Understanding star-forming galaxies
The more stars a typical spiral galaxy contains, the faster it makes new ones. Astronomers call this relatively tight correlation the "galaxy main sequence." The main sequence might be due simply to the fact that galaxies with more stars have more of everything, including material for making new stars. Alternatively, the mechanisms making new stars could be more efficient in some galaxies, or it could be some combination of these and other possibilities.
Star formation in spiral galaxies generates copious amounts of ultraviolet light that is absorbed by dust and re-radiated at infrared wavelengths, and infrared space missions have enabled scientists to measure more precisely the infrared emission from warm dust in galaxies. As astronomers probe very distant galaxies in the early universe and are forced to rely on measured fluxes rather than visual morphologies to interpret what is going on there, the main-sequence relationship has become an important tool for tracing when and how the universe generated its stars.
CfA astronomers Alexandros Maragkoudakis, Andreas Zezas, Matthew Ashby, and Steve Willner have recently investigated the galaxy main sequence with 246 star-forming galaxies that span a factor of ten thousand in their stellar masses and star formation rates, systematically exploring the main sequence relationship. They also separately explored discrete regions within these galaxies, including bright knots and circumnuclear regions, to determine whether they also followed a main-sequence-like relationship and if so, whether the correlations were identical or slightly different. Previous authors, for example, had found some clear variations in the correlation between galaxies when grouped by subtype, cosmological age, or other properties.
The CfA astronomers find that even across a wide range of stellar masses, at least for local galaxies the correlation between a galaxy's stellar mass and star formation rate is a tight one. They also find that a similarly close correlation holds within small subregions of galaxies, in particular the regions around the supermassive black hole nuclei.