Physics & Astronomy Colloquium

Higgs Discovery: Implications for Particle Physics - 2 Nov. 2012

The LHC has recently discovered a Higgs-like resonance with a mass of about 125 GeV. It may be the missing element of the so-called Standard Model of particle physics. This model was proposed a few decades ago, and, after the inclusion of neutrino masses, describes in an accurate way all measured observables not involving gravity. We shall discuss what are the possible implications of the Higgs Discovery for particle physics and, in particular, for theoretical and experimental physics High Energy Physics in the coming years.

From Voids to Clusters: Gas and Galaxy Evolution in the Local Universe - 12 Oct. 2012

Our understanding of the formation and evolution of galaxies and their large scale structure has advanced enormously over the last decade, thanks to an impressive synergy between theoretical and observational efforts. While the growth of the dark matter component seems well understood, the physics of the gas, during its accretion, removal and/or depletion is less well understood. Increasingly large scale optical surveys are tracing out the cosmic web of filaments and voids. Mathematical tools have been developed to describe these structures and to identify galaxies located in specific environments. HI imaging surveys begin to answer the question: how do galaxies get and lose their gas? The best evidence for ongoing gas accretion is found in the lowest density environments, while removal of gas in the highest density environments stops star formation and reddens the galaxies. Speaker: Jacquiline van Gorkom, Columbia University

From Voids to Clusters: Gas and Galaxy Evolution in the Local Universe

Our understanding of the formation and evolution of galaxies and their large scale structure has advanced enormously over the last decade, thanks to an impressive synergy between theoretical and observational efforts. While the growth of the dark matter component seems well understood, the physics of the gas, during its accretion, removal and/or depletion is less well understood. Increasingly large scale optical surveys are tracing out the cosmic web of filaments and voids. Mathematical tools have been developed to describe these structures and to identify galaxies located in specific environments. HI imaging surveys begin to answer the question: how do galaxies get and lose their gas? The best evidence for ongoing gas accretion is found in the lowest density environments, while removal of gas in the highest density environments stops star formation and reddens the galaxies. Speaker: Jacquiline van Gorkom, Columbia University

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