Reply to: Effects of density and temperature variations on the metallicity of Mrk 71
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| Format: | Preprint |
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2024
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| author | Chen, Yuguang Jones, Tucker Sanders, Ryan Fadda, Dario Sutter, Jessica Minchin, Robert Huntzinger, Erin Senchyna, Peter Stark, Daniel Spilker, Justin Weiner, Benjamin Roberts-Borsani, Guido |
| author_facet | Chen, Yuguang Jones, Tucker Sanders, Ryan Fadda, Dario Sutter, Jessica Minchin, Robert Huntzinger, Erin Senchyna, Peter Stark, Daniel Spilker, Justin Weiner, Benjamin Roberts-Borsani, Guido |
| contents | In Chen et al., 2023 (C23; arXiv:2304.09898), we introduced a new method to directly measure temperature fluctuations and applied it to a nearby dwarf galaxy, Mrk 71, finding a temperature fluctuation parameter $t^2 = 0.008\pm 0.043$. This result is lower by $\sim 2σ$ than the value required to explain the abundance discrepancy (AD) in this object. In the Matters Arising article submitted by Mendez-Delgado et al. (arXiv:2310.01197), the authors claim that using the same data presented in C23 in a different way, it is possible to conclude that the measurements are consistent with a larger $t^2 \simeq 0.1$ inferred indirectly from recombination lines (RLs). However, this requires a higher density such that the infrared [O III] 52 $μ$m and [O III] 88 $μ$m lines -- which form the basis of the direct measurement method -- are mutually inconsistent. Moreover, to reach agreement between the direct $t^2$ measurement and the larger $t^2$ value inferred from RLs requires systematically varying four parameters by $\sim 1σ$ from their best-determined values, which collectively amount to a $\sim2σ$ difference, consistent with the significance ($\sim 2 σ$) originally reported in C23. Therefore, we conclude that the results of C23 hold, and that the combined optical and infrared [O III] data disfavour $t^2 \simeq 0.1$ at the $\approx2σ$ level in Mrk 71. Future work is nonetheless warranted to better understand the AD associated with both optical and infrared emission line analysis. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2402_03105 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Reply to: Effects of density and temperature variations on the metallicity of Mrk 71 Chen, Yuguang Jones, Tucker Sanders, Ryan Fadda, Dario Sutter, Jessica Minchin, Robert Huntzinger, Erin Senchyna, Peter Stark, Daniel Spilker, Justin Weiner, Benjamin Roberts-Borsani, Guido Astrophysics of Galaxies In Chen et al., 2023 (C23; arXiv:2304.09898), we introduced a new method to directly measure temperature fluctuations and applied it to a nearby dwarf galaxy, Mrk 71, finding a temperature fluctuation parameter $t^2 = 0.008\pm 0.043$. This result is lower by $\sim 2σ$ than the value required to explain the abundance discrepancy (AD) in this object. In the Matters Arising article submitted by Mendez-Delgado et al. (arXiv:2310.01197), the authors claim that using the same data presented in C23 in a different way, it is possible to conclude that the measurements are consistent with a larger $t^2 \simeq 0.1$ inferred indirectly from recombination lines (RLs). However, this requires a higher density such that the infrared [O III] 52 $μ$m and [O III] 88 $μ$m lines -- which form the basis of the direct measurement method -- are mutually inconsistent. Moreover, to reach agreement between the direct $t^2$ measurement and the larger $t^2$ value inferred from RLs requires systematically varying four parameters by $\sim 1σ$ from their best-determined values, which collectively amount to a $\sim2σ$ difference, consistent with the significance ($\sim 2 σ$) originally reported in C23. Therefore, we conclude that the results of C23 hold, and that the combined optical and infrared [O III] data disfavour $t^2 \simeq 0.1$ at the $\approx2σ$ level in Mrk 71. Future work is nonetheless warranted to better understand the AD associated with both optical and infrared emission line analysis. |
| title | Reply to: Effects of density and temperature variations on the metallicity of Mrk 71 |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2402.03105 |