星系中远红外谱线的定标
Calibration of mid- to far-infrared spectral lines in galaxies
摘要：
中到远红外线（IR）线适合于研究星系中的尘埃遮蔽区域，因为IR光谱使我们能够探索最隐藏的区域，在这些区域中发生了严重遮蔽的恒星形成以及对超大质量黑洞的吸积。这在红移为1<z<3时最为重要，此时星系中的大多数重子质量已经聚集。我们提供了可靠的中到远红外离子精细结构线，最亮的H2纯旋转线和多环芳烃（PAH）特征的校准，这些特征将用于分析当前和未来在地面mm/submm范围内的观测，以及即将到来的詹姆斯韦伯太空望远镜的中红外光谱。我们使用三个样本的星系观察到在本地宇宙：恒星形成星系，活动星系核和低金属丰度矮星系。对于每个人口，我们得到不同的校准所观察到的线的光度与总的IR光度。我们推导出光谱测量的SFR和BHAR使用中，远红外精细结构线，H2纯转动线和PAH功能。我们根据[CII]158 $μ$ m谱线、[OI]63 $μ$ m谱线和[OIII]88 $μ$ m谱线的总和、氖和硫中红外谱线的组合、6.2和11.3 $μ$ m处明亮的PAH特征以及9.7、12.3和17 $μ$ m处的H2旋转谱线，推导出了强有力的恒星形成示踪剂。我们建议[CII]158 $μ$ m线，两条氖线的组合，以及可能拥有活动星系核的类太阳金属丰度星系，PAH 11.3 $μ$ m特征作为最好的SFR示踪剂。使用[OIV]25.9 $μ$ m和[NeV]14.3和24.3 $μ$ m谱线可获得BHAR的可靠测量值。对于最常见的精细结构线在远红外线，我们比较我们的校准与现有的ALMA观测高红移星系发现整体与当地的结果有很好的一致性。
英文摘要：
Mid- to far-infrared (IR) lines are suited to study dust obscured regions in galaxies, because IR spectroscopy allows us to explore the most hidden regions where heavily obscured star formation as well as accretion onto supermassive black-holes occur. This is mostly important at redshifts of 1<z<3, when most of the baryonic mass in galaxies has been assembled. We provide reliable calibrations of the mid- to far-IR ionic fine structure lines, the brightest H2 pure rotational lines and the Polycyclic Aromatic Hydrocarbons (PAHs) features, that will be used to analyse current and future observations in the mm/submm range from the ground, as well as mid-IR spectroscopy from the upcoming James Webb Space Telescope. We use three samples of galaxies observed in the local Universe: star forming galaxies, AGN and low-metallicity dwarf galaxies. For each population we derive different calibrations of the observed line luminosities versus the total IR luminosities. We derive spectroscopic measurements of SFR and BHAR using mid- and far-IR fine structure lines, H2 pure rotational lines and PAH features. We derive robust star-formation tracers based on the [CII]158 $μ$m line; the sum of the [OI]63$μ$m and [OIII]88$μ$m lines; a combination of the neon and sulfur mid-IR lines; the bright PAH features at 6.2 and 11.3 $μ$m, and the H2 rotational lines at 9.7, 12.3 and 17 $μ$m. We propose the [CII]158$μ$m line, the combination of two neon lines and, for solar-like metallicity galaxies that may harbor an AGN, the PAH11.3$μ$m feature as the best SFR tracers. A reliable measure of the BHAR can be obtained using the [OIV]25.9 $μ$m and the [NeV]14.3 and 24.3 $μ$m lines. For the most commonly observed fine-structure lines in the far-IR we compare our calibration with the existing ALMA observations of high redshift galaxies finding overall a good agreement with local results.
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