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.

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

0

Standard

Outflow → Astro-E2 XRS; Advection → Astro-E2 HXD

1

0.5-αα

0.500

Outflow

1

0.5-α1

0

0.5-α2

＋ α3

＋ α4

Advection

Accreting Black Holes

10-2

10-1

100

BHB

ULX?

AGN

100 102 104 106 108 1010

M82IMBH?

LLAGN

L/LE

NLSy1

M/M◎

Standard disk

Slim Disk

ADAF

Kubota + others

SugihoMatsumoto

Murakami

1. A hidden parameter -- the BH spin2. Possible violation of the mass scaling; ionization, mec2

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.

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

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 LEd.

3. Then, the average ULX luminosity would be ~0.03 LEd

→ the required mass would be several thousands M◎！

Are ULXs radiating at ~ LEd ?

Need to re-consider state assignments of ULXs

→ investigate Galactic/Magellanic BHBs

Four Spectral States of BHBs

0.1

0.01

1

L/LEd

Schw

arzs

child

Ext

rem

e K

err

1 10 100Energy (keV)

Miyamoto et al. ApJ 383, 784 (1991) ← GX339-4Watarai et al. PASJ 52, 133 (2000), ← theoryKubota et al. ApJ 560, L147 (2001) ← GRO J1655-40Kobayashi 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?

“Anomalous state” interpretation of PL-type ULX

Energy (keV) 1 2 5 10 1 2 5 10

ASCA spectrum of IC 342 Source 1 in 2000

PL fit below 4 keVΓ= 1.54 ±0.12

An MCD with Ti

n =1.1 keV, Comptonized by a cloud of Te=20 keV and τ 〜３

The PL-type ULXs may be in an anomalous regime;L 〜 LEd with strong disk Comptonization

(Kubota, Done & Makishima 2002, MNRAS, in press)

0.2 0.5 1 2

Tin (keV)

100

10

1

0.1

0.01

Dis

k bo

lom

etri

c lu

min

osit

y (1

0 38

erg

/s)

H-R Diagram of accreting BHs (Makishima et al. 2000)

XTE J1550-564 with RXTEKubota et al. (2002)

IC342 Source 1 with ASCA

Standard regime

Anomalous regimeSlim-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 ~ LEd

30 Msu

n

100 Msun

An intermediate-mass ( 〜 103- 4 M◎) BH? [Matsumoto]

0.5-10 keV (ASCA): a PL spectrum with Γ=1.7 〜 2.6, and Lx (2-10 keV) = (1.9 〜 5.2)×1040 erg/s (Matsumoto & Tsuru 1999).

2-20 keV (Ginga): a thermal Bremsstrahlung with kT ~ 10 keV, with Lx (2-10 keV) = 4.4 ×1040 erg/s (Tsuru 1992).

The M82 IMBH

The thermal Compton interpretation may again hold.

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 106 Msun

• 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