The PAH Emission Deficit In Low-Metallicity Galaxies - A Spitzer View

Details The PAH Emission Deficit In Low-Metallicity Galaxies - A Spitzer View The PAH Emission Deficit In Low-Metallicity Galaxies - A Spitzer View

2005-12-15

arxiv.org/abs/astro-ph/0512404v1

Astrophys.J.641:795-800,2006

Astronomy and Astrophysics

Astrophysics

19 pages, 4 figures, accepted for publication in ApJ

Scientific paper

10.1086/500529

Archival observations of 18 starburst galaxies that span a wide range in metallicity reveal for the first time a correlation between the ratio of emission line fluxes of [FeII] at 26 microns and [NeII] at 12.8 microns and the 7.7 micron PAH strength, with the [FeII]/[NeII] flux ratio decreasing with increasing PAH strength. We also find a strong correlation between the [FeII]/[NeII] flux ratio and the host galaxy metallicity, with the flux ratio decreasing with increasing metallicity. Since [FeII] emission has been linked primarily to supernova shocks, we attribute the high [FeII]/[NeII] ratios in low-metallicity galaxies to enhanced supernova activity. We consider this to be a dominant mechanism for PAH destruction, rather than grain destruction in photoionized regions surrounding young massive stars. We also consider whether the extreme youth of the low-metallicity galaxies is responsible for the lack of PAH emission.

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