Recurrent Activity from Active Asteroid (248370) 2005 QN173: A Main-Belt Comet

TL;DR

This paper reports the recurrent activity of asteroid (248370) 2005 QN173 near perihelion, classifying it as a Main-Belt Comet driven by sublimation, and introduces a new activity detection technique called 'wedge photometry.'

Contribution

The study provides evidence of recurrent activity in (248370) 2005 QN173, a rare characteristic among active asteroids, and develops a novel method for tail detection in solar system objects.

Findings

(248370) 2005 QN173 shows recurrent activity near perihelion.

The 'wedge photometry' technique effectively detects and analyzes tails.

The asteroid is likely a Main-Belt Comet driven by sublimation.

Abstract

We present archival observations of Main-belt asteroid (248370) 2005 QN173 (also designated 433P) that demonstrate this recently discovered active asteroid (a body with a dynamically asteroidal orbit displaying a tail or coma) has had at least one additional apparition of activity near perihelion during a prior orbit. We discovered evidence of this second activity epoch in an image captured 2016 July 22 with the Dark Energy Camera on the 4 meter Blanco telescope at the Cerro Tololo Inter-American Observatory in Chile. As of this writing, (248370) 2005 QN173 is just the 8th active asteroid demonstrated to undergo recurrent activity near perihelion. Our analyses demonstrate (248370) 2005 QN173 is likely a member of the active asteroid subset known as Main-Belt Comets, a group of objects that orbit in the Main Asteroid Belt which exhibit activity that is specifically driven by sublimation. We implement an activity detection technique, "wedge photometry," that has the potential to detect tails in images of solar system objects and quantify their agreement with computed anti-solar and anti-motion vectors normally associated with observed tail directions. We present a catalog and an image gallery of archival observations. The object will soon become unobservable as it passes behind the Sun as seen from Earth, and when it again becomes visible (late-2022) it will be farther than 3 au from the Sun. Our findings suggest (248370) 2005 QN173 is most active interior to 2.7 au (0.3 au from perihelion), so we encourage the community to observe and study this special object before December 2021.