Transcript Intermediate mass Black Holes, and Relation with AGN

Four States of Accreting Black Holes:
from Galactic BHs to AGNs
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]
→ Improved classification of spectral states.
What will happen when M-dot
approaches the critical value?
Standard Outflow
Grav. enegy release
= Radiation
+ Outflow
+ Advection
(Keplerian kinetic
+ radial kinetic
+ internal energy)
Advection
1
1
1
0.5
0.5-α
0.5-α1
0
α
0
0.5
0.5
0.5-α2
0
0
＋α3
0
0
＋α4
Outflow → Astro-E2 XRS; Advection → Astro-E2 HXD
Accreting Black Holes
Kubota + others
Murakami
L/LE
100
10-1
ULX?
B
H
B
M82
IMBH?
NLSy1
Matsumoto
Sugiho
10-2
Slim
Disk
AGN
Standard
disk
LLAGN
ADAF
100
102
104
106
108
1010
M/M◎
1. A hidden parameter -- the BH spin
2. Possible violation of the mass scaling; ionization, mec2
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.
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
MCD to PL
Two ULXs in IC342 : Kubota et
al. ApJL 547, L119 (2001)
Archival XMM-Newton data
(analyzed by H. Takahashi)
→ consistent with the ASCA
2000 results
PL to MCD
Are ULXs radiating at ~ LEd ?
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◎！
Need to re-consider state assignments of ULXs
→ investigate Galactic/Magellanic BHBs
Extreme Kerr
Schwarzschild
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
L/LEd
MCD-ULX? opt-thick
disk
1
opt-thick disk
Slim-Disk
(Opt-thick
thermally Comptonized
ADAF)
regimedisk emission
Anomalous
PL-ULX?
Low
(hard)
regime
0.1
0.01
1
broad FeK edge (very high)
regime
reflection
index~2.3
Standard
(high, soft)
regime
thermal
cutoff
10 Energy (keV) 100
“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)
Disk bolometric luminosity (10 38 erg/s)
H-R Diagram of accreting BHs (Makishima et al. 2000)
IC342 Source 1 with ASCA
100
10
Anomalous regime
1
0.1
XTE J1550-564 with RXTE
Kubota et al. (2002)
New state assignments
MCD-type ULX →slim disk [Watarai et al. 2001;
0.01Mizuno et al. 2001]
PL-type ULX → anomalous (Comptonized) regime
0.2
0.5
1
2
[Kubota,
Done & Makishima
2002]
Both are radiating at ~ LEdTin (keV)
The M82 IMBH
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 thermal Compton interpretation may again hold.
NLSy1s
Quiet disk
Standard state
Highly variable
(Miyamoto et al. 1991);
Kitamoto, this WS
Anomalous
state
Variable,
Γ〜2.3
Energy (keV)
1
0.1
10
1
100
10
NLSy1 with 106 Msun
NLSy1s may be in the anomalous state → [Murakami]
But we must examine the time variability [Negoro]
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.