K. Makishima (University of Tokyo / RIKEN)

1. Four States of Accreting Black Holes:from Galactic BHs to AGNs 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] K. Makishima (University of Tokyo / RIKEN) → Improved classification of spectral states.

2. Outflow Advection Standard 1 0.5 0 0.5 0 0 1 0.5-α α 0.5 0 0 1 0.5-α1 0 0.5-α2 ＋α3 ＋α4 What will happen when M-dot approaches the critical value? Grav. enegy release = Radiation + Outflow + Advection (Keplerian kinetic + radial kinetic + internal energy) Outflow → Astro-E2 XRS; Advection → Astro-E2 HXD

3. Kubota + others Murakami Matsumoto Sugiho 108 1010 106 100 102 104 Accreting Black Holes L/LE Slim Disk ULX? B H B NLSy1 AGN 100 M82 IMBH? 10-1 Standard disk LLAGN 10-2 ADAF M/M◎ A hidden parameter -- the BH spin Possible violation of the mass scaling; ionization, mec2

4. Hubble Discovers Black Holes in Unexpected Places 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. 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. MCD to PL PL to MCD ULXs ; their Two Spectral Types 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 Deconvolved ASCA GIS spectra Two ULXs in IC342 : Kubota et al. ApJL547, L119 (2001) Archival XMM-Newton data (analyzed by H. Takahashi) → consistent with the ASCA 2000 results

6. Are ULXs radiating at ~ LEd ? • 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). • In Galactic/Magellanic BHBs, the hard (low) vs.soft (high)state transition occurs at ~0.03 LEd. • Then, the average ULX luminosity would be ~0.03 LEd → the required mass would be several thousands M◎！ Need to re-consider state assignments of ULXs → investigate Galactic/Magellanic BHBs

7. L/LEd Slim-Disk (Opt-thick ADAF) regime opt-thick disk 1 thermally Comptonized disk emission Anomalous (very high) regime opt-thick disk MCD-ULX? Low (hard) regime 0.1 broad Fe-K edge PL-ULX? reflection Standard (high, soft) regime index~2.3 0.01 thermal cutoff Four Spectral States of BHBs 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 Schwarzschild Extreme Kerr 100 1 10 Energy (keV)

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

9. 100 PL state in 2000 analyzed in terms of disk Comptonization 10 100 Msun 30 Msun 1 0.1 0.01 Standard regime Slim-disk prediction (Watarai et al. 2001) H-R Diagram of accreting BHs (Makishima et al. 2000) IC342 Source 1 with ASCA MCD state in 1993 Anomalous regime Slim-disk regime Disk bolometric luminosity (10 38 erg/s) XTE J1550-564 with RXTE Kubota et al. (2002) • 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 ~ LEd 0.2 0.5 1 2 Tin (keV)

10. The M82 IMBH • An intermediate-mass (〜103- 4M◎) BH?[Matsumoto] • 0.5-10 keV(ASCA): a PL spectrum withΓ=1.7〜2.6, andLx (2-10 keV) = (1.9〜5.2)×1040 erg/s (Matsumoto & Tsuru 1999). • 2-20 keV(Ginga): a thermal Bremsstrahlung with kT ~ 10 keV, withLx (2-10 keV) = 4.4 ×1040 erg/s (Tsuru 1992). The thermal Compton interpretation may again hold.

11. Highly variable (Miyamoto et al. 1991); Kitamoto, this WS Quiet disk Variable,Γ〜2.3 0.1 10 1 NLSy1 with 106 Msun 100 10 1 NLSy1s Anomalous state Standard state Energy (keV) NLSy1s may be in the anomalous state → [Murakami] But we must examine the time variability [Negoro]

12. Summary • 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.