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Interaction effects on galaxy pairs with Gemini/GMOS- I: Electron density
Cosmology and Nongalactic Astrophysics · Submitted 29 Oct 2013
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Our results indicate that the electron density estimates obtained of HII regions from our sample of interacting galaxies are systematically higher than those derived for isolated galaxies.
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The abstract, sentence by sentence
We present an observational study about the impacts of the interactions in the electron density of \ion{H}{ii} regions located in 7 systems of interacting galaxies. The data consist of long-slit spectra in the range 4400-7300 A, obtained with the Gemini Multi-Object Spectrograph at Gemini South (GMOS). The electron density was determined using the ratio of emission lines [SII]6716/6731. Our results indicate that the electron density estimates obtained of HII regions from our sample of interacting galaxies are systematically higher than those derived for isolated galaxies. The mean electron density values of interacting galaxies are in the range of $N_{\rm e}=24-532$\,$ \rm cm^{-3}$, while those obtained for isolated galaxies are in the range of $N_{\rm e}=40-137\: \rm cm^{-3}$. Comparing the observed emission lines with predictions of photoionization models, we verified that almost all the \ion{H}{ii} regions of the galaxies AM\,1054A, AM\,2058B, and AM\,2306B, have emission lines excited by shock gas. For the remaining galaxies, only few HII regions has emission lines excited by shocks, such as in AM\,2322B (1 point), and AM\,2322A (4 points). No correlation is obtained between the presence of shocks and electron densities. Indeed, the highest electron density values found in our sample do not belong to the objects with gas shock excitation. We emphasize the importance of considering theses quantities especially when the metallicity is derived for these types of systems.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We present an observational study about the impacts of the interactions in the electron density of \ion{H}{ii} regions located in 7 systems of interacting galaxies. | contribution 1.00 | 0.92 | 0.05 | asserted 0.69 |
| s1 | The data consist of long-slit spectra in the range 4400-7300 A, obtained with the Gemini Multi-Object Spectrograph at Gemini South (GMOS). | method 1.00 | 0.90 | 0.01 | asserted 0.99 |
| s2 | The electron density was determined using the ratio of emission lines [SII]6716/6731. | method 1.00 | 0.89 | 0.02 | asserted 1.00 |
| s3 | Our results indicate that the electron density estimates obtained of HII regions from our sample of interacting galaxies are systematically higher than those derived for isolated galaxies. | result 1.00 | 0.96 | 0.81 | hedged possibility 0.86 |
| s4 | The mean electron density values of interacting galaxies are in the range of $N_{\rm e}=24-532$\,$ \rm cm^{-3}$, while those obtained for isolated galaxies are in the range of $N_{\rm e}=40-137\: \rm cm^{-3}$. | result 1.00 | 0.93 | 0.34 | asserted 1.00 |
| s5 | Comparing the observed emission lines with predictions of photoionization models, we verified that almost all the \ion{H}{ii} regions of the galaxies AM\,1054A, AM\,2058B, and AM\,2306B, have emission lines excited by shock gas. | result 0.95 | 0.95 | 0.06 | asserted 0.99 |
| s6 | For the remaining galaxies, only few HII regions has emission lines excited by shocks, such as in AM\,2322B (1 point), and AM\,2322A (4 points). | result 1.00 | 0.93 | 0.03 | asserted 0.99 |
| s7 | No correlation is obtained between the presence of shocks and electron densities. | result 0.98 | 0.95 | 0.11 | asserted 1.00 |
| s8 | Indeed, the highest electron density values found in our sample do not belong to the objects with gas shock excitation. | result 0.83 | 0.96 | 0.11 | asserted 1.00 |
| s9 | We emphasize the importance of considering theses quantities especially when the metallicity is derived for these types of systems. | interpretation 0.90 | 0.20 | 0.08 | asserted 0.87 |
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Original abstract
We present an observational study about the impacts of the interactions in the electron density of \ion{H}{ii} regions located in 7 systems of interacting galaxies. The data consist of long-slit spectra in the range 4400-7300 A, obtained with the Gemini Multi-Object Spectrograph at Gemini South (GMOS). The electron density was determined using the ratio of emission lines [SII]6716/6731. Our results indicate that the electron density estimates obtained of HII regions from our sample of interacting galaxies are systematically higher than those derived for isolated galaxies. The mean electron density values of interacting galaxies are in the range of $N_{\rm e}=24-532$\,$ \rm cm^{-3}$, while those obtained for isolated galaxies are in the range of $N_{\rm e}=40-137\: \rm cm^{-3}$. Comparing the observed emission lines with predictions of photoionization models, we verified that almost all the \ion{H}{ii} regions of the galaxies AM\,1054A, AM\,2058B, and AM\,2306B, have emission lines excited by shock gas. For the remaining galaxies, only few HII regions has emission lines excited by shocks, such as in AM\,2322B (1 point), and AM\,2322A (4 points). No correlation is obtained between the presence of shocks and electron densities. Indeed, the highest electron density values found in our sample do not belong to the objects with gas shock excitation. We emphasize the importance of considering theses quantities especially when the metallicity is derived for these types of systems.
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