PHANGS-MeerKAT and MHONGOOSE HI observations of nearby spiral galaxies: physical drivers of the molecular gas fraction, $R_{\mathrm{mol}}$
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2024
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| author | Eibensteiner, Cosima Sun, Jiayi Bigiel, Frank Leroy, Adam K. Schinnerer, Eva Rosolowsky, Erik Kurapati, Sushma Pisano, D. J. de Blok, W. J. G Barnes, Ashley T. Thorp, Mallory Colombo, Dario Koch, Eric W. Chiang, I-Da Ostriker, Eve C. Murphy, Eric J. Zabel, Nikki Laudage, Sebstian Maccagni, Filippo M. Healy, Julia Sekhar, Srikrishna Utomo, Dyas Brok, Jakob den Cao, Yixian Chevance, Mélanie Dale, Daniel A. Faesi, Christopher M. Glover, Simon C. O. He, Hao Jeffreson, Sarah Jiménez-Donaire, María J. Klessen, Ralf Neumann, Justus Pan, Hsi-An Pathak, Debosmita Querejeta, Miguel Teng, Yu-Hsuan Usero, Antonio Williams, Thomas G. |
| author_facet | Eibensteiner, Cosima Sun, Jiayi Bigiel, Frank Leroy, Adam K. Schinnerer, Eva Rosolowsky, Erik Kurapati, Sushma Pisano, D. J. de Blok, W. J. G Barnes, Ashley T. Thorp, Mallory Colombo, Dario Koch, Eric W. Chiang, I-Da Ostriker, Eve C. Murphy, Eric J. Zabel, Nikki Laudage, Sebstian Maccagni, Filippo M. Healy, Julia Sekhar, Srikrishna Utomo, Dyas Brok, Jakob den Cao, Yixian Chevance, Mélanie Dale, Daniel A. Faesi, Christopher M. Glover, Simon C. O. He, Hao Jeffreson, Sarah Jiménez-Donaire, María J. Klessen, Ralf Neumann, Justus Pan, Hsi-An Pathak, Debosmita Querejeta, Miguel Teng, Yu-Hsuan Usero, Antonio Williams, Thomas G. |
| contents | The molecular-to-atomic gas ratio is crucial to the evolution of the interstellar medium in galaxies. We investigate the balance between the atomic ($Σ_{\rm HI}$) and molecular gas ($Σ_{\rm H2}$) surface densities in eight nearby star-forming galaxies using new high-quality observations from MeerKAT and ALMA (for HI and CO, respectively). We define the molecular gas ratio as $R_{\rm mol} = Σ_{\rm H2} / Σ_{\rm HI}$ and measure how it depends on local conditions in the galaxy disks using multi-wavelength observations. We find that, depending on the galaxy, HI is detected at $>3σ$ out to 20-120 kpc in galactocentric radius ($r_{\rm gal}$). The typical radius at which $Σ_{\rm HI}$ reaches 1~$\rm M_\odot~pc^{-2}$ is $r_{\rm HI}\approx22$~kpc, which corresponds to 1-3 times the optical radius ($r_{25}$). $R_{\rm mol}$ correlates best with the dynamical equilibrium pressure, P$_{\rm DE}$, among potential drivers studied, with a median correlation coefficient of $<ρ>=0.89$. Correlations between $R_{\rm mol}$ and star formation rate, total gas and stellar surface density, metallicity, and $Σ_{\rm SFR}$/P$_{\rm DE}$ are present but somewhat weaker. Our results also show a direct correlation between P$_{\rm DE}$ and $Σ_{\rm SFR}$, supporting self-regulation models. Quantitatively, we measure similar scalings as previous works and attribute the modest differences that we find to the effect of varying resolution and sensitivity. At $r_{\rm gal} {\gtrsim}0.4~r_{25}$, atomic gas dominates over molecular gas, and at the balance of these two gas phases, we find that the baryon mass is dominated by stars, with $Σ_{*} > 5~Σ_{\rm gas}$. Our study constitutes an important step in the statistical investigation of how local galaxy properties impact the conversion from atomic to molecular gas in nearby galaxies. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2407_01716 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | PHANGS-MeerKAT and MHONGOOSE HI observations of nearby spiral galaxies: physical drivers of the molecular gas fraction, $R_{\mathrm{mol}}$ Eibensteiner, Cosima Sun, Jiayi Bigiel, Frank Leroy, Adam K. Schinnerer, Eva Rosolowsky, Erik Kurapati, Sushma Pisano, D. J. de Blok, W. J. G Barnes, Ashley T. Thorp, Mallory Colombo, Dario Koch, Eric W. Chiang, I-Da Ostriker, Eve C. Murphy, Eric J. Zabel, Nikki Laudage, Sebstian Maccagni, Filippo M. Healy, Julia Sekhar, Srikrishna Utomo, Dyas Brok, Jakob den Cao, Yixian Chevance, Mélanie Dale, Daniel A. Faesi, Christopher M. Glover, Simon C. O. He, Hao Jeffreson, Sarah Jiménez-Donaire, María J. Klessen, Ralf Neumann, Justus Pan, Hsi-An Pathak, Debosmita Querejeta, Miguel Teng, Yu-Hsuan Usero, Antonio Williams, Thomas G. Astrophysics of Galaxies The molecular-to-atomic gas ratio is crucial to the evolution of the interstellar medium in galaxies. We investigate the balance between the atomic ($Σ_{\rm HI}$) and molecular gas ($Σ_{\rm H2}$) surface densities in eight nearby star-forming galaxies using new high-quality observations from MeerKAT and ALMA (for HI and CO, respectively). We define the molecular gas ratio as $R_{\rm mol} = Σ_{\rm H2} / Σ_{\rm HI}$ and measure how it depends on local conditions in the galaxy disks using multi-wavelength observations. We find that, depending on the galaxy, HI is detected at $>3σ$ out to 20-120 kpc in galactocentric radius ($r_{\rm gal}$). The typical radius at which $Σ_{\rm HI}$ reaches 1~$\rm M_\odot~pc^{-2}$ is $r_{\rm HI}\approx22$~kpc, which corresponds to 1-3 times the optical radius ($r_{25}$). $R_{\rm mol}$ correlates best with the dynamical equilibrium pressure, P$_{\rm DE}$, among potential drivers studied, with a median correlation coefficient of $<ρ>=0.89$. Correlations between $R_{\rm mol}$ and star formation rate, total gas and stellar surface density, metallicity, and $Σ_{\rm SFR}$/P$_{\rm DE}$ are present but somewhat weaker. Our results also show a direct correlation between P$_{\rm DE}$ and $Σ_{\rm SFR}$, supporting self-regulation models. Quantitatively, we measure similar scalings as previous works and attribute the modest differences that we find to the effect of varying resolution and sensitivity. At $r_{\rm gal} {\gtrsim}0.4~r_{25}$, atomic gas dominates over molecular gas, and at the balance of these two gas phases, we find that the baryon mass is dominated by stars, with $Σ_{*} > 5~Σ_{\rm gas}$. Our study constitutes an important step in the statistical investigation of how local galaxy properties impact the conversion from atomic to molecular gas in nearby galaxies. |
| title | PHANGS-MeerKAT and MHONGOOSE HI observations of nearby spiral galaxies: physical drivers of the molecular gas fraction, $R_{\mathrm{mol}}$ |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2407.01716 |