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Introduction: Genetic polymorphisms in TCF7L2 are the strongest common risk variants for type 2 diabetes mellitus (T2D). We and others have shown that genetic variation in TCF7L2 and WFS1 affect incretin-stimulated insulin secretion. A recent genome-wide association study discovered genetic variants associated with incretin levels. We hypothesized that these SNPs (single nucleotide polymorphisms) interact with the well-known TCF7L2 variant rs7903146 on insulin secretion due to their incretin altering effect. Methods: In this retrospective analysis, we used data from the cross-sectional TUEF-cohort (n = 2929) and a hyperglycemic clamp study using additional GLP-1 infusion at the end of the clamp (n = 76). Insulin secretion was measured by evaluating OGTT-derived indexes of insulin secretion and insulin/C-peptide levels during clamp. We genotyped rs7903146 in TCF7L2, rs10010131 in WFS1, and six SNPs associated with GLP-1 and GIP levels. Results: One of the six incretin-associated SNPs, rs17681684 in GLP2R, exhibited significant SNP x SNP interactions with rs7903146 in TCF7L2 on insulin secretion (p = 0.0024) after correction for multiple testing. Three further SNP‘s showed nominally significant interactions (p < 0.05). In the hyperglycemic clamp study, rs7903146 in TCF7L2 also interacted with rs17681684 on AUC C-peptide during the GLP-1 stimulation phase, thereby replicating the above finding. Conclusion: The findings exemplify the role of SNP x SNP interactions in the genetics of type 2 diabetes mellitus and corroborate the existence of clinically relevant differences in incretin sensitivity.

Dawn Science Team is conducting a geologic mapping campaign for Ceres similar to that done for Vesta, including production of a Survey- and High Altitude Mapping Orbit (HAMO)-based global map, and a series of 15 Low Altitude Mapping Orbit (LAMO)-based quadrangle maps. In this abstract we discuss the geologic evolution of the Ac-H-6 Haulani Quadrangle

Ceres´ surface is affected by numerous impact cra-ters and some of them show features such as channels or multiple flow events forming a smooth, less cratered surface, indicating possible post-impact resurfacing

Das Lehrbuch richtet sich in erster Linie an Studierende an wissenschaftlichen Hochschulen, die im Rahmen ihres Grund- oder Bachelor-Studiums Lehrveranstaltungen zum Thema Marketing besuchen. Es ermöglicht dem Leser einen kompakten Einstieg in das moderne Marketing. Besonderer Wert wird hierbei auf die Vermittlung eines elementaren Methoden- und Modellverständnisses gelegt. Der Leser soll auf diese Weise in die Lage versetzt werden, qualitatives Faktenwissen mit analytischen Denkprinzipien zu verbinden, um so profunde Marketingentscheidungen treffen zu können.Das Lehrbuch richtet sich in erster Linie an Studierende an wissenschaftlichen Hochschulen, die im Rahmen ihres Grund- oder Bachelor-Studiums Lehrveranstaltungen zum Thema Marketing besuchen. Es ermöglicht dem Leser einen kompakten Einstieg in das moderne Marketing. Besonderer Wert wird hierbei auf die Vermittlung eines elementaren Methoden- und Modellverständnisses gelegt. Der Leser soll auf diese Weise in die Lage versetzt werden, qualitatives Faktenwissen mit analytischen Denkprinzipien zu verbinden, um so profunde Marketingentscheidungen treffen zu können.

NASA’s Dawn spacecraft entered orbit of Ceres on March 6, 2015, to spend one year characterizing the geology, elemental and mineralogical composition, topography, shape, and internal structure of the Ceres [1]. Ceres is supposed to be differentiated into a silicate core, a liquid water mantle and a solid ice crust with a surface temperature from 130K to 235K [2,3]. At the time of writing, the acquired image data from Ceres provide a spatial resolution of up to 2.1 km/pixel. The surface of Ceres reveals some albedo features that seem to be related to geomorphology. Those features show either a high or a low albedo compared to the surrounding.

The paper discusses the steep crater size-frequency distribution at kilometer-sized craters as a likely contribution caused by secondary craters on asteroid 4 Vesta and on Saturn's icy moon Tethys