![Figure CaptionLeft: SDSS image of Mrk 709 (RGB=zrg), which appears to be a pair of interacting dwarf galaxies. We designate the northern and southern galaxies Mrk 709 N and Mrk 709 S. A logarithmic scaling is used to show extended emission. The white circ Figure CaptionLeft: SDSS image of Mrk 709 (RGB=zrg), which appears to be a pair of interacting dwarf galaxies. We designate the northern and southern galaxies Mrk 709 N and Mrk 709 S. A logarithmic scaling is used to show extended emission. The white circ](/sites/default/files/styles/crop_square_2_2_to_320px/public/images/news/resultados132_143.jpg?itok=ZDZzn5Ly)
The incidence and properties of present-day dwarf galaxies hosting massive black holes (BHs) can provide important constraints on the origin of high-redshift BH seeds. Here we present high-resolution X-ray and radio observations of the low-metallicity, star-forming, dwarf-galaxy system Mrk 709 with the Chandra X-ray Observatory and the Karl G. Jansky Very Large Array (VLA). These data reveal spatially coincident hard X-ray and radio point sources with luminosities suggesting the presence of an accreting massive BH (M BH ∼ 10 5−7 M ⊙). Based on imaging from the Sloan Digital Sky Survey (SDSS)
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