CSiBORG Tools

Tools for analysing the suite of Constrained Simulations in BORG (CSiBORG) simulations. The interface is designed to work with the following suites of simulations: CSiBORG1 (dark matter-only RAMSES), CSiBORG2 (dark matter-only Gadget4), Quijote (dark-matter only Gadget2), however with little effort it can support other simulations as well.

TODO

• In flow models test in a script that indeed the parallelization is working.
• Extend the parallelization to supernovae/simple distances.

Ongoing projects

Data to calculate

• Process all CSiBORG1 snapshots (running).
• Calculate halo properties for CSiBORG1
• Calculate initial properties for CSiBORG1
• Calculate halo properties for CSiBORG2
• Calculate initial properties for CSiBORG2
• Process all Quijote simulations.
• Calculate halo properties for Quijote
• Calculate initial properties for Quijote

General

• Add new halo properties to the catalogues.
• Add initial halo properties to the catalogues.
• Add a new flag for flipping x- and z-coordinates fro catalogues, snapshots and field readers.
• Add radial velocity field loader.

Consistent halo reconstruction

• Make a sketch of the overlap definition and add it to the paper.
• Re-calculate the overlaps for CSiBORG1, Quijote and CSiBORG2
• Fix the script to calculate the initial lagrangian positions etc.

Enviromental dependence of galaxy properties

• Prepare the CSiBORG one particle files for SPH.
• Transfer, calculate the SPH density field for CSiBORG1 and transfer back.
• Check that the velocity-field flipping of x and z coordinates is correct.
• Evaluate and share the density field for SDSS and SDSSxALFALFA for both CSiBORG2 and random fields.
• Check and verify the density field of galaxy colours (cannot do this now! Glamdring is super slow.)
• Calculate the radial velocity field for random realizations (submitted)
• Send Catherine concatenated data.
• Start analyzing DiSPERSE results.

Mass-assembly of massive clusters

• Make a list of nearby most-massive clusters.
• Write code to identify a counterpart of such clusters.
• Write code to make a plot of mass-assembly of all clusters within a certain mass range from the random simulations.
• Write code to compare mass-assembly of a specific cluster with respect to random ones.

Effect of small-scale noise

• Study how the small-scale noise variation affects the overlap measure, halo concentration and spin.
• Add uncertainty on the halo concentration.

Gravitational-wave and large-scale structure

• Validate the velocity field results agains Supranta data sets.
• Write code to estimate the enclosed mass and bulk flow.
• Write code to estimate the average radial velocity in a spherical shell.
• Write code to calculate the power spectrum of velocities.
• Estimate the amplitude of the velocity field in radial shells around the observer, estimate analogous results for random simulations, and see if they agree within cosmic variance.
• Calculate power spectra of velocities and maybe velocity dispersion.
• Make the velocity field data available.

CSiBORG meets X-ray

• Make available one example snapshot from the simulation. Mention the issue with x- and z-coordinates.
• Answer Johan and make a comparison to the Planck clusters.

CSiBORG advertising

• Decide on the webpage design and what to store there.
• Write a short letter describing the simulations.

Calculated data

Enclosed mass & bulk velocity

• CSiBORG2_main, CSiBORG2_varysmall, CSiBORG2_arandom

SPH-density & velocity field

• CSiBORG2_main, CSiBORG2_random, CSiBORG2_varysmall
• Evaluated for SDSS and SDSSxALFALFA in: CSiBORG2_main, CSiBORG2_random

Radial velocity field

• *CSiBORG2_main, CSiBORG2_random