Presentation - Active Galactic Nuclei 8 - Inaf

Testing the LINERs paradigmwith Swiftsimultaneous UV to X-ray XdataPat RomanoINAF-IASF PalermoE. Pian, D. Maoz, A. Cucchiara, C. Pagani, V. La ParolaAGN8 MeetingTurin, May 19-22, 2008

LINERS ILow-Ionization Nuclear Emission Line Regionslow-luminosity active nuclei lacking thecharacteristic “big blue bump" observed in moreluminous Seyfert galaxies and QSOs.big blue bumpP. Romano - AGN8 Meeting - Turin 2

Kewley et al. 2006LINERs occupy a well-defined ‘cloud’ in emission-line ratiodiagnostic diagrams, a cloud that is distinct from the regionsoccupied by HII and Seyfert nuclei.The transition from the Seyfert region to the LINER region in thediagnostic diagrams corresponds to a decrease in the Eddingtonratio, L/L EddP. Romano - AGN8 Meeting - Turin 3

ParadigmSeyferts:(geometrically) thin accretion diskHigh radiative efficiency (~0.1)-BBB=thermal radiation from AD+Kα EL profile + L/L Edd ~1LINERS: Radiativelyinefficient accretionflows (RIAFs) Ho (2003)-kinetic energyadvected or redirectedinto an outflowP. Romano - AGN8 Meeting - Turin 4

Sample Selection I (Maoz 2005, 2007)17 LINERs UNOBSCUREDknown UV nuclei L(UV)~10 (39-41) erg/sNo dust lanes in optical imagesX-ray absorbing columns are N H

Results: UV variabilityF330F250P. Romano - AGN8 Meeting - Turin 6

Maoz et al. 2005, 2007Summary of LINER monitoring campaign:Most LINERs vary in the UV on short timescales, long timescales, orboth. At least some of UV is nonstellar.Variable UV flux gives lower limit on AGN component of UV luminosity– can constrain SED/ accretion modeScaled down versions of SeyfertsSeyfertsLINERsP. Romano - AGN8 Meeting - Turin 7

Need for Simultaneous dataWhile the arguments of Maoz (2007) are supported bygood spectra, the UV and X-ray data are notsimultaneous.LINERs exhibit variability, which, albeit notof very large amplitude (factor 2), may undermine theresults derived from non-simultaneous observations.Approach the problem usingsimultaneous X-ray and UV dataXMM or SwiftP. Romano - AGN8 Meeting - Turin 8

Swift InstrumentsSpacecraft•Autonomous re-pointing,

Sample Selection IIBrightest objects in Maoz 2007P. Romano - AGN8 Meeting - Turin 10

Sample Selection IIIBrightest objects in Maoz 2007ToONGC 3998: 27.4 ksNGC 4579: 20.8 ksXRT Observation logFill-insinsM81: 33.7 ksNGC 4203: 5.3 ksP. Romano - AGN8 Meeting - Turin 11

Swift/XRT data IM81NGC3998NGC4203NGC4579P. Romano - AGN8 Meeting - Turin 12

Swift/XRT data IIM81NGC3998NGC4203NGC4579P. Romano - AGN8 Meeting - Turin 13

M81P. Romano - AGN8 Meeting - Turin 14

NGC 3998P. Romano - AGN8 Meeting - Turin 15

Host galaxy X-ray contribution: ChandraGalaxycontribution inXRT extractionregion:M81NGC3998M81 10%M81 10%NGC 3998 6%NGC 4203 16%NGC 4579 25%NGC4203NGC4579P. Romano - AGN8 Meeting - Turin 16

Swift/XRT spectraNo absorptionfeaturesM81 KαKEW=639+531639+531-369eV369eV(2.996 σ)NGC 4579 KαKEW= 548+4067-309(2.1 σ)P. Romano - AGN8 Meeting - Turin 17

Swift/XRT Spectral Parametersb 1E- 12 erg/cm2/s-Fluxes within 20-40% of Chandra fluxes in Maoz 2007-Γ~2N H > N GHP. Romano - AGN8 Meeting - Turin 18

XRT lightcurves IP. Romano - AGN8 Meeting - Turin 19

XRT lightcurves IIP. Romano - AGN8 Meeting - Turin 20

XRT lightcurves IIIP. Romano - AGN8 Meeting - Turin 21

XRT light curves IVP. Romano - AGN8 Meeting - Turin 22

Swift/UVOT: uvw1 band images IM81P. Romano - AGN8 Meeting - Turin 23

Swift/UVOT: uvw1 band images IIM81P. Romano - AGN8 Meeting - Turin 24

UVOT photometryFlux (10 -15)Galaxycontribution:-dominant in u(up to x8 inNGC 4203)-decreases atshorterwavelengthsP. Romano - AGN8 Meeting - Turin 25

Swift SEDsP. Romano - AGN8 Meeting - Turin 26

Maoz 2007 SEDsP. Romano - AGN8 Meeting - Turin 27

Concluding remarks/Future WorkGalaxy contribution-dominant in u (up to x8 in NGC 4203), decreases at shorter λs-important in X band (never dominant)Variability-UVOT in NGC3998-XRT in M81 and NGC 3998 ? Correlated ?Construction of strictly simultaneous UV-toto-X X SEDs (WIP)-consistent results with Maoz 2007-LINERs as scaled down versions of Seyferts.No need to invoke different emission mechanismModelling of SEDs and variability assessmentP. Romano - AGN8 Meeting - Turin 28

The EndP. Romano - AGN8 Meeting - Turin 29