利用ALMA测量蛇夫座和L1641/L1647原行星盘的尘埃质量
Measuring Dust Masses of Protoplanetary Disks in Serpens and L1641/L1647 with ALMA
AI总结：
本研究利用ALMA数据测量蛇夫座和L1641/L1647原行星盘的尘埃质量，发现盘质量比以往报告高约2倍，因盘在毫米波长下可能部分光学厚，7毫米观测对准确表征尘埃质量至关重要。
AI中文摘要：
原行星盘是行星形成过程中的关键组成部分。盘中的尘埃和气体量限制了系统中能够形成行星的数量和大小。我们分析了178颗T-Tauri星，其中18颗位于蛇夫座，160颗位于L1641/L1647，并利用光谱能量分布（SED）建模和多波长数据，包括文献中的1.3毫米（ALMA带6）流量，测量了它们的盘尘埃质量。本研究计算出的盘质量比之前报告的高约2倍。我们得出结论，这是由于在毫米波长下盘可能部分光学厚，而大多数盘质量计算假设在1.3毫米处盘是光学薄的。我们计算了蛇夫座和L1641/L1647盘样本中一部分的1.3和7毫米光学深度，并显示大部分盘在更长的毫米波长下变得光学薄；因此，7毫米（即ALMA带1）的观测对于更好地表征盘尘埃质量至关重要。
英文摘要：
Protoplanetary disks are an essential component of the planet-formation process. The amount of dust and gas in the disk constrains the number and size of planets that can form in a system. We analyze 178 T-Tauri stars, 18 in Serpens and 160 in L1641/L1647, and measure their disk dust masses using spectral energy distribution (SED) modeling and multiwavelength data, including 1.3 mm (ALMA band 6) fluxes from the literature. The disk masses calculated in this work are up to $\sim$2 times higher than those previously reported. We conclude that this is because disks may be partially optically thick at millimeter wavelengths while most calculations of the disk mass assume that the disk is optically thin at 1.3 mm. We calculate optical depths at 1.3 and 7 mm for a subset of the Serpens and L1641/L1647 disk sample and show that the vast majority of disks become optically thin at longer millimeter wavelengths; thus, observations at 7 mm (i.e., ALMA band 1) are vital to better characterize disk dust masses.
