The shapes of galaxies

The shapes of galaxies
An image of the colliding galaxies NGC4676, "The Mice," as seen by Hubble. An analysis of eighteen thousand colliding galaxies in the computer simulation Illustris has found that mergers like this one are the dominant mechanism determining the shape of galaxies more massive than the Milky Way, while for lower mass galaxies mergers do not play a significant role. Credit: NASA/HST

Since Edwin Hubble proposed his galaxy classification scheme in 1926, numerous studies have investigated the physical mechanisms responsible for the shapes of spiral and elliptical galaxies. Because the processes are complex, however, studies frequently rely on computer simulations as their main tool. The discs of galaxies are believed to form through the collapse of gas which acquires its initial spin in the early Universe. During their subsequent evolution, galaxies undergo a wide range of phenomena, from the accretion of matter—or its outflow—to mergers with other galaxies, all of which modify the disk's spin and angular momentum.

Astronomers think that spiral with the largest galactic discs formed preferentially in protogalaxies with the highest , although early attempts to verify this prediction using computer simulations failed. (More recently, simulations have been able to verify this trend.) Elliptical galaxies, on the other hand, are believed to be the remnants of repeated , but their shapes depend on many details like the galaxies' masses, gas content, and the collision parameters. As a result, these mergers need to be considered over a cumulative, cosmological context with large numbers of examples to evaluate their development from a statistical perspective.

CfA astronomers Vicente Rodriguez-Gomez, Annalisa Pillepich and Lars Hernquist led a team that analyzed the morphologies of about eighteen thousand galaxies in the Illustris computer simulation. Both disc and spheroidal galaxies arise naturally in this simulation. They find that massive merging galaxies develop into spirals or spheroidal shapes depending on their gas content (as expected, since the star formation activity depends crucially on the gas). Unexpectedly, they find that for lower mass galaxies—roughly the mass of the Milky Way or smaller—mergers do not seem to play a significant role in determining the morphology. The reason appears to be that in higher mass mergers a galaxy accretes many more stars from the partner, and this plays the a critical role. Their significant conclusion is that only in are mergers the dominant factor in shaping the system.

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More information: Vicente Rodriguez-Gomez et al. The role of mergers and halo spin in shaping galaxy morphology, Monthly Notices of the Royal Astronomical Society (2017). DOI: 10.1093/mnras/stx305
Citation: The shapes of galaxies (2017, June 26) retrieved 26 May 2019 from
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Jun 26, 2017
An open access copy of the paper can be found here:

Jul 02, 2017
Stacy McGaugh and Federico Lelli say: "If you measure the distribution of starlight, you know the galaxy rotation curve, and vice versa." (McGaugh, 2016). There must be "One law to rule them all." Lelli, 2017.

Hard to discern any connection between the above Harvard CfA research (18,000 galaxies) and the McGaugh and Lelli work, which covers about 400 galaxies (153, then 240 more in a related article) and more than 3,000 data points. Both deal with aspects of galaxy morphology.

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