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Emission Line Velocity, Metallicity and Extinction Maps of the Small Magellanic Cloud
Astrophysics of Galaxies · Submitted 8 Nov 2024
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim These measurements enable a detailed examination of the SMC, highlighting its nature as a disrupted satellite galaxy.
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The abstract, sentence by sentence
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$\alpha$ radial velocity and H$\alpha$ 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$\alpha$ 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$\alpha$ and HI across the SMC have also been compared, with the H$\alpha$ 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.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | 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). | method 0.99 | 0.93 | 0.02 | asserted 1.00 |
| s1 | Interpolated maps of the gas-phase metallicity, extinction, H$\alpha$ radial velocity and H$\alpha$ velocity dispersion have been made from these measurements. | contribution 0.48 | 0.93 | 0.07 | asserted 1.00 |
| s2 | 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. | result 1.00 | 0.92 | 0.18 | asserted 1.00 |
| s3 | 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. | result 1.00 | 0.93 | 0.07 | asserted 1.00 |
| s4 | The SMC eastern arm has lower extinction than the main body. | result 1.00 | 0.89 | 0.04 | asserted 1.00 |
| s5 | The radial velocity of the gas from the H$\alpha$ line and the HI line have been compared across the SMC. | contribution 0.53 | 0.92 | 0.03 | asserted 1.00 |
| s6 | In general there is good agreement between the two measurements, though there are a few notable exceptions. | result 1.00 | 0.90 | 0.05 | asserted 0.93 |
| s7 | 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$^{-1}$. | result 1.00 | 0.93 | 0.08 | asserted 1.00 |
| s8 | The velocity dispersion from H$\alpha$ and HI across the SMC have also been compared, with the H$\alpha$ velocity dispersion usually the higher of the two. | result 0.98 | 0.93 | 0.04 | asserted 0.98 |
| s9 | The eastern arm of the SMC generally has lower velocity dispersion than the SMC's main body. | result 1.00 | 0.93 | 0.05 | asserted 0.98 |
| s10 | These measurements enable a detailed examination of the SMC, highlighting its nature as a disrupted satellite galaxy. | interpretation 0.98 | 0.53 | 0.67 | asserted 0.96 |
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The paper
Original abstract
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$\alpha$ radial velocity and H$\alpha$ 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$\alpha$ 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$\alpha$ and HI across the SMC have also been compared, with the H$\alpha$ 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.
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This is consistent with a gas-phase metallicity gradient across the SMC, and corresponds to the stellar metallicity gradient found by many authors [ref] .
Ca II Triplet Spectroscopy of Small Magellanic Cloud Red Giants. V. Abundances and Velocities for 12 Massive Clusters · Gas-Phase Metallicity · 0.87
Cites as background 1 paper
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The stellar metallicity across the SMC has been measured in detail by many authors including [ref] , [ref] , [ref] , [ref] , [ref] , [ref] , [ref] , [ref] , [ref] , [ref] and [ref] .
Ca II Triplet Spectroscopy of Small Magellanic Cloud Red Giants. V. Abundances and Velocities for 12 Massive Clusters · Introduction · 0.95
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