Transcript Document

High energy NLSy 1 galaxies
FRANCESCA PANESSA
on behalf of the IBIS survey/AGN team:
Loredana Bassani
Angela Bazzano
Alessandra De Rosa
Antony Dean
Maria Teresa Fiocchi
Raffaella Landi
Angela Malizia
Manuela Molina
ACTIVE GALACTIC NUCLEI 9
Ferrara, 25-27 Maggio 2010
Pietro Ubertini
Narrow Line Seyfert 1s
NLSy1 are a sub-class of type 1 Seyfert with peculiar optical properties
In X-RAYs:
 Steeper intrinsic hard X-ray continuum - Compton cooling of AD?
 Strong soft excess and extreme rapid variability
 High energy hump, reflection/light bending models
• Small black hole mass - High Eddington ratio!
BROAD-BAND data are crucial to define the continuum and discriminate models
However only a few NLSy1 > 10 keV
High energy observations of
Narrow Line Seyfert 1s (Malizia et al. 2008)
Five Hard X-ray selected
NLSy1s:
Analysis of the previous IBIS
catalogue spectra combined
with Swift/XRT
• Steep power law spectrum above 10 keV
• Absent or absorbed soft excess
• Low high energy cut-off (3/5: 30-50 keV)
Optical identification and classification
Criteria:
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[O III] λ5007/Hβ ratio <3
FWHM(Hβ) ≤ 2000 km/s
Fe II/Hβ > 0.5
Osterbrock & Pogge (1985)
Six NLSy1 (IGR)
newly identified
(Masetti et al. 2009, 2008, 2006,
Parisi et al. 2009)
Hard X-ray selected INTEGRAL NLSy1
Swift J0923.7+2255 (*Swift/BAT)
NGC 4051
Fourth IBIS Catalogue
Mrk 766
(Bird et al 2010, ApJS)
NGC 4748
Mrk 783
IGR J14552-5133
IRAS 15091-2107
IGR J16185-5928
13 Narrow Line Seyfert 1
IGR J16385-2057
IGR J16426+6536
10 never observed before below 10 keV
8 New XMM observation
IGR J19378-0617
2 New Suzaku
ESO 399-IG 020
Swift J2127.4+5654
…other new data are coming…
Reflection components
Suzaku 76 ks
IGR J16185-5928
Miniutti et al. in prep
IRAS 15091-2107
Strong reflection component
Panessa et al. in prep
Variable broad Fe: SWIFT J2127.4+5654
Suzaku 92 ks
• Energy cut-off at 50+40-20 keV
• Two narrow lines (5.8 and 6.4 keV)
• No strong reflection
Miniutti et al. 2009 MNRAS
 Broad relativistic iron emission line
(originating in reflection from the
innermost region of the AD)
!!!Evidence of variability!!!
XMM-Newton (10 ks) +IBIS
Panessa et al. in prep
Variability or poor S/N? 120 ks new XMM will tell …
Variable broad Fe: IGR J16385-2057
Broad FeK
..and variable?
Strong soft excess: IGR J19378-0617
Variability
Strong soft excess
Strong soft excess: Swift J0923.7+2255
Strong soft excess
No variability in the short LC
Average INTEGRAL spectra:
photon index
IBIS Seyfert 1
IBIS NLSy1
Molina et al. in prep
Hard X photon index broadly distributed
Average high energy properties
No relation with flux
Not always the extrapolation of the soft X-ray spectrum
Black hole mass and Eddington ratio
Panessa et al. in prep
The hard X-ray selection
is not producing any bias
in the accretion efficiency
Bianchi et al. 2009
Conclusions
SAMPLE of HARD X-ray NLSY1
• Hard X-ray and Soft X-ray Photon indeces distributed as in Sey1
• High energy cut-off in two sources out of 6
• Strong soft excess in 4/6 - not always related to variability/reflection
• Strong Fe line ALWAYS (broad/variable in at least 5 source)
The missed hard X-ray AGN sky:
Importance of follow-up of INTEGRAL AGN - very bright
sources - very easy to get high statistics spectra