A galactic bar is the approximately linear structure of stars and gas that stretches across the inner regions of some galaxies. The bar stretches from one inner spiral arm, across the nuclear region, to an arm on the other side. Found in about half of spiral galaxies, including the Milky Way, bars are thought to funnel large amounts of gas into the nuclear regions, with profound consequences for the region including bursts of star formation and the rapid growth of the supermassive black hole at the center. Quasars, for example, have been suggested as one result of this kind of activity. Eventually, however, feedback from such energetic events (supernovae, for example) terminates the inflow and stalls the black hole’s growth.
How bars and gas inflows form and evolve are not well understood — galaxy mergers are thought to play a role — nor are the physical properties of galactic nuclei that are still actively accumulating gas. A serious difficulty is that dust in the dense material around the nucleus is opaque to optical radiation and, depending in part on the geometry, can obscure observations. Infrared and submillimeter wavelength measurements that can peer through the dust offer the best way forward.
The luminous, barred galaxy ESO 320-G030 is about one hundred and fifty thousand light-years away and shows no signs of having been in a merger, yet this galaxy has a bar nearly sixty thousand light-years long, as well as a second bar about ten times smaller perpendicular to it. This galaxy shows high star formation activity in the nuclear region, but no clear evidence of an active nucleus, perhaps because of the high extinction. The galaxy is also seen with inflowing gas (and evidence of outflows simultaneously), making it a nearby prototype of isolated, rapidly evolving galaxies driven by their bars.
CfA astronomers Eduardo Gonzalez-Alfonso, Matt Ashby, and Howard Smith led a program of far infrared Herschel spectroscopy of this object coupled with ALMA submillimeter observations of the gas. By carefully modeling the shapes of the infrared absorption lines of water and several of its ionized and isotopic variations, with fifteen other molecular species including ammonia, OH and NH, they conclude that a nuclear starburst of about twenty solar-masses of stars per year is being sustained by gas inflow with short (twenty million year) lifetime.
They find evidence for three structural components: an envelope about five hundred light-years across, a dense circumnuclear disk about one hundred twenty light-years in radius, and a compact core or torus forty light-years in size and characterized by its very warm dust. These three components are responsible for about 70% of the galaxy’s luminosity.
Although ESO 320-G030 is an exceptional example, being both bright and nearby, the results suggest that similar complex nuclear structures, with inflows and outflows, may be common in luminous galaxies in the more distant universe including those during its most active epoch of star formation.
Reference: “A proto-pseudobulge in ESO 320-G030 fed by a massive molecular inflow driven by a nuclear bar” by E. González-Alfonso, M. Pereira-Santaella, J. Fischer, S. García-Burillo, C. Yang, A. Alonso-Herrero, L. Colina, M. L. N. Ashby, H. A. Smith, F. Rico-Villas, J. Martín-Pintado, S. Cazzoli and K. P. Stewart, Accepted 27 October 2020, Astronomy & Astrophysics.