We compare a very deep X-ray image of M87, at the center of the Virgo Cluster, to high-quality optical images of the low excitation emission-line gas in the same region. There are striking coincidences of detail between the two. We explore the possiblity that this represents a thermal interaction between hot gas at 10^7 K and warm gas at 10^4 K. We find two temperatures are present in the X-ray gas, with the lower more prevelant in the vicinity of the optical filaments. Electron conduction from the hot phase to the cooler one provides a quantitatively acceptable energy source for the optical filaments, and we show additionally that it can do so for the brightest X-ray cluster, Perseus. If operative, conduction in the presence of gas-rich galaxy mergers, may explain the presence of "cool cores" in clusters of galaxies.
@article{arxiv.astro-ph/0402204,
title = {X-ray and Optical Filaments in M87},
author = {William B. Sparks and Megan Donahue and Andres Jordan and Laura Ferrarese and Patrick Cote},
journal= {arXiv preprint arXiv:astro-ph/0402204},
year = {2009}
}