First Detection of Equatorial Dark Dust Lane in a Protostellar Disk at Submillimeter Wavelength

TL;DR

This paper reports the first observation of an equatorial dark dust lane in a very young protostellar disk at submillimeter wavelengths using ALMA, providing new insights into early disk formation.

Contribution

It presents the first detection and spatial resolution of a dark dust lane in a Class 0 protostellar disk at submillimeter wavelengths, advancing understanding of early disk structures.

Findings

Detection of a dark dust lane in a young protostellar disk

First submillimeter observation of such a feature

Supports theories of early disk formation and structure

Abstract

In the earliest (so-called "Class 0") phase of sunlike (low-mass) star formation, circumstellar disks are expected to form, feeding the protostars. However, such disks are difficult to resolve spatially because of their small sizes. Moreover, there are theoretical difficulties in producing such disks in the earliest phase, due to the retarding effects of magnetic fields on the rotating, collapsing material (so-called "magnetic braking"). With the Atacama Large Millimeter/submillimeter Array (ALMA), it becomes possible to uncover such disks and study them in detail. HH 212 is a very young protostellar system. With ALMA, we not only detect but also spatially resolve its disk in dust emission at submillimeter wavelength. The disk is nearly edge-on and has a radius of ~ 60 AU. Interestingly, it shows a prominent equatorial dark lane sandwiched between two brighter features, due to relatively low temperature and high optical depth near the disk midplane. For the first time, this dark lane is seen at submillimeter wavelength, producing a "hamburger"-shaped appearance that is reminiscent of the scattered-light image of an edge-on disk in optical and near infrared. Our observations open up an exciting possibility of directly detecting and characterizing small disks around the youngest protostars through high-resolution imaging with ALMA, which provides strong constraints on theories of disk formation.