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We present the results of observations of asteroid (248370) QN$_{173}$obtained during July 2021 - January 2022 with three telescopes. Our analysisrevealed the presence of the dust tail for about half of a year. The directimages of the asteroid were obtained with broad-band filters. No emissions wererevealed in the spectra, and the spectrum of the asteroid closely matched thatof a C-type asteroid. Created color and linear polarization variations alongthe tail were analyzed. The asteroid demonstrated a redder color compared tothe Sun. Dramatic changes in dust productivity obtained in different filterswere not detected. The $g-r$ color changes from $0.2^{m}$ to $0.7^{m}$ over thecoma, and the linear polarization degree varies from about $1.2$\% to $0.2$\%and from $-0.2$\% to $-1.5$\% at the phase angle of $23.2^{\circ}$ and$8.16^{\circ}$. The total dust mass ejected until the latest observation onOctober 10 is $4.2 \times 10^7$~kg, with a maximum rate of 2.6~kg\,s$^{-1}$based on the Monte Carlo modeling of the dust tail. The estimated asteroid sizeis 1.3~km. It is shown that large particles are concentrated around thenucleus, whereas smaller ones dominate in the tail. The evolution of (248370)QN$_{173}$ orbit and the orbits of the sample of the 464 short-periodic cometswere followed. Ten of them approached the asteroid's orbit. These objects arenot genetically related, despite the very close distance of their orbits for arelatively long time.

Long-lasting activity of asteroid (248370) 2005 QN 173