Austin Napier introduces center for scientific visualization

Welcome to the Department of Physics and Astronomy at Tufts University! Our nineteen faculty, approximately 30 graduate students, and around 50 undergraduates come from all over the globe to participate in and learn about research that is exploring the physical world on a range of scales. Students in our Physics and Astronomy program:

  • work on particle physics experiments at CERN and Fermilab,
  • develop new understandings of condensed matter (including soft matter and biological systems)
  • carry out pioneering work on galactic evolution,
  • study quantum computation and physics education,
  • and explore fundamental questions about the cosmos.

Our deep engagement with research informs much of the teaching that takes place here. In addition to our core set of physics courses, we help students develop their skills in instrumentation, computation, data analysis, and oral and written communication. We encourage them to see the physics in the real world, and to explore connections with other disciplines. These are all skills that are valuable in a wide range of careers and are attractive to employers. Moreover, many of our majors participate in research, and the ability to work collaboratively on cutting-edge research provides a deep and transformative learning experience for many students.

As scientists, we look to the coming years with a sense of excitement. The scientific questions we face — dark energy, dark matter, the search for a fundamental theory 'beyond the standard model', developing a deeper understanding of biophysical systems such as the brain — have the potential to revolutionize our understanding of the cosmos and our role in it. We welcome you to visit to hear more about the research and teaching that we are engaged in here at Tufts!

Department Chair

faculty photo

Danilo Marchesini

Astronomy; galaxy formation and evolution; extra-galactic surveys; active galactic nuclei; near-infrared astronomy Understanding how galaxies form and evolve means understanding how the tiny differences in the distribution of matter inferred from the cosmic microwave background radiation grew and evolved into the galaxies we see today. The working hypothesis is that galaxies form under the influence of gravity, and galaxy formation can be seen as a two-step process. First, the gravity of dark matter causes the tiny seeds in the matter distribution to grow bigger with time. As they grow more massive, the gravitational attraction becomes stronger, making it easier for these structures to attract additional matter. As the dark matter structures grow, they pull in also the gas, made of hydrogen and helium, which is the primary ingredient for the formation of stars, and hence for the formation of the stellar content of galaxies. The formation of the stellar content inside these dark matter structures involves many physical processes that are much more complicated and quite poorly understood from a theoretical perspective. These physical processes include, for example, how gas cools and collapses to form stars, the process of star formation itself, merging of galaxies, feedback from star formation and from active super-massive black holes. My research activity in the past decade has focused on understanding how galaxies formed after the Big Bang, and how their properties (e.g., the stellar mass, the level of star formation activity, the morphology and structural parameters, the level of activity of the hosted super-massive black hole, etc.) have changed as a function of cosmic time. Since we cannot follow the same galaxy evolving in time, we need to connect the galaxies we observe at a certain redshift (i.e. a certain snapshot in time) to those we observe at a smaller redshift (i.e., at a later time in cosmic history) in order to infer how the properties of galaxies have actually changed and what physical mechanisms are responsible for these changes. The better we understand the galaxy properties at a certain time and the more finely in time we can probe the cosmic history, the easier it becomes to connect galaxies' populations seen at different snapshots in time, linking progenitors and descendants across cosmic time. Ultimately, my research aims at understanding what galaxy population seen at one epoch will evolve into at a later epoch, and what physical processes are responsible for the inferred changes in the galaxies' properties. In order to do this, I have adopted two different but complementary approaches. The first approach consists of statistical studies of the galaxy populations at different cosmic times; the second approach consists of detailed studies of individual galaxies to robustly derive their properties.