Heath V. Shipley, Casey Papovich, George H. Rieke, Arjun Dey, Buell T. Jannuzi, John Moustakas, Benjamin Weiner
We use Spitzer IRS spectroscopy to study the nature 65 IR-luminous galaxies at 0.02 < z < 0.6 with F(24micron) > 1.2mJy. The IRS spectra cover wavelengths spanning the PAH features and important atomic diagnostic lines. Our sample corresponds to L(IR) = L(8-1000micron) = 10^10-10^12 Lsun. We divide our galaxies into those with Spitzer IRAC colors indicative of warm dust heated by an AGN (IRAGN) and those whose colors indicate star-formation processes (non-IRAGN). Compared to the non-IRAGN, the IRAGN show smaller PAH emission EWs, which we attribute to an increase in mid-IR continuum from the AGN. We find that in both the IRAGN and non-IRAGN samples, the PAH luminosities correlate strongly with the [Ne II] emission, from which we conclude that the PAH luminosity directly traces the instantaneous SFR in both the IRAGN and non-IRAGN galaxies. We compare the ratio of PAH luminosity to the total IR luminosity and show that for most IRAGN star-formation accounts for 10-50% of the L(IR). We also find no measurable difference between the PAH luminosity ratios of L(11.3)/L(7.7) and L(6.2)/L(7.7) for the IRAGN and non-IRAGN, suggesting that AGN do not significantly excite or destroy PAH molecules on galaxy-wide scales. A small subset of galaxies show excess of [O IV] emission compared to their PAH emission, which indicates the presence of heavily-obscured AGN, including 3 galaxies that are not otherwise selected as IRAGN. The low PAH emission and low [Ne II] emission of the IRAGN and [O IV]-excess objects imply they have low SFRs and their IR luminosity is dominated by processes associated with the AGN.
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http://arxiv.org/abs/1304.5231
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