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The disk-jet link: X-ray and radio monitoring of PKS 0558-504

The disk-jet link: X-ray and radio monitoring of PKS 0558-504. Mario Gliozzi (GMU) I. Papadakis (Crete) W. Brinkmann (MPE) L. Kedziora-Chudczer (Sidney). *Disk-jet connection *AGN-GBH analogy *PKS 0558-504 in Grand Unification Model

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The disk-jet link: X-ray and radio monitoring of PKS 0558-504

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  1. The disk-jet link:X-ray and radio monitoring of PKS 0558-504 Mario Gliozzi (GMU) I. Papadakis (Crete) W. Brinkmann (MPE) L. Kedziora-Chudczer (Sidney) *Disk-jet connection *AGN-GBH analogy *PKS 0558-504 in Grand Unification Model *Results from RXTE & radio monitoring *Conclusions & future work

  2. Disk & Jet *Basic Ingredients of BH systems: Most evident manifestations of BH presence *Growing evidence (theory, observations, simulations) of strong accretion-ejection link: No jet without accretion but not vice versa *Main Goals: 1) Understand the conditions leading to jet formation/quenching 2) Assess jet role in energetics of the system

  3. X-ray & Radio monitoring Previous studies demonstrate crucial role of radio X-ray monitoring: X-rays track the accretion activity Radio tracks the jetactivity Microquasar GRS1915+105 [Mirabel et al. 1998] BLRG 3C120 [Marscher et al. 2002] Same phenomena occur on different scales: analogy GBHs -AGN

  4. LS energy spectrum: HS energy spectrum: E [keV] E [keV] [Fig from Zdziarski & Gierlinski 2004] Grand Unification Model GBHs scaled down versions of AGN: AGN classes correspond to GBHs in different spectral states [e.g., Mc Hardy et al. 2006] 2 main spectral states: 1) Low/Hard State (LS) and2) High/Soft State (HS)

  5. GBHs scaled down versions of AGN: AGN classes correspond to GBHs in different spectral states [e.g.,Mc Hardy et al. 2006] 2 main spectral states: 1) Low/Hard State (LS) and2) High/Soft State (HS) Grand Unification Model LS power spectrum: HS power spectrum: [GX 339-4 Homan & Belloni 2004]

  6. GBHs scaled down versions of AGN: AGN classes correspond to GBHs in different spectral states [e.g.,Mc Hardy et al. 2006] 2 main spectral states: 1) Low/Hard State (LS) and2) High/Soft State (HS) Grand Unification Model LS radio properties: HS radio properties: Persistent radio emission Correlation with X-rays: LR~LX0.7 Emission from compact jet Weak/absent radio emission Jet quenching [Cyg X-1 Sterling et al. 2001] [Fender et al. 2004; E. Gallo et al. 2004;]

  7. IS energy spectrum: [Fig from Zdziarski & Gierlinski 2004] GBH Intermediate State HID: model-independent way to describe GBH evolution Existence of Intermediate spectral State (IS) [GX 339-4Homan & Belloni 2004]

  8. IS power spectrum: [Fig from Homan & Belloni 2004] GBH Intermediate State HID: model-independent way to describe GBH evolution Existence of Intermediate spectral State (IS)

  9. GBH Intermediate State HID: model-independent way to describe GBH evolution Existence of Intermediate spectral State (IS) IS radio properties: Transient & strong radio emission Steep spectrum Large bulk Lorentz factor Most powerful jet ejections [GRS1915+105 Mirabel & Rodriguez 1998]

  10. LS LLAGN Based on generalization of HID [Koerding et al. 2006] Based on “fundamental plane” [Merloni et al. 2003; Falke et al. 2004] HS Seyfert 1 Based on PSD [Uttley et al. 2002; Markowitz et al. 2003; McHardy et al. 2006] IS ? AGN-GBH Correspondence Importance of finding IS-analog AGN: frozen look of BH systems during major ejections IS requirements: * high accretion rate * strong radio emission * steep energy spectrum * PSD with QPOs

  11. PKS 0558-504 In principle any radio-loud NLS1 satisfies basic requirements for IS, but only few of these objects[Komossa et al. 2005] only PKS 0558-504 bright enough for RXTE monitoring (F2-10keV ~ 2x10-11 erg cm-2 s-1, L2-10keV ~ 1045 erg s-1) Radio-loud: R~30[Siebert et al. 1999] BH mass:MBH~4x107 Msolar[Wang et al. 2001] X-rays:Bright, Steep PL (Г~2.2), Variable [Gliozzi et al. 2007] Extremely variable: 67% flux variation in 3’ [Remillard et al. 1991]

  12. Yes Lbol ~ LEdd Even considering MBH~ 5 Mvirial[Marconi et al. 2008] and different bolometric corrections [Vasudevan & Fabian 2007] Maybe (but spectral degeneracy) Comptonization [O’Brien et al. 2001; Brinkmann et al. 2004] Ionized Reflection[Ballantyne et al. 2001; Crummy et al. 2006] SLIM disk [Haba et al. 2008] Beamed emission [Remillard et al. 1991; Gliozzi et al. 2001] Requirements for IS High accretion rate? Jet radio emission? Maybe (wait and see) No (at least not yet) Answer after XMM AO7 5 orbits (660ks PI Papadakis) PSD with QPO? Energy spectrum match?

  13. LS IS HS E [keV] Additional diagnostics for IS From model-independent studies of spectral variability: 1) Fractional variability flattens in IS from LS to HS [Gierlinski & Zdziarski 2005] 2) Short-term variability Cyg X-1 during IS characterized large flux changes without spectral variations [Malzac et al. 2006]

  14. Soft [2.5-5 keV]and Hard [5-15 keV] fluxes highly variable on day-month timescales. Flux variability accompanied by weak spectral variability. RXTE monitoring of PKS 0558-504 Campaign: Started in March 2005; monitoring campaign under way Sampling: 1 observation every 2 days + 3 periods of denser coverage (2 observations per day) [Gliozzi et al. 2007]

  15. Linear trend Intercept = 0 no spectral pivoting no contribution from hard component Flux-Flux Plot Plot Hard [5-15 keV] versus Soft [2.5-5 keV]count rate to characterize the spectral variability [e.g., Churazov et al. 2001; Taylor et al. 2003] . Two possible scenarios: 1) If power-law trend: Spectral variability explained by pivoting. 2) If linear trend: Constant spectral shape with 2 components [Zdziarski et al. 2002] Common physical origin for Soft & Hard

  16. Fvar=√(S2- <σerr2>)/<x> Constant trend reminiscent of GBHs in IS [Gierlinski & Zdziarski 2005] Different from typical jet-dominated behavior: FvarαE [Gliozzi et al. 2006] Mrk 501 Fvar- E Plot Plot Fractional variability Fvar vs energy

  17. Different from typical jet-dominated behavior: HR αct [Gliozzi et al. 2006] Mrk 501 HR-ct Plot Plot of hardness ratio HR=[5-15 keV]/[2.5-5 keV] vs. count rate Constant trend reminiscent of Cyg X-1 in IS [Malzac et al. 2006]

  18. Radio Observations ATCAImaging:18 GHz F.O.V= 9”x13” beam=0.5” (1”=2.4 kpc) Source unresolved

  19. Radio Observations ATCA Imaging: 8.6 GHz F.O.V= 18”x27” beam=1” (1”=2.4 kpc) 2 symmetric lobes resolved (d=14 kpc)

  20. Radio Observations ATCA Imaging: 4.8 GHz F.O.V= 38”x58” beam=2” (1”=2.4 kpc) 2 symmetric lobes resolved (d=14 kpc)

  21. Radio Observations VLBI Imaging [S. Tingay] jet resolved (R~100 pc)

  22. Radio Monitoring Radio emission highly variable Timescales longer compared to X-rays No trivial correlation with X-rays but longer baseline needed

  23. PKS 0558-504 IS-analog ? Yes High accretion rate? Jet radio emission? Yes Yes Typical Spectral variability? Energy spectrum match? Maybe: no evidence for reflection PKS 0558-504 extraordinary object: high accretion rate AGN with strong radio jet, very bright, highly variable on all timescales.

  24. Future Work - From September 2008 PKS 0558-504 weekly monitored with SWIFT in Optical, UV, and soft X-ray to complement hard X-rays (RXTE) and hopefully radio monitoring. -5 XMM-Newton orbits in AO7 for deep investigation of PSD (QPOs) and breaking spectral degeneracy via time-resolved spectroscopy. - Further VLBI observations to investigate possible changes in the inner jet structure.

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