Michele Cappellari Homepage

Voronoi 2D-Binning
Voronoi binning (4 colors)
E-mail: e-mail Michele
Postal Address:
JAM
JAM modelling
Sub-Department of Astrophysics
University of Oxford
Denys Wilkinson Building
Keble Road
OXFORD
OX1 3RH
ENGLAND
Office: 755 (top floor)
Tel: +44-1865-273-647
FAX: +44-1865-273-390
Web Address: http://purl.org/cappellari
Synthetic CV: I obtained my Ph.D. in astrophysics at the University of Padova. I was awarded a VENI Fellowhsip by NWO at the University of Leiden. I arrived at the University of Oxford with an Advanced Fellowship of STFC and now have a permanent position currently supported by a University Research Fellowship of The Royal Society.

Current Interests

elliptical galaxy
Figure 1: A grown-up elliptical galaxy in the early Universe. Read a description of the result in the press release from the University of Oxford.
Cappellari et al. (2012)
Figure 2: Differentiating between the stellar and dark matter with integral field stellar kinematics and JAM dynamical models. This analisys allowed us to discover a systematic variation of the stellar Initial Mass Function in early-type galaxies. Read about this finding in our Nature Letter or in some news coverage about it.
Cappellari et al. (2011)
Figure 3: Replacing the handle of Hubble's tuning fork. Read about the discovery behind the proposed change in our paper or in some news coverage of our finding.
Cappellari et al. (2004)
Figure 4: Schematic representation of Schwarzschild's numerical orbital-superposition dynamical modelling method. The figure was adapted from here, where a detailed explanation is given.

Formation and evolution of galaxies: Observations at high redshift, combined with detailed measurements of the cosmic microwave background (e.g. Spergel et al. 2007), have provided a scenario for galaxy formation in which the Universe is dominated by dark matter of unknown nature. The general scenario for the assembly of the dark matter seems to be rather well understood as it can be described by a hierarchical process driven by the sole influence of gravity (e.g. Springel et al. 2005). Much however still has to be learnt about the way the luminous matter, namely the stars and galaxies that we actually observe, form from the accretion of gas within the dark matter potential. The complication comes from the fact that these processes are driven by the hydrodynamic and chemistry of the gas, combined with complex feedback processes of the radiation on it.

In my work I am trying to understand how the galaxies were assembled using two complementary approaches. I am observing nearby objects, that can be analyzed in detail due to their vicinity, which contain the fossil record of billions of years of evolution. And I am observing the distant galaxies whose light reaches us after billions of years of travel through space. For this reason we can see them as they were when the Universe was young and the galaxies were still forming. My recent work has progressed along the following lines of reasearch:

Publications

Software

Old pages

Historic research pages and my Ph.D. thesis are still available here.
Last modified: 16/APR/2014

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