View
218
Download
0
Category
Preview:
Citation preview
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!
Recommended