G11.92–0.61 MM 1: A Fragmented Keplerian Disk Surrounding a Proto-O Star

Abstract

We present high-resolution (∼300 au) Atacama Large Millimeter/submillimeter Array observations of the massive young stellar object G11.92–0.61 MM 1. We resolve the immediate circumstellar environment of MM 1 in 1.3 mm continuum emission and CH 3 CN emission for the first time. The object divides into two main sources—MM 1a, which is the source of a bipolar molecular outflow, and MM 1b, located 0.″57 (1920 au) to the southeast. The main component of MM 1a is an elongated continuum structure, perpendicular to the bipolar outflow, with a size of 0.″141 × 0.″050 (480 × 170 au). The gas kinematics toward MM 1a probed via CH 3 CN trace a variety of scales. The lower energy J  = 12–11 K  = 3 line traces extended, rotating gas within the outflow cavity, while the v 8 = 1 line shows a clearly resolved Keplerian rotation signature. Analysis of the gas kinematics and dust emission shows that the total enclosed mass in MM 1a is 40 ± 5 M ⊙ (where between 2.2 and 5.8 M ⊙ is attributed to the disk), while MM 1b is <0.6 M ⊙ . The extreme mass ratio and orbital properties of MM 1a and MM 1b suggest that MM 1b is one of the first observed examples of the formation of a binary star via disk fragmentation around a massive young (proto)star.