论文标题
恒星形成和分子气体诊断中等和远红外发射
Star Formation and Molecular Gas Diagnostics with Mid- and Far-Infrared Emission
论文作者
论文摘要
随着JWST观察的开始，来自多环芳烃（PAHS），H $ _2 $旋转线，来自离子的精细结构线以及尘埃连续的旋转线和灰尘连续性将是各种红色速度的Galaxies的气体和恒星形成速率（SFR）的中红外（MIR）发射特征。这些示踪剂中的许多源自大型恒星的紫外光子照亮的灰尘和气体，因此它们通常会在不同程度上追踪SFR和气体。我们研究了miR光谱特征从5 $ $ m和从3.4到250 $μ$ m的光度法与由电离霓虹灯（15.6 $ $ m [ne III]和12.8 $μ$ m [ne II]）和由碳一氧化碳（CO）追踪的SFR相关。通常，我们发现miR发射功能（即pahs和h $ _2 $旋转线）比CO和SFR互相跟踪。 h $ _2 $行和PAH功能与离子的精细结构线最相关，与SFR最相关。尤其是在18.7和33.5 $μm处的[S III]线与SFR具有非常紧密的相关性，我们使用它们来校准具有可忽略的金属依赖性的SFR的新的单参数mir示踪剂。 17美元$ $ m/7.7 $ $ m pAh特征比率随CO发射的函数增加，这可能是PAH生长或分子气中中和的证据。灰尘连续发射轨迹SFR或CO的程度随波长的函数而变化，连续体在20至70美元$ $ m m的过程中更好地跟踪SFR，而更长的波长则更好。
With the start of JWST observations, mid-infrared (MIR) emission features from polycyclic aromatic hydrocarbons (PAHs), H$_2$ rotational lines, fine-structure lines from ions, and dust continuum will be widely available tracers of gas and star formation rate (SFR) in galaxies at various redshifts. Many of these tracers originate from dust and gas illuminated by UV photons from massive stars, so they generally trace both SFR and gas to varying degrees. We investigate how MIR spectral features from 5 to 35$μ$m and photometry from 3.4 to 250$μ$m correlate with SFR traced by ionized neon (15.6$μ$m [Ne III] and 12.8$μ$m [Ne II]) and molecular gas traced by carbon monoxide (CO). In general, we find MIR emission features (i.e. PAHs and H$_2$ rotational lines) trace both CO and SFR better than CO and SFR trace one another. H$_2$ lines and PAH features correlate best with CO. Fine-structure lines from ions correlate best with SFR. The [S III] lines at 18.7 and 33.5$μ$m, in particular, have a very tight correlation with SFR, and we use them to calibrate new single-parameter MIR tracers of SFR that have negligible metallicity dependence. The 17$μ$m/7.7$μ$m PAH feature ratio increases as a function of CO emission which may be evidence of PAH growth or neutralization in molecular gas. The degree to which dust continuum emission traces SFR or CO varies as a function of wavelength, with continuum between 20 to 70$μ$m better tracing SFR, while longer wavelengths better trace CO.
