#simulateduniverses — Public Fediverse posts
Live and recent posts from across the Fediverse tagged #simulateduniverses, aggregated by home.social.
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Tomography of a simulated cluster of galaxies with the eulerian Enzo code, covering about 2 Megaparsec along the line of sight, slice by slice (each slice being 4kpc deep).
Many many substructures, mostly filamentary and mostly driven by B-fields on small scales (<10-100kpc). This assumes an ideal MHD picture for the intracluster medium, while we know well it is a weakly collisional plasma, yet this structures at these scales might be realistic 🤞🏼
#SimulatedUniverses #astrophysics #science -
Release of magnetic fields from the simulated version of radio galaxies in my cosmological simulation, where the G/R color coding is for the magnetic field strength, while the blue is for the baryonic matter. The map integrates the release of B-field across a comoving 42Mpc volume. By associating a relativistic electron density to the events, I get a distribution function of radio emission in agreement with observations.
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Smooth rotation around the 3 dimensional gas distribution in an ENZO simulated cluster of galaxies in a still frame at the end of cosmic evolution, by former PhD student M. Angelinelli. The region approximately covers 6 cubic million lightyears.
#SimulatedUniverses #astrophysics #science -
RGB rendering done with SAO's DS9 on the evolution of my simulated cluster of galaxies. Thered colors and the contours show the projected gas temperature (useful to visualise shock waves after the major merger), the blue colors trace the baryon density while the green colors show the magnetic field strength, which grows by many orders of magnitude in the cluster as a result of turbulent dynamo amplification.
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Small experiment using Lagragian passive tracers injected in the sequence of outputs of an ENZO MHD cosmological simulations, to track the formation history of filaments and threads in the intracluster medium .
tracer propagation code in #Julia language
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Continuous rotation around the centre of the innermost 2Mpc^3 region of a cluster of galaxies simulated with ideal MHD with the ENZO code (Constrained Transport method here). Each cell is 4kpc large and the quantity on display is the temperature of the intracluster medium gas, almost towards the end of the simulation (z=0.2).
3D rendering done with SAO's DS9.
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Continuous rotation around the centre of the innermost 2Mpc^3 region of a cluster of galaxies simulated with ideal MHD with the ENZO code (Constrained Transport method here). Each cell is 4kpc large and the quantity on display is the magnetic field strength almost towards the end of the simulation.
3D rendering done with SAO's DS9.
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A woman merging with a beautiful full screen rendering of the simulated cosmic web in a simulation of mine...
This is was a segment from "Destinazione Terra" (Destination Earth) a video using scientific simulations by Daniela Paoletti and Diego Molinari, together the VisitLab at #CINECA, the biggest supercomputing centre in #Italy
It was presented at the Genova Science festival, and you can see the
full video here https://www.youtube.com/watch?v=5SAybgEBiXE -
A woman merging with a beautiful full screen rendering of the simulated cosmic web in a simulation of mine...
This is was a segment from "Destinazione Terra" (Destination Earth) a video using scientific simulations by Daniela Paoletti and Diego Molinari, together the VisitLab at #CINECA, the biggest supercomputing centre in #Italy
It was presented at the Genova Science festival, and you can see the
full video here https://www.youtube.com/watch?v=5SAybgEBiXE -
A woman merging with a beautiful full screen rendering of the simulated cosmic web in a simulation of mine...
This is was a segment from "Destinazione Terra" (Destination Earth) a video using scientific simulations by Daniela Paoletti and Diego Molinari, together the VisitLab at #CINECA, the biggest supercomputing centre in #Italy
It was presented at the Genova Science festival, and you can see the
full video here https://www.youtube.com/watch?v=5SAybgEBiXE -
A woman merging with a beautiful full screen rendering of the simulated cosmic web in a simulation of mine...
This is was a segment from "Destinazione Terra" (Destination Earth) a video using scientific simulations by Daniela Paoletti and Diego Molinari, together the VisitLab at #CINECA, the biggest supercomputing centre in #Italy
It was presented at the Genova Science festival, and you can see the
full video here https://www.youtube.com/watch?v=5SAybgEBiXE -
A woman merging with a beautiful full screen rendering of the simulated cosmic web in a simulation of mine...
This is was a segment from "Destinazione Terra" (Destination Earth) a video using scientific simulations by Daniela Paoletti and Diego Molinari, together the VisitLab at #CINECA, the biggest supercomputing centre in #Italy
It was presented at the Genova Science festival, and you can see the
full video here https://www.youtube.com/watch?v=5SAybgEBiXE -
#paperday on #astroph:
"Galaxy clusters in the LoTSS-DR3:
Catalogues and detection pipeline for diffuse radio emission" by Chiara Stuardi et al. including me
https://arxiv.org/pdf/2605.06400It presents the automated detection of diffuse radio emission in clusters observed in radio, using a Convolutional neural network (RADIO-UNET) trained on my #SimulatedUniverses !
Once in a while, a decent use of #AI to do something humans cannot do on this scale (as quickly).
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#paperday on #astroph:
"Galaxy clusters in the LoTSS-DR3:
Catalogues and detection pipeline for diffuse radio emission" by Chiara Stuardi et al. including me
https://arxiv.org/pdf/2605.06400It presents the automated detection of diffuse radio emission in clusters observed in radio, using a Convolutional neural network (RADIO-UNET) trained on my #SimulatedUniverses !
Once in a while, a decent use of #AI to do something humans cannot do on this scale (as quickly).
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#paperday on #astroph:
"Galaxy clusters in the LoTSS-DR3:
Catalogues and detection pipeline for diffuse radio emission" by Chiara Stuardi et al. including me
https://arxiv.org/pdf/2605.06400It presents the automated detection of diffuse radio emission in clusters observed in radio, using a Convolutional neural network (RADIO-UNET) trained on my #SimulatedUniverses !
Once in a while, a decent use of #AI to do something humans cannot do on this scale (as quickly).
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#paperday on #astroph:
"Galaxy clusters in the LoTSS-DR3:
Catalogues and detection pipeline for diffuse radio emission" by Chiara Stuardi et al. including me
https://arxiv.org/pdf/2605.06400It presents the automated detection of diffuse radio emission in clusters observed in radio, using a Convolutional neural network (RADIO-UNET) trained on my #SimulatedUniverses !
Once in a while, a decent use of #AI to do something humans cannot do on this scale (as quickly).
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#paperday on #astroph:
"Galaxy clusters in the LoTSS-DR3:
Catalogues and detection pipeline for diffuse radio emission" by Chiara Stuardi et al. including me
https://arxiv.org/pdf/2605.06400It presents the automated detection of diffuse radio emission in clusters observed in radio, using a Convolutional neural network (RADIO-UNET) trained on my #SimulatedUniverses !
Once in a while, a decent use of #AI to do something humans cannot do on this scale (as quickly).
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A few rotating views around a massive (1e15 Msol) simulated cluster of galaxies using ENZO, the almost uniform resolution in the centre is 4kpc/cell and the total volume on display here is (2Mpc)^3.
Left: magnetic field strength (a lot of filaments!).
Right: baryonic density
All rotations are done using SAO's DS9 after post-processing in #Julia
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Tomography of magnetic field strength in my latest favourite cluster of galaxies simulated with ENZO and constrained transport, the scanned region is approximately (2 Mpc)^3.
I am constantly trying to step out of the world of clusters of galaxies, but they keep looking very nice from the point of view of simulations!
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A very nice collective movie showing the effect of different AGN feedback implementations in the ENZO code by Stefano Sotira, who has just been awarded his #PhD title from the University of #Bologna
His two papers so far, where he investigated the relations between multi-phase gas in the intracluster medium and different feedback modalities:
https://arxiv.org/pdf/2410.07314
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A couple of 3D continuous rotations around the density (left) and magnetic field (right) simulated distributions in a Coma-like cluster of galaxies, ENZO-MHD simulation using Constrained Transport, and visualisation using SAO's DS9 viewer on reconstructed fits files
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Experiments in the generation (across several timesteps) and advection of Lagragian passive tracers to track the propagation of gas matter in new cosmological simulations of clusters of galaxies.
(tracers code in #Julia language, on top of ENZO-MHD simulations)
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So now colleagues have started asking me cover pictures for their press releases, even if I am not even in the paper and I do not know what the paper is about (embargo!) except that it has to do with intergalactic magnetism, so here we go with some new attempts to display the complexity of gas flows and magnetic fields in a cosmological MHD simulation...
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A few central slices at different times showing the structure of the simulated magnetic field in a new 1e15Msol clusters of galaxies simulated with the ENZO code and 7 levels of Adaptive Mesh Refinement at CINECA, and using the Constrained Transport (CT) method.
So cool and clean!
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Experiment in the propagation of ultra high energy (>1e18-1e21 eV) protons injected in a simulated cosmic volume at the very late redshift of z=0.02. In the left experiment their trajectories are deflected by the lorentz force (F=q (v x B)) on protons exerted by extragalactic magnetic fields, in the right case we assume for comparison that B=0 everywhere (so they just proceed in a straight line and loos energy by other processes).
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Exciting map of the day for a cosmological simulation, first timestep at redshift 99.73, already a lot of problems comparing this to a parallel run done with another code....
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The large scale distribution of magnetic fields in a realistic (hopefully) simulation of the cosmic web, and what might be detected in the future using the low-frequency part of the Square Kilometre Array.
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Testing a very small N-body simulation with a colleague, to introduce self-gravity in another code. Here are 32^3 dark matter particles, evolving from redshift 100 to 0.
As expected and I politely suggested, plotting them in intervals of equal redshift is a poor choice: each frame here is for an interval of Δz=10 starting from z=100, almost nothing happens until z=10, then we have the first caustics, then halos appear only at z=0.
#SimulatedUniverses #astrophysics #science -
Can you do any science using fewer than the 32^3 dark matter particles in the left mage? (the other are 64^3 and 128^3 dark matter particles)
No, and this is also ridiculously small, yet this is the start of a potentially powerful comparison with another code, which did not use to have dark matter and self-gravity, so even a comparison with this tiny tiny N-body simulations may be opening something big in the future! -
The rich texture of the dark matter cosmic web in one of the largest simulations I have run with the ENZO code, a few years ago (some material for incoming cycle of lectures).
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Reviving a small simulation (2D in Julia) to show how the onset of cosmic structure formation can essentially be captured by the Zeldovich approximation - meaning you just keep displacing the initial distribution of particles following the path traced by the initial tiny gravitational perturbations, which are imprinted in the initial conditions.
Actual N-body dynamics will take place only at the first crossing of streams of particles (in filaments, halos..)
#simulatedUniverses #astrophysics -
#SimulatedUniverses #astronomy #science simulated structure formation in an accelerated way, in a small portion of the universe. The inverted gray tones I think best highlight tiny threads and filaments in voids
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Rotation around a 1280^3 cube containig the tangled magnetic field strength of a simulated massive cluster of galaxies (ENZO code) at redshift z=0.
Visualisation done with SAO's DS9.
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Today experiment with new strategies to use passive Lagrangian tracers in the post-processing of large cosmological simulations.
Here tracers are continuously generated at all timesteps, providing a more volume-filling sampling of the flow even at late redshift.
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Full evolution (from redshift 30 to 0, about 13 million years) of a 1e15Msol cluster newly born at CINECA, the quantity shown in projection across 20 Mpc is the density of baryons along the line of sight.
This exact cosmic ballet of matter is not unexpected to me: I am actually resimulating the same "lucky" initial conditions i selected during my PhD, in 2009, which always produce the systems I know!
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New murmuration movie of tracers following ordinary matter collapsing into a forming cluster of galaxies, in a fully Eulerian MHD Enzo simulation run at #CINECA (Italy).
Notice how this cluster assembles its mass mostly along filaments in the N-S direction.About 10 million tracers evolved in @julialang , covering about 10 billions of years of cosmic evolution
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New murmuration movie of tracers following ordinary matter collapsing into a forming cluster of galaxies, in a fully Eulerian MHD Enzo simulation run at #CINECA (Italy).
Notice how this cluster assembles its mass mostly along filaments in the N-S direction.About 10 million tracers evolved in @julialang , covering about 10 billions of years of cosmic evolution
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New murmuration movie of tracers following ordinary matter collapsing into a forming cluster of galaxies, in a fully Eulerian MHD Enzo simulation run at #CINECA (Italy).
Notice how this cluster assembles its mass mostly along filaments in the N-S direction.About 10 million tracers evolved in @julialang , covering about 10 billions of years of cosmic evolution
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New murmuration movie of tracers following ordinary matter collapsing into a forming cluster of galaxies, in a fully Eulerian MHD Enzo simulation run at #CINECA (Italy).
Notice how this cluster assembles its mass mostly along filaments in the N-S direction.About 10 million tracers evolved in @julialang , covering about 10 billions of years of cosmic evolution
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New murmuration movie of tracers following ordinary matter collapsing into a forming cluster of galaxies, in a fully Eulerian MHD Enzo simulation run at #CINECA (Italy).
Notice how this cluster assembles its mass mostly along filaments in the N-S direction.About 10 million tracers evolved in @julialang , covering about 10 billions of years of cosmic evolution
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Simulation of how magnetised relativistic plasma ejected by one active galactic nucleus mixes over time with the moving intracluster medium of a galaxy group.
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Massive run advecting 1e7 passive Lagrangian tracers in the simulation of a forming supercluster, from z=1 to z=0, in an Enzo simulation post processed with Julia.
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CW: Strobing light
Done by mistake: I mounted the visualisation of two different fields at once, in an alternate way.
It has some value, though. The bg color map show baryons forming a large cluster of galaxies in a simulation
The green contours show the location of Lagrangian tracers, just tracking the bulk of matter.
The blue contours show instead where radio emission forms (Fermi I and II acceleration on relativistic electrons).
Flashy but interesting
#astronomy #SimulatedUniverses #astrophysics -
Continued from https://mastodon.social/@franco_vazza/115768829300108976
Another murmuration of Lagrangian tracer particles from z=1.5 to z=0, here for a 1.4e15Msol cluster with a major merger at redshift z=0.2
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I have produced a lot of new "murmuration" movies of Lagrangian tracers in @julialang to follow the transport of matter fluxes in my latest ENZO Eulerian Adaptive Mesh Refinement simulations of clusters of galaxies.
Going to produce a small suite of movies here day by day!
1) Here is cluster E2 (1.12e15 Msol cluster with an ongoing merger towards the end) from redshift 1.5 to redshift 0.
The box is (15Mpc)^3 at it contains 1e6 tracers -
Murmuration of 1e6 Lagrangian tracers which are used track the propagation of baryonic matter in a region where a simulated cluster of galaxies form (all done in @julialang ).
The tracer allow to visualise something not entirely trivial: despite he overall full collapse into an halo of this region of the universe, a fraction of these tracers "bounce back" to a few Megaparsec from the cluster centre - after having crossing it in a merger.
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Wow, spent two good hours having remote interviews with two journalists who wanted to know more about "The simulation hypothesis" and (its negation using physics).
my contribution to that was indeed born like a "summer project" last yearhttps://mastodon.social/@franco_vazza/112602495770701830
and then it makes sense it is again discussed as a "summer divertissement"
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Simulated growth of magnetic fields (left) and of baryonic matter (right) at the birth location of a massive cluster of galaxies, simulated with the Enzo code at #CINECA (Italy)
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Simulated growth of magnetic fields (left) and of baryonic matter (right) at the birth location of a massive cluster of galaxies, simulated with the Enzo code at #CINECA (Italy)
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Simulated growth of magnetic fields (left) and of baryonic matter (right) at the birth location of a massive cluster of galaxies, simulated with the Enzo code at #CINECA (Italy)