Learning about the Recent Star Formation History of Galaxy Disks by Comparing their Far-Infrared and Radio Morphologies: Cosmic-Ray Electron Diffusion after Star Formation Episodes

Details Learning about the Recent Star Formation History of Galaxy Disks by Comparing their Far-Infrared and Radio Morphologies: Cosmic-Ray Electron Diffusion after Star Formation Episodes Learning about the Recent Star Formation History of Galaxy Disks by Comparing their Far-Infrared and Radio Morphologies: Cosmic-Ray Electron Diffusion after Star Formation Episodes

2008-02-15

arxiv.org/abs/0802.2279v1

Astronomy and Astrophysics

Astrophysics

8 pages, 2 Figures; To appear in the proceeding from "The Evolving ISM in the Milky Way and Nearby Galaxies"

Scientific paper

We present results on the interstellar medium (ISM) properties of 29 galaxies based on a comparison of {\it Spitzer} far-infrared and Westerbork Synthesis Radio Telescope radio continuum imagery. Of these 29 galaxies, 18 are close enough to resolve at $\la$1 kpc scales at 70 $\micron$ and 22 cm. We extend the \citet{ejm06a,ejm06b} approach of smoothing infrared images to approximate cosmic-ray (CR) electron spreading and thus largely reproduce the appearance of radio images. Using a wavelet analysis we decompose each 70 $\micron$ image into one component containing the star-forming {\it structures} and a second one for the diffuse {\it disk}. The components are smoothed separately, and their combination compared to a free-free corrected 22 cm radio image; the scale-lengths are then varied to best match the radio and smoothed infrared images. We find that late-type spirals having high amounts of ongoing star formation benefit most from the two-component method. We also find that the disk component dominates for galaxies having low star formation activity, whereas the structure component dominates at high star formation activity. We propose that this result arises from an age effect rather than from differences in CR electron diffusion due to varying ISM parameters. The bulk of the CR electron population in actively star-forming galaxies is significantly younger than that in less active galaxies due to recent episodes of enhanced star formation; these galaxies are observed within $\sim10^{8}$ yr since the onset of the most recent star formation episode. The sample irregulars have anomalously low best-fit scale-lengths for their surface brightnesses compared to the rest of the sample spirals which we attribute to enhanced CR electron escape.

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