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BP Psc is an active late-type (sp:G9) star with unclear evolutionary statuslying at high galactic latitude $b=-57^{\circ}$. It is also the source of thewell collimated bipolar jet. We present results of the proper motion and radialvelocity study of BP Psc outflow based on the archival $H\alpha$ imaging withthe GMOS camera at 8.1-m Gemini-North telescope as well as recent imaging andlong-slit spectroscopy with the SCORPIO multi-mode focal reducer at 6-m BTAtelescope of SAO RAS. The 3D kinematics of the jet revealed the full spatialvelocity up to $\sim$140 km$\cdot$s$^{-1}$ and allows us to estimate thedistance to BP Psc system as $D=135\pm40$ pc. This distance leads to anestimation of the central source luminosity $L_*\approx1.2L_{\odot}$,indicating that it is the $\approx$1.3$M_{\odot}$ T Tauri star with an age$t\lesssim$ 7 Myr. We measured the electron density of order $N_e\sim10^2$cm$^{-3}$ and mean ionization fraction $f\approx0.04$ within the jet knots andestimated upper limit of the mass-loss rate in NE lobe as$\dot{M}_{out}\approx1.2\cdot10^{-8}M_{\odot}\cdot yr^{-1}$. The physicalcharacteristics of the outflow are typical for the low-excitation YSO jets andconsistent with the magnetocentrifugal mechanism of its launching andcollimation. Prominent wiggling pattern revealed in $H\alpha$ images allowed usto suppose the existence of a secondary substellar companion in a non-coplanarorbit and estimate its most plausible mass as $M_p\approx 30M_{Jup}$. Weconclude that BP Psc is one of the closest to the Sun young jet-driving systemsand its origin is possibly related to the episode of star formation triggeredby expanding supershells in Second Galactic quadrant.

Jet from the enigmatic high-latitude star BP Psc and evolutionary status of its driving source