The Illustris++ Project: The Next Generation of Cosmological Hydrodynamical Simulations of Galaxy Formation

Volker Springel (), Annalisa Pillepich (), Rainer Weinberger (), Rüdiger Pakmor (), Lars Hernquist (), Dylan Nelson (), Shy Genel (), Mark Vogelsberger (), Federico Marinacci (), Jill Naiman () and Paul Torrey ()
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Volker Springel: Zentrum für Astronomie der Universität Heidelberg, Astronomisches Recheninstitut
Annalisa Pillepich: Max-Planck Institute for Astronomy
Rainer Weinberger: Heidelberg Institute for Theoretical Studies
Rüdiger Pakmor: Heidelberg Institute for Theoretical Studies
Lars Hernquist: Harvard University, Center for Astrophysics
Dylan Nelson: Max-Planck Institute for Astrophysics
Shy Genel: Columbia University, Department of Astronomy
Mark Vogelsberger: MIT, Kavli Institute for Astrophysics and Space Research
Federico Marinacci: MIT, Kavli Institute for Astrophysics and Space Research
Jill Naiman: Harvard University, Center for Astrophysics
Paul Torrey: MIT, Kavli Institute for Astrophysics and Space Research

A chapter in High Performance Computing in Science and Engineering ´16, 2016, pp 5-20 from Springer

Abstract: Abstract Cosmological simulations of galaxy formation provide the most powerful technique for calculating the non-linear evolution of cosmic structure formation. This approach starts from initial conditions determined during the Big Bang – which are precisely specified in the cosmological standard model – and evolves them forward in time to the present epoch, thereby providing detailed predictions that test the cosmological paradigm. Here we report first preliminary results from a new generation of hydrodynamical simulations that excel with new physics, enlarged dynamic range and more accurate numerical techniques. The simulations of our ongoing Illustris++ project on HazelHen successfully reproduce the appearance of a red sequence of galaxies that are quenched by accreting supermassive black holes, while at the same time yielding a population of disk galaxies with properties that closely match observational data. Also, we are able to predict the amplification of magnetic fields through small-scale dynamo processes in realistic simulations of large galaxy populations, thereby providing novel predictions for the field strength and topology expected for galaxies of different size and type.

Date: 2016
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DOI: 10.1007/978-3-319-47066-5_1

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