Rutgers University Department of Physics and Astronomy

2005-06 Handbook for Physics and Astronomy Graduate Students

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Research Programs


The astrophysics group at Rutgers has grown in stature in recent years, achieving parity with other world-class astronomy programs and joining AURA, the Association of Universities for Research in Astronomy. Some research highlights are: The observers and theorists in the group interact closely, and many recent student theses have included both theoretical and observational projects. Most theoretical research is heavily computational, and dynamics often involves N-body simulations. There are also links to the particle-astrophysics interests of the New High Energy Theory Center.

Our observations are carried out in all regions of the spectrum, including X-ray, ultraviolet, optical, and radio wavelengths. Data are obtained using both ground-based telescopes and space observatories. The imaging Fabry-Perot interferometer resides at the Cerro-Tololo Inter-American Observatory in Chile. We have a network of Sun and alpha workstations for the analysis of astronomical observations and for theoretical numerical computations. Data from a wide variety of sources can be processed, enhanced, and viewed using most major astronomy software packages, such as IRAF, STSDAS, DAOPHOT, IDL, and AIPS. There are also opportunities for instrument development for both space- and ground-based telescopes, including for SALT.

Graduate students who intend to carry out thesis work in astrophysics are encouraged to follow the astronomy option, which allows them to replace several of their upper division course requirements with astrophysics courses.

Professor Thomas Devlin

I am working on projects directed at studying the large-scale structure of the universe. One is to use the fully-steerable 100-meter radio telescope in Greenbank, W.Va., to measure the polarization of 30 GHz radiation from galaxies. This is a potential foreground source which must be understood to correct future measurements of polarization in Cosmic Microwave Background (CMB). Another project is participation in a multi-university collaboration building ACT, a 6-meter microwave telescope to be operated on the Atacama Plateau in Chile. This instrument will study CMB and dark matter distributions in Galaxy clusters at several frequencies with very high resolution.

Professor John P. Hughes

I study the X-ray properties and Sunyaev-Zel'dovich effect of clusters of galaxies in order to measure the expansion factor of the Universe, the so-called Hubble constant. This research also aims at understanding the origin, evolution, and nature of these systems, which are the largest dynamically organized structures known. My research interests also include observational and theoretical studies of supernova remnants as probes of stellar and explosive nucleosynthesis, the nature of the interstellar medium, the physics of supersonic shock waves, and the formation and evolution of instabilities in supernova ejecta. I also am involved in the planning and development of new X-ray satellite missions including AXAF and Astro-E.

Professor Charles Joseph

My research interests include the interstellar medium, studies of the origin and evolution of galaxies, and technology development for optical/ultraviolet space instrumentation. I will be collecting and analyzing data taken with the Primary-Focus Instrument on the SALT telescope, which will be commissioned in November 2005. New technology initiatives include the development of ultraviolet detectors made of III-Nitrides, which offer significant performance improvements over existing UV image sensors. I and a team of internationally recognized astronomers will be proposing to NASA to build, fly, and operate a series of long-duration balloon flights. The balloon-borne telescope will have a floatation altitude of 35 km (19 miles) and will provide spatial resolutions comparable to the Hubble Space Telescope. Typical flights are expected to last 2-3 weeks and be flown once per year. We will use this series of balloon missions to perform detailed velocity maps over wide fields of view to determine the formation and evolution of galaxies.

Professor Charles Keeton

I use gravitational lensing to study galaxies and cosmology. Strong lens systems provide the only direct probe of dark matter distributions on subgalactic scales, and therefore provide crucial constraints on the fundamental nature of dark matter. The connection between lenses and their environments offers clues about the processes that drive galaxy evolution. Lenses act as natural telescopes that help us to resolve the internal structure of quasars. They are beginning to let us measure supermassive black holes in distant galaxies. In the future, lensing will provide precise tests of general relativity and alternative gravity theories. My work involves a broad array of research methods, from observations (including HST and SALT) to data modeling to numerical theory to formal mathematics.

Professor Terry Matilsky

Most recently, I have become interested in fundamental theories of gravitation. It appears that all of the standard "dark matter" scenarios are significantly flawed, and recent work in string theory has pointed us toward modification of our current ideas concerning gravitational dynamics. I have examined a new idea that postulates an additional interaction in four spatial dimensions that has the potential to solve the dark matter problem, as well as address some fundamental questions in both cosmology and high-energy physics. The most up-to-date paper concerning this can be found at: by clicking on "gravity".

Professor Carlton Pryor

My research interests are centered on observational and theoretical studies of the structure and evolution of both star clusters and individual galaxies. I am currently surveying the kinematics, mass distributions, and stellar contents of the dense centers of globular star clusters, the oldest clusters in our Galaxy. With the Rutgers Imaging Fabry-Perot Spectrometer in Chile, we have been able to increase the kinematical data in these regions by an order of magnitude, thus providing a much clearer picture of some of the most extreme stellar environments known. I am also studying the spatial distribution of dark matter in the dwarf spheroidal companions of our Galaxy in an attempt to determine what the dark matter is.

Professor Jerry Sellwood

My main interest is in the formation and evolution of galaxies. In particular, I try to understand the dynamics of these large stellar systems and to determine the amount and distribution of Dark Matter within them. My findings is challenge predictions from the current Cold Dark Matter model of the universe. Other interests include such questions as: What causes the graceful spiral patterns seen in most disc galaxies? And why do many, but not all, have bars? Although analytical methods can be used to some extent, I find that the most fruitful line of attack on these questions is through large N-body simulations.

Professor Ted Williams

My interests include optical observations of extragalactic objects and instrument development. One current project involves the measurement of the kinematics of both stars and gas in barred spiral galaxies, in order to determine the structure and dynamics of these galaxies. Other active research involves measuring the velocities of stars in the dense cores of globular clusters, detecting and measuring the velocities of planetary nebula surrounding elliptical galaxies, and refining the Tully-Fisher technique for measuring the distances to galaxies.

Professor Harry Zapolsky

I am currently studying the physics of gravitational collapse. My interest is specifically in astrophysical systems (young globular clusters and elliptical galaxies) in which the dynamics of the constituent stars is essentially collisionless, so that the system is not constrained to evolve towards the Boltzmann distribution. Questions of fundamental physical significance include the nature and uniqueness of the ultimate steady state distribution produced by "violent relaxation" during the collapse, and how such systems manage to acquire (approximate) constants of motion.

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Revised July, 2005