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THE RADIAL AND ROTATIONAL VELOCITIES OF PSO J318.5338-22.8603, A NEWLY CONFIRMED PLANETARY-MASS MEMBER OF THE β PICTORIS MOVING GROUP

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  • Katelyn N. Allers
  • J F Gallimore
  • Michael C. Liu
  • Trent Dupuy

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https://arxiv.org/abs/1601.04717
Original languageEnglish
JournalAstrophysical Journal
Volume819
Issue number2
DOIs
Publication statusPublished - 8 Mar 2016

Abstract

PSO J318.5338−22.8603 is an extremely red planetary-mass object that has been identified as a candidate member of the β 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, $-{6.0}_{-1.1}^{+0.8}$ km s−1, and ${17.5}_{-2.8}^{+2.3}$ 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 β Pictoris moving group. Adopting an age of 23 ± 3 Myr for PSO J318.5−22, we determine a mass of 8.3 ± 0.5 MJup and an effective temperature of ${1127}_{-26}^{+24}$ K using evolutionary models. PSO J318.5338−22.8603 is intermediate in mass and temperature to the directly imaged planets β Pictoris b and 51 Eridani b, making it an important benchmark object in the sequence of the planetary-mass members of the β 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° and its rotational period to 5–10.2 hr. 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.

ID: 163975491