Science Operations & Data Systems Division Research & Scientific Support Department Page 1 XMM-Newton XMM-Newton “Did I say radio quiet?” Radio-loudness in radio-quiet Seyferts [and a note on X-ray core spectra in low- power radio RGs] Matteo Guainazzi European Space Astronomy Center of ESA Villafranca del Castillo (Spain)
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Matteo Guainazzi European Space Astronomy Center of ESA Villafranca del Castillo (Spain)
Matteo Guainazzi European Space Astronomy Center of ESA Villafranca del Castillo (Spain) . “Did I say radio quiet?” Radio-loudness in radio-quiet Seyferts [and a note on X-ray core spectra in low-power radio RGs]. AGN SED. (Elvis et al. 1994) . Gallery of radio emission in Seyferts. - PowerPoint PPT Presentation
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Science Operations & Data Systems Division Research & Scientific Support Department
Page 1
XMM-NewtonXMM-Newton
“Did I say radio quiet?”Radio-loudness in radio-quiet
Seyferts [and a note on X-ray core spectra in low-power
radio RGs]
Matteo GuainazziEuropean Space Astronomy Center of ESA
Villafranca del Castillo (Spain)
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
AGN SEDAGN SED
(Elv
is e
t al.
1994
)
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
Gallery of radio emission in Gallery of radio emission in SeyfertsSeyferts
Unresolved Sub-pc scale
0.1 pc
NGC4395
pc-scale, sub-relativistic
Mkn231(V
LB
A, A
nder
son
et a
l. 20
04)
(VL
BI,
Wro
bel &
Ho
2006
)
(VL
BA
, Ulv
esta
d et
al.
1999
)
kpc-scale (44% of 43 CfA galaxies – AGN driven)
(VL
A, G
allim
ore
et a
l. 20
06)
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
OutlineOutline
Radio emission in Seyfert galaxies: core and jet Radio emission in Seyfert galaxies: core and jet emissionemission
Jet-ISM interaction and the ionization Jet-ISM interaction and the ionization mechanism of the [E]NLRmechanism of the [E]NLR
Lessons and questions on Radio Galaxies core Lessons and questions on Radio Galaxies core X-ray spectra from Seyfert Galaxies X-ray X-ray spectra from Seyfert Galaxies X-ray spectraspectra
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
OutlineOutline
Radio emission in Seyfert galaxies: core and Radio emission in Seyfert galaxies: core and jet emissionjet emission
Jet-ISM interaction and the ionization Jet-ISM interaction and the ionization mechanism of the [E]NLRmechanism of the [E]NLR
Lessons and questions on RG core X-ray Lessons and questions on RG core X-ray spectra from Seyfert Galaxies X-ray spectraspectra from Seyfert Galaxies X-ray spectra
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
Multiple scales in individual objectsMultiple scales in individual objects
1 kpc
1.5 kpc
7.5 kpc
Multiple kpc-components in Mkn 6
(Kharb et al. 2004)
From pc- to kpc-scale in Mkn 231
(Ulvestad et al. 1999)
NGC1068
Internal shock in a jet?
Free-free absorbed, variableIonized cocoon?
Resolved ∟ radio axisFree-free thermal emission from the inner side of the maser disk
YES: Strittmatter et al. (1980), Kellermann et al. (1989), Wadadekar & Kembhhavi (1999),
Ivezic et al. (2002), Panessa et al. (2007)
NO: White et al. (2000), Hewett et al. (2001), Cirasuolo et al. (2003)
Possible alternative R definitions:• Relative Lradioradio/LFIR (Rush et al. 1996, Thean et al. 2000)
• IRAS severely contaminated by the host galaxy
• Relative Lradioradio/LX (Terashima & Wilson 2003)
• Good for highly obscured and LLAGN
• Absolute radio power (Miller et al. 1990)
• Radio-loudness should be w.r.t. other λλ
Seyferts nuclei are not radio-quiet![60% have R>10, for:R≡Lν(6 cm)/ Lν(B)]
(Ho & Peng 2001)
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
Spectral indicesSpectral indices(Thean et al. 2001)
(Ulvestad & Ho et al. 2001)
Palomar Seyferts have a largefraction of flat spectra (α≥-0.7)
• No optically-thin synchrotron emission• Synchrotron self-absorption?• Free-free emission?• Free-free absorption?• Radiative inefficient accretion?• Link with Giga-Hertz Peaked Sources?
• Spectral turnover• Sub-relativistic jets
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
Radio-power dependenceRadio-power dependence
3 Low-luminosity AGN: α = -0.3-0.1
(Ulv
esta
d &
Ho
et a
l. 20
01)
(Doi et al. 2005)
• Pure ADAF models over-predicts the X-ray emission by ≥10 (Yi & Boughn 1998, Quataert et al. 2001)
• → Co-presence of an ADAF and a compact jet• Weaker sources have weaker jets → ADAF emission starts become visible at low radio L
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
Radio-loudness vs. accretion rateRadio-loudness vs. accretion rate(Panessa et al. 2007)
(Greene & Ho 2006)
State transition at Lbol/LEdd≈0.01:• Below this value: radiatively inefficient accretion flow + outflow• Above this value: optically-thick, geometrically-thin disk, radiation pressure dominated slim disk
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
Is there a X-ray/radio correlation?Is there a X-ray/radio correlation?
YES: Panessa et al. (2007)
NO (distance effect in flux-limited samples): Bianchi et al. (2008)
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
Fundamental plane of BH activityFundamental plane of BH activity
(Mer
loni
et a
l. 20
03, 2
006;
Fal
cke
et a
l. 20
04)
• Scale-invariant jets [Heinz & Sunyaev 2003]• Radio luminosity scales with BH mass and accretion rate, independently of the jet model• Scaling depends on α, and the electron distribution index → on accretion physics only
• X-ray emission from BH accretion at a few percent Eddington is consistent with radiative inefficient flow only
• In low accretion rate sources, jet power is proportional to accretion power
• Challenges? Seyferts and LL RGs seem to follow different planes [Wang et al. 2006; Panessa et al. 2007]
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
Jet/ISM interactionsJet/ISM interactions
IIIZw2
43 GHz(jet hotspots)
15 GHz(external shell)
(Bru
nthh
aler
et a
l. 20
05) NGC3079
[Earlier results: Wilson & Ulvestad 1982, Oosterloo et al. 2000)]
“Slower-when-brighter” behaviour(Saxton et al. 2005)
Interaction with clumpy ISM could “frustrate” the jet in Seyfert galaxiesAlternative: continuous emission of
“aborted jets” (Ghisellini et al. 2004)
(Mid
delb
erg
et a
l. 20
08)
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
OutlineOutline
Radio emission in Seyfert galaxies: core and Radio emission in Seyfert galaxies: core and jet emissionjet emission
Jet-ISM interaction and the ionization Jet-ISM interaction and the ionization mechanism of the [E]NLRmechanism of the [E]NLR
Lessons and questions on RG core X-ray Lessons and questions on RG core X-ray spectra from Seyfert Galaxies X-ray spectraspectra from Seyfert Galaxies X-ray spectra
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
Radio/NLR interactionRadio/NLR interactionCorrelation between radio and optical power (de Bruyn & Wilson 1978, Wilson & Willis 1980, Heckman et al. 1981, Meurs & Wilson 1984, Whittle 1985, Wilson 1991, Whittle 1992)
(Ho
& P
eng
2001
)
Correlation between radio and line width (Wilson & Willis 1980, Whittle 1985, 1992)
(Ulv
esta
d &
Ho
2001
)
Jet vs. NLR power(Nagar et al. 2005)
In LLAGN the jet is the primaryoutput channel of accretionenergy
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
Do radio jets affect NLR …Do radio jets affect NLR …
(Capetti et al. 1998)
(Axon et al. 1998)
Morphology?
Kinematics?(Yes, but see Das et al. 2006
for a counter-example on NGC1068)
(Capetti et al. 1996)
Ionization? position of radio knot
Contours: radioGrayscale: O[III]
Contours: radioGrayscale: O[III]
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
Role of shock ionizationRole of shock ionization(ESO428-G14; Riffel et al. 2006)
[Fe II] [O III] 2cm
<80-90%
<70-80%
Chandra(NGC2110; Evans et al. 2006)
Contribution to ionization by
shocks
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
Shock ionizationShock ionization
Ionizing shock model:• Could explain extended soft X-ray emission in obscured AGN (Wilson & Raymond 1999)• Would require a jet dominated by thermal plasma [Bicknell 2002] where radio emission is just a tracer of the underlying flow• “ACIS measurements will be crucial to test it”
(Dop
ita 1
995;
Dop
ita &
Sut
herl
and
1995
)
(Wilson &
Raym
ond 1999)
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
Soft X-ray extended emission and NLRSoft X-ray extended emission and NLR
Circinus Galaxy(Smith & Wilson 2001)
NGC4151(Yang et al. 2001)
NGC1386(Bianchi et al. 2006)
NGC5643(Bianchi et al. 2006)
NGC3393(Bianchi et al. 2006)
600 pc 600 pc 500 pc 600 pc
500 pc700 pc
1000 pc
2000 pc
Images: O[III] – Contours: soft X-rays
NGC1068(Young et al. 2001)
NGC5347(Bianchi et al. 2006)
Mkn3(Sako et al. 2000)
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
High-resolution soft X-ray spectra are dominated by AGN photoionization
Contribution by thermal plasma negligible (Brinkman et al. 2002, Bianchi et al. 2006)
(Sambruna et al. 2001)
(Kinkhabwala et al. 2002; Gallimore et al. 2004)
(Sako et al. 2000)
(Guainazzi & Bianchi 2007)
Narrow (<10 eV) Radiative Recombination Continua in a sample of Seyfert 2 galaxies with the RGS
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
OutlineOutline
Radio emission in Seyfert galaxies: core and Radio emission in Seyfert galaxies: core and jet emissionjet emission
Jet-ISM interaction and the ionization Jet-ISM interaction and the ionization mechanism of the [E]NLRmechanism of the [E]NLR
Lessons and questions on RG core X-ray Lessons and questions on RG core X-ray spectra from Seyfert Galaxies X-ray spectraspectra from Seyfert Galaxies X-ray spectra
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
X-ray core emission of low-L RGsX-ray core emission of low-L RGs
FRI [Donato et al. 2004; Evans et al. 2006]
– Unobscured, Г=1.88±0.02– Correlation between X-ray, radio, optical → origin at the base of
the relativistically beamed radio jet
FRII [Evans et al. 2006]
– Obscured (NH>1023 cm-2), Г=1.76±0.02, Fe Kα line
– Torus-surrounded accretion disk emission– Soft excess → jet-related origin
Anticorrelation between Fe Kα EW and R in heterogeneous radio-loud samples [Reeves & Turner 2000, Grandi et al. 2007]
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
Seyfert X-ray emissionSeyfert X-ray emission
(Courtesy of I.George)
Seyfert 2s
Unobscured Seyfert 2s
Seyfert 1-1.5s
There is nothing like a “power-law” X-ray spectrum in Seyfert Galaxies
(Malizia et al. 1997)
Disk(how?)
Disk outflowTorus + disk
Torus + disk
Disk corona
(1021 cm-2)
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
Open questionsOpen questions
If we see the accretion disk in the X-ray spectra of RGs– Where are the relativistically smeared features?– Is there any Compton reflection?
– BeppoSAX: weak (Grandi et al. 2006)
– Where is the warm absorber?– Are warm absorber outflows and radio jets two different
manifestations of the same underlying medium?– Why there is no soft excess in FRI?– Which is the true nature of the soft excess in FRIIs?– Is the distribution of absorbing column densities consistent
between RGs and Seyferts?
(Evans et al. 2006)
RG Seyfert
(Tüller et al. 2008)
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
Soft excess in FRIIs: 3C344Soft excess in FRIIs: 3C344
pn3C445
26 Starburst(after Wu et al. 2002)
Maximum jet contribution in the
soft X-ray band
(Sambruna et al. 2007; Grandi et al. 2007)
Sy2s
(Guainazzi 2008)
• Soft X-ray emission lines in both the XMM-Newton EPIC and RGS shows that the soft X-ray emission is dominated by AGN-photoionized gas• This constraints the contribution of any jet-related non-thermal emission• These measurements are challenging, but possible. Similar example: 3C33 (Torresi et al., in prep.)
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
Specific Specific Chandra Chandra contributionscontributions
Spatial resolution required to resolve the nuclear emission
Spatially resolved low-resolution spectroscopy (coupled with high-throughput, serendipitous high-resolution spectroscopy with the XMM-Newton RGS) is key to understand the nature of the emission on 0.1-1 kpc scale → ionization mechanism of the [E]NLR
My pledge for the future:– Completeness! (see, e.g., Massaro’s talk)
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
ConclusionsConclusions
At least 50% of Seyfert galaxies are radio emitters on different scales (from sub-pc to kpc-scale)
Core radio emission probably due to a combonation of jet and low-efficiency accretion (the latter more important for weak sources)
Interaction with (clumpy?) ISM frustrates sub-relativistic jets in radio-quiet AGN
Fundamental plane indicative of scale-invariant jet physics
Combination of high-resolution measurements in the spatial (Chandra) and spectral (Chandra, XMM-Newton) domain key to rule out shocks as the main source of [E]NLR ionization
How close/different are the X-ray cores of Seyfert and Radio Galaxies? We need extended study of complete samples to tell
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
Back-up material
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
Statistics (just a few examples!)Statistics (just a few examples!)
Sub-pc scale jets: 45%Seyferts: 47%
LINERS: 44%
Transition: 16%
VLA (0”.15)
VLBA (2-5 mas)
VLA: 197 VLBA+I: 44
Palomar Galaxies
(96% LLAGN)
Nagar et al. (2005)
Unresolved: 50%
Slightly recolved: 20%
Two components: 10%
Linear: 20%
87% (8.4 GHz)VLA-A (0”.25)
9812-μ AGNThean et al. (2001b)
Unresolved: 21%
Resolved: 79%
100% (18 cm; only >2mJy 8.4GHz sources observed)
MERLIN (0”.1-0”.3)
19CfAThean et al. (2001a)
Unresolved: 52%
Slightly resolved: 30%
[Linear: 32%]
85% (3σ, 6 cm)
71% (3σ, 20 cm)
VLA (1”)52Palomar Seyfert
Ho & Ulvestad (1999)
MorphologiesDetection fraction
Instnt
(reson)
#SamplePaper
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
““Frustrated jets” in Seyferts?Frustrated jets” in Seyferts?
Large fraction of Seyfert Galaxies have large-scale bipolar super-bubbles [Colbert et al. 1996a,b]
(Cecil et al. 2001, 2002)
• Spectra of components A and B is similar to GPS spectra → regions of interactions between jet and dense external medium• Time evolution of radio continuum emission behave as expected for a jet interacting with a clumpy medium• Jet momentum spread in the interaction site may explain the bubbles (Saxton et al. 2005)
• Generalizing this scenario may explain why jets in Seyfert rarely propagate on kpc scales
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
Interpretation of the fundamental Interpretation of the fundamental planeplane Scale-invariant jetsScale-invariant jets [Heinz & Sunyaev 2003][Heinz & Sunyaev 2003]
– Radio luminosity scales with BH mass and accretion Radio luminosity scales with BH mass and accretion rate independently of the jet modelrate independently of the jet model
– Scaling depends on Scaling depends on α, and the electron distribution index → α, and the electron distribution index → on accretion physics onlyon accretion physics only
X-ray emission from BH accretion at a few percent X-ray emission from BH accretion at a few percent Eddington is consistent with radiative inefficient flow onlyEddington is consistent with radiative inefficient flow only
In low accretion rate sources, jet power is proportional to In low accretion rate sources, jet power is proportional to accretion poweraccretion power
Challenges? Seyferts and LL RGs Challenges? Seyferts and LL RGs seem to follow different planes seem to follow different planes [Wang et al. 2006; Panessa et al. 2007][Wang et al. 2006; Panessa et al. 2007]
(Wan
g et
al.
2006
)
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
Role of absorptionRole of absorption
Mkn348
• pc-scale double sources with brightness temperature 1010-11K → synchrotron emission• Historical variability → one sided-jet• One sideness → free-free absorption by ne≥2·105 cm-3 T≥8000 K (X-ray absorption) or ne≥107 cm-3 T≥ 106.6 K• [Exceptional sources: they more powerful than many 12μ sources, against the general correlation between radio power and size → jet starts very luminous and then decay, CSO/GPS link?]
(Ulv
esta
d et
al.
1999
b)
(Ulv
esta
d et
al.
1999
a)
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
NLSy1NLSy1
• ≤7% of NLSy1s are radio-loud (against 10-20% of “normal” Seyfert 1s)
• Stack of 19 VLA observations of undetected NLSy1 (R≤0.27)
• 5/6 radio-loud NLSy1 are GPS/CSS
NLSy1 vs. GPS[Guainazzi et al. 2006; Vink et al. 2006]
(Komossa et al. 2006)(Gallo et al. 2006)
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
This implies that the electron to positron fraction is This implies that the electron to positron fraction is small (≈0.01)small (≈0.01)
Jets flows in Seyferts could start from the inner 10 Jets flows in Seyferts could start from the inner 10 gravitational radii as magnetically-driven windsgravitational radii as magnetically-driven winds
Radio emerges from internal schoks in the Radio emerges from internal schoks in the plasma.plasma.
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
LLAGN (LLLAGN (LHHαα<10<104040 erg s erg s-1-1))
(Nagar et al. 2005)
Main differences between LINERS and Seyfers lower nuclear gas densities lower accretion rate more efficient in launching sub-pc scale jets GBC analogy?
LINERS are in a "low/hard state" Seyfert in a "high/soft" state
Cor
rela
tion
bet
wee
n s
ub
-pc
rad
io
pow
er a
nd
BH
mas
s, g
alax
y lu
min
osit
x
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
Radio jet orientationRadio jet orientation
The distribution of angles between the radio jets and the galaxy disk is consistent with being random, provided that a galaxy is recognized as a Seyfert only if the angle
between the jet and the l.o.s. is ≤40º
[consistent with a basic assumption of the Seyfert unified scenarios]
(Schmitt et al. 2001)(Kinney et al. 2000)
Misalignment between the accretion disk and the host galaxy disk [also Ulvestad & Ho 2001]:• Feeding of a misaligned disk: warping by slef-irradiation instabilities, misaligned gravitational potential, nuclear star clusters, Bardeen-Petterson instabilities …• Misaliged inflow: minor mergers, capture of nuclear star clusters or individual molecular clouds …
Matteo Guainazzi - “Did I say radio-quiet?” – Radio Galaxies in the Chandra era (Cambridge, U.S.A.), 10/7/2008
Unification scenario and radio Unification scenario and radio emissionemission
Seyfert 1s and 2s are indistinguishable in:
• radio luminosity• radio size
Oddities:
• Sources with ionization cones host larger radio sources