Credit goes to: M. Dadina, G. Ponti, F. Tombesi, M.Giustini, G. Palumbo INAF Univ. Bologna G. Matt,

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Outflows and winds in AGNs the case for Simbol-X
Massimo Cappi INAF-IASF, Sezione di Bologna
Outline

• Framework
• Outflows/winds
• X-ray Observations latest results
• Blue-shifted abs. lines
• Current Interpretations
• Outflows/winds
• Critical Issues
• Significance, Identifications
• Importance
• Astrophysics, cosmology
• Future
• Simbol-X simulations

Kato et al. 2003
Credit goes to M. Dadina, G. Ponti, F. Tombesi,
M.Giustini, G. Palumbo (INAFUniv. Bologna) G.
Matt, S. Bianchi (Roma3)
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Framework (i/ii) Fast winds/outflows/ejecta in
AGNs
known/seen in AGNs since long ago
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Framework (ii/ii) Warm absorbersprobe highest-v
gas
50 of all Sey 1s exhibit WAs
ASCA
Fabian, et al. 94 Otani, 95, PhD Reynolds et
al. '97 Georges et al. '97
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X-ray Observations (i/iii) Blue-shifted
absorption lines/edges High-v
New and unexpected results from Chandra and
XMM-Newton observations
PG1211143 (z0.08) v0.1c
2 Energy (keV) 5 7
10
Pounds et al. 2003a,b
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X-ray Observations (ii/iii) Blue-shifted
absorption lines/edges High-v z
Massive outflowsalso (mostly?) at high redshift
2 high-z BAL QSOs
Chartas et al. 2002, Hasinger, Schartel
Komossa 2002
APM 082795255 (z3.91) v0.2-0.4c
See also Wang et al. 05 (v0.8c in qso_at_z2.6)
N.B. Would have been undetected at z0...
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X-ray Observations (iii/iii) Blue-shifted
absorption lines/edges - Variability
WA variability on timescales 1000-10000s
Mrk 509 (long-look, 200ks)
Obs1
Obs2
Obs3
Cappi et al., in preparation Dadina et al. 05
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Interpretation (Three main) Wind dynamical models
i) ? Large R, low v ii) and iii) ? Low R and
large v
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Importance (i/ii) Feedback in the (co?)evolution
of galaxies
First unexpected revolution in extragal.
astrophysics not only most (all?) galaxies have
SMBHs in their centers, but these correlate with
bulge properties ?evidence for feedback
mechanism between SMBH(AGN) and its host galaxy?
Magorrian et al. '98 Tremaine '02 Gebhardt
'02...etc
Mbh ?4
(see e.g. King and Pounds '03, Crenshaw, Kraemer
George '03, ARAA)
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Importance (ii/ii) Reheating of groups and
clusters of galaxies
Second unexpected revolution in extragal.
astrophysics need preheating to recover L-T
relations cooling flows extra-heating ? Energy
feedback from AGNs/QSOs and groupsclusters?
Grav. scaling
With SN preheating
With AGN pre-heating
With QSO ejection/outflows
Lapi, Cavaliere Menci, 05
Perseus Cluster, Fabian et al. 05
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Critical Issues (i/ii) Observations

• Lines statistical significance? (transient
  features, number of trials in time and energy,
  etc)
• Identifications of edges/lines energies? (Kallman
  et al. 2005, Kaspi et al. for PG1211)
• Local contamination? (PDS456 at risk? McKernan
  et al. 04, 05)
• N.B Overall evidence is robust

Outflow v (km/s)
cz (km/s)
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As far as the local contamination is concerned
Credit Margherita Giustini
No relation with warm emitting gas and Nwltlt1e21
cm-2

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Critical Issues (ii/ii) Interpretation/Theory

• Fundamental to
• PHYSICS of accelerated and accreted flows
  (winds?, blobs?, etc.), i.e. understand how BHs
  accelerate earth-like quantities of gas to
  relativistic velocities
• COSMOLOGY i.e. estimate the mass outflow rate,
  thus the impact of AGN outflows on ISM and IGM
  enrichment and heating!

• Nw (cm-2)
• Location (R, DeltaR)
• Ionization state (?)
• Velocity
• Covering factor
• Frequency in AGNs

Elvis et al. 00, Creenshaw et al. 03, King et
al. 03, Chartas et al. 03, Yaqoob et al. 05,
Blustin et al. 05, Risaliti et al. 05,
Krongold et al. 07
Current estimates have order of magnitude
uncertainties, they go from dM/dt (?Lkin) few
to several times dMacc/dt (?Ledd) This is a
fundamental (open) issue
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Future (i/vii) In my opinion
The tip of the Iceberg?

• BECAUSE
• - Physical bias against highest ionization
  in/outflowing gas (detectable only with Fe)
• - Detection bias against transient features
• - Observational bias against highest-v
  blueshifted features (poor high-E
  sensitivitycut-off at 7 keV)
• WHILE
• X-ray absorption lines are naturally expected in
  models involving blobby/winds ejecta/outflows,
  such as those predicted by MHD simulations of
  accretion disks

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Future (ii/vii) Two main directions
1) Probe the HIGHEST VELOCITIES (v gt 0.3c), and
thus masses/kinetic energy, in outflowing
components (? require high-energy coverage)
2) Probe the outflow DYNAMICS ! i.e. measure
delta v, not only v! (? require high throughput)
1) 2) ? require highest possible throughput
between 2-20 keV
Daniel Proga, 2005 (failed disk winds)
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Future (iii/vii) Simbol-X simulation (SDDCdTe)
Simulations of narrow emission and absorption
lines
Simulations
Model PL 2 emission lines 4 abs. lines
Model with narrow emission and absorption lines
PL (?1.9, F(2-10)10-11erg/cm2s, Exp.50 ks) 2
FeK emission lines (E15 keV, E26.4 keV, s1
s250 eV, EW1EW2100eV) 4 FeK absorption lines
(E1,2,3,47, 9, 12, 15 keV, s1,2,3,4lt50 eV,
EW1,2,3,4-100eV)
Edges and absorption lines at E7.1-9.0 keV
(rest-frame) vout 0.1-0.5c
? Eobserved 8-14 keV !!
Deceleration
Acceleration
?Eabslt100 eV ? Idea would be to follow the
evolution of blobs ejecta N.B Masses involved
can be greater than Mearth (1027g/ejecta)
gtgt10-11g in accelerators
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Future (v/vii) S-X simulations SDD
NGC1365 F(2-10)10-11cgs
CreditF. Tombesi (see Poster)
Simbol-X MPD simulation
FeKa XXV
FeKa XXVI
FeKß XXV
FeKß XXVI
XMM EPIC pn (real) spectrum Risaliti et al. 2005
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5
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Future (v/vii) S-X simulations SDD
S-X capability of detecting blueshifted
absorption lines
-25eV50 ks
-25eV100 ks
few sources
gt20 sources (Piccinotti sample)
-50eV50 ks
-50eV100 ks
CreditF. Tombesi (see Poster)
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Future (vi/vii) Simbol-X simulation SDD
Time-energy Map SX simulation - NGC1365 -
F(2-10)10-11cgs
S-X Simulation CreditF. Tombesi (see poster)
Acceleration 0.02c ? 0.2c
Deceleration 0.2c ? 0.02c
Highest throughput up to 15 keV for time-resolved
detections of abs. lines ? real-time, extreme
dynamics, outward accelerations!? (line ?v/?t)
....blobtest particle to probe launching regions
of winds/jets
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Future (vi/vii) Simbol-X simulation SDD
PDS 456 A bright nearby quasar with a huge and
complex warm absorber
Simulations
Edges and absorption lines at E7.1-9.0 keV
(rest-frame) vout 0.1-0.5c
? Eobserved 8-14 keV !!
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Summary
I briefly presented the current evidence for
blue-shifted absorption lines from highly ionized
Fe in AGNs (both Sey and QSOs) These indicate
existence of highly-ionized, high velocity,
massive outflows in AGNs, BUT STILL ORDER OF
MAGNITUDES UNCERTAINTIES on energy/momentum and
mass involved. This topic still requires
better measurements of intensity, energy and
frequency/recurrency but has a great potential
for the study of launching mechanisms/character
istics of outflows/jets (mechanical energy
emerging from BH), important not only for
(relativistic) physics but also for link with
cosmology

• Prospects for future progress are to
• Confirm/secure these findings with longer
  XMM/Chandra observations
• Probe highest-velocity gas with higher-energies
  (i.e Simbol-X)
• Probe dynamics with lower time-scales (i.e. S-X,
  and then XEUS-like mission)

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Thanks for your attention
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Framework (i/iii) The AGN paradigm and main open
issues
Open Issue

Jet
Characterise the geometry, particle content, and
velocity of the outflow/jet
Characterise the geometry and velocity of the
outflow/wind, and its impact on the host galaxy
and cluster
Open Issue
Characterise the geometry and mode of the
accretion flow
Hot corona
Open Issue
Credit A. Mueller
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Interpretation II (i/ii) Gravitational redshift
ii) In an outflowing nuclear wind/jet (e.g.
Reeves et al. 05)
i) In a rotating absorbing corona
(Ruszkowski Fabian, 00)
(Picture from Elvis 00)
N.B Origin in gravitational redshift require
Rltfew Rg
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Interpretation II (ii/ii) Inflowing
wind/blobs/clumps
iv) Aborted jet (Ghisellini, Haardt, Matt 03)
iii) Failed disk wind (Proga et al. 00)
Density
Optical depth
Temperature
? gt 1 out and inflow
N.B If Infalling blobs/clouds ? may represent
suitable test-particles to probe GR under strong
field
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Ejection/outflows Massive outflows (ii/iii)
PDS456
PG1211143
McKernan, Yaqoob Reynolds 2004
Cast doubts on the AGN origin of high-velocity
absorption gas...because consistent with local
WHIGM (N.B. PDS456 is along Gal. Plane)
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X-ray spectra of winds/outflows