论文标题
一个新的估计器的分子气体在附近星系中的分子气体
A new estimator of resolved molecular gas in nearby galaxies
论文作者
论文摘要
近期恒星形成的粉尘粉的光与星系中恒星形成气体的数量之间的关系产生了明智的12 $ $ m $ m发射与CO线排放之间的相关性。在这里，我们在kiloparsec尺度上探索了与CO（1-0）地图的kiloparsec量表，从分辨率匹配到明智的12 $μ$ m图像。我们发现每个星系中有强的CO-12 $ $ M相关性，我们表明全局CO-12 $μ$ M相关性中的散射主要是由星系到星系的差异驱动的。相关性比星形形成率与H $ _2 $表面密度（$σ（\ Mathrm {H_2}）$之间的相关性更强。我们探索多变量回归，以预测$σ（\ mathrm {h_2}）$在星形成像素中，使用明智的12 $μ$ m数据与全球和解决的星系属性相结合，并为最佳估计器提供拟合参数。我们发现，包括$σ（\ MathRM {\ MathRM {12 \>μm}）$包括$σ（\ MathRM {H_2}）$估计器能够预测$σ（\ m athrm {h_2}）$，比包括分辨率属性的估计器更准确，而不是包括溶液属性，而不是$ c（\ mathrmmathrm mathrm mathrm mathrm} $）。这些结果表明，由CO排放所追踪的12美元$ M排放和H $ _2 $在千乘量表上进行了物理连接。这可能是由于多环芳烃（PAH）发射与H $ _2 $的存在之间的联系。最佳的单期估计器是$ \ log \ frac {σ（\ mathrm {h_2}）}} {\ mathrm {m_ \ odot \> pc^{ - 2}}}} =（0.48 \ pm 0.01） +（0.71 \ pm 0.01 \ pm 0.01 \ pm pm 0.01 \ pm 0.01 \ pm 0.01 \ log \ frac {σ（\ mathrm {12 \>μm}）}} {\ Mathrm {l_ \ odot \> pc^{ - 2}}}} $。该相关性可用于有效估计$σ（\ mathrm {h_2}）$降至至少$ 1 \> m_ \ odot \> \ mathrm {pc^{ - 2}} $在附近星系中的星形区域中。
A relationship between dust-reprocessed light from recent star formation and the amount of star-forming gas in a galaxy produces a correlation between WISE 12 $μ$m emission and CO line emission. Here we explore this correlation on kiloparsec scales with CO(1-0) maps from EDGE-CALIFA matched in resolution to WISE 12 $μ$m images. We find strong CO-12 $μ$m correlations within each galaxy and we show that the scatter in the global CO-12 $μ$m correlation is largely driven by differences from galaxy to galaxy. The correlation is stronger than that between star formation rate and H$_2$ surface densities ($Σ(\mathrm{H_2})$). We explore multi-variable regression to predict $Σ(\mathrm{H_2})$ in star-forming pixels using the WISE 12 $μ$m data combined with global and resolved galaxy properties, and provide the fit parameters for the best estimators. We find that $Σ(\mathrm{H_2})$ estimators that include $Σ(\mathrm{12\>μm})$ are able to predict $Σ(\mathrm{H_2})$ more accurately than estimators that include resolved optical properties instead of $Σ(\mathrm{12\>μm})$. These results suggest that 12 $μ$m emission and H$_2$ as traced by CO emission are physically connected at kiloparsec scales. This may be due to a connection between polycyclic aromatic hydrocarbon (PAH) emission and the presence of H$_2$. The best single-property estimator is $\log \frac{Σ(\mathrm{H_2})}{\mathrm{M_\odot\>pc^{-2}}} = (0.48 \pm 0.01) + (0.71 \pm 0.01)\log \frac{Σ(\mathrm{12\>μm})}{\mathrm{L_\odot\>pc^{-2}}}$. This correlation can be used to efficiently estimate $Σ(\mathrm{H_2})$ down to at least $1 \> M_\odot \> \mathrm{pc^{-2}}$ in star-forming regions within nearby galaxies.
