High Resolution H alpha Images of the Binary Low-mass Proplyd LV 1 with the Magellan AO System

TL;DR

This study uses advanced adaptive optics imaging to analyze the binary proplyd LV 1 in Orion, revealing its structure, possible low-mass components, and the magnetopause size, providing insights into low-mass star formation.

Contribution

First AO images of LV 1 in visible wavelengths, showing detailed structure and potential low-mass stellar components, with astrometric and physical analysis.

Findings

LV 1 shows no significant relative motion over 18 years.

The binary may consist of a very-low-mass star and a brown dwarf.

The magnetopause radius is estimated at 110 AU.

Abstract

We utilize the new Magellan adaptive optics system (MagAO) to image the binary proplyd LV 1 in the Orion Trapezium at H alpha. This is among the first AO results in visible wavelengths. The H alpha image clearly shows the ionization fronts, the interproplyd shell, and the cometary tails. Our astrometric measurements find no significant relative motion between components over ~18 yr, implying that LV 1 is a low-mass system. We also analyze Large Binocular Telescope AO observations, and find a point source which may be the embedded protostar's photosphere in the continuum. Converting the H magnitudes to mass, we show that the LV 1 binary may consist of one very-low-mass star with a likely brown dwarf secondary, or even plausibly a double brown dwarf. Finally, the magnetopause of the minor proplyd is estimated to have a radius of 110 AU, consistent with the location of the bow shock seen in H alpha.