The morphology of star-forming gas and its alignment with galaxies and dark matter haloes in the EAGLE simulations. Hill, A. D., Crain, R. A., Kwan, J., & McCarthy, I. G. arXiv e-prints, 2102:arXiv:2102.13603, February, 2021. ![The morphology of star-forming gas and its alignment with galaxies and dark matter haloes in the EAGLE simulations [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper abstract bibtex We present measurements of the morphology of star-forming gas in galaxies from the EAGLE simulations, and its alignment relative to stars and dark matter (DM). Imaging of such gas in the radio continuum enables weak lensing experiments that complement traditional optical approaches. Star-forming gas is typically more flattened than its associated stars and DM, particularly for present-day subhaloes of total mass \${\textbackslash}sim\$\$10{\textasciicircum}\{p̌hantom{\}} 12-12.5p̌hantom{\{}\} {\textbackslash}mathrm\{M_\{ {\textbackslash}odot\}\}\$, which preferentially host star-forming galaxies with rotationally-supported stellar discs. Such systems have oblate, spheroidal star-forming gas distributions, but in both less- and more-massive subhaloes the distributions tend to be prolate, and its morphology correlates positively and significantly with that of its host galaxy's stars, both in terms of sphericity and triaxiality. The minor axis of star-forming gas most commonly aligns with the minor axis of its host subhalo's DM, but often aligns more closely with one of the other two principal axes of the DM distribution in prolate subhaloes. Star-forming gas aligns with DM less strongly than is the case for stars, but its morphological minor axis aligns closely with its kinematic axis, affording a route to observational identification of the unsheared morphological axis. The projected ellipticities of star-forming gas in EAGLE are consistent with shapes inferred from high-fidelity radio continuum images, and they exhibit greater shape noise than is the case for images of the stars, owing to the greater characteristic flattening of star-forming gas with respect to stars.
@article{hill_morphology_2021,
title = {The morphology of star-forming gas and its alignment with galaxies and dark matter haloes in the {EAGLE} simulations},
volume = {2102},
url = {http://adsabs.harvard.edu/abs/2021arXiv210213603H},
abstract = {We present measurements of the morphology of star-forming gas in
galaxies from the EAGLE simulations, and its alignment relative to stars
and dark matter (DM). Imaging of such gas in the radio continuum enables
weak lensing experiments that complement traditional optical approaches.
Star-forming gas is typically more flattened than its associated stars
and DM, particularly for present-day subhaloes of total mass \${\textbackslash}sim\$\$10{\textasciicircum}\{\vphantom{\}}
12-12.5\vphantom{\{}\} {\textbackslash}mathrm\{M\_\{ {\textbackslash}odot\}\}\$, which preferentially host star-forming
galaxies with rotationally-supported stellar discs. Such systems have
oblate, spheroidal star-forming gas distributions, but in both less- and
more-massive subhaloes the distributions tend to be prolate, and its
morphology correlates positively and significantly with that of its host
galaxy's stars, both in terms of sphericity and triaxiality. The minor
axis of star-forming gas most commonly aligns with the minor axis of its
host subhalo's DM, but often aligns more closely with one of the other
two principal axes of the DM distribution in prolate subhaloes.
Star-forming gas aligns with DM less strongly than is the case for
stars, but its morphological minor axis aligns closely with its
kinematic axis, affording a route to observational identification of the
unsheared morphological axis. The projected ellipticities of
star-forming gas in EAGLE are consistent with shapes inferred from
high-fidelity radio continuum images, and they exhibit greater shape
noise than is the case for images of the stars, owing to the greater
characteristic flattening of star-forming gas with respect to stars.},
urldate = {2021-03-04},
journal = {arXiv e-prints},
author = {Hill, Alexander D. and Crain, Robert A. and Kwan, Juliana and McCarthy, Ian G.},
month = feb,
year = {2021},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
pages = {arXiv:2102.13603},
}
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Star-forming gas is typically more flattened than its associated stars and DM, particularly for present-day subhaloes of total mass \\${\\textbackslash}sim\\$\\$10{\\textasciicircum}\\{p̌hantom{\\}} 12-12.5p̌hantom{\\{}\\} {\\textbackslash}mathrm\\{M_\\{ {\\textbackslash}odot\\}\\}\\$, which preferentially host star-forming galaxies with rotationally-supported stellar discs. Such systems have oblate, spheroidal star-forming gas distributions, but in both less- and more-massive subhaloes the distributions tend to be prolate, and its morphology correlates positively and significantly with that of its host galaxy's stars, both in terms of sphericity and triaxiality. The minor axis of star-forming gas most commonly aligns with the minor axis of its host subhalo's DM, but often aligns more closely with one of the other two principal axes of the DM distribution in prolate subhaloes. Star-forming gas aligns with DM less strongly than is the case for stars, but its morphological minor axis aligns closely with its kinematic axis, affording a route to observational identification of the unsheared morphological axis. 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Imaging of such gas in the radio continuum enables\nweak lensing experiments that complement traditional optical approaches.\nStar-forming gas is typically more flattened than its associated stars\nand DM, particularly for present-day subhaloes of total mass \\${\\textbackslash}sim\\$\\$10{\\textasciicircum}\\{\\vphantom{\\}}\n12-12.5\\vphantom{\\{}\\} {\\textbackslash}mathrm\\{M\\_\\{ {\\textbackslash}odot\\}\\}\\$, which preferentially host star-forming\ngalaxies with rotationally-supported stellar discs. Such systems have\noblate, spheroidal star-forming gas distributions, but in both less- and\nmore-massive subhaloes the distributions tend to be prolate, and its\nmorphology correlates positively and significantly with that of its host\ngalaxy's stars, both in terms of sphericity and triaxiality. The minor\naxis of star-forming gas most commonly aligns with the minor axis of its\nhost subhalo's DM, but often aligns more closely with one of the other\ntwo principal axes of the DM distribution in prolate subhaloes.\nStar-forming gas aligns with DM less strongly than is the case for\nstars, but its morphological minor axis aligns closely with its\nkinematic axis, affording a route to observational identification of the\nunsheared morphological axis. 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