2026/07/24 by Cade J. Bürgy, Myriam Benisty, Hala Alqubelat +2
#astro-ph.EP #astro-ph.SR
While hundreds of protoplanetary discs have been studied in great detail, the detection of protoplanets still embedded in their native discs remains rare. WISPIT 2 is only the second laboratory allowing for direct study of planet formation while in progress. The recently discovered system hosts two giant protoplanets in a multi-ringed disc. Here, we aim at characterising the WISPIT 2 host star spectroscopically to determine its stellar properties, accretion rate, and inner disc diagnostics, providing a more complete picture of the system. We present optical and near-infrared spectroscopic observations obtained with the ESO VLT/X-Shooter and 2.2 m/FEROS instruments. We model the stellar spectrum to determine the spectral type and effective temperature, analyse the emission lines to estimate the accretion rate, and search for evidence of a close stellar companion using radial velocity measurements. Our observations reveal that WISPIT 2 is a spectroscopic binary. The binary has a period of 4.8± 0.1 days, which corresponds to a semi-major axis of 0.072 au or 15.54 R_\odot, assuming co-planarity with the disc and a circular orbit. The binary system consists of a ∼ 0.97 M\odot primary of spectral type K3 (T\rm eff ∼ 4700K), and a ∼ 0.33M_\odot secondary (mass ratio ∼0.34). We detect weak Hα emission, implying an accretion rate of ∼ 2 × 10-11 M\odot yr-1. However, this value is below the chromospheric level, suggesting little to no ongoing accretion onto the young stars. This discovery makes the WISPIT 2 disc the first circumbinary system with directly imaged protoplanets, establishing this system as a unique benchmark for studying planet formation and disc evolution around binary stars.