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The incidence and properties of present-day dwarf galaxies hosting massiveblack holes (BHs) can provide important constraints on the origin ofhigh-redshift BH seeds. Here we present high-resolution X-ray and radioobservations of the low-metallicity, star-forming, dwarf-galaxy system Mrk 709with the Chandra X-ray Observatory and the Karl G. Jansky Very Large Array.These data reveal spatially coincident hard X-ray and radio point sources withluminosities suggesting the presence of an accreting massive BH (M_BH ~10^5-10^7 Msun). Based on imaging from the Sloan Digital Sky Survey (SDSS), wefind that Mrk 709 consists of a pair of compact dwarf galaxies that appear tobe interacting with one another. The position of the candidate massive BH isconsistent with the optical center of the southern galaxy (Mrk 709 S), while noevidence for an active BH is seen in the northern galaxy (Mrk 709 N). We derivestellar masses of M ~ 2.5 x 10^9 Msun and M ~ 1.1 x 10^9 Msun for Mrk 709 S andMrk 709 N, respectively, and present an analysis of the SDSS spectrum of theBH-host Mrk 709 S. At a metallicity of just ~10% solar, Mrk 709 is among themost metal-poor galaxies with evidence for an active galactic nucleus.Moreover, this discovery adds to the growing body of evidence that massive BHscan form in dwarf galaxies and that deep, high-resolution X-ray and radioobservations are ideally suited to reveal accreting massive BHs hidden atoptical wavelengths.

A Candidate Massive Black Hole in the Low-metallicity Dwarf Galaxy Pair Mrk 709