1. K. Makishima (University of Tokyo / RIKEN) Construct a unified view of BHs under high accretion rates ・ Some BHBs, including micro-quasars in particular [Kubota, Kobayashi, Yamaoka, Inoue,..] ・ ULXs (Ultra-Luminous X-ray Souces) [Sugiho] ・ The intermediate-mass BH in M82 [Matsumoto] ・ Narrow Line type 1 Seyfert Galaxies [Murakami] Four States of Accreting Black Holes: from Galactic BHs to AGNs → Improved classification of spectral states.

2. What will happen when M-dot approaches the critical value? Grav. enegy release = Radiation + Outflow + Advection (Keplerian kinetic + radial kinetic + internal energy) 1 0.5 0 0.5 0 Standard Outflow → Astro-E2 XRS; Advection → Astro-E2 HXD 1 0.5-α α 0.5 0 Outflow 1 0.5-α 1 0 0.5-α 2 ＋ α 3 ＋ α 4 Advection

3. Accreting Black Holes 10 -2 10 -1 10 0 BHBBHB ULX? AGN 10 0 10 2 10 4 10 6 10 810 M82 IMBH? LLAGN L/LEL/LE NLSy1 M/M◎M/M◎ Standard disk Slim Disk ADAF Kubota + others Sugiho Matsumoto Murakami 1.A hidden parameter -- the BH spin 2.Possible violation of the mass scaling; ionization, m e c 2

4. Medium-size black holes actually do exist, according to the latest findings from NASA's Hubble Space Telescope, but scientists had to look in some unexpected places to find them. The previously undiscovered black holes provide an important link that sheds light on the way in which black holes grow. Hubble Discovers Black Holes in Unexpected Places Even more odd, these new black holes were found in the cores of glittering, "beehive" swarms of stars called globular star clusters, which orbit our Milky Way and other galaxies. The black hole in globular cluster M15 [left] is 4,000 times more massive than our Sun. G1 [right], a much larger globular cluster, harbors a heftier black hole, about 20,000 times more massive than our Sun.

5. Deconvolved ASCA GIS spectra Two ULXs in IC342 : Kubota et al. ApJL 547, L119 (2001) MCD to PL PL to MCD ULXs with MCD-type and PL-type spectra (Mizuno 2000; etc.)  The two types are nearly equally abundant [Sugiho]  They are likely to be the same population of objects ULXs ; their Two Spectral Types Archival XMM-Newton data (analyzed by H. Takahashi) → consistent with the ASCA 2000 results

6. 1.The MCD-type and PL-type ULXs have been assigned to the soft (high) state and hard (low) state of BHBs, respectively (Makishima et al. 2000; Kubota et al. 2001). 2.In Galactic/Magellanic BHBs, the hard (low) vs. soft (high) state transition occurs at ~0.03 L Ed. 3.Then, the average ULX luminosity would be ~0.03 L Ed → the required mass would be several thousands M ◎ ！ Are ULXs radiating at ~ L Ed ? Need to re-consider state assignments of ULXs → investigate Galactic/Magellanic BHBs

7. Four Spectral States of BHBs 0.1 0.01 1 L/L Ed Schwarzschild Extreme Kerr 110 100 Energy (keV) Miyamoto et al. ApJ 383, 784 (1991) ← GX339-4 Watarai et al. PASJ 52, 133 (2000), ← theory Kubota et al. ApJ 560, L147 (2001) ← GRO J1655-40 Kobayashi et al. PASJ, submitted (2002) Kubota et al., in preparation (2002) ← XTE J1550-564 Low (hard) regime broad Fe- K edge reflection thermal cutoff opt-thick disk index~2.3 opt-thick disk thermally Comptonized disk emission Slim-Disk (Opt-thick ADAF) regime Anomalous (very high) regime Standard (high, soft) regime MCD-ULX? PL-ULX?

8. “Anomalous state” interpretation of PL-type ULX Energy (keV) 1 2 5 10 ASCA spectrum of IC 342 Source 1 in 2000 PL fit below 4 keV Γ= 1.54 ±0.12 An MCD with T in =1.1 keV, Comptonized by a cloud of T e =20 keV and τ 〜３ The PL-type ULXs may be in an anomalous regime; L 〜 L Ed with strong disk Comptonization (Kubota, Done & Makishima 2002, MNRAS, in press)

9. 0.2 0.5 1 2 T in (keV) 100 10 1 0.1 0.01 Disk bolometric luminosity (10 38 erg/s) H-R Diagram of accreting BHs ( Makishima et al. 2000) XTE J1550-564 with RXTE Kubota et al. (2002) IC342 Source 1 with ASCA Standard regime Anomalous regime Slim-disk regime MCD state in 1993 Slim-disk prediction (Watarai et al. 2001) PL state in 2000 analyzed in terms of disk Comptonization New state assignments  MCD-type ULX →slim disk [Watarai et al. 2001; Mizuno et al. 2001]  PL-type ULX → anomalous (Comptonized) regime [Kubota, Done & Makishima 2002] Both are radiating at ~ L Ed 30 Msun 100 Msun

10.  An intermediate-mass ( 〜 10 3- 4 M ◎ ) BH? [Matsumoto]  0.5-10 keV (ASCA): a PL spectrum with Γ=1.7 〜 2.6, and L x ( 2-10 keV ) = (1.9 〜 5.2) × 10 40 erg/s (Matsumoto & Tsuru 1999).  2-20 keV (Ginga): a thermal Bremsstrahlung with kT ~ 10 keV, with L x ( 2-10 keV ) = 4.4 × 10 40 erg/s (Tsuru 1992). The M82 IMBH The thermal Compton interpretation may again hold.

11. NLSy1s NLSy1s may be in the anomalous state → [Murakami] But we must examine the time variability [Negoro] 1 10 100 Energy (keV) Standard state Quiet disk Highly variable (Miyamoto et al. 1991); Kitamoto, this WS Variable, Γ 〜 2.3 Anomalous state 0.1 1 10 NLSy1 with 10 6 Msun

12. We suggest that the accreting BHs exhibit four characteristic spectral states; [i] low (hard) [ii] high (soft, standard) [iii] anomalous (very high, Comptonized) [iv] slim-disk (apparently standard) BHBs, ULXs, the M82 IMBH, and NLSy1s may be consistentky understood in this unified scheme. Summary