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Comment on the observational aspects of M82X-1: intermediate-mass BH?

Comment on the observational aspects of M82X-1: intermediate-mass BH?. Hironori Matsumoto (Kyoto Univ.). First Discovery of M82 X-1. M 82 X-1. M82 X-1. +. +. galactic center. galactic center. ( Matsumoto et al. 2001). Chandra HRC. 30” x 30” (~570pc x 570pc).

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Comment on the observational aspects of M82X-1: intermediate-mass BH?

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  1. Comment on the observational aspects of M82X-1:intermediate-mass BH? Hironori Matsumoto (Kyoto Univ.)

  2. First Discovery of M82 X-1 M82 X-1 M82 X-1 + + galacticcenter galacticcenter (Matsumoto et al. 2001) Chandra HRC 30” x 30” (~570pc x 570pc) Oct. 28, 1999 Exp.=2788s Jan. 20, 2000 Exp.=17684s 170pc away from the galactic center

  3. ASCA Observation (Matsumoto & Tsuru 1999) • LX=4.5x1040~ 1.6x1041 erg/s (assuming isotropic radiation) • Δt=a few hours ~ a month The origin of the hard X-ray emission is M82 X-1.

  4. XMM & RXTE observation (Strohmayer & Mushotzky 2003) QPO (0.05 – 0.1 Hz) was discovered.

  5. BH mass • Supermassive BH? … No • Off-center position • Rapid time variability M<2x104 Msun • Stellar mass BH? … No • Extremely bright (assuming isotropic radiation) M>1000 Msun Strong candidate for an intermediate-mass BH

  6. Origin of M82 X-1 • At the center of the molecular super bubble • Ek ~ 1055 erg • R/v ~ 106 yrs • (Matsushita et al. 2000) M82X-1 Violent starburst activity?

  7. Runaway merging Maybe inside a globular cluster (MGG11) Runaway merging? (Ebisuzaki, this work shop and Ebisuzaki et al. 2001) (Portegies Zwart et al. 2004)

  8. Summary M82X-1 is a strong candidate for an IMBH. • Another possibility: • a stellar-mass BH with non-isotropic emission The key to clarify is the X-ray spectrum. No one has ever obtained the pure spectrum of M82X-1 . (too bright, too crowded region)

  9. X-ray H-R diagram M82X-1 vs Ultra-luminous X-ray Sources (ULX) • Lbol(M82 X-1) > Lbol (ULX) • kTin(M82 X-1) > kTin(ULX) • No correlation between Lbol and kTin

  10. Suzaku is alive! Suzaku Japanese 5th X-ray Satellite 7/10@Kagoshima XRS: Calorimeter XIS: CCDx4 HXD: hard X-ray

  11. XIS: X-ray CCD Chandra BI CCD SNR E0102-72 FI CCD XMM Good Energy Resolution!

  12. XIS: X-ray CCD • Large effective area at high energy band. • Low back ground

  13. HXD: Hard X-ray Detector Wide energy band and low background

  14. Advantage of Suzaku • Good energy resolution • (especially for diffuse emission) • Wide dynamic range • (0.3 keV – 200 keV) • Low background Call for Guest Observing Proposals will be announced in mid-October!

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