- The Mid-Life Crisis of the Milky Way and M31
- Simon J. Mutch, Darren J. Croton & Gregory B. Pool
- Centre for Astrophysics and Supercomputing, Swinburne University of Technology
The best analogy given to me describing the study our our galaxy was, “It’s like you’re a blueberry buried deep inside a pancake, and want to understand the global features of the pancake.” Lucky for us, the Milky Way is not the only galaxy in the universe, and so based on what we do know, we can infer the rest based on observations of other galaxies thought to be similar to our own. Despite our disadvantaged position to study the entire galaxy, we know a substantial amount about our own small quadrant; however, we still lack solid estimates of basic comparable properties like star formation rate and color.
The authors are primarily interested in taking existing assumptions about our Milky Way based on previous observations and comparing them to morphological, color, and other characteristics of M31, a large sample of similar galaxies derived from the Galaxy Zoo classification of SDSS galaxies, and a host of galaxies derived from a semi-analytic simulation. The Galaxy Zoo control sample is trimmed to contain galaxies with low redshifts () and . They then only select a sample of Milky Way/M31 analogue galaxies which:
- are spirals
- have stellar masses within
- have an approximate Sb/c morphology (like our Milky Way) based on an SDSS estimator
- are face-on (to minimize the systematic reddening effects of intrinsic interstellar absorption)
The semi-analytic galaxies are chosen to:
- dominate their halo
- have stellar masses within
- posses a bulge-total luminosity ratio of
- be face on (same reason as observations above)
One way to infer a galaxy’s evolutionary stage is through its color. As a galaxy ages, the cold molecular gas used to build new stars is depleted causing star formation to slow. The stellar population will, on average, then grow older and make the galaxy appear redder. In contrast, galaxies with a blue appearance also exhibit recent or ongoing star formation and are thought of as “younger”. These two color classes of galaxies, termed the “red sequence” and the “blue cloud”, are spliced by an underpopulated region in color-magnitude diagrams which are now referred to as “green valley” galaxies (See Galaxy and AGN types and Dissecting a Merger Between a Quasar and a Green Valley Galaxy). The authors find a color for M31 consistent with the green valley, however, the uncertainty on our own Milky Way doesn’t allow for a color classification.
The authors use the Galaxy Zoo sample to find that approximately 1 in 6 local Milky Way type galaxies lie red-ward of the blue cloud. Statistically, this indicates that it is plausible for both the Milky Way and M31 to be green valley galaxies. The semi-analytic data suggests that the Milky Way is 3-5 times more likely to be associated with the green valley than the blue cloud relative to the model population. According to the models, M31 is also more likely to fall in the green valley.
The authors then tackle several explanations for how the Milky Way could be ‘green’. First, they rule out that a redder galaxy implies an earlier formation time based on the distributions of each color regime as a function of redshift. Next, the authors use their models to see that the star formation histories seem to exhibit a more gradual decline rather than a sharp shut-off. The conclusion is that the cold, star forming gas is being depleted. They determine from their models that this is a result of heating from an active supermassive black hole. Both the Milky Way and M31 are not considered to be active galaxies, but observational evidence of ‘bubbles’ far above the disk of our galaxy indicates that the Milky Way may once have hosted an active center.
The main result that both the Milky Way and M31 may be ‘green’ has several implications. One is that they may not be “typical” spirals and instead be in a more transitional phase that is allowed when not harassed or involved in major mergers. The authors also suggest that it may be more common than previously thought for galaxies to first evolve onto the red sequence BEFORE going through a major merger as our own galaxy and M31 are expected to accomplish. This paper provides an alternative view of our galaxy that will be tested more thoroughly when new, high-powered surveys like GAIA and HERMES arrive.