MAXI Status and ISS Science

Masaru MatsuokaMatsuoka.masaru@nasda.go.jp

NASDA(JAXA* from October 1,2003)

Tsukuba Space CenterMAXI TMM Overview

* Japan Aerospace Exploration Agency (=ISAS+NASDA+NAL)

August 2 ２ , 2003 Max-Planck Inst.

Monitor of All-sky X-ray Monitor of All-sky X-ray Image (MAXI)Image (MAXI)

358 mm

GSC GSC SSC

MAXI

RIKENNASDA

- To be placed on the International Space Station in 2008 ?

- Energy range is 0.5 – 30 keV for combined CCD camera and Gas Slit Camera (SSC:200 cm2 ,GSC: 5350 cm2)

GSC: 2-30 keV

MAXI Overview and Scanning Process

SSC: 0.5-10 keVWeight: 490 kg

Now MAXI is in a final phase for FM.

Sen

siti

vity

(m

Cra

bs)

Dwell Time (seconds)

SSCGSC

MAXI Sensitivity

Systematic error level

MAXI 　 Sensitivity

OneWeek

OneDay(100sources)

(1000sources)

MAXI will monitor

extra-galactic

objects as well as

Galactic sources

above 1 m Crab.

RIKENNASDA

One Orbit (30 sources)

Appendix AAppendix A

　　　　　 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

SIMULATION of GSC observations

ISS one orbit(90 min)　　　　 2 months

~30 Galactic sources ~ 1000 sources incld. AGN

MAXI Mission• 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 (Distribution of distant active galactic nuclei) Fluctua

tion detection limit: a few % @ 1.5 deg.2 for two years.

RIKENNASDA

A Light Curve of An X-Ray Nova during Rising

Phase

GS 2000+25

with Ginga-ASM

Tsunemi et al . ApJ.L 　　 337 (1989), L81

Long-term X-ray Intensity Variations in Cyg X-2

Paul et al. Ap.J. 528 (2000), 410

X-ray Light Curves

Power Density Spectrum

1990 era

1980 era

1970 era

1960 era

Galactic OVII & VIII Map with SSC

ROSAT all-sky map of CXB

Galactic Soft X-ray Spectra correspond’g to each Sky Region.

Snowden et al. 1997 ApJ.

Markevitch et al. 2003 ApJ.

MAXI SSC expected counts: 80- 310 counts in 1.5°x1.5° for 2 yr operation. Obs.eff.=0.7

AGN Topics• Multiwavelength Simultenous Obs. of ~ 100? AG

N’s (Long-term variability of Blazars, Sy etc)– Radio– Opt (MAGNAM etc)– Gamma (GLAST etc)– TeV Gamma (CANGAROO etc)

• Connection between BLSy and NLSy and between AGN and BHC

• Binary AGNs?

• CXB: Fluctuation in All Sky Background < a few % in 1.5x1.5 deg2 < 0.5 mcrab

Multi-wavelength Observations of “Blazar”

- Rapid time-variability as short as 1 day ： ~ 1016 cm (0.01 pc)

- Wide-band spectra from radio to TeV -ray ： acceleration up to 1012 eV

TeV

RXTE (8-15keV)

ASCA(0.5-7keV)

EUVE

SAX

1 day

radi

o

optic

alX-

ray

GeV

-

TeV-

Mrk 421

Mrk 421

synchrotronInverse Compton

Successful SSC Model

Takahashi et al. 2000, ApJL 542, L105

R-band and X-ray correlation of N3516

sampling inteval ~ 4.3 - 17 d

Smoothed R-band

(advanced)

Maoz et al. 2002, AJ 124, 1988

AGN mass estimation from X-ray variabilityHayashida et al 1998 ApJ 500

Cyg X-1

AGN

AGN mass estimation in comprison with Cyg X-1

(Cyg X-1)

Hayashida et al 1998 ApJ 500

MAXI/ISS Schedule and ISS Science

• 1992: ISS completion goal in 1982 ?• 2000: ISS completion goal in 1992 ?• 2003: ISS-JEM-MAXI completion goal in 1996• 2008: present ISS-JEM-MAXI completion goal ?• Payloads for ISS (JEM), an omnibus system = 　 Schedule is changeable. = 　 Science should not become out-of-date. = Resources & attitude system are restricted. • ASM or Monitor astronomy could be one of reaso

nable sciences? MAXI is delayed and then Lobster-ISS follows complementarily.

Summary

・ Dynamics of Galactic and Extra-galactic Objects: Multi-color Observations.

・ 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.

・ MAXI launching time: ready in 2007 with the best ASM sensitivity. But Lobster-ISS will follow complementarily with better sensitivity.

Thank you for your

attention.

ASCA long-look of BlazarsASCA Light Curve Power Spectra

1 day

1 day

Kataoka et al. ApJ 2001Tanihata et al. ApJ 2001

- Every day flares : tvar ~ 105 [s]

- Steep PSD spectra ( t < tvar)

R ~ ctvar~ 1016 [cm]

Mrk421

Mrk501

PKS2155-304

Appendix BAppendix B