shaping the gas: understanding gas shapes in dark matter haloes with interpretable machine learning

@article{MachadoPolettiValle2021shapingTG,
  title={shaping the gas: understanding gas shapes in dark matter haloes with interpretable machine learning},
  author={Luis Fernando Machado Poletti Valle and Camille Avestruz and David J Barnes and Arya Farahi and Erwin T Lau and Daisuke Nagai},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2021}
}
The non-spherical shapes of dark matter and gas distributions introduce systematic uncertainties that affect observable–mass relations and selection functions of galaxy groups and clusters. However, the triaxial gas distributions depend on the non-linear physical processes of halo formation histories and baryonic physics, which are challenging to model accurately. In this study, we explore a machine learning approach for modelling the dependence of gas shapes on dark matter and baryonic… 
View PDF on arXiv
1 Citations

Figures and Tables from this paper

One Citation

KLLR: A Scale-dependent, Multivariate Model Class for Regression Analysis
TLDR
This work introduces and implements a class of kernel localized linear regression (KLLR) models, a natural extension to the commonly used linear models that allows the parameters of the linear model—normalization, slope, and covariance matrix—to be scale dependent.

References

SHOWING 1-10 OF 73 REFERENCES
Correlations between triaxial shapes and formation history of dark matter haloes
The shape of dark matter haloes plays a critical role in constraining cosmology with upcoming large-scale structure surveys. In this paper, we study the correlations between the triaxial shapes and…
Shapes of Gas, Gravitational Potential, and Dark Matter in ΛCDM Clusters
We present analysis of the three-dimensional shape of intracluster gas in clusters formed in cosmological simulations of the Lambda CDM cosmology and compare it to the shape of dark matter…
Some like it triaxial: the universality of dark matter halo shapes and their evolution along the cosmic time
We present a detailed analysis of dark matter halo shapes, studying how the distributions of ellipticity, prolateness and axial ratios evolve as a function of time and mass. With this purpose in…
The shapes and alignments of dark matter halos
We present measurements of the triaxial dark matter halo shapes and alignment correlation functions in the Millennium and Millennium-2 dark matter N-body simulations. These two simulations allow us…
The Effect of Gas Cooling on the Shapes of Dark Matter Halos
We analyze the effect of dissipation on the shapes of dark matter (DM) halos using high-resolution cosmological gasdynamics simulations of clusters and galaxies in the ΛCDM cosmology. We find that…
The dark side of galaxy colour
We present age distribution matching, a theoretical formalism for predicting how galaxies of luminosity L and color C occupy dark matter halos. Our model supposes that there are just two fundamental…
The impact of baryonic physics on the structure of dark matter haloes: the view from the FIRE cosmological simulations
We study the distribution of cold dark matter (CDM) in cosmological simulations from the FIRE (Feedback In Realistic Environments) project, for M_* ∼ 10^(4–11) M_⊙ galaxies in M_h ∼ 10^(9–12) M_⊙…
Shape of dark matter haloes in the Illustris simulation: effects of baryons
We study the effect of baryonic processes on the shapes of dark matter (DM) haloes from Illustris, a suite of hydrodynamical (Illustris) and DM-only (Illustris-Dark) cosmological simulations…
The Connection Between Galaxies and Their Dark Matter Halos
In our modern understanding of galaxy formation, every galaxy forms within a dark matter halo. The formation and growth of galaxies over time is connected to the growth of the halos in which they…
The structure of dark matter haloes in hierarchical clustering models
We use a set of large cosmological N-body simulations to study the internal structure of dark matter haloes which form in scale-free hierarchical clustering models (initial power spectra P(k) ∞ kn…
...
...