Stacy McGaugh

Who is Stacy McGaugh?

Stacy McGaugh is an American astronomer and professor in the Department of Astronomy at Case Western Reserve University in Cleveland, Ohio. His fields of specialty include low surface brightness galaxies, galaxy formation and evolution, tests of dark matter and alternative hypotheses, and measurements of cosmological parameters.

Stacy McGaugh was an undergraduate student at MIT and a graduate student at Princeton and the University of Michigan. He held postdoctoral appointments at Cambridge University, the Carnegie Institution of Washington, and Rutgers University before joining the faculty of the University of Maryland in 1998. He moved to Case Western in 2012. He is married with two children. During his tenure at the University of Maryland he was an example of the academic two body problem, commuting between Maryland and Cleveland on a weekly basis for over a decade. He is a Distinguished Alumnus of Flint Northern High School and of the Astronomy Department of the University of Michigan.

Known in the field of extragalactic astronomy for his early work on Low Surface Brightness Galaxies and the elemental abundances in HII Regions, McGaugh has also contributed to the study of the kinematics of galaxies, being among the first to point out that low surface brightness galaxies are dark matter dominated and that they pose the cuspy halo problem. He also coined the expression "baryonic Tully–Fisher relation." He is the only scientist to correctly predict a priori the first to second peak amplitude ratio of the acoustic power spectrum of the Cosmic microwave background radiation. McGaugh found surprising support for the Modified Newtonian dynamics proposed by Mordehai Milgrom as an alternative to Dark matter in his work on Low Surface Brightness Galaxies. This has proven to be very controversial since it implies the non-existence of the non-baryonic dark matter that is central to physical cosmology. Nevertheless, his predictions for the mass distribution of the Milky Way and the velocity dispersions of the dwarf Spheroidal satellites of the Andromeda spiral galaxy have largely been confirmed by subsequent observations.