Probing the Excitation of Extreme Starbursts: High Resolution Mid-IR Spectroscopy of Blue Compact Dwarfs

Abstract

We present an analysis of the mid-infrared emission lines for a sample of 12 low metallicity Blue Compact Dwarf (BCD) galaxies based on high resolution observations obtained with Infrared Spectrograph on board the {\rm Spitzer} Space Telescope. We compare our sample with a local sample of typical starburst galaxies and active galactic nuclei (AGNs), to study the ionization field of starbursts over a broad range of physical parameters and examine its difference from the one produced by AGN. The high-ionization line [OIV]25.89$\hat{I}¼$m is detected in most of the BCDs, starbursts, and AGNs in our sample. We propose a diagnostic diagram of the line ratios [OIV]25.89$\hat{I}¼$m/[SIII]33.48$\hat{I}¼$m as a function of [NeIII]15.56$\hat{I}¼$m/[NeII]12.81$\hat{I}¼$m which can be useful in identifying the principal excitation mechanism in a galaxy. Galaxies in this diagram split naturally into two branches. Classic AGNs as well as starburst galaxies with an AGN component populate the upper branch, with stronger AGNs displaying higher [NeIII]/[NeII] ratios. BCDs and pure starbursts are located in the lower branch. We find that overall the placement of galaxies on this diagram correlates well with their corresponding locations in the log([NII]/H$\hat{I}\pm$) vs. log([OIII]/H${\hat{I}}^2$) diagnostic diagram, which has been widely used in the optical. The two diagrams provide consistent classifications of the excitation mechanism in a galaxy. On the other hand, the diagram of [NeIII]15.56$\hat{I}¼$m/[NeII]12.81$\hat{I}¼$m vs. [SIV]10.51$\hat{I}¼$m/[SIII]18.71$\hat{I}¼$m is not as efficient in separating AGNs from BCDs and pure starbursts. (abridged)

15 pages, including 1 table and 14 figures. Accepted by ApJ