Download ! • Supermassive Black Holes (SMBH) at Work:  Effects of

Supermassive Black Holes (SMBH) at Work: Effects of
SMBH Outbursts on Clusters, Groups and Galaxies
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Bill Forman/Christine Jones/Eugene Churazov - SAO/CfA
Family of dark matter halos + hot gas
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Galaxies, groups, clusters
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Outburst up close
M87
Classic shock
Buoyant bubbles
Collaborators: Scott Randall,
Ralph Kraft, Paul Nulsen, Larry
David, Jan Vrtilek, Simona
Giacintucci, Marie Machacek, Ming
Sun, Maxim Markevitch, Alexey
Vikhlinin
Early type galaxies with SMBH
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Feedback present in X-ray luminous systems
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Driver of galaxy evolution
Hot X-ray coronae - mechanism to capture
SMBH energy
Setting the stage - Gas Rich Systems
Family of increasing mass, temperature, and luminosity
• Galaxy family
discovered with
Einstein (Forman
+79, +85)
• Mini cooling flows
described by
Thomas et al.
(1986)
E/S0 Galaxies
Lx
Gas Temp
M
10
Groups
10
Clusters
10
0.5-1.0 keV
1-3 keV
2-15 keV
0.02
1
5
• Compared to groups/clusters, galaxy physical processes are identical
• Optically Luminous E/S0 Galaxies have as much gas as spirals - BUT kT ~ 1keV
X-ray and Radio View of M87
• Multiple - at least three - AGN outbursts
• Two X-ray “arms” - produced/uplifted by
buoyant radio bubbles
• Eastern arm - classic buoyant bubble with
torus i.e., “smoke ring” (Churazov et al 2001)
– XMM-Newton shows cool arms of uplifted gas
(Belsole et al 2001; Molendi 2002)
Forman+05,+07
Million+10, Werner+10
Radio 90Mhz
Owen et al. 2001
Old bubbles no apparent
spectral aging
- still powered
M87
by AGN?
Fate of Bubble Energy
Rising bubble loses energy to
surrounding gas
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Generates gas motions in wake
Kinetic energy (eventually)
converted to thermal energy (via
turbulence)
non-relativistic
Bubble energy
remaining
vs. radius
ΔEgas = −ΔEBubble
relativistic
1−1 / γ
&
#
, P)
γ
!
= −Δ
PV = E0 $1 − ** ''
γ −1
$% + P0 (
!"
Classical Shock in M87
2
∫ P dl
<--Same Scales -->
SHOCK
Chandra (0.5-1.0 keV)
Chandra (3.5-7.5 keV)
23 kpc (75 lyr)
• Black hole = 6.6x109 solar masses (Gebhardt+11)
• SMBH drives jets and shocks
• Inflates “bubbles” of relativistic plasma
• Heats surrounding gas
• Model to derive detailed shock properties
Stars are just “bystanders”
Optical
Piston drives shocks
Shock Model - the data
Hard (3.5-7.5 keV) pressure
soft (1.2-2.5 keV) density profiles
Projected
Deprojected
Gas Pressure (3.5-7.5 keV)
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Textbook Example of Shocks
Consistent density and temperature jumps
Rankine-Hugoniot Shock Jump Conditions
γ + 1) M 2
(
ρ 2 / ρ1 =
(γ + 1) + (γ −1)( M 2 −1)
ρ 2 / ρ1 = 1.34
€
(γ + 1) + 2γ ( M
[
T /T =
2
1
€
2
−1)
][(γ + 1) + (γ −1)( M
(γ + 1)
2
2
−1)
]
M2
T2/T1= 1.18
yield same Mach number:
(MT=1.24 Μρ=1.18)
M=1.2
M87 Outburst Energy Partition
Detect shock (X-ray) and driving piston (radio)
Classical (textbook) shock M=1.2 (temperature and density independently)
Outburst constrained by:
Gas Pressure (3.5-7.5 keV)
Size of driving piston (radius of cocoon)
Measured T2/T1, ρ2 /ρ1 (p2/p1)
Outburst Model
Age ~ 12 Myr
Energy ~ 5x1057 erg
Bubble 50%
Shocked gas 25% (25% carried away by weak wave)
Outburst duration ~ 2 Myr
Outburst energy "balances" cooling (few 1043 erg/sec)
AGN outbursts - key to feedback in galaxy evolution, growth of
SMBH
Feedback from Supermassive Black Holes
key component in galaxy formation
SN feedback+photoionization
Dark halos
(const M/L)
galaxies
• Feedback - mass closely tied to mass of
surrounding stars - MSMBH ≈ 10-3Mbulge
• SMBH key to regulating star formation in
evolutionary models at high mass end
AGN feedback
e.g. Croton+06, White & Frenk
91, Cole+92 Benson+‘03
Best+06, Teyssier+11,
Massive SMBH, with enough fuel can disrupt galaxy atmospheres e.g., Fornax A = NGC1316
LX/LK vs. LK
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NGC1316 = Fornax A
NGC4291
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Fomalont/NRAO
NGC4342
350 kpc
•Outskirts of Fornax cluster (>1.4 Mpc from
Scatter in LX-opt mag relation
is partly due to gas removal
and partly due to environment
(galaxies in the centers of
“groups”)
NGC1399)
•Lnuc~2x1042 erg/s
•Likely merger driven outburst (e.g., Mackie/
Fabbiano98)
•Massive SMBH is willing and able to disrupt
atmosphere given sufficient fuel; outburst
power ~ 5x1058 ergs (Lanz+10)
•Such outbursts at early epochs could
disrupt star formation
Massive Black Holes - two
outliers
BOGDÁN
ET AL.
4
9
10
MBH, Msun
NGC4291
NGC4342
8
10
7
n
o
7
a
l
e
r
n
10
d
n
a
s
i
d
ea
6
10
9
10
M
The 0.5 − 2 keV band X-ray image of N
a diffuse hot gas component associated w
which exhibits a significantly broader di
the stellar light
1). To compute
•NGC4342
and (Fig.
NGC4291
mass profile of NGC4342 we assume tha
host
dark matter
halos
in hydrostatic
equlibrium
(Mathews 1978
1985; Humphrey et al. 2006) and use the
•measured using X-ray gas
tion:
!
(hydrostatic equil)
kTgas (r)r ∂ ln ne
+
Mtot (< r) = −
Gµmp
∂ ln r
n
o
i
s
r
pe
• Black holes are too
where
Tgas for
and their
ne are bulges
radial profiles
massive
NGC4342
NGC4291
10
10
11
Mbulge, Msun
10
12
10
Fig. 3.— Black hole mass as
8 a function of bulge mass. Thick
NGC4342
~ 4.6
Mbulge
⊙ relation from Häring & Rix
solid
line shows the
mean×M10
−
M
•
(2004), whereas the thin dashed line represent the intrinsic scatter
of NGC4291
the relation. Both
NGC4342
~ 9.6
× 108 and
M⊙NGC4291 are highly significant
outliers from the trend.
(Cretton & van den Bosch 1999; Haring & Rix 2004;
black
hole &masses
are2011)
7.7 × 106 M⊙ and 7.4 × 107 M⊙
Schultze
Gebhardt
in NGC4342 and NGC4291, respectively. Thus, the ob- an
extreme
outlier
(5.1σ
outlier)
served
values are
factors
of ≈60
and ≈13
times
larger
•NGC4342
than the predicted ones. From the intrinsic scatter of
is less
(3.4σ outlier)
•NGC4291
the
relation (0.30
dex) extreme
and the uncertainty
of the black
hole mass measurements (0.18 dex and 0.12 dex), we con-
temperature and density, respectively.
projected
use thefor
techniqu
•MBHprofiles
/Mbulgewe=0.069
Churazov et al. (2003). Namely, we mod
NGC4342
and
0.019 of spec
spectra
as the linear
combination
shells plus the contribution of the outer la
for NGC4391
that emissivity
in the outer shell declines
with radius at all energies. The matrix
•60x and
13xshells
larger
the projection
of the
into annuli
the deprojected
spectra are calculated b
than expected
inverted matrix to the observed spectra.
Due the head-tail distribution of the h
ting gas (Fig. 1 right panel; Bogdán e
assumption of hydrostatic equilibrium is
radii larger than ∼5 kpc. To account f
NGC4342 and NGC4291 - star formation disrupted
at early times - see Akos Bogdan poster
Extra energetic SMBH
terminates star formation at
early times (e.g. Fornax A like outburst)
NGC4342
(Bogdan et al. 2012a, b)
•Evolutionary scenario for
NGC4342 and NGC4291
Star formation suppressed:
black hole grew faster than
stars
Recall early SMBH growth (see
REFERENCE??)
eRosita will inventory
massive halos
SZ Detections of hot gaseous galaxy coronae
!
– already see 25% of
baryons in local Universe in
SZ (Planck XI)
!
Planck XI
– Detect lower mass early
type galaxies
– Detect onset of winds
– decrease in SZ signal
– Detect hot halos of spirals!! see Andersen+11;Bogdan+13a,13b
(NGC1961, NGC6751)
Conclusions
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M87 - bubbles & shocks
X-ray
(soft
&
hard)
• Cavities (and shocks) - BEST way
to measure black hole outburst
history
– Measure energy, age, duration
– SMBH governs correlation with
bulge/halo
– SMBH can disrupt star
formation at early times (e .g.,
NGC4342 - see Bogdan poster)
– Can break “tight” correlation
of MSMBH with Mbulge
NGC4342
SMART-X (1” 30 x Chandra): Growth of galaxy groups
and 109 M☉ black holes from z = 6 to the present
Sloan quasar at z=6
“nursing home” at z=0
M87, Chandra, 1″ pixels
(DM simulation by Springel et al.)
data and folded model
XMIS, z = 0, 300 ksec
10−4
Halo
LX = 5 1043 erg/s
T = 2 keV
r = 45 kpc = 8
0.1
normalized counts s−1 keV−1
10−3
QSO
Lx = 1045 erg/s
Jet + gas
T = 1.2 keV
Gas
T = 1.4 keV
10−3
10−6
10−5
normalized counts s−1 keV−1
0.01
1
APSI, z = 6, 300 ksec
0.01
0.1
data and folded model
0.2
0.5
1
Energy (keV)
2
5
10
✓ Sensitivity + angular resolution — detect
alexey 18−Oct−2011 17:15
and resolve quasar host halos and galaxy
groups at z=6
0.5
1
2
5
Energy (keV)
✓ High-res spectroscopy on 1″ scales —
feedback and physics in clusters,
galaxies, SNRs
alexey 18−Oct−2011 18:03
15
Finis