Millimeter mapping at z~1: dust-obscured bulge building and disk growth

Abstract

A randomly chosen star in today's Universe is most likely to live in a galaxy with a stellar mass between that of the Milky Way and Andromeda. Yet it remains uncertain how the structural evolution of these bulge-disk systems proceeded. Most of the unobscured star formation we observe building Andromdeda progenitors at 0.7<z<1.5 occurs in disks, but >90% of their star formation is reprocessed by dust and remains unaccounted for. Here we map 500micron dust continuum emission in an Andromeda progenitor at z=1.25 to probe where it is growing through dust-obscured star formation. Combining resolved dust measurements from the NOEMA interferometer with Hubble Space Telescope Halpha maps and multicolor imaging (including new UV data from the HDUV survey), we find a bulge growing by dust-obscured star formation: while the unobscured star formation is centrally suppressed, the dust continuum is centrally concentrated, filling in the ring-like structures evident in the Halpha and UV emission. Reflecting this, the dust emission is more compact than the optical/UV tracers of star formation with r_e(dust)=3.4kpc, r_e(Halpha)/r_e(dust)=1.4, and r_e(UV)/r_e(dust)=1.8. Crucially, however, the bulge and disk of this galaxy are building simultaneously; although the dust emission is more compact than the rest-optical emission (r_e(optical)/r_e(dust)=1.4), it is somewhat less compact than the stellar mass (r_e(M_*)/r_e(dust)=0.9). Taking the 500micron emission as a tracer of star formation, the expected structural evolution of this galaxy can be accounted for by star formation: it will grow in size by Delta(r_e)/Delta(M_*)~0.3 and central surface density by Delta(Sigma_cen)/Delta(M_*)~0.9. Finally, our observations are consistent with a picture in which merging and disk instabilities drive gas to the center of galaxies, boosting global star formation rates above the main sequence and building bulges.

arXiv commentSubmitted to ApJ, key new result of paper shown in Fig. 2

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