Slit of GSC
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Transcript of Slit of GSC
High sensitivity all sky X-ray monitorHigh sensitivity all sky X-ray monitor and survey with MAXI and survey with MAXI
N. Isobe (RIKEN, [email protected]) , Mihara, M. kohama, M. Suzuki (RIKEN), Mihara, M. kohama, M. Suzuki (RIKEN),
M. Matsuoka, S. Ueno, H. Tomida (JAXA), N. Kawai, J. Kataoka (Tokyo Tech. Univ.), A. Yoshida, K. Yamaoka (Aoyama GM. Matsuoka, S. Ueno, H. Tomida (JAXA), N. Kawai, J. Kataoka (Tokyo Tech. Univ.), A. Yoshida, K. Yamaoka (Aoyama Gakuin Univ.), H. Tsunemi, E. Miyata (Osaka Univ), H. Negoro (Nihon Univ.), M. Morii (Rikkyo Univ.), and MAXI teamakuin Univ.), H. Tsunemi, E. Miyata (Osaka Univ), H. Negoro (Nihon Univ.), M. Morii (Rikkyo Univ.), and MAXI team
Web : http//www-maxi.tksc.jaxa.jpWeb : http//www-maxi.tksc.jaxa.jpSlit of GSC
Slit of SSC
What is MAXI (Monitor of All sky X-ray Image)
What to be explored with MAXI
All sky X-ray monitor on the Japanese Experimental Module (JEM) of the International Space Station (ISS) Launch : autumn, 2008.Orbital period : 96 minute (ISS).Mission life : more than 2 yearsSensitivity : 1 mCrab @ 1 week
Instruments on MAXI
ISS Motion
ISS Motion
Concept of slit camera
GSC SSC
X-ray source 1X-ray source 2
Detector
Energy RangeEffective AreaField of viewEnergy ResolutionPosition Accuracy
Proportional counters (10m Carbon anode, Xe + CO2 @ 1.4 atom)
2 – 30 keV5350 cm2
1.5 x 160 degree2
18 % @ Mo-K0.1 degree
X-ray CCDs (made in Japan)
0.5 – 10 keV200 cm2
1.5 x 90 degree2
140 eV 0.1 degree
Field of views of MAXI
Quick alert of X-ray transients flare of known sources-ray bursts and their afterglowDistribution of distant AGNs (X-ray BGD)etc.
GSC SSC (without collimators)
Sensitivity of MAXI
1 mCrab @ 1 week
3 mCrab @ 1 day10 mCrab @ 1 orbit (96 min)
CCD chip
MAXI can monitor more than 1000 X-ray sources, especially active galactic
nuclei (AGNs).
X-ray flux of known sources, plotted against distance
RXTE-ASM ( ~ 30 mCrab )
A simulated lightcurve of MCG-6-3015, with MAXI Power spectrum density,
(multiplying by frequency; Hayashida et al. 1998)
“Dynamic” Catalog of X-ray sources
Long-term variability of AGNs
Day
cts/
sec
Simulated all sky image to be obtained with MAXI GSC(Diffuse sources excluded)
1 orbit
2 weeks
Mrk 421
Star Sensor
1d-position sensitive detector
Slit
Zenith FoVForward FoV
ScanCollimator
Black hole mass on various scales will be estimated with MAXI
sec min hour day
Time scale ∝ Mass-1
Mrk 501
Cyg X-1
AGNs
(Kataoka 2000)(Takahashi 1998)
Emission line mapping with SSCMonitoring Galactic sources
MAXI and GLAST can trace the highest energy electrons in jet
Monitoring of blazars
Black HolesNeutron Stars
MAXI can monitor fainter objects.(MAXI sensitivity is 0.075 cts/s in the figures !)
MAXI team (2003)
JEM
ISS
MAXI
ROSAT All Sky Map (3/4 keV)
MAXI SSC will make a detailed map of emission lines (e.g., Oxygen) in our Galaxy
(Local bubble, galactic ridge, etc,).
MAXIMAXI GLAST GLAST
Earth
MAXI
collimator
Proportional Counters Slit
RXTE/ASM Lightcurve (Bradt et al. 2002)
Snowden et al. 1997
MAXI carries two scanning camera Gas Slit Camera (GSC) & Solid-state Slit Camera (SSC)Both cameras
consist of 1-d position sensitive detector, collimator and slit. have a narrow rectangular field of view. are set up toward zenith and forward direction, to compensate non-operational periods (e.g. South Atlantic Anomaly).