演講資訊

摘要：

Over the past few years, there has been a significant push to develop new imaging techniques that can improve the fidelity of observations in super-resolution regimes. These techniques have the potential to greatly enhance the interferometric observation of protoplanetary disks (PPDs), such as those obtained through the Atacama Large Millimeter/submillimeter Array (ALMA). In this talk, I will introduce a novel super-resolution imaging technique that employs sparse modeling to enhance the fidelity and spatial resolution of ALMA images. We describe the principle behind this technique and present our recent results, which demonstrate high-resolution images of 43 Taurus-Auriga protoplanetary disks. Our images achieve spatial resolutions ranging from 0.01 to 0.1 arcseconds (1-14 au at a distance of 140 pc), which is 2-3 times higher than those obtained through conventional imaging techniques. Our analysis of the resolved dust disks reveals a wide range of radii, from 8 to 238 au. We also observe various substructures, including gaps and rings, irrespective of disk size. The locations of these gaps exhibit a bimodal distribution, with peaks at 10-20 au and 30-100 au. We find that the gaps and rings show a linear relationship, though several systems do not conform to this correlation. These outliers have gap widths that are 2-3 times larger than typical sizes at corresponding locations. Finally, we discuss two types of disks with different gap sizes, which suggest the presence of two distinct planet-forming mechanisms. Our findings demonstrate the potential of our super-resolution imaging technique to provide new insights into the structure and dynamics of protoplanetary disks, which will further our understanding of planet formation. At the end of my talk, I will introduce recommended data analysis focused on near future trend for graduate students.