13 October, 2016Scientific Paper
A joint team of University of Tokyo researchers and their collaborators, using the Atacama Large Millimeter/submillimeter Array (ALMA) and other telescopes that utilize radio waves for space observation, revealed that dense molecular gas disks a few hundred light-years in scale located at the centers of galaxies supply gas to supermassive black holes situated within them. This finding provides important insights on the growth of supermassive black holes over cosmic time.
Supermassive black holes more than a million times the mass of our sun exist at the centers of many galaxies, but how they came to be is unclear. Meanwhile, a correlation between the rate at which stars form in the central regions of galaxies and the amount of gas that falls into supermassive black holes (mass accretion rate) was known to exist, leading some scientists to suggest that the activity involved in star formation fuels the growth of black holes.
The joint research team led by graduate student and JSPS fellow Takuma Izumi at the Graduate School of Science at the University of Tokyo revealed for the first time—with observational data collected by ALMA in Chile, and other telescopes—that dense molecular gas disks occupying regions as large as a few light-years at the centers of galaxies are supplying gas directly to the supermassive black holes.
The team also succeeded in explaining, with a theoretical model, that the actual changes (balance of inflow and outflow) in gas levels they observed were the result of the increasing amount of gas falling into the supermassive black holes within the gas disks enhanced by strong turbulence generated by supernova explosions (an activity associated with star formation) when a star inside the dense gas disks dies.
“The central regions of faraway galaxies, comprising a few light-years in scale, are hard to observe in detail because of their compactness, and there haven’t been many studies showing how black holes grow due to the lack of extensive research. So, this outcome is a big step forward as we successfully revealed one aspect of that process,” says Izumi. He continues, “We hope to expand our research to farther expanses of the universe by utilizing the superb capability of ALMA to help us understand comprehensively the growth of supermassive black holes over cosmic time.”
These observation results were published as Izumi et al. “Do Circumnuclear Dense Gas Disks Drive Mass Accretion onto Supermassive Black Holes?” in the Astrophysical Journal Letters, issued in August 2016.
The research team members are: Takuma Izumi (The University of Tokyo), Nozomu Kawakatu (National Institute of Technology, Kure College), and Kotaro Kohno (The University of Tokyo).
The Atacama Large Millimeter/submillimeter Array (ALMA), an international astronomy facility, is a partnership of the European Organisation for Astronomical Research in the Southern Hemisphere (ESO), the U.S. National Science Foundation (NSF) and the National Institutes of Natural Sciences (NINS) of Japan in cooperation with the Republic of Chile. ALMA is funded by ESO on behalf of its Member States, by NSF in cooperation with the National Research Council of Canada (NRC) and the National Science Council of Taiwan (NSC) and by NINS in cooperation with the Academia Sinica (AS) in Taiwan and the Korea Astronomy and Space Science Institute (KASI).
ALMA construction and operations are led by ESO on behalf of its Member States; by the National Radio Astronomy Observatory (NRAO), managed by Associated Universities, Inc. (AUI), on behalf of North America; and by the National Astronomical Observatory of Japan (NAOJ) on behalf of East Asia. The Joint ALMA Observatory (JAO) provides the unified leadership and management of the construction, commissioning and operation of ALMA.
The University of Tokyo