A parsec-scale radio jet launched by the central intermediate-mass black hole in the dwarf galaxy SDSS J090613.77+561015.2?. (arXiv:2003.11412v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Yang_J/0/1/0/all/0/1">Jun Yang</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Gurvits_L/0/1/0/all/0/1">Leonid I. Gurvits</a> (2, 3 and 4), <a href="http://arxiv.org/find/astro-ph/1/au:+Paragi_Z/0/1/0/all/0/1">Zsolt Paragi</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Frey_S/0/1/0/all/0/1">Sandor Frey</a> (5, 6), <a href="http://arxiv.org/find/astro-ph/1/au:+Conway_J/0/1/0/all/0/1">John E. Conway</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_X/0/1/0/all/0/1">Xiang Liu</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Cui_L/0/1/0/all/0/1">Lang Cui</a> (7) ((1) Chalmers University of Technology, Sweden, (2) JIVE, Netherlands, (3) Delft University of Technology, Netherlands, (4) CSIRO Astronomy and Space Science, Australia, (5) Konkoly Observatory, Hungary, (6) ELTE Eötvös Loránd University, Hungary, (7) Xinjiang Astronomical Observatory, China)
The population of intermediate-mass black holes (IMBHs) in nearby dwarf
galaxies plays an important “ground truth” role in exploring black hole
formation and growth in the early Universe. In the dwarf elliptical galaxy SDSS
J090613.77+561015.2 (z=0.0465), an accreting IMBH has been revealed by optical
and X-ray observations. Aiming to search for possible radio core and jet
associated with the IMBH, we carried out very long baseline interferometry
(VLBI) observations with the European VLBI Network (EVN) at 1.66 GHz. Our
imaging results show that there are two 1-mJy components with a separation of
about 52 mas (projected distance 47 pc) and the more compact component is
located within the 1-sigma error circle of the optical centroid from available
Gaia astrometry. Based on their positions, elongated structures and relatively
high brightness temperatures, as well as the absence of star-forming activity
in the host galaxy, we argue that the radio morphology originates from the jet
activity powered by the central IMBH. The existence of the large-scale jet
implies that violent jet activity might occur in the early epochs of black hole
growth and thus help to regulate the co-evolution of black holes and galaxies.
The population of intermediate-mass black holes (IMBHs) in nearby dwarf
galaxies plays an important “ground truth” role in exploring black hole
formation and growth in the early Universe. In the dwarf elliptical galaxy SDSS
J090613.77+561015.2 (z=0.0465), an accreting IMBH has been revealed by optical
and X-ray observations. Aiming to search for possible radio core and jet
associated with the IMBH, we carried out very long baseline interferometry
(VLBI) observations with the European VLBI Network (EVN) at 1.66 GHz. Our
imaging results show that there are two 1-mJy components with a separation of
about 52 mas (projected distance 47 pc) and the more compact component is
located within the 1-sigma error circle of the optical centroid from available
Gaia astrometry. Based on their positions, elongated structures and relatively
high brightness temperatures, as well as the absence of star-forming activity
in the host galaxy, we argue that the radio morphology originates from the jet
activity powered by the central IMBH. The existence of the large-scale jet
implies that violent jet activity might occur in the early epochs of black hole
growth and thus help to regulate the co-evolution of black holes and galaxies.
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