High energy NLSy 1 High energy NLSy 1 galaxiesgalaxies

FRANCESCA PANESSA

on behalf of the IBIS survey/AGN team:on behalf of the IBIS survey/AGN team: Loredana Bassani

Angela BazzanoAlessandra De Rosa

Antony DeanMaria Teresa Fiocchi

Raffaella LandiAngela MaliziaManuela Molina

Pietro Ubertini

ACTIVE GALACTIC NUCLEI 9Ferrara, 25-27 Maggio 2010

Narrow Line Seyfert 1sNarrow Line Seyfert 1s

In X-RAYs:In X-RAYs:

Steeper intrinsic hard X-ray continuum - Compton Steeper intrinsic hard X-ray continuum - Compton cooling of AD?cooling of AD? Strong soft excess and extreme rapid variabilityStrong soft excess and extreme rapid variability High energy hump, reflection/light bending modelsHigh energy hump, reflection/light bending models

NLSy1 are a sub-class of type 1 Seyfert with peculiar optical propertiesNLSy1 are a sub-class of type 1 Seyfert with peculiar optical properties

BROAD-BAND data are crucial to define the continuum and discriminate models data are crucial to define the continuum and discriminate models

However only a few NLSy1 > 10 keVHowever only a few NLSy1 > 10 keV

• Small black hole mass - High Eddington ratio! Small black hole mass - High Eddington ratio!

High energy observations of High energy observations of Narrow Line Seyfert 1sNarrow Line Seyfert 1s

Five Hard X-ray selected Five Hard X-ray selected NLSy1sNLSy1s: :

Analysis of the previous IBIS Analysis of the previous IBIS catalogue spectra combined catalogue spectra combined

with Swift/XRT with Swift/XRT

(Malizia et al. 2008)(Malizia et al. 2008)

• Steep power law spectrum above 10 keV Steep power law spectrum above 10 keV • Absent or absorbed soft excessAbsent or absorbed soft excess• Low high energy cut-off (3/5: 30-50 keV)Low high energy cut-off (3/5: 30-50 keV)

Optical identification and Optical identification and classificationclassification

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 Hard X-ray selected INTEGRAL NLSy1NLSy1

Swift J0923.7+2255 (*Swift/BAT)NGC 4051Mrk 766NGC 4748Mrk 783IGR J14552-5133IRAS 15091-2107IGR J16185-5928IGR J16385-2057IGR J16426+6536IGR J19378-0617ESO 399-IG 020Swift J2127.4+5654

Fourth IBIS Catalogue(Bird et al 2010, ApJS)

13 Narrow Line Seyfert 1

10 never observed before below 10 keV10 never observed before below 10 keV8 New XMM observation8 New XMM observation2 New Suzaku2 New Suzaku … …other new data are coming…other new data are coming…

Reflection componentsReflection components

IGR J16185-5928

Strong reflection component

Miniutti et al. in prep

Suzaku 76 ks

IRAS 15091-2107

Panessa et al. in prep

Variable broad Fe: SWIFT J2127.4+5654Variable broad Fe: SWIFT J2127.4+5654

• Energy cut-off at 50Energy cut-off at 50+40+40-20 -20 keVkeV

• Two narrow lines (5.8 and 6.4 keV)Two narrow lines (5.8 and 6.4 keV)• No strong reflectionNo strong reflection

Broad relativistic iron emission lineBroad relativistic iron emission line (originating in reflection from the (originating in reflection from the innermost region of the AD)innermost region of the AD) !!!Evidence of variability!!!!!!Evidence of variability!!!

Miniutti et al. 2009 MNRASSuzaku 92 ks

XMM-Newton (10 ks) +IBIS

Variability or poor S/N? 120 ks new XMM will tell …Variability or poor S/N? 120 ks new XMM will tell …

Panessa et al. in prep

..and variable? Broad FeK

Variable broad Fe: IGR J16385-2057Variable broad Fe: IGR J16385-2057

Strong soft excess: IGR J19378-0617Strong soft excess: IGR J19378-0617

Strong soft excess

Variability

Strong soft excess

Strong soft excess: Swift J0923.7+2255Strong soft excess: Swift J0923.7+2255

No variability in the short LC

Average INTEGRAL spectra: Average INTEGRAL spectra: photon indexphoton index

Hard X photon index broadly distributed Hard X photon index broadly distributed

Molina et al. in prepMolina et al. in prep

IBIS NLSy1IBIS NLSy1

IBIS Seyfert 1IBIS Seyfert 1

Average high energy propertiesAverage high energy properties

No relation with fluxNo relation with fluxNot always the extrapolation of the soft X-ray spectrumNot always the extrapolation of the soft X-ray spectrum

Black hole mass and Eddington Black hole mass and Eddington ratioratio

Bianchi et al. 2009

The hard X-ray selectionis not producing any bias in the accretion efficiency

Panessa et al. in prep

• Hard X-ray and Soft X-ray Photon indeces Hard X-ray and Soft X-ray Photon indeces distributed as in Sey1distributed as in Sey1

• High energy cut-off in two sources out of 6High energy cut-off in two sources out of 6

• Strong soft excess in 4/6 - not always related to Strong soft excess in 4/6 - not always related to variability/reflectionvariability/reflection

• Strong Fe line ALWAYS (broad/variable in at least Strong Fe line ALWAYS (broad/variable in at least 5 source)5 source) The missed hard X-ray AGN sky: The missed hard X-ray AGN sky:

Importance of follow-up of INTEGRAL AGN - Importance of follow-up of INTEGRAL AGN - very bright sources - very easy to get high very bright sources - very easy to get high

statistics spectra statistics spectra

SAMPLE of HARD X-ray NLSY1

ConclusionsConclusions