The High-energy emission of jetted AGN. (arXiv:1901.00462v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Schwartz_D/0/1/0/all/0/1">Daniel A. Schwartz</a>
Quasars with flat radio spectra and one-sided, arc-second scale, ~100 mJy GHz
radio jets are found to have similar scale X-ray jets in about 60% of such
objects, even in short 5 to 10 ks Chandra observations. Jets emit in the GHz
band via synchrotron radiation, as known from polarization measurements. The
X-ray emission is explained most simply, i.e. with the fewest additional
parameters, as inverse Compton (iC) scattering of cosmic microwave background
(CMB) photons by the relativistic electrons in the jet. With physics based
assumptions, one can estimate enthalpy fuxes upwards of 10^46 erg s$^{-1}$,
suffcient to reverse cooling flows in clusters of galaxies, and play a
signifcant role in the feedback process which correlates the masses of black
holes and their host galaxy bulges. On a quasar-by-quasar basis, we can show
that the total energy to power these jets can be supplied by the rotational
energy of black holes with spin parameters as low as a = 0.3. For a few bright
jets at redshifts less than 1, the Fermi gamma ray observatory shows upper
limits at 10 Gev which fall below the fluxes predicted by the iC/CMB mechanism,
proving the existence of multiple relativistic particle populations. At large
redshifts, the CMB energy density is enhanced by a factor (1+z)^4, so that
iC/CMB must be the dominant mechanism for relativistic jets unless their rest
frame magnetic field strength is hundreds of micro-Gauss.
Quasars with flat radio spectra and one-sided, arc-second scale, ~100 mJy GHz
radio jets are found to have similar scale X-ray jets in about 60% of such
objects, even in short 5 to 10 ks Chandra observations. Jets emit in the GHz
band via synchrotron radiation, as known from polarization measurements. The
X-ray emission is explained most simply, i.e. with the fewest additional
parameters, as inverse Compton (iC) scattering of cosmic microwave background
(CMB) photons by the relativistic electrons in the jet. With physics based
assumptions, one can estimate enthalpy fuxes upwards of 10^46 erg s$^{-1}$,
suffcient to reverse cooling flows in clusters of galaxies, and play a
signifcant role in the feedback process which correlates the masses of black
holes and their host galaxy bulges. On a quasar-by-quasar basis, we can show
that the total energy to power these jets can be supplied by the rotational
energy of black holes with spin parameters as low as a = 0.3. For a few bright
jets at redshifts less than 1, the Fermi gamma ray observatory shows upper
limits at 10 Gev which fall below the fluxes predicted by the iC/CMB mechanism,
proving the existence of multiple relativistic particle populations. At large
redshifts, the CMB energy density is enhanced by a factor (1+z)^4, so that
iC/CMB must be the dominant mechanism for relativistic jets unless their rest
frame magnetic field strength is hundreds of micro-Gauss.
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