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, 25-27 Maggio 2010

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

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: [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 Mrk 766 NGC 4748 Mrk 783 IGR J14552-5133 IRAS 15091-2107 IGR J16185-5928 IGR J16385-2057 IGR J16426+6536 IGR J19378-0617 ESO 399-IG 020 Swift J2127.4+5654 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…

Reflection components Miniutti et al. in prep Suzaku 76 ks IRAS 15091-2107 IGR J16185-5928 IRAS Partial convering + C= 2 e riga larga Sigma= 0.19 + 0.50 - 0.10 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

Variable broad Fe: SWIFT J2127.4+5654 Miniutti et al. 2009 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 50+40-20 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 …

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 20 100= 1.7e-11 F 210= 0.5-0.7e-11

Strong soft excess: IGR J19378-0617 Variability F2-10 2.4, F 0.1-2=3 F20-100=1.5, Tin=0.2 2-10 keV flux = 8.3e-12 Strong soft excess

Strong soft excess: Swift J0923.7+2255 NO soft variability Swift09 = R = 0.4 sigma= 0.28+0.36-0.11 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= 0.19 + 0.50 - 0.10 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

Average INTEGRAL spectra: photon index Molina et al. in prep IBIS NLSy1 IBIS Seyfert 1 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

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