the radio look of the hard x‑ray agn seen by · pdf filethe radio look of the hard x‑ray...
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TheRadiolookofthehardX‑rayAGNseenbyINTEGRAL
Francesca Panessa
Loredana Bassani, Angela Bazzano, Paola Castangia, Elisabetta Maiorano, Angela Malizia, Paola Parma, Andrea Tarchi
ʺINTEGRALʹsjourneythroughthehighenergysky”
Rome 15‑18 October 2013
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How do bright INTEGRAL AGN look like in the radio band?
Bright, large scales, lobes, jets?
Weak, sub-pc scale, unresolved or slightly resolved?
How is the hard X-ray emission related to the radio emission?
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Complete sample between 20-40 keV (Malizia et al. 2009 MNRAS): 88 Seyfert galaxies: - 41 type 1 - 33 type 2 - 6 NLSy1 - 9 Blazars
HardX‐rayselectedINTEGRALAGNCompletesample
Hard X-ray selected sample of luminous AGN: -> INTEGRAL 20-100 keV (Malizia et al 2009)
-> 2-10 keV X-ray data (Malizia et al. + literature) -> NVSS radio data (Panessa et al. in preparation)
VLA-VLBI data (literature, new observations)
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Radioemissionintype1‑1.5Seyferts
Mrk6 Theradioemissionoccursonthreedifferentspatialscales:7.5kpcbubbles,1.5kpcbubbleslyingnearlyorthogonaltothem,anda1kpcradiojetlyingorthogonaltothekiloparsec‑scalebubble.
(Kharb+2006)
..some examples
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VLBA image at 1.6 GHz of the central region of NGC 3783: unresolved component No extended extra-nuclear
emission
Orienti M , and Prieto M A MNRAS 2010
Radioemissionintype1‑1.5Seyferts ..some examples
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Radioemissionintype1.8‑2Seyferts
VLBAemissionconsistentwithfree‑freeemissionfromthehotX‑raycorona
NGC1068 Gallimoreetal.2004
..some examples
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Radioemissionintype1.8‑2Seyferts
MCG‑5‑23‑16
VLAimageat8.4GHz
Thesourceisresolvedinthenorthdirection,suggestingthepresenceofajet‑likestructure.
Orienti M , and Prieto M A MNRAS 2010
..some examples
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Radioemissionintype1.8‑2Seyferts Presenceofajet:
Nodata13lackofVLA/VLBIdata
Jet7cleardetectionofoneortwosidedlobeorjetcomponent
Nojet(?)13unresolvedradioemission(needdeeperinspection)
Radioemissionintype1‑1.5Seyferts Presenceofajet:
Nodata18lackofVLA/VLBIdata
Jet10cleardetectionofoneortwosidedlobesorjetcomponent
Nojet(?)13unresolvedradioemission(needdeeperinspection)
…summarizing
Wide range of morphologies, radio powers, spectral indices, etc.
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At 1.6 GHz 3 sub-mJy components:
Two associated with the VLA small scale double structure
Third is symmetric to the easternmost one
H2O Maser coincident with core
Jet base? Mini radio-lobes? Thermal emission from an outflow/molecular disk/nuclear wind?
Giroletti & Panessa, 2009, ApJL
RadioemissioninNarrowLineSeyfert1
+
NGC 4051
Giroletti & Panessa, 2009, ApJL
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RadioemissioninNarrowLineSeyfert1
theEVNandMERLIN6cmimageofthenuclearregionofNGC5506byMiddelbergetal.(2004)
Tarchi et al. 2011 D
EC
LIN
AT
ION
(J2000)
RIGHT ASCENSION (J2000)14 13 14.895 14.890 14.885 14.880 14.875 14.870 14.865 14.860
-03 12 27.3
27.4
27.5
27.6
27.7
27.8
27.9
VLAA‑arrayK‑bandcontinuumimageofthenuclearregionofNGC5506
NGC5506,wefindthatthewatermaseremissionislocatedwithin5and12pc,respectively,ofnuclearradiocontinuumknots,whichare
interpretedascore‑jetstructures
NGC 5506
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NGC 4258
The discovery of a water mega-maser in IGR J16385-2057: - it is a NLSy1 (masers are tipically found in obscured AGN) - it resides in an elliptical galaxy (masers are rare in ellipticals)
Watermaseremissiontracesadisk,ajetoroutflow
Tarchietal2011
RadioemissioninNarrowLineSeyfert1 ..an INTEGRAL discovered NLSy1: IGR J16385-2057
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INTEGRALAGN22GHzwatermasersurvey
WatermaserdetectionrateintheINTEGRALsampleof17% (Castangiaetal.inpreparation)
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HardX‐rayselectedINTEGRALAGNCompletesample
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RadioLoudness
-> Log L R/LX = -4.5 (Terashima & Wilson 2003) -> Half of the sample is RADIO LOUD
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ScalingRelaCons:LradioversusLX‐ray
*RLInagreementwiththeEFFICIENTBRANCHlawof1.4*
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FundamentalplaneforBHacCvity
-> Large scatter, INTEGRAL AGN sample the high Eddington accretion regime more radio with respect to that expected from the Fundamental Plane
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VLBI < 0.1 pc
NVSS up to tens of kpc
VLA tens of pc up to kpc scales
VLA
VLBI
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X‐rayversusRadiocorrelaConinLLAGN
ty 1 - flat sp
ty 2 - flat sp
ty 1 - steep sp
ty 2 - steep sp
ty 1 - flat sp
ty 2 - flat sp
ty 1 - steep sp
ty 2 - steep sp
NosignificantcorrelationatVLBIsub‑pcscales
Panessa&Girolehi2013MNRAS/arXiv:1304.0794
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Resolvedradioemission
Excess of extended radio emission in more luminous AGN
ty 1 - flat sp
ty 2 - flat sp
ty 1 - steep sp
ty 2 - steep sp
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Wide range of radio morphologies and properties High fraction (almost 50%) of RADIO LOUD AGN in a hard X-ray selected sample Strong Radio versus X-ray correlation both for RL and RQ AGN in the sample
New exciting results from: water maser follow up deeper radio observations
Conclusions