1. 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
Pietro Ubertini
ACTIVE GALACTIC NUCLEI 9
Ferrara, Maggio 2010

2. However only a few NLSy1 > 10 keV
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

3. 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: keV)

4. Optical identification and classification
Criteria:
[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)

5. Hard X-ray selected INTEGRAL NLSy1
Swift J (*Swift/BAT)
NGC 4051
Mrk 766
NGC 4748
Mrk 783
IGR J
IRAS
IGR J
IGR J
IGR J
IGR J
ESO 399-IG 020
Swift J
Fourth IBIS Catalogue
(Bird et al 2010, ApJS)
13 Narrow Line Seyfert 1
10 never observed before below 10 keV
8 New XMM observation
2 New Suzaku
…other new data are coming…

6. Reflection components
Miniutti et al. in prep
Suzaku 76 ks
IRAS
IGR J
IRAS Partial convering + C= 2 e riga larga Sigma= oppure PCFABS + PEXRAV R=3 e sigma narrow- EW (fe) 65 eV (too low for the R)- Short period of var in the hardd LC
Strong reflection component
Panessa et al. in prep

7. Variable broad Fe: SWIFT J2127.4+5654
Miniutti et al MNRAS
Suzaku 92 ks
Broad relativistic iron emission line
(originating in reflection from the
innermost region of the AD)
!!!Evidence of variability!!!
Ionized reflection naturally produces a soft X-ray excess, fluorecent emission lines and a reflection continuum
Energy cut-off at keV
Two narrow lines (5.8 and 6.4 keV)
No strong reflection
XMM-Newton (10 ks) +IBIS
Panessa et al. in prep
Variability or poor S/N? 120 ks new XMM will tell …

8. Variable broad Fe: IGR J16385-2057
Broad FeK
..and variable?
No soft variability. A factor of 1.3 variation between XMM1/XMM. IBIS data suggest reflection. F = 1.7e-11 F 210= e-11

9. Strong soft excess: IGR J19378-0617
Variability
F , F 0.1-2=3 F20-100=1.5, Tin=0.2
2-10 keV flux = 8.3e-12
Strong soft excess

10. Strong soft excess: Swift J0923.7+2255
NO soft variability Swift09 = R = 0.4 sigma= Tin=0.22 mekal=0.11 Flux 0.1-2=1.5e-11, F2-10=1.7e-11
IRAS Partial convering + C= 2 e riga larga Sigma= oppure PCFABS + PEXRAV R=3 e sigma narrow- EW (fe) 65 eV (too low for the R)- Short period of var in the hardd LC
No variability in the short LC

11. Average INTEGRAL spectra: photon index
Molina et al. in prep
IBIS NLSy1
IBIS Seyfert 1
Hard X photon index broadly distributed

12. Average high energy properties
No relation with flux
Not always the extrapolation of the soft X-ray spectrum

13. 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

14. The missed hard X-ray AGN sky:
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