A Deep X-Ray View of the Hot Halo in the Edge-on Spiral Galaxy NGC 891

NGC 891 is a nearby edge-on galaxy that is similar to the Milky Way and has a hot X-ray-emitting halo that could arise from accretion, a galactic fountain, or a combination of the two. The metallicity of the gas can help distinguish between these models, and here we report on results that use 138 ks of archival Chandra data and 92 ks of new XMM-Newton data to measure the temperature and metallicity of the hot halo of the galaxy. We find good fits for a thermal model with kT ~ 0.2 keV and Z ~ 0.1 Z _⊙, and rule out solar metallicity to more than 99% confidence. This result suggests accretion from the intergalactic medium as the origin for the hot halo. However, it is also possible to fit a two-temperature thermal model with solar metallicity where kT ₁ ~ 0.1 keV and kT ₂ ~ 0.25 keV. A consideration of the cooling rate and scale height prefers the single-temperature model. We also find that the cooling rate in the hot gas cannot explain the massive H I halo in the steady state. In addition, a galactic fountain model cannot eject enough mass to account for the H I halo, and we speculate that the neutral halo may be gas from a prior outflow that has since cooled.