The role of mergers and halo spin in shaping galaxy morphology
Vicente Rodriguez-Gomez,Vicente Rodriguez-Gomez,Laura V. Sales,Shy Genel,Shy Genel,Annalisa Pillepich,Annalisa Pillepich,Jolanta Zjupa,Jolanta Zjupa,Dylan Nelson,Brendan F. Griffen,Paul Torrey,Gregory F. Snyder,Mark Vogelsberger,Volker Springel,Volker Springel,Chung-Pei Ma,Lars Hernquist +17 more
TLDR
In this paper, the authors consider 18,000 central galaxies with stellar masses from the Illustris cosmological hydrodynamic simulation and find that the fraction of accreted stars increases with galaxy stellar mass, from less than 5% in dwarfs to 80% in the most massive objects.Abstract:
Mergers and the spin of the dark matter halo are factors traditionally believed to determine the morphology of galaxies within a $\Lambda$CDM cosmology. We study this hypothesis by considering approximately 18,000 central galaxies at $z=0$ with stellar masses $M_{\ast} = 10^{9}-10^{12} \, {\rm M}_{\odot}$ selected from the Illustris cosmological hydrodynamic simulation. The fraction of accreted stars -- which measures the importance of massive, recent and dry mergers -- increases steeply with galaxy stellar mass, from less than 5 per cent in dwarfs to 80 per cent in the most massive objects, and the impact of mergers on galaxy morphology increases accordingly. For galaxies with $M_{\ast} \gtrsim 10^{11} \, {\rm M}_{\odot}$, mergers have the expected effect: if gas-poor they promote the formation of spheroidal galaxies, whereas gas-rich mergers favour the formation and survivability of massive discs. This trend, however, breaks at lower masses. For objects with $M_{\ast} \lesssim 10^{11} \, {\rm M}_{\odot}$, mergers do not seem to play any significant role in determining the morphology, with accreted stellar fractions and mean merger gas fractions that are indistinguishable between spheroidal and disc-dominated galaxies. On the other hand, halo spin correlates with morphology primarily in the least massive objects in the sample ($M_{\ast} \lesssim 10^{10} \, {\rm M}_{\odot}$), but only weakly for galaxies above that mass. Our results support a scenario where (1) mergers play a dominant role in shaping the morphology of massive galaxies, (2) halo spin is important for the morphology of dwarfs, and (3) the morphology of medium-sized galaxies -- including the Milky Way -- shows little dependence on galaxy assembly history or halo spin, at least when these two factors are considered individually.read more
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Journal ArticleDOI
First results from the IllustrisTNG simulations: the galaxy colour bimodality
Dylan Nelson,Annalisa Pillepich,Volker Springel,Volker Springel,Rainer Weinberger,Lars Hernquist,Ruediger Pakmor,Shy Genel,Paul Torrey,Mark Vogelsberger,Guinevere Kauffmann,Federico Marinacci,Jill Naiman +12 more
TL;DR: The first two simulations of the IllustrisTNG project were presented in this article, focusing on the optical colors of galaxies at low redshift, and the results showed that the simulated (g-r) colors of 10^9 10^11 Msun which redden at z < 1 accumulate on average ~25% of their final z=0 mass post-reddening; at the same time, ~18% of such massive galaxies acquire half or more of their last stellar mass while on the red sequence.
Journal ArticleDOI
The IllustrisTNG simulations: public data release
Dylan Nelson,Volker Springel,Volker Springel,Volker Springel,Annalisa Pillepich,Vicente Rodriguez-Gomez,Paul Torrey,Paul Torrey,Shy Genel,Mark Vogelsberger,Ruediger Pakmor,Ruediger Pakmor,Federico Marinacci,Federico Marinacci,Rainer Weinberger,Luke Zoltan Kelley,Mark R. Lovell,Mark R. Lovell,Benedikt Diemer,Lars Hernquist +19 more
TL;DR: The full public release of all data from the TNG100 and TNG300 simulations of the IllustrisTNG project is presented in this article, which includes a comprehensive model for galaxy formation physics, and each TNG simulation selfconsistently solves for the coupled evolution of dark matter, cosmic gas, luminous stars, and supermassive black holes from early time to the present day.
Journal ArticleDOI
First results from the TNG50 simulation: the evolution of stellar and gaseous discs across cosmic time
Annalisa Pillepich,Dylan Nelson,Volker Springel,Rüdiger Pakmor,Paul Torrey,Rainer Weinberger,Mark Vogelsberger,Federico Marinacci,Federico Marinacci,Shy Genel,Arjen van der Wel,Arjen van der Wel,Lars Hernquist +12 more
TL;DR: In this paper, the authors present a new cosmological, magnetohydrodynamical simulation for galaxy formation, TNG50, which reaches a numerical resolution typical of zoom-in simulations, with a baryonic element mass of 8.5 x 10(4) M-circle dot and an average cell size of 70-140pc in the star-forming regions of galaxies.
Posted Content
The IllustrisTNG Simulations: Public Data Release
Dylan Nelson,Volker Springel,Volker Springel,Volker Springel,Annalisa Pillepich,Vicente Rodriguez-Gomez,Paul Torrey,Paul Torrey,Shy Genel,Mark Vogelsberger,Ruediger Pakmor,Ruediger Pakmor,Federico Marinacci,Federico Marinacci,Rainer Weinberger,Luke Zoltan Kelley,Mark R. Lovell,Mark R. Lovell,Benedikt Diemer,Lars Hernquist +19 more
TL;DR: Improvements and new functionality in the web-based API are described, including on-demand visualization and analysis of galaxies and halos, exploratory plotting of scaling relations and other relationships between galactic and halo properties, and a new JupyterLab interface that provides an online, browser-based, near-native data analysis platform enabling user computation with local access to TNG data, alleviating the need to download large datasets.
Journal ArticleDOI
The optical morphologies of galaxies in the IllustrisTNG simulation: A comparison to Pan-STARRS observations
Vicente Rodriguez-Gomez,Gregory F. Snyder,Jennifer M. Lotz,Dylan Nelson,Annalisa Pillepich,Volker Springel,Shy Genel,Shy Genel,Rainer Weinberger,Sandro Tacchella,Rüdiger Pakmor,Paul Torrey,Federico Marinacci,Federico Marinacci,Mark Vogelsberger,Lars Hernquist,David A. Thilker +16 more
TL;DR: In this article, the authors generated synthetic images of 27,000 galaxies from the IllustrisTNG and the original Illustris hydrodynamic cosmological simulations, designed to match Pan-STARRS observations of approximately 9.8$-$11.3$ galaxies.
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