General comments: the astrophysics-particle physics connection

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Messenger particle II.
proton, electron (cosmic rays): subject to energy losses, deflection by magnetic field neutrino: straight line propagation, usually impossible to stop in source, smoking gun probe for hadronic processes, but almost equally impossible to detect [e.g., ICECUBE, right sensitivity level to finally start seeing something besides nearby supernova] gravity waves: straight line propagation, need only to detect strain (amplitude not power) => can see to high redshift, but expected strains miniscule, no convincing detections yet [LIGO, LISA]
When you look in new ways …

A "boring" object in the sky: the nearby elliptical galaxy M87
Optical
Radio
Black holes one of most extreme environments can imagine --- strong gravity, spinning black hole can extract up to ~0.4 of the rest mass energy of infalling matter huge power outputs, and densities: Black hole environments probe extreme physics! Because they are often so bright, accreting black holes very useful as cosmological probes (can see them to very high redshifts). Background/noise for exotic particle astro. sources, e.g., probably dominate GeV gamma-ray background and may produce UHECR. Better understand them and what they can do!
Extended X-Ray Emission from Jets!! – Potential GeV/TeV Sources!
Cygnus A - FRII (powerful jet )
X-RAY
M87 – FRI (weak jet)
X-RAY
HST M87 Superluminal Motion
X-ray variability seen in HST-1 knot too!!
M87 jet is not wimpy!!!
D. Harris,2003
GeV Blazars… EGRET
TeV Blazars…
Mkn 421
Fossati et al. 2002
Mkn 421
Gaidos et al. 1996
Pian et al. 1998
Rapid spectral variability!
C. von Montigny 1995
Summary of EGRET Gamma-Ray Data … FSRQ
LBL
HBL
L_x and L_gamma correlated ! v_peak(bump_1) and v_peak(bump_2) correlated
Grand Unified Blazar Scheme
(synchrotron & Compton from SAME e+/e- ; γ peak ∝ Lum1 ) Donati et al. 2001 (cf. Fossati el. 1998)

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