Slit of GSC

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High sensitivity all sky X-ray monit High sensitivity all sky X-ray monit or or and survey with MAXI and survey with MAXI N. Isobe (RIKEN, [email protected] ) , Mihara, M. kohama, M. Suzuki Mihara, M. kohama, M. Suzuki (RIKEN), (RIKEN), M. Matsuoka, S. Ueno, H. Tomida (JAXA), N. Kawai, J. Kataoka (Tokyo Tech. Univ.), A. Yoshida, 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.), K. Yamaoka (Aoyama Gakuin Univ.), H. Tsunemi, E. Miyata (Osaka Univ), H. Negoro (Nihon Univ.), M. Morii (Rikkyo Univ.), and MAXI team M. Morii (Rikkyo Univ.), and MAXI team Web : http//www-maxi.tksc.jaxa.jp Web : http//www-maxi.tksc.jaxa.jp Slit of GSC Slit of SSC hat is MAXI (Monitor of All sky X-ray Image) What to be explored with MAXI All sky X-ray monitor on t he Japanese Experimental Mo dule (JEM) of the Internati onal Space Station (ISS) Launch : autumn, 2008. Orbital period : 96 minut e (ISS). Mission life : more than 2 years Sensitivity : 1 mCrab @ 1 week Instruments on MAXI ISS Motion ISS Motion Concept of slit camera GSC SSC X-ray source 1 X-ray source 2 Detector Energy Range Effective Area Field of view Energy Resolution Position Accuracy Proportional counters (10m Carbon anode, Xe + CO 2 @ 1.4 atom) 2 – 30 keV 5350 cm 2 1.5 x 160 degree 2 18 % @ Mo-K 0.1 degree X-ray CCDs (made in Japan) 0.5 – 10 keV 200 cm 2 1.5 x 90 degree 2 140 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) GSC SSC (without collimators) Sensitivity of MAXI 1 mCrab @ 1 wee k 3 mCrab @ 1 da y 10 mCrab @ 1 orbit (96 min) CCD chip MAXI can monitor mor e than 1000 X-ray so urces, especially ac tive 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 42 1 Star Sensor 1d-position sensitive detector Slit Zenith FoV Forward FoV Scan C ollimator Black hole mass on various scales will be estimated with MAXI sec min hour day Time scale Mass -1 Mrk 50 1 Cyg X-1 AGNs (Kataoka 2000) (Takahashi 1998) Emission line mapping with SS Monitoring Galactic sources MAXI and GLAST can trace the highest energy electrons in jet Monitoring of blazars Black Holes Neutron 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,). MAXI MAXI 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).

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cts/sec. Day. ROSAT All Sky Map (3/4 keV). - PowerPoint PPT Presentation

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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).