Eccentric Dust Ring in the IRS 48 Transition Disk

Abstract

Crescent-shaped structures in transition disks hold the key to studying the putative companions to the central stars. The dust dynamics, especially that of different grain sizes, is important to understanding the role of pressure bumps in planet formation. In this work, we present deep dust continuum observation with high resolution towards the Oph IRS 48 system. For the first time, we are able to significantly trace and detect emission along $95\%$ of the ring crossing the crescent-shaped structure. The ring is highly eccentric with an eccentricity of $0.27$. The flux density contrast between the peak of the flux and its counter part along the ring is $\sim 270$. In addition, we detect a compact emission toward the central star. If the emission is an inner circumstellar disk inside the cavity, it has a radius of at most a couple of astronomical units with a dust mass of $1.5\times 10^{-8}{\mathrm{M}}_{\odot }$, or $0.005{\mathrm{M}}_{\oplus }$. We also discuss the implications of the potential eccentric orbit on the proper motion of the crescent, the putative secondary companion, and the asymmetry in velocity maps.

9 pages, 5 figures, accepted for publication on AAS Journals

References in corpus (6)

• On the origin of horseshoes in transitional discs
• Spatial separation of small and large grains in the transitional disk around the young star IRS 48
• Signatures of an eccentric disc cavity: Dust and gas in IRS 48
• Solving grain size inconsistency between ALMA polarization and VLA continuum in the Ophiuchus IRS 48 protoplanetary disk
• Modeling the accretion disk around the high-mass protostar GGD 27-MM1
• Dust Populations in the Iconic Vega Planetary System Resolved by ALMA