M onitor of A ll-sky X -ray I mage MAXI mission on ISS
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M onitor of A ll-sky X -ray I mage MAXI mission on ISS Covering fraction of the sky 160 deg (long) ×1.5 deg (FWHM) × 2 .FO.V. F.O.V. 2 % Scans 90 ～ 98% with 96 minutes rotation of ISS. Position resolution Point spread function: 1.5 deg (FWHM) Localization accuracy: 6 arcminutes. Energy band, resolution 2 ～ 30 keV, 18% ＠ 5.9 keV. Timing accuracy 120μsec to GPS time. Detection limit (5σ) 7 mCrab (1orbit), 1 mCrab (1week). Covering fraction of the sky 90 deg (long) ×1.5 deg (FWHM) × 2 .FO.V. F.O.V. 1.3 % Scans 70% with 96 minutes rotation of ISS. Position resolution Point spread function: 1.5 deg (FWHM) Localization accuracy: 6 arcminutes. Energy band, resolution 0.5 ～ 10keV, < 150 eV ＠ 5.9 keV. Timing resolution 3 ～ 16sec depending on the readout mode of CCDs. Detection limit (5σ) 20 mCrab (1orbit), 2 mCrab (1week) Real time data Real time contact will be in more than 50% of the observation time. Alert delay is less than 30 s after the MAXI scan. Stored data Off-contact data are stored in the data recorder and Abstract MAXI can discover a distant X-ray nova and trace its light curve, which cannot be obse rved with previous ASMs. Much more bursts w ill be detected. A bright nova will be moni tored from the rising phase to the decaying end. Intensity [mCrab] Distance [light-yr] MAXI sensiti vity Current sensiti vity Observational Targets Time [ days ] Intensity [mCrab] 0 100 200 1 10 1 10 2 10 4 10 5 10 3 1orbit X-ray nova ! (Tanaka et al.) Long-term High-sensitivity X-ray monitoring MAXI sensitivi ty Current sensiti vity GSC SSC User Alert MAXI website ： http://www-maxi.tksc.j axa.jp/ E-mail: [email protected] Spectra obtained with SSC Solid-state Slit Camera (SSC) Gas Slit Camera (GSC) Zenithal view Forward view One-dim. detector collimat or sl it Slit camera and Field of view X-ray from the sources goes through the slit and is detected by the one-dimensional detector. The X-ray position in the detector corresponds to the location of the source in the F.O.V. The collimator defines the long F.O.V. Thus the source position (α,δ) is obtained. MAXI has two kinds of slit cameras: GSC and SSC. Six GSC and two SSC can cover two F.O.V.s: forward and zenithal. The F.O.V.s scan almost the whole sky with 96 minutes rotation of ISS. GSC utilizes gas proportional counters sen sitive to 2 - 30 keV. The one-dimensional X -ray position is given by the charge divisi on method of the carbon fiber anodes with 1 0μm diameter. The 12 counters makes very la rge 5000 cm 2 area. Metorex (Oxford) manufact ures large-area sealed Xe counters with spa ce quality. SSC utilizes X-ray CCDs sensitive to 0.5 - 10 keV. One stage Peltier cooler is attached under each chip. Pixel size is 24× 24μm, and pixel nu mber is 1024×1024. The 16 CCD × 2 cameras makes 200 cm 2 . Hamamatsu CCD has a deep depletion lay er and a good energy resolution. Real time contact will be established in 12 ～ 17 hours per day. The data is automatically processed in JAXA Tsukuba space center. When a burst or a nova is detected, an alert is issued within 30 s to observers in all over the world. The MAXI data goes public within 1 day. Alert and data publication MAXI instruments Solid-state Solid-state Slit Camera Slit Camera (SSC) (SSC) Weight 500 kg, Size 1.8 ×1.2×0.8m Gas Slit Camera (GSC) Gas Slit Camera (GSC) Proportional counter collimato r International Space Station (ISS) Japanese Experiment Module (JEM) Japanese Experiment Module forward altitude: 330 ～ 480 km inclination: 51.6 deg. orbital period: 96 m inutes MAXI Robot arm Pressuriz ed Module Exposed facility Tatehiro Mihara, Mitsuhiro Kohama, Motoki Nakajima (RIKEN), Masaru Matsuoka, Shiro Ueno, Hiroshi Tomida, Naoki Isobe, Haruyoshi Katayama, Mikio Morii (JAXA), Hiroshi Tsunemi, Emi Miyata (Osaka U), Nobuyuki Ka wai, Jun Kataoka (Tokyo Tech U), Atsumasa Yoshida, Kazutaka Yamaoka (Aoyama U), Hitoshi Negoro (Nihon U) • 2004.3. Critical Design Review (CDR) was p assed. The fabrication of flight counters a nd parts and their calibration have started. • 2006.4. The first assembly of the whole pa yload. • 2008 Launch by H-IIA rocket. ○GSC • Counters: 15 counters were already made out of 12 flight and ４ spare counters. The calibration of five of them were finished. • Collimators: Test of EM model was finis hed. PFM is in fabrication. ○SSC • Cameras: Test of EM camera was finishe d. PFM camera is being designed and manufac tured. Temperature control is being improve d. • CCD chips: Fabrication and screening we The Monitor of All-sky X-ray Image (MAXI) is a highly sensitive all-sky monitor which will be attached t o the Japanese Experiment Module of the International Space Station in 2008. MAXI utilizes scanning X-ray slit-cameras which consist of two kinds of instruments. The Gas Slit Camera (GSC) is the proportional coun ter with Xe and is sensitive to 2 - 30 keV. The Solid-state Slit Camera (SSC) is the CCD sensitive to 0.5 - 10 keV. The slit cameras have long field of views, and scan almost the whole sky in one orbit of ISS. As an X-ray all-sky monitor, MAXI will have an unprecedented sensitivity of 7 mCrab in one orbit scan, and 1 mCrab in one week. MAXI can monitor extragalactic objects as well as the galactic objects. MAXI will make a dynamic catalog of more than 1000 X-ray sources in time scales from hours to years. The alert of bursts and novae will be promptly informed to the world through the internet. The flight detectors were already b uilt, and the assembling and calibration of the detectors and collimators are in progress. H-IIA / HTV launch 2000 2001 2002 2003 2004 2005 2006 2007 2008 2009 2010 2011 1 st assembly MAXI operation Detailed design Fabrication and assembly Basic design CDR PDR Payload test software GSC fabri. & calibration SSC fabri. & calibration ASTRO-E2 Swift INTEGRAL GLAST Chandra XMM-Newton Lobster- ISS RXTE Missions MAXI schedule now Simulated MAXI observation. X-ray sources are picked up from this MAXI map and light curves for all the sources are obtained. MAXI monitors flux changes of more than 1000 X-ray sources in time scales from 96 minutes to years. MAXI takes “movies” of the X-ray sky. Previous ASMs targeted bright galactic objects. MAXI can observe beyond our g alaxy. MAXI status and schedule 20cm SSC camera and CCD ΔE=145eV 36cm 48cm Galactic coordinates observers Ale rt Low-rate data 1553B Mid-rate data Ethernet MAXI operation data request Databas e Data- base Spectrum in one day Detection in one day 1week MAXI data sheets
description
Zenithal view. Forward view. XMM-Newton. Chandra. RXTE. software. GSC fabri. & calibration. SSC fabri. & calibration. ASTRO-E2. Swift. INTEGRAL. Basic design. Detailed design. Fabrication and assembly. MAXI operation. now. 2000. 2001. 2002. 2003. 2004. 2005. 2006. 2007. - PowerPoint PPT Presentation
Transcript of M onitor of A ll-sky X -ray I mage MAXI mission on ISS
Monitor of All-sky X-ray Image
MAXI mission on ISS
Covering fraction
of the sky
160 deg (long) ×1.5 deg (FWHM) × 2 .FO.V.
F.O.V. 2 %
Scans 90 ～ 98% with 96 minutes rotation of ISS.
Position resolution Point spread function: 1.5 deg (FWHM)
Localization accuracy: 6 arcminutes.
Energy band, resolution 2 ～ 30 keV, 18% ＠ 5.9 keV.
Timing accuracy 120μsec to GPS time.
Detection limit (5σ) 7 mCrab (1orbit), 1 mCrab (1week).
Covering fraction
of the sky
90 deg (long) ×1.5 deg (FWHM) × 2 .FO.V.
F.O.V. 1.3 %
Scans 70% with 96 minutes rotation of ISS.
Position resolution Point spread function: 1.5 deg (FWHM)
Localization accuracy: 6 arcminutes.
Energy band, resolution 0.5 ～ 10keV, < 150 eV ＠ 5.9 keV.
Timing resolution 3 ～ 16sec depending on the readout mode of CCDs.
Detection limit (5σ) 20 mCrab (1orbit), 2 mCrab (1week)
Real time data Real time contact will be in more than 50% of the observation time.
Alert delay is less than 30 s after the MAXI scan.
Stored data Off-contact data are stored in the data recorder and are down-linked in the next contact.
Alert delay is 20 minutes ～ 3 hours.
Alert Bursts and novae are alerted to the users through the internet.
Data Images, spectra, and light curves of any X-ray sources and sky-areas can be obtained through web browsers in the internet.
Abstract
MAXI can discover a distant X-ray nova and trace its light curve, which cannot be observed with previous ASMs. Much more bursts will be detected. A bright nova will be monitored from the rising phase to the decaying end.
Inte
nsity
[m
Crab
]
Distance [light-yr]
MAXIsensitivity
Currentsensitivity
Observational Targets
Time [ days ]
Inte
nsity
[m
Crab
]
0 100 2001
101
102
104
105
103
1orbit
X-ray nova !
(Tanaka et al.)
Long-term High-sensitivity X-ray monitoring
MAXIsensitivity
Currentsensitivity
GS
CS
SC
Use
rA
lert
MAXI website ： http://www-maxi.tksc.jaxa.jp/ E-mail: [email protected]
Spectra obtained with SSC
Solid-state Slit Camera (SSC) Gas Slit Camera (GSC)
Zenithal view
Forward view
One-dim. detector
collimator
slit
Slit camera and Field of view
X-ray from the sources goes through the slit and is detected by the one-dimensional detector. The X-ray position in the detector corresponds to the location of the source in the F.O.V. The collimator defines the long F.O.V. Thus the source position (α,δ) is obtained. MAXI has two kinds of slit cameras: GSC and SSC. Six GSC and two SSC can cover two F.O.V.s: forward and zenithal. The F.O.V.s scan almost the whole sky with 96 minutes rotation of ISS.
GSC utilizes gas proportional counters sensitive to 2 - 30 keV. The one-dimensional X-ray position is given by the charge division method of the carbon fiber anodes with 10μm diameter. The 12 counters makes very large 5000 cm2 area. Metorex (Oxford) manufactures large-area sealed Xe counters with space quality.
SSC utilizes X-ray CCDs sensitive to 0.5 - 10 keV. One stage Peltier cooler is attached under each chip. Pixel size is 24× 24μm, and pixel number is 1024×1024. The 16 CCD × 2 cameras makes 200 cm2. Hamamatsu CCD has a deep depletion layer and a good energy resolution.
Real time contact will be established in 12～ 17 hours per day. The data is automatically processed in JAXA Tsukuba space center. When a burst or a nova is detected, an alert is issued within 30 s to observers in all over the world. The MAXI data goes public within 1 day.
Alert and data publication
MAXI instruments
Solid-state Slit Solid-state Slit Camera (SSC)Camera (SSC)
Weight 500 kg, Size 1.8 ×1.2×0.8m
Gas Slit Camera (GSC)Gas Slit Camera (GSC)
Proportional counter collimator
International Space Station (ISS)
Japanese Experiment Module (JEM)
Japanese Experiment
Module
forward
altitude: 330 ～ 480 kminclination: 51.6 deg.orbital period: 96 minutes
MAXI
Robot armPressurizedModule
Exposed facility
Tatehiro Mihara, Mitsuhiro Kohama, Motoki Nakajima (RIKEN), Masaru Matsuoka, Shiro Ueno, Hiroshi Tomida, Naoki Isobe, Haruyoshi Katayama, Mikio Morii (JAXA), Hiroshi Tsunemi, Emi Miyata (Osaka U), Nobuyuki Kawai, Jun Kataoka (Tokyo Tech U), Atsumasa Yoshida, Kazutaka Yamaoka (Aoyama U), Hitoshi Negoro (Nihon U)
• 2004.3. Critical Design Review (CDR) was passed. The fabrication of flight counters and parts and their calibration have started.• 2006.4. The first assembly of the whole payload.• 2008 Launch by H-IIA rocket.
○GSC • Counters: 15 counters were already made out of 12 flight and ４ spare counters. The calibration of five of them were finished.• Collimators: Test of EM model was finished. PFM is in fabrication.
○SSC• Cameras: Test of EM camera was finished. PFM camera is being designed and manufactured. Temperature control is being improved.• CCD chips: Fabrication and screening were finished. 48 flight chips are ready.
The Monitor of All-sky X-ray Image (MAXI) is a highly sensitive all-sky monitor which will be attached to the Japanese Experiment Module of the International Space Station in 2008. MAXI utilizes scanning X-ray slit-cameras which consist of two kinds of instruments. The Gas Slit Camera (GSC) is the proportional counter with Xe and is sensitive to 2 - 30 keV. The Solid-state Slit Camera (SSC) is the CCD sensitive to 0.5 - 10 keV. The slit cameras have long field of views, and scan almost the whole sky in one orbit of ISS. As an X-ray all-sky monitor, MAXI will have an unprecedented sensitivity of 7 mCrab in one orbit scan, and 1 mCrab in one week. MAXI can monitor extragalactic objects as well as the galactic objects. MAXI will make a dynamic catalog of more than 1000 X-ray sources in time scales from hours to years. The alert of bursts and novae will be promptly informed to the world through the internet. The flight detectors were already built, and the assembling and calibration of the detectors and collimators are in progress.
H-IIA / HTV launch
2000 2001 2002 2003 2004 2005 2006 2007 2008 2009 2010 2011
1st assembly
MAXI operationDetailed design Fabrication and assemblyBasic design
CDRPDR
Payload test
software
GSC fabri. & calibration
SSC fabri. & calibration
ASTRO-E2Swift
INTEGRAL
GLAST
ChandraXMM-Newton
Lobster-ISSRXTE
M
issi
ons
M
AX
I sch
edu
le
now
Simulated MAXI observation. X-ray sources are picked up from this MAXI map and light curves for all the sources are obtained. MAXI monitors flux changes of more than 1000 X-ray sources in time scales from 96 minutes to years. MAXI takes “movies” of the X-ray sky.
Previous ASMs targeted bright galactic objects. MAXI can observe beyond our galaxy.
MAXI status and schedule
20cm
SSC camera and CCD
ΔE=145eV
36cm
48cm
Galactic coordinates
observers
Alert
Low-rate data 1553B
Mid-rate data Ethernet
MAXI operation
data
request
Database
Data- base
Spectrum in one day
Detection in one day
1week
MAXI data sheets
