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

Abstract

BP Psc is an active late-type (sp:G9) star with unclear evolutionary status lying at high galactic latitude $b=-57^{\circ }$. It is also the source of the well collimated bipolar jet. We present results of the proper motion and radial velocity study of BP Psc outflow based on the archival $H\alpha$ imaging with the GMOS camera at 8.1-m Gemini-North telescope as well as recent imaging and long-slit spectroscopy with the SCORPIO multi-mode focal reducer at 6-m BTA telescope of SAO RAS. The 3D kinematics of the jet revealed the full spatial velocity up to $\sim$140 km$\cdot$s${}^{-1}$ and allows us to estimate the distance to BP Psc system as $D=135\pm 40$ pc. This distance leads to an estimation of the central source luminosity $L_{\ast }\approx 1.2L_{\odot }$, 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 $N_e\sim 10^2$ cm${}^{-3}$ and mean ionization fraction $f\approx 0.04$ within the jet knots and estimated upper limit of the mass-loss rate in NE lobe as ${\dot{M}}_{out}\approx 1.2\cdot 10^{-8}{M}_{\odot }\cdot y{r}^{-1}$. The physical characteristics of the outflow are typical for the low-excitation YSO jets and consistent with the magnetocentrifugal mechanism of its launching and collimation. Prominent wiggling pattern revealed in $H\alpha$ images allowed us to suppose the existence of a secondary substellar companion in a non-coplanar orbit and estimate its most plausible mass as $M_p\approx 30M_{Jup}$. We conclude that BP Psc is one of the closest to the Sun young jet-driving systems and its origin is possibly related to the episode of star formation triggered by expanding supershells in Second Galactic quadrant.

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