HI within and around observed and simulated galaxy discs -- Comparing MeerKAT observations with mock data from TNG50 and FIRE-2

A. Marasco; W. J. G. de Blok; F. M. Maccagni; F. Fraternali; K. A. Oman; T. Oosterloo; F. Combes; S. S. McGaugh; P. Kamphuis; K. Spekkens; D. Kleiner; S. Veronese; P. Amram; L. Chemin; E. Brinks

HI within and around observed and simulated galaxy discs -- Comparing MeerKAT observations with mock data from TNG50 and FIRE-2

A. Marasco, W. J. G. de Blok, F. M. Maccagni, F. Fraternali, K. A. Oman, T. Oosterloo, F. Combes, S. S. McGaugh, P. Kamphuis, K. Spekkens, D. Kleiner, S. Veronese, P. Amram, L. Chemin, E. Brinks

Research output: Contribution to journal › Article › peer-review

Abstract

Atomic hydrogen (HI) is an ideal tracer of gas flows in and around galaxies, and it is uniquely observable in the nearby Universe. Here we make use of wide-field (~1 square degree), spatially resolved (down to 22"), high-sensitivity (~$10^{18}$ cm$^{-2}$) HI observations of 5 nearby galaxies with stellar mass of $5\times10^{10}$ M$_\odot$, taken with the MeerKAT radio telescope. Four of these were observed as part of the MHONGOOSE survey. We characterise their main HI properties and compare these with synthetic HI data from a sample of 25 similarly massive star-forming galaxies from the TNG50 (20) and FIRE-2 (5) suites of cosmological hydrodynamical simulations. Globally, the simulated systems have HI and molecular hydrogen (H$_2$) masses in good agreement with the observations, but only when the H$_2$ recipe of Blitz & Rosolowsky (2006) is employed. The other recipes that we tested overestimate the H$_2$-to-HI mass fraction by up to an order of magnitude. On a local scale, we find two main discrepancies between observed and simulated data. First, the simulated galaxies show a more irregular HI morphology than the observed ones due to the presence of HI with column density $

Original language	English
Journal	Astronomy & Astrophysics
Publication status	Accepted/In press - 3 Mar 2025

Keywords

astro-ph.GA

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2503.03818v1Accepted author manuscript, 19.2 MB

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Marasco, A., de Blok, W. J. G., Maccagni, F. M., Fraternali, F., Oman, K. A., Oosterloo, T., Combes, F., McGaugh, S. S., Kamphuis, P., Spekkens, K., Kleiner, D., Veronese, S., Amram, P., Chemin, L., & Brinks, E. (Accepted/In press). HI within and around observed and simulated galaxy discs -- Comparing MeerKAT observations with mock data from TNG50 and FIRE-2. Astronomy & Astrophysics.

@article{b27451f39be64dc2ac72b3b9188b7f13,

title = "HI within and around observed and simulated galaxy discs -- Comparing MeerKAT observations with mock data from TNG50 and FIRE-2",

abstract = "Atomic hydrogen (HI) is an ideal tracer of gas flows in and around galaxies, and it is uniquely observable in the nearby Universe. Here we make use of wide-field (~1 square degree), spatially resolved (down to 22{"}), high-sensitivity (~$10^{18}$ cm$^{-2}$) HI observations of 5 nearby galaxies with stellar mass of $5\times10^{10}$ M$_\odot$, taken with the MeerKAT radio telescope. Four of these were observed as part of the MHONGOOSE survey. We characterise their main HI properties and compare these with synthetic HI data from a sample of 25 similarly massive star-forming galaxies from the TNG50 (20) and FIRE-2 (5) suites of cosmological hydrodynamical simulations. Globally, the simulated systems have HI and molecular hydrogen (H$_2$) masses in good agreement with the observations, but only when the H$_2$ recipe of Blitz & Rosolowsky (2006) is employed. The other recipes that we tested overestimate the H$_2$-to-HI mass fraction by up to an order of magnitude. On a local scale, we find two main discrepancies between observed and simulated data. First, the simulated galaxies show a more irregular HI morphology than the observed ones due to the presence of HI with column density $",

keywords = "astro-ph.GA",

author = "A. Marasco and {de Blok}, {W. J. G.} and Maccagni, {F. M.} and F. Fraternali and Oman, {K. A.} and T. Oosterloo and F. Combes and McGaugh, {S. S.} and P. Kamphuis and K. Spekkens and D. Kleiner and S. Veronese and P. Amram and L. Chemin and E. Brinks",

note = "25 pages, 21 figures, accepted by A&A",

year = "2025",

month = mar,

day = "3",

language = "English",

journal = "Astronomy & Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

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TY - JOUR

T1 - HI within and around observed and simulated galaxy discs -- Comparing MeerKAT observations with mock data from TNG50 and FIRE-2

AU - Marasco, A.

AU - de Blok, W. J. G.

AU - Maccagni, F. M.

AU - Fraternali, F.

AU - Oman, K. A.

AU - Oosterloo, T.

AU - Combes, F.

AU - McGaugh, S. S.

AU - Kamphuis, P.

AU - Spekkens, K.

AU - Kleiner, D.

AU - Veronese, S.

AU - Amram, P.

AU - Chemin, L.

AU - Brinks, E.

N1 - 25 pages, 21 figures, accepted by A&A

PY - 2025/3/3

Y1 - 2025/3/3

N2 - Atomic hydrogen (HI) is an ideal tracer of gas flows in and around galaxies, and it is uniquely observable in the nearby Universe. Here we make use of wide-field (~1 square degree), spatially resolved (down to 22"), high-sensitivity (~$10^{18}$ cm$^{-2}$) HI observations of 5 nearby galaxies with stellar mass of $5\times10^{10}$ M$_\odot$, taken with the MeerKAT radio telescope. Four of these were observed as part of the MHONGOOSE survey. We characterise their main HI properties and compare these with synthetic HI data from a sample of 25 similarly massive star-forming galaxies from the TNG50 (20) and FIRE-2 (5) suites of cosmological hydrodynamical simulations. Globally, the simulated systems have HI and molecular hydrogen (H$_2$) masses in good agreement with the observations, but only when the H$_2$ recipe of Blitz & Rosolowsky (2006) is employed. The other recipes that we tested overestimate the H$_2$-to-HI mass fraction by up to an order of magnitude. On a local scale, we find two main discrepancies between observed and simulated data. First, the simulated galaxies show a more irregular HI morphology than the observed ones due to the presence of HI with column density $

AB - Atomic hydrogen (HI) is an ideal tracer of gas flows in and around galaxies, and it is uniquely observable in the nearby Universe. Here we make use of wide-field (~1 square degree), spatially resolved (down to 22"), high-sensitivity (~$10^{18}$ cm$^{-2}$) HI observations of 5 nearby galaxies with stellar mass of $5\times10^{10}$ M$_\odot$, taken with the MeerKAT radio telescope. Four of these were observed as part of the MHONGOOSE survey. We characterise their main HI properties and compare these with synthetic HI data from a sample of 25 similarly massive star-forming galaxies from the TNG50 (20) and FIRE-2 (5) suites of cosmological hydrodynamical simulations. Globally, the simulated systems have HI and molecular hydrogen (H$_2$) masses in good agreement with the observations, but only when the H$_2$ recipe of Blitz & Rosolowsky (2006) is employed. The other recipes that we tested overestimate the H$_2$-to-HI mass fraction by up to an order of magnitude. On a local scale, we find two main discrepancies between observed and simulated data. First, the simulated galaxies show a more irregular HI morphology than the observed ones due to the presence of HI with column density $

KW - astro-ph.GA

M3 - Article

SN - 0004-6361

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

ER -

HI within and around observed and simulated galaxy discs -- Comparing MeerKAT observations with mock data from TNG50 and FIRE-2

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Keywords

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