Impact of dark matter sub-haloes on the outer gaseous discs of galaxies

M. Shah, K. Bekki, K. Vinsen, S. Foster

Research output: Contribution to journalArticle

2 Citations (Scopus)

Abstract

Late-type disc galaxies are observed to have extended gas discs that are significantly larger than their optical discs. The Λ cold dark matter (ΛCDM) cosmological model predicts that luminous galaxies, such as the Milky-Way (MW), are hosts to a large number of low-mass dark matter sub- haloes (DMSHs), which are capable of interacting with the discs of galaxies. We aim to understand the kinematic impact of a DMSH collision with the extended gas disc of a galaxy. In order to study this, we use hydrodynamical simulations with a variety of parameters such as galaxy inclination, DMSH mass, and galaxy mass. To analyse the simulation results, we present two-dimensional (2D) kinematic and gas density maps of galaxies to investigate their unique features and structures. Along with this, we also implement a deep learning (DL) model to classify kinematic images of the simulated galaxies as either impacted (by the DMSH) or isolated. Through the use of these techniques, we have found that the impact of the DMSH causes features in both the 2D kinematic and gas density plots, most notably the development of a {̃ }1 {kpc} size H I hole in the gas-rich DMSH impact. Through the study of these maps, we identify certain features and the specific conditions required to induce them. The study of these features is important, as they can be observed with large upcoming H I surveys such as WALLABY and SKA.
Original languageEnglish
Pages (from-to)4188-4202
Number of pages15
JournalMonthly Notices of the Royal Astronomical Society
Volume482
Issue number3
DOIs
Publication statusPublished - 2019

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halos
dark matter
galaxies
kinematics
gas
gas density
gases
optical disks
disk galaxies
learning
inclination
simulation
collision
plots
collisions
causes

Cite this

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title = "Impact of dark matter sub-haloes on the outer gaseous discs of galaxies",
abstract = "Late-type disc galaxies are observed to have extended gas discs that are significantly larger than their optical discs. The Λ cold dark matter (ΛCDM) cosmological model predicts that luminous galaxies, such as the Milky-Way (MW), are hosts to a large number of low-mass dark matter sub- haloes (DMSHs), which are capable of interacting with the discs of galaxies. We aim to understand the kinematic impact of a DMSH collision with the extended gas disc of a galaxy. In order to study this, we use hydrodynamical simulations with a variety of parameters such as galaxy inclination, DMSH mass, and galaxy mass. To analyse the simulation results, we present two-dimensional (2D) kinematic and gas density maps of galaxies to investigate their unique features and structures. Along with this, we also implement a deep learning (DL) model to classify kinematic images of the simulated galaxies as either impacted (by the DMSH) or isolated. Through the use of these techniques, we have found that the impact of the DMSH causes features in both the 2D kinematic and gas density plots, most notably the development of a {̃ }1 {kpc} size H I hole in the gas-rich DMSH impact. Through the study of these maps, we identify certain features and the specific conditions required to induce them. The study of these features is important, as they can be observed with large upcoming H I surveys such as WALLABY and SKA.",
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Impact of dark matter sub-haloes on the outer gaseous discs of galaxies. / Shah, M.; Bekki, K.; Vinsen, K.; Foster, S.

In: Monthly Notices of the Royal Astronomical Society, Vol. 482, No. 3, 2019, p. 4188-4202.

Research output: Contribution to journalArticle

TY - JOUR

T1 - Impact of dark matter sub-haloes on the outer gaseous discs of galaxies

AU - Shah, M.

AU - Bekki, K.

AU - Vinsen, K.

AU - Foster, S.

PY - 2019

Y1 - 2019

N2 - Late-type disc galaxies are observed to have extended gas discs that are significantly larger than their optical discs. The Λ cold dark matter (ΛCDM) cosmological model predicts that luminous galaxies, such as the Milky-Way (MW), are hosts to a large number of low-mass dark matter sub- haloes (DMSHs), which are capable of interacting with the discs of galaxies. We aim to understand the kinematic impact of a DMSH collision with the extended gas disc of a galaxy. In order to study this, we use hydrodynamical simulations with a variety of parameters such as galaxy inclination, DMSH mass, and galaxy mass. To analyse the simulation results, we present two-dimensional (2D) kinematic and gas density maps of galaxies to investigate their unique features and structures. Along with this, we also implement a deep learning (DL) model to classify kinematic images of the simulated galaxies as either impacted (by the DMSH) or isolated. Through the use of these techniques, we have found that the impact of the DMSH causes features in both the 2D kinematic and gas density plots, most notably the development of a {̃ }1 {kpc} size H I hole in the gas-rich DMSH impact. Through the study of these maps, we identify certain features and the specific conditions required to induce them. The study of these features is important, as they can be observed with large upcoming H I surveys such as WALLABY and SKA.

AB - Late-type disc galaxies are observed to have extended gas discs that are significantly larger than their optical discs. The Λ cold dark matter (ΛCDM) cosmological model predicts that luminous galaxies, such as the Milky-Way (MW), are hosts to a large number of low-mass dark matter sub- haloes (DMSHs), which are capable of interacting with the discs of galaxies. We aim to understand the kinematic impact of a DMSH collision with the extended gas disc of a galaxy. In order to study this, we use hydrodynamical simulations with a variety of parameters such as galaxy inclination, DMSH mass, and galaxy mass. To analyse the simulation results, we present two-dimensional (2D) kinematic and gas density maps of galaxies to investigate their unique features and structures. Along with this, we also implement a deep learning (DL) model to classify kinematic images of the simulated galaxies as either impacted (by the DMSH) or isolated. Through the use of these techniques, we have found that the impact of the DMSH causes features in both the 2D kinematic and gas density plots, most notably the development of a {̃ }1 {kpc} size H I hole in the gas-rich DMSH impact. Through the study of these maps, we identify certain features and the specific conditions required to induce them. The study of these features is important, as they can be observed with large upcoming H I surveys such as WALLABY and SKA.

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