XMMNewtonViewofTeVBlazars.pptVIP

XMM-Newton View of TeV Blazars 张有宏 清华大学天体物理中心 Outline Introduction to Blazars X-ray variability properties of TeV blazars Blazars vs GRBs vs micro-quasars/blazars Multi-wavelength observations of PKS2155-304 with XMM-Newton (our work); comparisons with other coordinated multi-wavelength observations XMM-Newton timing mode observations of Mrk 421 (other work) Physical implications inferred from the observations Blazar SED Sequence Nonthermal emission Low energy: Synchrotron High energy: Inverse Compton Luminosity-related SED? Peak energy (synchrotron) HBLs, LBLs, FSRQs Cooling-dependent Variability comparison Same mechanism ? GRBs and micro-quasars (micro-blazars) Jet/Synchrotron Emission (Mirabel, Sky and Telescope, May 2002, 32) TeV Blazars 6 TeV blazars (confirmed): Mrk 421, PKS 2155-304, Mrk 501 HBLs: synchrotron component peaks at UV-X-rays X-ray emission are the high energy tail of synchrotron emission ? X-rays are expected to be violently variable ? To probe particle acceleration and cooling of relativistic particles 由李-马公式的引用看甚高能伽玛射线天文学的兴衰 X-ray Variability of TeV blazars: ASCA/SAX/RXTE Flux variations: Timescales: ~ days with rapid flicker superimposed Variability amplitude: energy dependent PSD: not useful, slpoe ~ 2.5 Cross-correlation function (CCF) ? time lags Spectral evolution: The higher flux, the harder spectrum Peak energy shifts to higher energy with higher flux Mrk 501: ~100 keV by SAX (Pian et al. 1998) Similar optical variability in LBLs (e.g., BL Lac observed with Tsinghua 80cm telescopes) X-ray time lags of TeV blazars Time lags are different from flare to flare: Soft lags: soft photons lag hard ones Hard lags: hard photons lag soft ones Amplitude of lags: 0 - ~3 hours? Time lags appear to correlate with Photon energy Flare’s duration Spectral slope Timescale (Fourier frequency) ? Lags: TeV blazars vs microquasars and GRBs TeV blazars: X-ray soft/hard lags GRBs: gamma-ray soft lags (hard lags?): ?cooling/accelerating time scales