标题： 连续中红外恒星形成率指示器：0<z<3星系形成恒星的诊断方法 显示英文标题

标题： Continuous Mid-Infrared Star Formation Rate Indicators: Diagnostics for 0<z<3 Star Forming Galaxies

摘要： 我们展示了在中红外波长范围6-70微米内的连续单色恒星形成率（SFR）指标。 我们使用了红移小于0.2的斯皮策-SDSS-GALEX光谱调查（SSGSS）中的58个恒星形成星系（SFGs）样本，这些星系从紫外到红外都有丰富的多波段测光和光谱数据。 这些星系的斯皮策红外光谱仪（IRS）数据覆盖5-40微米，并与它们的测光对应物相匹配。 40-70微米的光谱区域通过尘埃模型拟合IRS光谱以及斯皮策70和160微米的测光数据进行插值。 由于该区域没有明显的光谱特征，我们预计这些插值是稳健的。 通过使用几种参考SFR指标来减轻潜在偏差，该光谱范围被校准为SFR诊断工具。 我们的特定波段连续SFR指标被发现与本地宇宙中的单色校准一致，这些校准来自斯皮策、WISE和赫歇尔的测光数据。 我们的本地综合模板和连续SFR诊断工具可通过NASA/IPAC红外科学档案（IRSA）公开使用，其典型离散度为30%或更小。 我们讨论了在揭示星系形成和演化背景下的SFR指标的有效性和适用范围。 此外，在詹姆斯·韦布空间望远镜时代，这将成为一种灵活的工具，适用于红移高达~3的任何SFG。 显示英文摘要

摘要： We present continuous, monochromatic star formation rate (SFR) indicators over the mid-infrared wavelength range of 6-70 micron. We use a sample of 58 star forming galaxies (SFGs) in the Spitzer-SDSS-GALEX Spectroscopic Survey (SSGSS) at z<0.2, for which there is a rich suite of multi-wavelength photometry and spectroscopy from the ultraviolet through to the infrared. The data from the Spitzer infrared spectrograph (IRS) of these galaxies, which spans 5-40 micron, is anchored to their photometric counterparts. The spectral region between 40-70 micron is interpolated using dust model fits to the IRS spectrum and Spitzer 70 and 160 micron photometry. Since there are no sharp spectral features in this region, we expect these interpolations to be robust. This spectral range is calibrated as a SFR diagnostic using several reference SFR indicators to mitigate potential bias. Our band-specific continuous SFR indicators are found to be consistent with monochromatic calibrations in the local universe, as derived from Spitzer, WISE, and Herschel photometry. Our local composite template and continuous SFR diagnostics are made available for public use through the NASA/IPAC Infrared Science Archive (IRSA) and have typical dispersions of 30% or less. We discuss the validity and range of applicability for our SFR indicators in the context of unveiling the formation and evolution of galaxies. Additionally, in the era of the James Webb Space Telescope this will become a flexible tool, applicable to any SFG up to z~3.