Quantifying inhomogeneities in the HI distributions of simulated galaxies

Hind Al Noori, Andrea V. Maccio, Aaron A. Dutton, Keri L. Dixon

Research output: Contribution to journalConference article

Abstract

The NIHAO cosmological simulations form a collection of a hundred high-resolution galaxies. We used these simulations to test the impact of stellar feedback on the morphology of the HI distribution in galaxies. We ran a subsample of twenty of the galaxies with different parameterizations of stellar feedback, looking for differences in the HI spatial distribution and morphology. We found that different feedback models do leave a signature in HI, and can potentially be compared with current and future observations. These findings can help inform future modeling efforts in the parameterization of stellar feedback in cosmological simulations of galaxy formation and evolution.

Original languageEnglish (US)
Article number012023
JournalJournal of Physics: Conference Series
Volume1258
Issue number1
DOIs
StatePublished - Oct 21 2019
Event1st Sharjah International Conference on Particle Physics, Astrophysics and Cosmology, FISICPAC 2018 - Sharjah, United Arab Emirates
Duration: Nov 11 2018Nov 13 2018

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inhomogeneity
galaxies
parameterization
simulation
galactic evolution
spatial distribution
signatures
high resolution

ASJC Scopus subject areas

  • Physics and Astronomy(all)

Cite this

Quantifying inhomogeneities in the HI distributions of simulated galaxies. / Al Noori, Hind; Maccio, Andrea V.; Dutton, Aaron A.; Dixon, Keri L.

In: Journal of Physics: Conference Series, Vol. 1258, No. 1, 012023, 21.10.2019.

Research output: Contribution to journalConference article

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AB - The NIHAO cosmological simulations form a collection of a hundred high-resolution galaxies. We used these simulations to test the impact of stellar feedback on the morphology of the HI distribution in galaxies. We ran a subsample of twenty of the galaxies with different parameterizations of stellar feedback, looking for differences in the HI spatial distribution and morphology. We found that different feedback models do leave a signature in HI, and can potentially be compared with current and future observations. These findings can help inform future modeling efforts in the parameterization of stellar feedback in cosmological simulations of galaxy formation and evolution.

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