 mC
X-ray Nova Light Curves
Flux (Crab unit)
X-ray spectra are
detectable every day
One Crab
Detectable in one day
Detectable in one week
Time (days after outburst)
Tanaka & Shibazaki, Annu. Rev.Astron. Astrophys. 34 (1996), 607
One m Crab
Discovery of γ-ray Bursts
• Gamma-ray Bursts were discovered
with ASM/Burst (Atomic Bomb)
Monitor on Vela a&b of LANL (USA)
in 1967.
Field of View of MAXI
NASDA
RIKEN
MAXI は 1.5x160度の二つの細長い視野を持つ。
視野方向はそれぞれ、 ISS (International Space Station)
の進行方向と天頂方向である(左図の赤線)。
ISS が90分で軌道を一周するのに伴い
全天をスキャンする。
天頂方向
天頂方向の視野
Ｘ線入射スリット
野
視
スキ
ャン
方
ISS の進行方向
向
スキャン方向
検
ISS進行方向の視野
X線
感
置
地球方向
元
次
一
位
型
応
器
出
Overview of MAXI
Grapple Fixture for a robot arm
Radiator for X-ray CCDs
Electronics
Optical Star Sensor
ATCS
180cm
Gas Slit Cameras (GSC)
: X-ray gas proportional counter
100cm
80cm
Solid-state Slit
Cameras (SSC)
: X-ray CCD
Total weight: 490 kg
One dimensional
Proportional counter
X-ray CCD
358 mm
12 units for flight
32 pieces for flight
Radiation Damage of CCD
CTI/transfer
CTI=Charge Transfer In-efficiency
Protons
particls/cm2
No damage
Electrons
Loop Heat Pipe
& Radiator
System
CCD Peltier Power Out
X-ray Nova Light Curves and MAXI Detectability
Flux (Crab unit)
X-ray spectra are
detectable every day
One Crab
Detectable in one day
Detectable in one week
Time (days after outburst)
Tanaka & Shibazaki, Annu. Rev.Astron. Astrophys. 34 (1996), 607
One m Crab
Detectability of MAXI
NASDA
RIKEN
MAXI は1mCrab 以上
の強度をもつX線源
（約1000個もの銀河
系内および系外天
体）
を監視する。
1軌道周期
(30 sources)
1日
(100 sources)
1週間
(1000 sources)
Simulation of MAXI Observation
One Orbit
5-month
MAXI Data Communication System
ISS-JEM
MAXI
DRTS
Ethernet/Command
NASDA
NASA
Alart data
Stored data
MAXI Science team
Concept of Lobster-ISS (ESA)
Field of
View
6 units
Image
Detector
Launch: 2009 or later !
Micro channel mirror
MAXI Schedule
1997
H 9
採択
10
1999
11
開発確認審査
12
2001
13
2003
15
14
PDR/SR-1 CDR/SR-2
NASA/SR1 NASA/SR2
概念設計
基本設計
詳細設計
部分試作
部分試験
TMM試験
16
SR-3
NASA/SR3
2005
17
18
打上運用
?
設計維持
FM製作
各部試験
一部のEM
総合試験
射場試験
?
PFM物品の調達
Now under TMM test!
待機 ?
19
Summary（日）
• 全天Ｘ線監視(ASM)は宇宙観測の重要な分野。
• MAXI は90分で太陽避けない場合98%, 太陽避けて
も90%の宇宙を走査可能。
一時には、
Chandra/HST では 5/10000% の宇宙のみを観測。
• ASMで予想外の発見がなされてきた。例えば、
HSTやChandraよりも遠い天体を捉える可能性あり。
• ISS は全天走査観測に最も適している。
• X線ASMは1960年代からなされほぼ10年毎に機器
及びサイエンスが発展。
• JEM-MAXIそして ESA-Lobster-ISSは21世紀初頭の
ASM の役割を果たし、宇宙物理学に貢献可能。
Summary(E)
• X-ray ASM: one of the most important fields in the
space astronomy.
• MAXI mission: to scan the entire sky every 90
minutes with X-ray slit cameras in order to record
patterns of X-ray emission from thousands of
astronomical objects.
• MAXI sensitivity: the best of so far realized X-ray
ASM.
• MAXI enables us to monitor a short-term and longterm activities of weak extra-galactic objects as
well as Galactic objects accompanying BH & NS.
Appendix A
ASM and Narrow Field Telescope
ASM
• Observe many targets
together
• Bursting objects
• Discovery, then inform to
general observatories
• Long-term variability of
many targets
• Wide field sky population
of X-ray sources
• Redshift: l/l0 ~ 10 ?
Narrow Field Teles.
• Observe only one target
precisely for a certain time
• A scheduled target
• Follow up observations
after ASM informations
• Short-term variability of
some scheduled targets
• Detailed obs. of spectra
and structure in narrow fov.
• Redshift: l/l0 ~ 7
Appendix B
Why is the X-ray band
favorable for ASM?
• Flux in X-ray band is variable for most targets.
• Variety of targets: X-ray binaries, X-ray novae,
AGN, Transients(BH, NS), Pulsars, g-ray bursts.
• Multi-colour observations stimulated by ASM
discovery, they open new field of astronomy.
• Space detectors enable a whole sky obs.
• Now ASM astronomy is established, started
from parasite instrument on main observatory.

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