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Diffuse X-Ray Emission from M101
The total 0.45-1.0 keV luminosity of M101 is 3.2×1039ergs s-1, of which 2.3×1039 ergss-1 is due to diffuse emission. (Chandra observes only ~60%of the diffuse emission observed by ROSAT because of its superiorpoint-source detection.) Of the diffuse emission seen by Chandra, nomore than 6% can be due to luminous unresolved point sources, such asX-ray binaries, and ~10% is likely due to dwarf stars. The diffuseemission traces the spiral arms and is roughly correlated with theHα and far-UV emission. The radial distribution closely followsthe optical profile. The bulk of the diffuse emission is characterizedby a two-thermal component spectrum with kT=0.20 and 0.75 keV, and theratio of the emission measures of the two components is roughly constantas a function of both radius and surface brightness. The softercomponent has a sufficiently large covering factor that the bulk of theemission is likely extraplanar. We find no evidence of an extendedaxisymmetric X-ray halo, suggesting that any such halo has a strengthmuch smaller than current predictions.
| The H II regions of M101. I - an atlas of 1264 emission regions
A previous survey of the H II regions in M101 (Hodge and Kennicutt) hasbeen extended by a series of CCD images and image tube plates of thegalaxy, approximately tripling the number of known emission regions.This paper provides maps and a catalog of a total of 1264 H II regionsin M101.
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