MAXI - Monitor of All-sky X-ray ImageMAXI - Monitor of All-sky X-ray Image

Physics of X-ray All Sky Monitors and MAXI Mission for 　

International Space StationM.Matsuoka(1),

H.Katayama(1), K.Kawasaki(1), N.Kuramata(1), M.Morii(1), N.Tomida(1), S.Ueno(1), T.Yokota(1), T.Mihara(2), N.Isobe(2), M.Kohama(2), I.Sakurai(2), M.Nakajima(2), H.Tsunemi(3), E.Miyata(3), N.Kawai(4), J.Kata

oka(4), A.Yoshida(5) and H.Negoro(6)

(1)JAXA(Japan Aerospace Exploration Agency), (2)RIKEN, (3)Osaka Univ., (4)Tokyo Inst. Tech., (5)Aoyama G. Univ., and (6)Nihon Univ.

APRIM 2005, Bali, 2005 July 26-29

Japan Aerospace Exploration Agency

MAXI - Monitor of All-sky X-ray ImageMAXI - Monitor of All-sky X-ray Image

Contents

Wide Field Camera vs. Narrow Field Telescope

History of ASM

Scientific Results with ASM

MAXI Mission 　 　　• MAXI Mission • MAXI Hardware / Sensitivity

MAXI Ground System

Multi-wavelength Observations with MAXI

Summary

MAXI - Monitor of All-sky X-ray ImageMAXI - Monitor of All-sky X-ray Image

ASM vs. Narrow Field Telescope

ASM Narrow Field Telescope Observe many targets together continuously

Transient & bursting objts

Discovery, then inform to general observatories

Long-term variability of many targets

Wide field sky population of X-ray sources

Redshift: ~ 10 ?

Observe only one target precisely for a certain time

A scheduled target

Follow up observations after ASM information

Short-term variability of some scheduled targets

Detailed obs. of spectra and structure in narrow fov.

Redshift: ~ 7

MAXI - Monitor of All-sky X-ray ImageMAXI - Monitor of All-sky X-ray Image

History of ASM

Satellite Cnty Active Period Sensit. Results

Vela5 a&b USA late 1960era >100 mC

2-10 keV-ray bursts, X-ray novae

Ariel 5 UK late 1970era >50 mC

2-10 keVSystem. Obs. of X-ray novae

Ginga Jpn late 1980era >30 mC

2-20 keVSpectra of X-ray novae

RXTE USA mid’90-present >10 mC

2-10 keVSystem. Obs. of Galactic obj.

Swift USA ’05-present > 1 mC

15-200 keV-ray bursts monitor satellite

MAXI Jpn 2008? > 1 mC

2-20 keVSystematic obs. of Galactic & 　 extra-Galactic objects

ASTROSAT India 2007? > 10 mC

2-10 keVSimilar to RXTE

Lobster-ISS ESA after 2010 ? > 0.1 mC

0.2-2 keVHaving multi small mirrors

Wide band spectrum of Blazar

　 Radio 　　　　 Optical 　　　 X-ray 　　　 1012γ-ray 　　 1015γ-ray

Mrk 421 Ｅ vidence of SSC model!

MAXI Mission• Promotion of Multi-wavelength Observations.

• Dynamics of Galactic and Extra-galactic Objects. Close Binary X-ray sources （ Black holes, Neutron

stars ） Active Galactic Nuclei （ Giant black holes, Cosmic jets ）

• Creation of Data Base for Variable X-ray Sources. hours, days, months, year since 1960 era!

• Large Scale Mapping of Diffuse X-ray Sky. Soft X-ray Sky (Galactic ridge structure with atomic compon’t)

CXB Fluctuation detection: <1 % @ 1.5 deg.2 for two years.

Two-Year Mission on the Space Station

MAXI scans almost the whole sky once every orbit (= every 90 mins)

Grapple Fixture for a robot armGrapple Fixture for a robot arm

ElectronicsElectronics

Gas Slit Camera (GSC)Gas Slit Camera (GSC): X-ray gas proportional counter: X-ray gas proportional counter

Solid-state SlitSolid-state SlitCamera (SSC)Camera (SSC): X-ray CCD: X-ray CCD

Optical Star SensorOptical Star Sensor

Radiator for X-ray CCDsRadiator for X-ray CCDs

180cm180cm

80cm80cm

100cm100cm

Total weight: 490 kgTotal weight: 490 kg

MAXI Payload

ATCS

PIU

RLG

GPS

GSC(Gas PC)

SSC(X-ray CCD)

Sky Coverage

Instant 2 % 1.3 %

1 orbit 90-98% Max 70%

Imaging PSF 1.5 deg (FWHM)

Position Accuracy < 6 arcmin

Spectroscopy(FWHM@5.9keV)

2-30 keV

( 18 % )

0.5-10 keV

( <150 eV)

Timing Accuracy 120 sec 3-16 sec

Sensitiv-ity (5)

1 orbit 10 mCrab 20 mCrab

1 week 1 mCrab 2 mCrab

Real data

(> 50 % )

From Detection to Alert

30 sec (Goal)~100 min

Stored

(< 50 %)

From Detection to Alert

20 min – 3 hours

User

Interf-ace

Alert Internet (mail, socket)

Data Image, Spectum, Light curve via Web browser

Alertdelay

Specification of MAXIThermal Mechanical Model

160 deg

1.5 deg (FWHM)

　　　　　 Time (days after outburst)

Flu

x (

Cra

b

un

it)

X-ray spectra are detectable every day

Detectable in one day

Detectable in one week

One Crab

= 2.4x10-9 erg sec-1 cm-2

One m Crab

Tanaka & Shibazaki, Annu. Rev.Astron. Astrophys. 34 (1996), 607

X-ray Nova Light Curves 　　　　　　 and MAXI 　 Detectability

Observation

Simulation

NASA/JAXA

Real Data

NASA

On-board Stored Data

JAXA

On-board Stored Data

Scan Time

Po

siti

on

in F

OV

First ComeFirst AnalyzedAlert

Alert

Alert

a Month ago, a Week ago, Yesterday, Today

Longer-term& Sensitive

Alert

X-ray Nova Search Concept

Quickness

Completeness

Multi-wavelength Observations

• X-ray Novae, X-ray Transients Black hole binaries, Neutron star binaries • AGN’s Long-term variability of Blazars, Seyfert

galaxies, etc• Multi-Wavelength Observatories

– Radio, Optical telescope (small size is OK!)– In Japan Optical telescopes > 60 cm – MAGNAM (Mauna Kea, Univ. of Tokyo) – GLAST etc (Gamma-ray)– CANGAROO etc (TeV Gamma-ray)

MAXI/ISS Schedule

• 2008: ISS-JEM-MAXI completion goal ?• Payloads for ISS (JEM), an omnibus system

= 　 Schedule is changeable.

= 　 ASM Science would not become out-of-date. • ASM or Monitor astronomy could be one of important scien

ces? • Please participate in multi-wavelength observations of activ

e astronomical objects with MAXI.• Please contact MAXI team if you are interesting in MAXI! • E-mail: 　　 　　　　　　　　　　　　　　　　　　 or

　

MAXI - Monitor of All-sky X-ray ImageMAXI - Monitor of All-sky X-ray Image

SummaryDynamics of Galactic and Extra-galactic Objects: Multi-wavelength Observations are desirable.

Creation of Data Base for Variable X-ray Sources: Necessity of Continuation of ASM missions.

Large Scale Mapping of Diffuse X-ray Sky: Toward better Energy Resolution, Doppler-shift and Absorption etc at the enery band of 0.5~20 keV.

Please participate in multi-wavelength observations with your telescopes.

　 Please contact by E-mail: 　　　　　　　　　　　　　 or

MAXI launching time: 2008.

MAXI - Monitor of All-sky X-ray ImageMAXI - Monitor of All-sky X-ray Image

Thank you for your attention!