Survey of Fine-Scale Structure in the Far-Infrared Milky Way

Details Survey of Fine-Scale Structure in the Far-Infrared Milky Way Survey of Fine-Scale Structure in the Far-Infrared Milky Way

1996-12-27

arxiv.org/abs/astro-ph/9612233v1

Astronomy and Astrophysics

Astrophysics

Paper format (LaTeX); length of paper (3); 1 encapsulated postscript figure file; 1 gif color plate file; uses style file crck

Scientific paper

Using the IRAS Infrared Sky Survey Atlas, we have made 60 x 60 deg mosaics of the far-infrared emission in the Milky Way. By applying a median normalizing spatial filter, we were able to eliminate the strong gradient in brightness towards the Galactic midplane. The resulting images reveal a "froth" of superposed filaments, voids, and shells. This fine-scale structure extends all the way down to the Galactic midplane. Moreover, it scales in intensity with the smoothly varying background, independent of latitude, thus indicating that the fine-scale residual emission is co-extensive with the smooth background. We conclude that the fine-scale structure is not merely of local origin, but consists of both nearby and more distant features in the disk. Although we had expected to find morphological evidence for supernova-driven "worms" or "chimneys" rooted in the Galactic plane, our processing shows the FIR fine-scale structure to be more complex (e.g. less coherent and less rooted) as viewed in projection. Analysis of the spatial statistics shows that the FIR fine-scale structure is self-similar with a spatial power-law exponent of -3 and a fractal dimension of 2.5 --- similar behavior to that found in isolated cirrus and molecular clouds. On scales larger than 1.5 deg, the power-law exponent flattens to -2.5, perhaps indicating a change in the characteristic structure. This could be due to different dynamical inputs organizing the small and large-scale structures (e.g. turbulence and diffusion on small scales vs. macroscopic winds and shock fronts on larger scales).

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