In this picture, a combined optical (Maurogordato et al.), X-ray (Sauvageot et al.) and radio (Ferrari et al.) analysis of a sample of nearby clusters (z ∼0.09), covering all the main phases of the collision process, has been undertaken.
Star formation in the merging galaxy cluster Abell 3921
As already mentioned in the introduction, a number of observational facts from X –ray data point against the simple self–similar picture.
Thermodynamical properties of the ICM from hydrodynamical simulations
In conclusion, whereas indirect evidence of ion acceleration exists in X rays from the modiﬁed shock thermodynamics, no clear picture has emerged yet from the beautiful γ-ray images of shell supernova remnants.
The Galactic gamma-ray club
Within this picture, the agreement with the Vink et al. predictions for early O dwarfs may be understood, since their winds are not seriously affected by X-rays.
Analysis of Galactic late-type O dwarfs: more constraints on the weak wind problem
The different X-ray morphology could be related, in this picture, to the short cooling time of X-ray emitting electrons.
Detection of an X-ray jet in 3C 371 with Chandra
Much like for the ICM, the suppressed X –ray emission is consistent with the picture of non– gravitational heating placing the gas on a higher adiabat, and preventing it from reaching high densities within large–scale ﬁlamentary structures.
Summary: Clusters of Galaxies and the High Redshift Universe Observed in X-Rays
Thus we can imagine that the UV absorbers are embedded in the X-ray gas. A similar picture is emerging from the handful of other AGN which have been studied simultaneously in the UV and X-ray band (e.g.
New Chandra/HST-STIS results on Seyfert I AGN: Photoionized Outflows
This picture ﬁts nicely with the cooling thermal components observed during these X-ray tails.
An Extended Burst Tail from SGR 1900+14 with a Thermal X-ray Spectrum
The X-ray total intensity and temperature imaging add to the already complicated picture.
The Cluster of Galaxies Surrounding Cygnus A II: New Velocities and a Dynamical Model
These studies, combined with optical and X-ray studies, yield arguably the most detailed picture of the galactic nuclei.
Extragalactic Relativistic Jets and Nuclear Regions in Galaxies
In Elitzur’s theoretical picture the dominant X-ray absorber, along with the BLR, is identiﬁed with the dust-free inner part of a wind emanating from the accretion disk.
Conference Summary: The Central Engine of Active Galactic Nuclei
The occurrence of the X-ray spike on the limb of the secondary at the same orbit phase in sequential eclipses is consistent with the conventional picture of synchronous rotation as suggested by a number of investigations (e.g., Verbunt & Phinney 1995).
Possible Magnetic Activity in the Low Mass X-ray Binary EXO 0748-676
This, together with the tight X-ray/TeV correlation, lends strong support to the the picture that, in BL Lacs at least, we are seeing SSC emission (with the synchrotron component dominating at X-ray energies and below, and the Compton component dominating at gamma-ray energies).
Workshop Summary for Cracow 1997: Relativistic Jets in AGNs
An alternative picture would be to explain all the BHC X-ray emission as coronal and the optical/UV excess as from a truncated outer disk.
Coronal X-Ray Emission from the Stellar Companions to Transiently Accreting Black Holes
In particular the relationship between the X-ray and UV absorbers has presented considerable problems for formulating a consistent picture of the inner nucleus in active galaxies.
X-ray spectroscopy of NGC 5548