The Radial and Rotational Velocities of PSO J318.5338$-$22.8603, a Newly Confirmed Planetary-Mass Member of the $\beta$ Pictoris Moving Group

TL;DR

This study measures the radial and rotational velocities of PSO J318.5338-22.8603, confirming its membership in the beta Pictoris moving group and providing insights into its physical properties and rotation, serving as a benchmark for planetary-mass objects.

Contribution

First measurement of radial velocity and v sin(i) for PSO J318.5-22, confirming its group membership and characterizing its physical and rotational properties.

Findings

Confirmed beta Pictoris group membership.

Estimated mass of 8.3 Jupiter masses.

Rotation period between 5 and 10.2 hours.

Abstract

PSO J318.5338$-$22.8603 is an extremely-red planetary-mass object that has been identified as a candidate member of the $\beta$ Pictoris moving group based on its spatial position and tangential velocity. We present a high resolution $K$-band spectrum of PSO J318.5338$-$22.8603. Using a forward-modeling Markov Chain Monte Carlo approach, we report the first measurement of the radial velocity and $v$ sin($i$) of PSO J318.5$-$22, $-$6.0$^{+0.8}_{-1.1}$ km s$^{-1}$ and 17.5$^{+2.3}_{-2.8}$ km s$^{-1}$, respectively. We calculate the space velocity and position of PSO J318.5$-$22 and confirm that it is a member of the $\beta$ Pictoris moving group. Adopting an age of 23$\pm$3 Myr for PSO J318.5$-$22, we determine a mass of $8.3\pm0.5$ $M_{\rm{Jup}}$ and effective temperature of $1127^{+24}_{-26}$ K using evolutionary models. PSO J318.5338$-$22.8603 is intermediate in mass and temperature to the directly-imaged planets $\beta$ Pictoris b and 51 Eridani b, making it an important benchmark object in the sequence of planetary-mass members of the $\beta$ Pictoris moving group. Combining our $v$ sin($i$) measurement with recent photometric variability data, we constrain the inclination of PSO J318.5$-$22 to $>29^{\circ}$ and its rotational period to 5-10.2 hours. The equatorial velocity of PSO J318.5$-$22 indicates that its rotation is consistent with an extrapolation of the velocity-mass relationship for solar system planets.