NGTS-33b: A Young Super-Jupiter Hosted by a Fast Rotating Massive Hot Star

Abstract

In the last few decades planet search surveys have been focusing on solar type stars, and only recently the high-mass regimes. This is mostly due to challenges arising from the lack of instrumental precision, and more importantly, the inherent active nature of fast rotating massive stars. Here we report NGTS-33b (TOI-6442b), a super-Jupiter planet with mass, radius and orbital period of 3.6 ± 0.3 M<SUB>j</SUB>, 1.64 ± 0.07 R<SUB>j</SUB> and 2.827972 ± 0.000001 days, respectively. The host is a fast rotating (0.6654 ± 0.0006 day) and hot (T<SUB>eff</SUB> = 7437 ± 72 K) A9V type star, with a mass and radius of 1.60 ± 0.11 M<SUB>⊙</SUB> and 1.47 ± 0.06 R<SUB>⊙</SUB>, respectively. Planet structure and Gyrochronology models shows that NGTS-33 is also very young with age limits of 10-50 Myr. In addition, membership analysis points towards the star being part of the Vela OB2 association, which has an age of ~ 20-35 Myr, thus providing further evidences about the young nature of NGTS-33. Its low bulk density of 0.19±0.03 gcm<SUP>-3</SUP> is 13<inline-formula><tex-math id=TM0001 notation=LaTeX>$\%$</tex-math></inline-formula> smaller than expected when compared to transiting hot Jupiters with similar masses. Such cannot be solely explained by its age, where an up to 15<inline-formula><tex-math id=TM0002 notation=LaTeX>$\%$</tex-math></inline-formula> inflated atmosphere is expected from planet structure models. Finally, we found that its emission spectroscopy metric is similar to JWST community targets, making the planet an interesting target for atmospheric follow-up. Therefore, NGTS-33b's discovery will not only add to the scarce population of young, massive and hot Jupiters, but will also help place further strong constraints on current formation and evolution models for such planetary systems.