Constraining the three-dimensional orbits of galaxies under ram pressure stripping with convolutional neural networks. (arXiv:1811.04553v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Bekki_K/0/1/0/all/0/1">Kenji Bekki</a>
Ram pressure stripping (RPS) of gas from disk galaxies has long been
considered to play vital roles in galaxy evolution within groups and clusters.
For a given density of intracluster medium (ICM) and a given velocity of a disk
galaxy, RPS can be controlled by two angles (theta and phi) that define the
angular relationship between the direction vector of the galaxy’s
three-dimensional (3D) motion within its host cluster and the galaxy’s spin
vector. We here propose a new method in which convolutional neutral networks
(CNNs) are used to constrain theta and phi of disk galaxies under RPS. We first
train a CNN by using ~10^5 synthesized images of gaseous distributions of the
galaxies from numerous RPS models with different theta and phi. We then apply
the trained CNN to a new test RPS model to predict theta and phi. The
similarity between the correct and predicted theta and $phi$ is measured by
cosine similarity (cos-Theta) with cos-Theta =1 being perfectly accurate
prediction. We show that the average cos-Theta among test models is ~0.95,
which means that theta and phi can be constrained well by applying the CNN to
the spatial distributions of their gas. This result suggests that if the ICM is
in hydrostatic equilibrium (thus not moving), the 3D orbit of a disk galaxy
within its host cluster can be constrained by the spatial distribution of the
gas being stripped by RPS. We discuss the applications of the method to HI
surveys such as WALLABY and SKA projects.
Ram pressure stripping (RPS) of gas from disk galaxies has long been
considered to play vital roles in galaxy evolution within groups and clusters.
For a given density of intracluster medium (ICM) and a given velocity of a disk
galaxy, RPS can be controlled by two angles (theta and phi) that define the
angular relationship between the direction vector of the galaxy’s
three-dimensional (3D) motion within its host cluster and the galaxy’s spin
vector. We here propose a new method in which convolutional neutral networks
(CNNs) are used to constrain theta and phi of disk galaxies under RPS. We first
train a CNN by using ~10^5 synthesized images of gaseous distributions of the
galaxies from numerous RPS models with different theta and phi. We then apply
the trained CNN to a new test RPS model to predict theta and phi. The
similarity between the correct and predicted theta and $phi$ is measured by
cosine similarity (cos-Theta) with cos-Theta =1 being perfectly accurate
prediction. We show that the average cos-Theta among test models is ~0.95,
which means that theta and phi can be constrained well by applying the CNN to
the spatial distributions of their gas. This result suggests that if the ICM is
in hydrostatic equilibrium (thus not moving), the 3D orbit of a disk galaxy
within its host cluster can be constrained by the spatial distribution of the
gas being stripped by RPS. We discuss the applications of the method to HI
surveys such as WALLABY and SKA projects.
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