First Results from the TNG50 Simulation: Galactic outflows driven by supernovae and black hole feedback. (arXiv:1902.05554v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Nelson_D/0/1/0/all/0/1">Dylan Nelson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pillepich_A/0/1/0/all/0/1">Annalisa Pillepich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Springel_V/0/1/0/all/0/1">Volker Springel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pakmor_R/0/1/0/all/0/1">Ruediger Pakmor</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weinberger_R/0/1/0/all/0/1">Rainer Weinberger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Genel_S/0/1/0/all/0/1">Shy Genel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Torrey_P/0/1/0/all/0/1">Paul Torrey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vogelsberger_M/0/1/0/all/0/1">Mark Vogelsberger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marinacci_F/0/1/0/all/0/1">Federico Marinacci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hernquist_L/0/1/0/all/0/1">Lars Hernquist</a>
We present the new TNG50 cosmological, magnetohydrodynamical simulation —
the third and final volume of the IllustrisTNG project. This simulation
occupies a unique combination of large volume and high resolution, with a 50
Mpc box sampled by 2160^3 gas cells (baryon mass of 8×10^4 solar masses). The
median spatial resolution of star-forming ISM gas is ~100-140 parsecs (from z=0
to z=6). This resolution approaches or exceeds that of modern ‘zoom’
simulations of individual massive galaxies, while the volume contains ~20,000
resolved galaxies with M* > 10^7 solar masses. Herein we show first results
from TNG50, focusing on galactic outflows driven by supernovae as well as
supermassive black hole feedback.
We find that the outflow mass loading is a non-monotonic function of galaxy
stellar mass, turning over and rising rapidly above 10^10.5 solar masses due to
the action of the central black hole (BH). Outflow velocity increases with
stellar mass, and at fixed stellar mass, outflows are faster at higher
redshift. The phase structure of galactic winds is complex, and we demonstrate
that the TNG model can produce high velocity, multi-phase outflows which
include cool, dense components. These outflows reach speeds in excess of 3000
km/s with an ejective, BH-driven origin. Critically, we show how the relative
simplicity of model inputs (and scalings) at the injection scale produces
complex behavior at galactic and halo scales. For example, despite isotropic
wind launching, outflows exhibit natural collimation and an emergent
bipolarity. We present a correlation between outflow velocity and offset from
the star-forming main sequence — galaxies above the SFMS drive faster
outflows, although this correlation inverts at high mass with the onset of
quenching, whereby low luminosity, slowly accreting, massive black holes drive
the strongest outflows.
We present the new TNG50 cosmological, magnetohydrodynamical simulation —
the third and final volume of the IllustrisTNG project. This simulation
occupies a unique combination of large volume and high resolution, with a 50
Mpc box sampled by 2160^3 gas cells (baryon mass of 8×10^4 solar masses). The
median spatial resolution of star-forming ISM gas is ~100-140 parsecs (from z=0
to z=6). This resolution approaches or exceeds that of modern ‘zoom’
simulations of individual massive galaxies, while the volume contains ~20,000
resolved galaxies with M* > 10^7 solar masses. Herein we show first results
from TNG50, focusing on galactic outflows driven by supernovae as well as
supermassive black hole feedback.
We find that the outflow mass loading is a non-monotonic function of galaxy
stellar mass, turning over and rising rapidly above 10^10.5 solar masses due to
the action of the central black hole (BH). Outflow velocity increases with
stellar mass, and at fixed stellar mass, outflows are faster at higher
redshift. The phase structure of galactic winds is complex, and we demonstrate
that the TNG model can produce high velocity, multi-phase outflows which
include cool, dense components. These outflows reach speeds in excess of 3000
km/s with an ejective, BH-driven origin. Critically, we show how the relative
simplicity of model inputs (and scalings) at the injection scale produces
complex behavior at galactic and halo scales. For example, despite isotropic
wind launching, outflows exhibit natural collimation and an emergent
bipolarity. We present a correlation between outflow velocity and offset from
the star-forming main sequence — galaxies above the SFMS drive faster
outflows, although this correlation inverts at high mass with the onset of
quenching, whereby low luminosity, slowly accreting, massive black holes drive
the strongest outflows.
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