标题： 使用ALMA、HST、VLT/MUSE和VLA测量近邻塞弗特星系NGC 1068的60秒差距尺度的恒星形成率 显示英文标题

标题： Measuring 60-pc-scale Star Formation Rate of the Nearby Seyfert Galaxy NGC 1068 with ALMA, HST, VLT/MUSE, and VLA

摘要： 星形成率（SFR）是描述星系并推断其演化过程的基本参数。 HII区域是测量星系中瞬时SFR的最佳方法，尽管所得到的SFR可能因示踪剂和假设的不同而存在较大的不确定性。 我们基于新的高灵敏度ALMA 100GHz连续谱数据，在55pc（=0.8）分辨率下结合HST Pa{\alpha }线数据，对邻近塞弗特星系NGC 1068整个分子气体盘进行了SFR校准。 在该校准中，我们根据公开的多波长数据考虑了尘埃消光的空间变化、HII区域的电子温度、活动星系核（AGN）污染以及弥散电离气体（DIG）的影响。 特别是，考虑到DIG的扩展性质及其可能对总SFR有不可忽略的贡献，对DIG的仔细考虑是必要的。 通过两种修正电离气体示踪剂（自由-自由连续谱&Pa{\alpha }）之间的交叉校准，NGC 1068盘的总SFR估计为3.2\pm 0.5 Msol/yr，仅为未考虑DIG时SFR（9.1\pm 1.4 Msol/yr）的三分之一。 我们确认了南部棒状结构末端和共转半径附近的高SFR，这与之前的SFR测量结果一致。 此外，我们的总SFR比基于8{\mu }m尘埃辐射的总SFR高出1.5倍。 我们将这种差异归因于每个示踪剂所追踪的不同演化阶段的年轻恒星及其各自的时间尺度。 本研究提供了一个例子，说明传统SFR测量中的各种不确定性及其可能导致显著的SFR误算的潜力。 显示英文摘要

摘要： Star formation rate (SFR) is a fundamental parameter for describing galaxies and inferring their evolutionary course. HII regions yield the best measure of instantaneous SFR in galaxies, although the derived SFR can have large uncertainties depending on tracers and assumptions. We present an SFR calibration for the entire molecular gas disk of the nearby Seyfert galaxy NGC 1068, based on our new high-sensitivity ALMA 100GHz continuum data at 55pc (=0."8) resolution in combination with the HST Pa{\alpha} line data. In this calibration, we account for the spatial variations of dust extinction, electron temperature of HII regions, AGN contamination, and diffuse ionized gas (DIG) based on publicly available multi-wavelength data. Especially, given the extended nature and the possible non-negligible contribution to the total SFR, a careful consideration of DIG is essential. With a cross-calibration between two corrected ionized gas tracers (free-free continuum&Pa{\alpha}), the total SFR of the NGC 1068 disk is estimated to be 3.2\pm0.5 Msol/yr, one-third of the SFR without accounting for DIG (9.1\pm1.4 Msol/yr). We confirmed high SFR around the southern bar-end and the corotation radius, which is consistent with the previous SFR measurements. In addition, our total SFR exceeds the total SFR based on 8{\mu}m dust emission by a factor of 1.5. We attribute this discrepancy to the differences in the young stars at different stages of evolution traced by each tracer and their respective timescales. This study provides an example to address the various uncertainties in conventional SFR measurements and their potential to lead to significant SFR miscalculations.