Does the partial molar volume of a solute reflect the free energy of hydrophobic solvation?

Halogenated heterocyclic ligands are widely used as the potent and frequently selective inhibitors of protein kinases. However, the exact contribution of the hydrophobic solvation of a free ligand is rarely accounted for the balance of interactions contributing to the free energy of ligand binding. Herein, we propose a new experimental method based on volumetric data to estimate the hydrophobicity of a ligand. We have tested this approach for a series of ten variously halogenated benzotriazoles, the binding affinity of which to the target protein kinase CK2 was assessed with the use of thermal shift assay. According to the hierarchical clustering procedure, the excess volume, defined as the difference between the experimentally determined partial molar volume and the calculated in silico molecular volume, was found to be distant from any commonly used hydrophobicity descriptors of the ligand. The excess volume, however, properly predicts solute binding affinity. On the way, we have proved that the binding of halogenated benzotriazoles to the protein kinase CK2 is driven mostly by hydrophobic interaction

TIC 172900988: A transiting circumbinary planet detected in one sector of TESS data

We report the first discovery of a transiting circumbinary planet detected from a single sector of Transiting Exoplanet Survey Satellite (TESS) data. During Sector 21, the planet TIC 172900988b transited the primary star and then five days later it transited the secondary star. The binary is itself eclipsing, with a period P ≈ 19.7 days and an eccentricity e ≈ 0.45. Archival data from ASAS-SN, Evryscope, KELT, and SuperWASP reveal a prominent apsidal motion of the binary orbit, caused by the dynamical interactions between the binary and the planet. A comprehensive photodynamical analysis of the TESS, archival and follow-up data yields stellar masses and radii of M1 = 1.2384 ± 0.0007 Me and R1 = 1.3827 ± 0.0016 Re for the primary and M2 = 1.2019 ± 0.0007 Me and R2 = 1.3124 ± 0.0012 Re for the secondary. The radius of the planet is R3 = 11.25 ± 0.44 R (1.004 ± 0.039RJup). The planet's mass and orbital properties are not uniquely determined-there are six solutions with nearly equal likelihood. Specifically, we find that the planet's mass is in the range of 824 M3 981 M (2.65 M3 3.09MJup), its orbital period could be 188.8, 190.4, 194.0, 199.0, 200.4, or 204.1 days, and the eccentricity is between 0.02 and 0.09. At V = 10.141 mag, the system is accessible for high-resolution spectroscopic observations, e.g., the Rossiter-McLaughlin effect and transit spectroscopy