Note: that everything on this page is intended for public distribution. Anyone is welcome to download, distribute, and share images/videos presented here. For presentation in talks, posters, a text credit to the "TNG Simulations" or "TNG Collaboration" is sufficient.

For any commercial (non-academic) uses please contact us first.

Images:

D. Nelson

The stellar content of the Universe on the largest scales: a projection of the distribution of stars across a 50 Mpc region of space. Taken from the TNG100-1 simulation at the present day (z=0). [large]

A. Pillepich, D. Nelson

Comparison of the three TNG simulations: TNG50, TNG100, and TNG300. For each projected dark matter density is shown. The three volumes are roughly though not exactly to scale. [large] [black]

D. Nelson

Composite image combining gas temperature and shock mach number, in black and white. The horizontal scale of the image is ~100 Mpc (~320 million light years), around the second most massive cluster in TNG100-1.

D. Nelson

Overview comparison of the TNG100 and TNG300 simulations at redshift zero (present day). Three views of TNG300-1 centered on the most massive cluster in the box: gas density (left), gas temperature (center), and magnetic field amplitude (right). The 50 most massive halos are indicated by circles. In the inset in the upper right, we show the TNG100-1 volume in dark matter density (left) and gas density (right). [large]

F. Marinacci

X-ray map (in color) overlayed with synchrotron emission contours for the most massive halo of the TNG300-1 simulation. The panels are 3.5 Mpc on a side, each of the four representing a hypothetical observation by a different radio telescope (current or future). [large]

D. Nelson

TNG100-1: Fullbox composite which combines gas temperature (as the color) and shock mach number (as the brightness). Red indicates 10 million Kelvin gas at the centers of massive galaxy clusters, while bright structures show diffuse gas from the intergalactic medium shock heating at the boundary between cosmic voids and filaments. [large]

A. Pillepich

Ensemble of the extended intracluster light (ICL) of the twenty most massive clusters in TNG300-1 at redshift zero (present day). This diffuse component of stars arises as satellite galaxies fall into the cluster and are subsequently tidally disrupted. [large]

D. Nelson

Mock stellar light images of two galaxy samples: blue, star-forming systems (35 galaxies on the left) versus red, quenched systems (35 galaxies on the right). Both are taken from the same halo mass bin (12.0 - 12.2 total mass) in TNG100-1 at redshift zero. Imaged in JWST NIRCam f200W, f115W, and F070W filters (face-on). Each panel is 60 kpc on a side.

D. Nelson

Render of the gas velocity on 10 Mpc scales, although only in a very thin slice of 100 physical kiloparsecs (in the viewing direction). Where the image is black, the gas is hardly moving, while white regions have velocities which exceed 1000 km/s. Centered on the second most massive cluster in TNG100-1 at z=0, gas motions in cosmic filaments are contrasted against the fireball of the deep gravitational potential sitting at their intersection. [large]

A. Pillepich

Composite image of the TNG300 and TNG100 simulations: in the background, the full dark matter map of the large TNG300 volume, the backbone of structure formation. In the upper right inset, the distribution of stellar mass across the full ~100 Mpc TNG100 volume. Panels on the left show galaxy-galaxy interactions and the fine-grained structure of extended stellar halos. Panels on the right show stellar light projections from two massive central galaxies at the present day. [large]

D. Nelson

Gas column density across the full large-volume TNG300-1 simulation at redshift zero. We center on the most massive cluster in the box, which emerges as a 10 Mpc scale gas overdensity in the center of this image. Otherwise, the homogeneity of large-scale structure begins to emerge across the extent of this volume. Here a thin slice of only 100 kpc in depth is shown. [large]

D. Nelson

Composite image combining the predicted x-ray (free-free) emission from hot gas in halos (purple to orange) with the mach number of hydrodynamical shocks (from red to white, showing increasing strength). This view shows an extremely thin slice (only 100 pkpc thick) of the full TNG100-1 volume at z=0, centered on the second most massive cluster. Low mach number shocks at intergalactic filaments (red) converge into quasi-spherical, high mach number accretion shocks (white) which mark the boundaries between voids and gaseous halos. [large]

D. Nelson

Composite image (of the full TNG100-1 box) which overlays a projection of the dark matter density with the output of our on-the-fly cosmological shock finder, here used to derive the average mach number of shocks along each line of sight. All the gravitationally collapsed structures (in orange/white) are surrounded by successive shock surfaces (blue) which encode their formation histories. [large]

F. Marinacci

Gas density (left) and magnetic field strength (right) across the TNG300 box, centered on the most massive galaxy cluster. Zoomed panels show: magnetic field orientation and stellar light (top), or xray and radio emission from massive cluster (bottom). [large]



Videos:

Typically encoded in H.264 format for 1080p widescreen HD (1920x1080), H.265 for 4K widescreen (3840x2160), and/or 2000x2000 for square movies.

M. Vogelsberger

The interstellar magnetic field strength: blue/purple shows regions of low magnetic energy arranged along filaments of the cosmic web, while orange and white show regions with significant magnetic energy inside halos and galaxies. Time evolution of the inside of a 10Mpc (comoving) region within TNG100-1 from the start of the simulation to z=0. (01:45) [4K version]

D. Nelson

Comparison of the distribution of intergalactic gas (mass), between TNG100-1 and Illustris-1. Low-density voids (black/dark blue) transition to cosmic filaments (yellow/green), gas halos (light blue) and individual galaxies (white). The time evolution of the exact same 10Mpc (comoving) region is compared between the two simulations, which distribute gas differently on large scales as a result of the differences in the galaxy formation models. (01:37) [4K version]

D. Nelson

Comparison of four properties of intergalactic matter between the TNG100-1 and Illustris-1 simulations. These are (left to right): gas density, gas temperature, the abundance of heavy elements (metallicity), and the distribution of stars. The time-synchronized evolution of the same 10Mpc (comoving) region is compared between the two simulations. (01:37) [4K version]

S. Genel

Contrasting the large-scale distribution of stellar light between the original Illustris simulation (on the left) and the analogous TNG100 simulation (on the right). The same 10Mpc (comoving) region is shown between the two simulations, and because these were run with the same "phases" of the initial conditions, the same individual galaxies form in the same regions of space, allowing object-by-object comparison. (01:14) [4K version]

M. Vogelsberger

Time evolution of a 10Mpc (comoving) cubic region, rendered from outside. The movie shows the gas temperature (blue: cold, green: warm: white: hot), comparing original Illustris (left) to TNG100 (right). In both cases, the rapid temperature fluctuations and outbursts around nodes in the cosmic web are due to various energetic "feedback" processes in the simulation. These include energy from stars (supernovae explosions) as well as heat and high-velocity winds from supermassive black holes. (01:48)

D. Nelson

Eight views: the evolving structure of a small 10Mpc region of cosmic space is visualized from TNG100-1. Each view shows a different output of the simulation (from left to right, top): gas matter density, dark matter density, stellar mass, magnetic field strength, (bottom) gas temperature, gas metallicity, the velocity field of the gas, and column density of OVI - the fifth ionization state of oxygen (O5+). Each view shows the same region of space, all of these components co-evolving together as the simulation runs. (01:37) [4K version]

S. Genel

Formation of a massive "late-type", star-forming disk galaxy: an individual system is tracked through time, and its stellar light is shown in a 500 kilo-parsec region. This galaxy exhibits rapid ongoing star formation in an extended, clumpy disk, until it experiences a late-time merger (at approximately z ~ 0.3) with a nearly equal mass companion. (01:24)

S. Genel

Formation of an "early-type", quiescent elliptical galaxy: an individual galaxy is tracked through time, and its stellar light is shown in a 1 mega-parsec region. Between the start of the movie at high redshift and the end at z=0 (present day), this massive "red-and-dead" galaxy experiences a large number of galaxy mergers which bring in stars and other material, building up the final spheroidal morphology. (02:23)

F. Marinacci

The most massive cluster of TNG300 at z=0 (with a halo mass of ~ 1015 times the mass of the sun). Fixed in time, the video slowly rotates in space to show the structure from different view points. Each of the four panels shows the same predicted X-ray emission (in background color), while the overlaid contours show the predicted synchrotron emission, as would be observed by one of four radio telescopes: VLA, LOFAR, ASKAP, or SKA. (00:32)

M. Vogelsberger

Full simulation cubes of TNG300 (on the top) and TNG100 (on the bottom), showing dark matter, gas temperature, and magnetic field strength, all at the present day (z=0). Fixed in time, the movie shows the full matter distribution being built up by slowly adding slices from the bottom of each cube to the top. (00:58)



Additional Images and Videos:

Check back soon!