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First results from the IllustrisTNG simulations: radio haloes and magnetic fields

Federico MarinacciKavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USAMark VogelsbergerKavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USARüdiger PakmorHeidelberger Institut für Theoretische Studien, Schloss-Wolfsbrunnenweg 35, 69118 Heidelberg, GermanyPaul TorreyKavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USAVolker SpringelHeidelberger Institut für Theoretische Studien, Schloss-Wolfsbrunnenweg 35, 69118 Heidelberg, GermanyLars HernquistHarvard–Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USADylan NelsonMax-Planck-Institut für Astrophysik, Karl-Schwarzschild-Straße 1, 85741 Garching bei München, GermanyRainer WeinbergerHeidelberger Institut für Theoretische Studien, Schloss-Wolfsbrunnenweg 35, 69118 Heidelberg, GermanyAnnalisa PillepichMax-Planck-Institut für Astronomie, Königstuhl 17, 69117, Heidelberg, GermanyJill NaimanHarvard–Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAShy GenelCenter for Computational Astrophysics, Flatiron Institute, 162 Fifth Avenue, New York, NY 10010, USA

2018en

ABI

Annotatsiya

We introduce the IllustrisTNG project, a new suite of cosmological magnetohydrodynamical simulations performed with the moving-mesh code AREPO employing an updated Illustris galaxy formation model. Here we focus on the general properties of magnetic fields and the diffuse radio emission in galaxy clusters. Magnetic fields are prevalent in galaxies, and their build-up is closely linked to structure formation. We find that structure formation amplifies the initial seed fields (10(-14) comoving Gauss) to the values observed in low-redshift galaxies (1-10 mu G). The magnetic field topology is closely connected to galaxy morphology such that irregular fields are hosted by early-type galaxies, while large-scale, ordered fields are present in disc galaxies. Using two simple models for the energy distribution of relativistic electrons we predict the diffuse radio emission of 280 clusters with a baryonic mass resolution of 1.1 x 10(7) M-circle dot, and generate mock observations for Very Large Array (VLA), Low-Frequency Array (LOFAR), Australian Square Kilometre Array Pathfinder (ASKAP), and Square Kilometre Array (SKA). Our simulated clusters show extended radio emission, whose detectability correlates with their virial mass. We reproduce the observed scaling relations between total radio power and X-ray emission, M500, and the Sunyaev-Zel'dovich Y500 parameter. The radio emission surface brightness profiles of our most massive clusters are in reasonable agreement with VI.A measurements of Coma and Perseus. Finally, we discuss the fraction of detected extended radio haloes as a function of virial mass and source count functions for different instruments. Overall our results agree encouragingly well with observations, but a refined analysis requires a more sophisticated treatment of relativistic particles in large-scale galaxy formation simulations.

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DOI: 10.1093/mnras/sty2206

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