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MAXI Status and ISS Science

MAXI Status and ISS Science. August 2 ２ , 2003 Max-Planck Inst. Masaru Matsuoka Matsuoka.masaru@nasda.go.jp NASDA(JAXA * from October 1,2003) Tsukuba Space Center. MAXI TMM Overview. * Japan Aerospace Exploration Agency (=ISAS+NASDA+NAL). 358 mm. Monitor of All-sky X-ray Image (MAXI).

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MAXI Status and ISS Science

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  1. MAXI Status and ISS Science August 2２, 2003 Max-Planck Inst. Masaru Matsuoka Matsuoka.masaru@nasda.go.jp NASDA(JAXA* from October 1,2003) Tsukuba Space Center MAXI TMM Overview * Japan Aerospace Exploration Agency (=ISAS+NASDA+NAL)

  2. 358 mm Monitor of All-sky X-ray Image (MAXI) MAXI GSC GSC SSC - 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)

  3. Now MAXI is in a final phase for FM. GSC: 2-30 keV SSC: 0.5-10 keV Weight: 490 kg MAXI Overview and Scanning Process

  4. MAXI Sensitivity Sensitivity (mCrabs) SSC GSC Systematic error level Dwell Time (seconds)

  5. Appendix A MAXISensitivity MAXI will monitor extra-galactic objects as well as Galactic sources above 1 m Crab. One Orbit (30 sources) O n e D a y ( 1 0 0 s o u r c e s ) O n e W e e k ( 1 0 0 0 s o u r c e s )

  6. X-ray Nova Light Curves and MAXI Detectability X-ray spectra are detectable every day Flux (Crab unit) One Crab = 2.4x10-9 erg sec-1 cm-2 Detectable in one day One m Crab Detectable in one week Time (days after outburst) Tanaka & Shibazaki, Annu. Rev.Astron. Astrophys. 34 (1996), 607

  7. SIMULATION of GSC observations ISS one orbit(90 min)2 months ~ 1000 sources incld. AGN ~30 Galactic sources

  8. 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) Fluctuation detection limit: a few % @ 1.5 deg.2for two years.

  9. 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

  10. Long-term X-ray Intensity Variations in Cyg X-2 Power Density Spectrum 1990 era X-ray Light Curves 1980 era 1970 era 1960 era Paul et al. Ap.J. 528 (2000), 410

  11. Galactic OVII & VIII Map with SSC MAXI SSC expected counts: 80- 310 counts in 1.5°x1.5° for 2 yr operation. Obs.eff.=0.7 Galactic Soft X-ray Spectra correspond’g to each Sky Region. Markevitch et al. 2003 ApJ. ROSAT all-sky map of CXB Snowden et al. 1997 ApJ.

  12. AGN Topics • Multiwavelength Simultenous Obs. of ~ 100? AGN’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

  13. 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 g-ray： acceleration up to 1012eV Takahashi et al. 2000, ApJL 542, L105 Successful SSC Model Mrk 421 TeV g Mrk 421 Inverse Compton synchrotron RXTE (8-15keV) ASCA(0.5-7keV) SAX EUVE optical X-ray GeV-g radio TeV-g 1 day

  14. R-band and X-ray correlation of N3516 Smoothed R-band (advanced) sampling inteval ~ 4.3 - 17 d Maoz et al. 2002, AJ 124, 1988

  15. AGN mass estimation from X-ray variability Hayashida et al 1998 ApJ 500 AGN Cyg X-1

  16. AGN mass estimation in comprison with Cyg X-1 (Cyg X-1) Hayashida et al 1998 ApJ 500

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

  18. 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.

  19. Thank you for your attention.

  20. Appendix B ASCA long-look of Blazars ASCA Light Curve Power Spectra 1 day Mrk421 Mrk501 1 day PKS2155-304 - Every day flares : tvar ~ 105[s] • Steep PSD spectra ( t < tvar) R ~ ctvard~ 1016 [cm] Kataoka et al. ApJ 2001 Tanihata et al. ApJ 2001

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