High sensitivity all sky X-ray monitor and survey with MAXI Mihara, M. kohama, M. Suzuki (RIKEN), M. Matsuoka, S. Ueno, H. Tomida (JAXA), N. Kawai, J.

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High sensitivity all sky X-ray monitor and survey with MAXI 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 Gakuin Univ.), H. Tsunemi, E. Miyata (Osaka Univ), H. Negoro (Nihon Univ.), M. Morii (Rikkyo Univ.), and MAXI team Web : http//www-maxi.tksc.jaxa.jp High sensitivity all sky X-ray monitor and survey with MAXI N. Isobe (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 Gakuin Univ.), H. Tsunemi, E. Miyata (Osaka Univ), H. Negoro (Nihon Univ.), M. Morii (Rikkyo Univ.), and MAXI team Web : Slit 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, Orbital period : 96 minute (ISS). Mission life : more than 2 years Sensitivity : 1 1 week  Instruments on MAXI ISS Motion Concept of slit camera GSCSSC X-ray source 1 X-ray source 2 Detector Energy Range Effective Area Field of view Energy Resolution Position Accuracy Proportional counters (10  m Carbon anode, Xe + CO 1.4 atom) 2 – 30 keV 5350 cm x 160 degree 2 18 Mo-K  0.1 degree X-ray CCDs (made in Japan) 0.5 – 10 keV 200 cm x 90 degree eV 0.1 degree Field of views of MAXI Quick alert of X-ray transients flare of known sources  -ray bursts and their afterglow Distribution of distant AGNs (X-ray BGD) etc. GSC SSC (without collimators) Sensitivity of MAXI 1 1 week 3 1 day 10 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 , 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 FoV Forward FoV Scan Collimator 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 SSC Monitoring 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 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,). MAXI GLAST Earth MAXI collimator Proportional Counters Slit RXTE/ASM Lightcurve (Bradt et al. 2002) Snowden et al 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).