论文标题
所有PAH：Akari-Spitzer横档档案光谱调查星系中的芳族排放调查
All the PAHs: an AKARI-Spitzer Cross Archival Spectroscopic Survey of Aromatic Emission in Galaxies
论文作者
论文摘要
我们提供了大量样本，由2.5-38 $ $ $ $的星系光谱从Akari-Spitzer Spitzer外层次频谱调查（ASESS）中的跨体积比较中得出，并研究了113个恒星形成星系的子集，具有突出的多环芳烃（PAH）发射范围，具有星星形成范围的范围。借助Akari的扩展2.5-5 $μm$波长的覆盖范围，我们首次使用修改版的Pahfit版本自动建模。我们发现$ l_ \ mathrm {pah \，3.3}/l_ \ mathrm {ir} $ $ \ sim $ 0.1％和3.3 $μm$ $ pah功能贡献$ \ sim $ \ sim $ \ sim $ \ sim $ 1.5-3％，对总PAH功率$ 1.5-3％ - 比以前假设的尘埃模型要少一些。我们建立了3.3美元的$ pah发射率和恒星形成速率之间的校准，但也可以找到它失去可靠性的机制，包括高发光性和低金属性。还对3.4美元的脂肪族排放和以3.47 $μm$为中心的广泛高原功能进行了建模。作为最短的波长PAH功能，3.3 $μm$容易受到衰减的影响，导致$ \ sim $ \ sim $ 3 $ 3的$ 3差异在高度遮盖的情况下，具有不同的假定衰减几何形状。令人惊讶的是，$ l_ \ mathrm {pah \，3.3} / l_ \ mathrm {σ\，pah} $在高发光性下没有下降的迹象，低金属型矮人Galaxy ii ZW 40 ZW 40表现出异常强的3.3 $ 3.3 $μm$μm$μm$μm$μm;这两个结果都表明，最小的PAHs比假定的强烈辐射场能够更好地生存，或者PAH发射在强烈和高能辐射环境中转移到较短的波长。提供了使用JWST/NIRCAM的3.3 $ $ PAH光度的光度替代物，并发现在低红移时非常可靠。
We present a large sample of 2.5-38 $μm$ galaxy spectra drawn from a cross-archival comparison in the AKARI-Spitzer Extragalactic Spectral Survey (ASESS), and investigate a subset of 113 star-forming galaxies with prominent polycyclic aromatic hydrocarbon (PAH) emission spanning a wide range of star formation properties. With AKARI's extended 2.5-5 $μm$ wavelength coverage, we self-consistently model for the first time all PAH emission bands using a modified version of PAHFIT. We find $L_\mathrm{PAH\,3.3}/L_\mathrm{IR}$ $\sim$ 0.1% and the 3.3 $μm$ PAH feature contributes $\sim$1.5-3% to the total PAH power -- somewhat less than earlier dust models have assumed. We establish a calibration between 3.3 $μm$ PAH emission and star formation rate, but also find regimes where it loses reliability, including at high luminosity and low metallicity. The 3.4 $μm$ aliphatic emission and a broad plateau feature centered at 3.47 $μm$ are also modeled. As the shortest wavelength PAH feature, 3.3 $μm$ is susceptible to attenuation, leading to a factor of $\sim$ 3 differences in the inferred star formation rate at high obscuration with different assumed attenuation geometries. Surprisingly, $L_\mathrm{PAH\, 3.3} / L_\mathrm{Σ\, PAH}$ shows no sign of decline at high luminosities, and the low metallicity dwarf galaxy II Zw 40 exhibits an unusually strong 3.3 $μm$ band; both results suggest either that the smallest PAHs are better able to survive under intense radiation fields than presumed, or that PAH emission is shifted to shorter wavelengths in intense and high energy radiation environments. A photometric surrogate for 3.3 $μm$ PAH luminosity using JWST/NIRCam is provided and found to be highly reliable at low redshift.
