Quantification of Risperidone Contained in Precipitates Produced by Tea Catechins Using Nuclear Magnetic Resonance.

A mixture of risperidone and eight major tea catechins: (-)-epicatechin-3-O-gallate (ECg), (-)-epigallocatechin-3-O-gallate (EGCg), (-)-catechin-3-O-gallate (Cg), (-)-gallocatechin-3-O-gallate (GCg), (-)-epicatechin (EC), (-)-epigallocatechin (EGC), (+)-catechin (CA), or (+)-gallocatechin (GC), in tartaric acid buffer (pH 3.0) afforded a precipitate. Amounts of risperidone and these catechins in the precipitate were measured by quantitative 1H-NMR (qNMR). About half or more of risperidone used was precipitated by gallated catechins ECg, EGCg, Cg, and GCg; on the other hand, it was precipitated little by non-gallated catechins EC, EGC, CA, and GC. Furthermore, risperidone was precipitated more by 2,3-trans gallated catechins Cg and GCg than 2,3-cis gallated catechins ECg and EGCg. Regarding the amount of tea catechins in the precipitate obtained by a mixture of risperidone and Catechin Mixture, the amounts of 2,3-cis gallated catechins EGCg and ECg were much larger than those of the other green tea catechins GCg, EC, EGC, CA, and GC. It was considered that risperidone was mainly precipitated by EGCg and ECg in Catechin Mixture. Therefore, it can be concluded that when patients take risperidone with catechin-rich beverages, the efficacy of risperidone reduces, mainly because the 2,3-cis gallated catechins EGCg and ECg form complexes with risperidone and precipitate.

Testing The Lamp-Post and Wind Reverberation Models with XMM-Newton Observations of NGC 5506.

The lamp-post geometry is often used to model X-ray data of accreting black holes. Despite its simple assumptions, it has proven to be powerful in inferring fundamental black hole properties such as the spin. Early results of X-ray reverberations showed support for such a simple picture, though wind-reverberation models have also been shown to explain the observed delays. Here, we analyze new and old XMM-Newton observations of the variable Seyfert-1 galaxy NGC 5506 to test these models. The source shows an emission line feature around 6.7 keV that is delayed relative to harder and softer energy bands. The spectral feature can be modeled with either a weakly relativistic disk line or by scattering in distant material. By modeling both the spectral and timing signatures, we find that the reflection fraction needed to explain the lags is larger than observed in the time-averaged spectrum, ruling out both a static lamp-post and simple wind reverberation models.