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We report a new evaluation of the accretion properties of PDS 70b obtained with the Very Large Telescope/Multi Unit Spectroscopic Explorer. The main difference from the previous studies of Haffert et al. and Aoyama & Ikoma is in the mass accretion rate. Simultaneous multiple line observations, such as H alpha and H beta, can better constrain the physical properties of an accreting planet. While we clearly detected H alpha emissions from PDS 70b, no H beta emissions were detected. We estimate the line flux of H beta with a 3 sigma upper limit to be 2.3 x 10(-16) erg s(-1) cm(-2). The flux ratio F-H beta/F-H alpha for PDS 70b is F-H beta/F-H alpha should be close to unity if the extinction is negligible. We attribute the reduction of the flux ratio to the extinction, and estimate the extinction of H alpha (A(H alpha)) for PDS 70b to be >2.0 mag using the interstellar extinction value. By combining with the H alpha linewidth and the dereddening line luminosity of H alpha, we derive the PDS 70b mass accretion rate to be greater than or similar to 5 x 10(-7) M-Jup yr(-1). The PDS 70b mass accretion rate is an order of magnitude larger than that of PDS 70. We found that the filling factor f(f) (the fractional area of the planetary surface emitting H alpha) is greater than or similar to 0.01, which is similar to the typical stellar value. The small value of f(f) indicates that the H alpha emitting areas are localized at the surface of PDS 70b.

Stellar multiplicity is believed to influence planetary formation and evolution, although the precise nature and extent of this role remain ambiguous. We present a study aimed at testing the role of stellar multiplicity in the formation and/or evolution of the most massive, closein planetary and substellar companions. Using past and new direct imaging observations, as well as the Gaia DR2 catalogue, we searched for wide binary companions to 38 stars hosting massive giant planets or brown dwarfs (M > 7 M-Jup) on orbits shorter than similar to 1 au. We report the discovery of a new component in theWASP-14 system, and present an independent confirmation of a comoving companion to WASP-18. From a robust Bayesian statistical analysis, we derived a binary fraction of 79.0(-14.7)(+13.2) per cent between 20 and 10 000 au for our sample, twice as high as for field stars with a 3 sigma significance. This binary frequency was found to be larger than for lower-mass planets on similar orbits, and we observed a marginally higher binary rate for inner companions with periods shorter than 10 d. These results demonstrate that stellar companions greatly influence the formation and/or evolution of these systems, suggesting that the role played by binary companions becomes more important for higher-mass planets, and that this trend may be enhanced for systems with tighter orbits. Our analysis also revealed a peak in binary separation at 250 au, highlighting a shortfall of close binaries among our sample. This indicates that the mechanisms affecting planet and brown dwarf formation or evolution in binaries must operate from wide separations, although we found that the Kozai-Lidov mechanism is unlikely to be the dominant underlying process. We conclude that binarity plays a crucial role in the existence of very massive short-period giant planets and brown dwarf desert inhabitants, which are almost exclusively observed in multiple systems.