The origin of the H$α$ line profiles in simulated disc galaxies
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| Formato: | Preprint |
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2024
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| _version_ | 1866929500513632256 |
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| author | Ejdetjärn, Timmy Agertz, Oscar Östlin, Göran Rey, Martin P. Renaud, Florent |
| author_facet | Ejdetjärn, Timmy Agertz, Oscar Östlin, Göran Rey, Martin P. Renaud, Florent |
| contents | Observations of ionised H$α$ gas in high-redshift disc galaxies have ubiquitously found significant line broadening, $σ_{\rm Hα}\sim10-100$ km s$^{-1}$. To understand whether this broadening reflects gas turbulence within the interstellar medium (ISM) of galactic discs, or arises from out-of-plane emission in mass-loaded outflows, we perform radiation hydrodynamic (RHD) simulations of isolated Milky Way-mass disc galaxies in a gas-poor (low-redshift) and gas rich (high-redshift) condition and create mock H$α$ emission line profiles. We find that the majority of the total (integrated) H$α$ emission is confined within the ISM, with extraplanar gas contributing $\sim45$% of the extended profile wings ($v_z\geq200$ km s$^{-1}$) in the gas-rich galaxy. This substantiates using the H$α$ emission line as a tracer of mid-plane disc dynamics. We investigate the relative contribution of diffuse and dense H$α$ emitting gas, corresponding to diffuse ionised gas (DIG; $ρ\lesssim0.1$ cm$^{-3}$, $T\sim8\,000$ K) and HII regions ($ρ\gtrsim10$ cm$^{-3}$, $T\sim10\,000$ K), respectively, and find that DIG contributes $f_{\rm DIG}\lesssim10$% of the total L$_{\rm Hα}$. However, the DIG can reach upwards of $σ_{\rm Hα}\sim60-80$ km s$^{-1}$ while the HII regions are much less turbulent $σ_{\rm Hα}\sim10-40$ km $s^{-1}$. This implies that the $σ_{\rm Hα}$ observed using the full H$α$ emission line is dependent on the relative H$α$ contribution from DIG/HII regions and a larger $f_{\rm DIG}$ would shift $σ_{\rm Hα}$ to higher values. Finally, we show that $σ_{\rm Hα}$ evolves, in both the DIG and HII regions, with the galaxy gas fraction. Our high-redshift equivalent galaxy is roughly twice as turbulent, except for in the DIG which has a more shallow evolution. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2401_04160 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The origin of the H$α$ line profiles in simulated disc galaxies Ejdetjärn, Timmy Agertz, Oscar Östlin, Göran Rey, Martin P. Renaud, Florent Astrophysics of Galaxies Observations of ionised H$α$ gas in high-redshift disc galaxies have ubiquitously found significant line broadening, $σ_{\rm Hα}\sim10-100$ km s$^{-1}$. To understand whether this broadening reflects gas turbulence within the interstellar medium (ISM) of galactic discs, or arises from out-of-plane emission in mass-loaded outflows, we perform radiation hydrodynamic (RHD) simulations of isolated Milky Way-mass disc galaxies in a gas-poor (low-redshift) and gas rich (high-redshift) condition and create mock H$α$ emission line profiles. We find that the majority of the total (integrated) H$α$ emission is confined within the ISM, with extraplanar gas contributing $\sim45$% of the extended profile wings ($v_z\geq200$ km s$^{-1}$) in the gas-rich galaxy. This substantiates using the H$α$ emission line as a tracer of mid-plane disc dynamics. We investigate the relative contribution of diffuse and dense H$α$ emitting gas, corresponding to diffuse ionised gas (DIG; $ρ\lesssim0.1$ cm$^{-3}$, $T\sim8\,000$ K) and HII regions ($ρ\gtrsim10$ cm$^{-3}$, $T\sim10\,000$ K), respectively, and find that DIG contributes $f_{\rm DIG}\lesssim10$% of the total L$_{\rm Hα}$. However, the DIG can reach upwards of $σ_{\rm Hα}\sim60-80$ km s$^{-1}$ while the HII regions are much less turbulent $σ_{\rm Hα}\sim10-40$ km $s^{-1}$. This implies that the $σ_{\rm Hα}$ observed using the full H$α$ emission line is dependent on the relative H$α$ contribution from DIG/HII regions and a larger $f_{\rm DIG}$ would shift $σ_{\rm Hα}$ to higher values. Finally, we show that $σ_{\rm Hα}$ evolves, in both the DIG and HII regions, with the galaxy gas fraction. Our high-redshift equivalent galaxy is roughly twice as turbulent, except for in the DIG which has a more shallow evolution. |
| title | The origin of the H$α$ line profiles in simulated disc galaxies |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2401.04160 |