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| Auteurs principaux: | , , , , |
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| Format: | Preprint |
| Publié: |
2024
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| Sujets: | |
| Accès en ligne: | https://arxiv.org/abs/2411.05523 |
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- Optical emission lines across the Small Magellanic Cloud (SMC) have been measured from multiple fields using the Australian National University (ANU) 2.3m telescope with the Wide-Field Spectrograph (WiFeS). Interpolated maps of the gas-phase metallicity, extinction, H$α$ radial velocity and H$α$ velocity dispersion have been made from these measurements. There is a metallicity gradient from the centre to the north of the galaxy of ~-0.095 dex/kpc with a shallower metallicity gradient from the centre to the south of the galaxy of ~-0.013 dex/kpc. There is an extinction gradient of ~-0.086 E(B-V)/kpc from the centre going north and shallower going from the centre to the south of ~-0.0089 E(B-V)/kpc. The SMC eastern arm has lower extinction than the main body. The radial velocity of the gas from the H$α$ line and the HI line have been compared across the SMC. In general there is good agreement between the two measurements, though there are a few notable exceptions. Both show a region that has different radial velocity to the bulk motion of the SMC in the southern western corner by at least 16 kms$^{-1}$. The velocity dispersion from H$α$ and HI across the SMC have also been compared, with the H$α$ velocity dispersion usually the higher of the two. The eastern arm of the SMC generally has lower velocity dispersion than the SMC's main body. These measurements enable a detailed examination of the SMC, highlighting its nature as a disrupted satellite galaxy.