Very compact millimeter sizes for composite star-forming/AGN submillimeter galaxies

Abstract

We report the study of far-IR sizes of submillimeter galaxies (SMGs) in relation to their dust-obscured star formation rate (SFR) and active galactic nuclei (AGN) presence, determined using mid-IR photometry. We determined the millimeter-wave (${\lambda }_{\mathrm{obs}}=1100\mu$m) sizes of 69 ALMA-identified SMGs, selected with $\ge 10$$\sigma$ confidence on ALMA images ($F_{1100\mu \mathrm{m}}=1.7$--7.4 mJy). We found that all the SMGs are located above an avoidance region in the millimeter size-flux plane, as expected by the Eddington limit for star formation. In order to understand what drives the different millimeter-wave sizes in SMGs, we investigated the relation between millimeter-wave size and AGN fraction for 25 of our SMGs at $z=1$--3. We found that the SMGs for which the mid-IR emission is dominated by star formation or AGN have extended millimeter-sizes, with respective median $R_{\mathrm{c},\mathrm{e}}=1.6_{-0.21}^{+0.34}$ and 1.5${}_{-0.24}^{+0.93}$ kpc. Instead, the SMGs for which the mid-IR emission corresponds to star-forming/AGN composites have more compact millimeter-wave sizes, with median $R_{\mathrm{c},\mathrm{e}}=1.0_{-0.20}^{+0.20}$ kpc. The relation between millimeter-wave size and AGN fraction suggests that this size may be related to the evolutionary stage of the SMG. The very compact sizes for composite star-forming/AGN systems could be explained by supermassive black holes growing rapidly during the SMG coalescing, star-formation phase.

9 pages, 4 figures, 1 table. Accepted for publication in ApJ Letter

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