Revisiting the Vertical Distribution of HI Absorbing Clouds in the Solar Neighborhood. II. Constraints from a Large Catalog of 21 cm Absorption Observations at High Galactic Latitudes
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2024
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| _version_ | 1866909327557656576 |
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| author | Rybarczyk, Daniel R. Wenger, Trey V. Stanimirović, Snezana |
| author_facet | Rybarczyk, Daniel R. Wenger, Trey V. Stanimirović, Snezana |
| contents | The cold neutral medium (CNM) is where neutral atomic hydrogen (HI) is converted into molecular clouds, so the structure and kinematics of the CNM are key drivers of galaxy evolution. Here we provide new constraints on the vertical distribution of the CNM using the recently-developed $\texttt{kinematic_scaleheight}$ software package and a large catalog of sensitive HI absorption observations. We estimate the thickness of the CNM in the solar neighborhood to be $σ_z\sim50$$\unicode{x2013}$$90~\mathrm{pc}$, assuming a Gaussian vertical distribution. This is a factor of $\sim2$ smaller than typically assumed, indicating the thickness of the CNM in the solar neighborhood is similar to that found in the inner Galaxy, consistent with recent simulation results. If we consider only structures with HI optical depths $τ>0.1$ or column densities $N(\mathrm{HI})>10^{19.5}~\mathrm{cm^{-2}}$, which recent work suggests are thresholds for molecule formation, we find $σ_z\sim50~\mathrm{pc}$. Meanwhile, for structures with $τ<0.1$ or column densities $N(\mathrm{HI})<10^{19.5}~\mathrm{cm^{-2}}$, we find $σ_z\sim120~\mathrm{pc}$. These thicknesses are similar to those derived for the thin- and thick-disk molecular cloud populations traced by CO emission, possibly suggesting that cold HI and CO are well-mixed. Approximately $20\%$ of CNM structures are identified as outliers, with kinematics that are not well-explained by Galactic rotation. We show that some of these CNM structures $\unicode{x2014}$ perhaps representing intermediate velocity clouds $\unicode{x2014}$ are associated with the Local Bubble wall. We compare our results to recent observations and simulations, and we discuss their implications for the multiphase structure of the Milky Way's interstellar medium. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2409_18190 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Revisiting the Vertical Distribution of HI Absorbing Clouds in the Solar Neighborhood. II. Constraints from a Large Catalog of 21 cm Absorption Observations at High Galactic Latitudes Rybarczyk, Daniel R. Wenger, Trey V. Stanimirović, Snezana Astrophysics of Galaxies The cold neutral medium (CNM) is where neutral atomic hydrogen (HI) is converted into molecular clouds, so the structure and kinematics of the CNM are key drivers of galaxy evolution. Here we provide new constraints on the vertical distribution of the CNM using the recently-developed $\texttt{kinematic_scaleheight}$ software package and a large catalog of sensitive HI absorption observations. We estimate the thickness of the CNM in the solar neighborhood to be $σ_z\sim50$$\unicode{x2013}$$90~\mathrm{pc}$, assuming a Gaussian vertical distribution. This is a factor of $\sim2$ smaller than typically assumed, indicating the thickness of the CNM in the solar neighborhood is similar to that found in the inner Galaxy, consistent with recent simulation results. If we consider only structures with HI optical depths $τ>0.1$ or column densities $N(\mathrm{HI})>10^{19.5}~\mathrm{cm^{-2}}$, which recent work suggests are thresholds for molecule formation, we find $σ_z\sim50~\mathrm{pc}$. Meanwhile, for structures with $τ<0.1$ or column densities $N(\mathrm{HI})<10^{19.5}~\mathrm{cm^{-2}}$, we find $σ_z\sim120~\mathrm{pc}$. These thicknesses are similar to those derived for the thin- and thick-disk molecular cloud populations traced by CO emission, possibly suggesting that cold HI and CO are well-mixed. Approximately $20\%$ of CNM structures are identified as outliers, with kinematics that are not well-explained by Galactic rotation. We show that some of these CNM structures $\unicode{x2014}$ perhaps representing intermediate velocity clouds $\unicode{x2014}$ are associated with the Local Bubble wall. We compare our results to recent observations and simulations, and we discuss their implications for the multiphase structure of the Milky Way's interstellar medium. |
| title | Revisiting the Vertical Distribution of HI Absorbing Clouds in the Solar Neighborhood. II. Constraints from a Large Catalog of 21 cm Absorption Observations at High Galactic Latitudes |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2409.18190 |