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Tackling the Disk/Jet Connection in AGN: Timing Analysis Methods and Outlook for GLAST

Tackling the Disk/Jet Connection in AGN: Timing Analysis Methods and Outlook for GLAST. Martin Mueller SLAC AstroGamma GLAST Lunch Oct. 06, 2005. Advisor: Greg Madejski Collaborators: Chris Done (Durham U.) Piotr Życki (CAMK Warsaw). Outline.

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Tackling the Disk/Jet Connection in AGN: Timing Analysis Methods and Outlook for GLAST

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  1. Tackling the Disk/Jet Connection in AGN: Timing Analysis Methods and Outlook for GLAST Martin Mueller SLAC AstroGamma GLAST Lunch Oct. 06, 2005 Advisor: Greg Madejski Collaborators: Chris Done (Durham U.) Piotr Życki (CAMK Warsaw)

  2. Outline • The Big Black Box around the AGN Central Engine • Time Series Analysis – Power Density Spectra • Introduction to Method of Light Curve Simulations • Results for NGC 4945 (Seyfert 2 galaxy) • Application to GLAST • Summary 2 M. Mueller, GLAST Lunch, 10/06/05

  3. Big Black Box Big Black Box The Big Black Box around the AGN Central Engine NGC 4945 Mrk421 A. Simmonet, Sonoma State U. Kataoka et al. 2001 Mueller et al., in preparation 3 M. Mueller, GLAST Lunch, 10/06/05

  4. Timing Studies with AGN and Blazars • characteristic time scales, search for QPOs • determination of black hole mass • evidence for accretion statesin massive black holes Unification of AGN phenomena • multiwavelength campaigns: correlation functions  time lags flares, spectral changes McHardy et al. 2004 4 M. Mueller, GLAST Lunch, 10/06/05

  5. Understanding Power Density Spectra Kataoka et al. 2001 time domain (light curve) frequency domain (power density spectrum) 5 M. Mueller, GLAST Lunch, 10/06/05

  6. Understanding Power Density Spectra P(f) = P0 f-1 P(f) = P0 f-2 Timmer & Koenig 1995 6 M. Mueller, GLAST Lunch, 10/06/05

  7. The Trouble with Uneven Sampling • distortions • spurious peaks,troughs • slope changes NGC 4945 (Mueller et al., in preparation) 7 M. Mueller, GLAST Lunch, 10/06/05

  8. More on Uneven Sampling Unevenly sampled light curves unavoidable in Astrophysics • observation scheduling • Earth occultations • SAA passages • observation mode (scanning vs. pointing) • sparse photon data 8 M. Mueller, GLAST Lunch, 10/06/05

  9. Method of Light Curve Simulations Conceptual basis: • need to incorporate window function • need reliable way to calculate uncertainties in frequency domain • cannot remove effect of window function from distorted periodogram (unfolding problem)  solution: use ideas from X-ray spectral fitting: forward-propagation of model for observed data 9 M. Mueller, GLAST Lunch, 10/06/05

  10. Method of Light Curve Simulations • model for shape of PDS  simulated light curve  apply window function in time domain • use Lomb-Scargle periodogram for frequency analysis • compare periodogram from observed light curveagainst simulated set  goodness-of-fit • iterate to find best-fitting parameters of model Done et al. (1992) Uttley, McHardy, Papadakis (2002) Markowitz et al. (2003) Mueller et al. (2003, astro-ph/0312466) 10 M. Mueller, GLAST Lunch, 10/06/05

  11. Results from Light Curve Simulations get goodness-of-fit as a function of the input model parameters: NGC 4945 unbroken power law fit broken power law fit 11 M. Mueller, GLAST Lunch, 10/06/05

  12. Application to GLAST EGRET: very sparse data, no point in trying this method 3EG J1746-2851 3EG J0530+1323 = PKS 0528+134 GLAST: increased collection area, better sensitivity  count rate higher • range of time scales accessible to GLAST: • each source in the sky viewed at least once a day • mission lifetime: ~5 years orbit: 95 min (<40 min continuous on any object) SAA passages: 24 hours orbit precession: ~55 days (from Jim Chiang’s 2002 presentation) unevenly sampled? OH, YES! Wallace et al. 2000 12 M. Mueller, GLAST Lunch, 10/06/05

  13. Interesting Target: 3C 273 Probing the disk/jet connection: need an object where both disk and jet visible Marshall et al. 2001 Kriss et al. 1999 jet resolved in radio, optical, X-ray spectrum showing evidence of both accretion flow and jet 13 M. Mueller, GLAST Lunch, 10/06/05

  14. Summary • GLAST: expect unevenly sampled light curves for astrophysically interesting sources (e.g. blazars) • observing pattern ideal for detecting transient sources(e.g. 3C 279) • method of light curve simulations well suited for analysis of these data sets • probing the disk/jet connection viable science goalfor GLAST in connection with observations inother wavelength bands Thank you! 14 M. Mueller, GLAST Lunch, 10/06/05

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