Effects of tofogliflozin on adrenocorticotropic hormone, renin and aldosterone, and cortisol levels in elderly patients with diabetes mellitus: A retrospective study of a patient cohort.

ABSTRACT: Adrenocorticotropic hormone (ACTH) and cortisol reportedly play a role in glycemic control in patients with type 2 diabetes mellitus (T2DM); however, the underlying mechanism remains controversial. We retrospectively investigated the effect of tofogliflozin on serum ACTH and cortisol levels in elderly patients with T2DM.Patients received 20 mg tofogliflozin daily for 3 months. Serum ACTH and cortisol levels were measured at baseline, as well as after 1 month and 3 months of tofogliflozin therapy.Serum ACTH levels were significantly reduced 3 months after tofogliflozin treatment (P < .01). Additionally, serum cortisol levels were reduced 3 months after tofogliflozin treatment, demonstrating borderline significance (P = .05). The higher body mass index (BMI; ≥25 kg/m2) group showed higher ACTH and cortisol levels than the lower BMI (<25 kg/m2) group, with borderline significance (P = .05). Renin levels were significantly increased 1 month after treatment (P < .05), maintaining serum aldosterone levels in parallel with the extracellular fluid.Our findings suggested that tofogliflozin decreased both serum ACTH and cortisol levels, with higher levels observed in the high BMI group. Tofogliflozin increased serum renin levels while maintaining serum aldosterone and extracellular fluid levels. Collectively, tofogliflozin could affect the hypothalamic-pituitary-adrenal pathway in patients with T2DM, especially in the low BMI group.

Atomic scattering factor of the ASTRO-H (Hitomi) SXT reflector around the gold's L edges.

The atomic scattering factor in the energy range of 11.2-15.4 keV for the ASTRO-H Soft X-ray Telescope (SXT) is reported. The large effective area of the SXT makes use of photon spectra above 10 keV viable, unlike most other X-ray satellites with total-reflection mirror optics. Presence of gold's L-edges in the energy band is a major issue, as it complicates the function of the effective area. In order to model the area, the reflectivity measurements in the 11.2-15.4 keV band with the energy pitch of 0.4 - 0.7 eV were made in the synchrotron beam-line Spring-8 BL01B1. We obtained atomic scattering factors f1 and f2 by the curve fitting to the reflectivities of our witness sample. The edges associated with the L-I, II, and III transitions are identified, of which the depths are found to be roughly 60% shallower than those expected from the Henke's atomic scattering factor.

Hard x-ray telescopes to be onboard ASTRO-H.

The new Japanese x-ray astronomy satellite, ASTRO-H, will carry two identical hard x-ray telescopes (HXTs), which cover the energy range of 5 to 80 keV. The HXT mirrors employ tightly nested, conically approximated thin-foil Wolter-I optics, and the mirror surfaces are coated with Pt/C depth-graded multilayers to enhance the hard x-ray effective area by means of Bragg reflection. The HXT comprises foils 120-450 mm in diameter and 200 mm in length, with a focal length of 12 m. To obtain a large effective area, 213 aluminum foils 0.2 mm in thickness are tightly nested confocally. The requirements for HXT are a total effective area of >300 cm2 at 30 keV and an angular resolution of <1.7' in half-power diameter (HPD). Fabrication of two HXTs has been completed, and the x-ray performance of each HXT was measured at a synchrotron radiation facility, SPring-8 BL20B2 in Japan. Angular resolutions (HPD) of 1.9' and 1.8' at 30 keV were obtained for the full telescopes of HXT-1 and HXT-2, respectively. The total effective area of the two HXTs at 30 keV is 349 cm2.

X-ray telescope onboard Astro-E. III. Guidelines to performance improvements and optimization of the ray-tracing simulator.

We present a detailed study of the performance of the Astro-E x-ray telescope (XRT) onboard the Astro-E satellite. As described in preceding papers the ground-based calibrations of the Astro-E XRT revealed that its image quality and effective area are somewhat worse than that expected from the original design. Conceivable causes for such performance degradation are examined by x-ray and optical microscopic measurements at various levels, such as individual reflectors, sectors, and quadrants of the XRT and their alignments. We can attribute, based on detailed measurements, the degradation of the image quality to a slope error in the individual reflectors and the positioning error of reflectors. As for the deficit of the effective area, the shadowing of x rays within the XRT body is the dominant factor. Error budgets for the performance degradation of the Astro-E XRT are summarized. The ray-tracing simulator, which is needed to construct the response function for arbitrary off-axis angles and spatial distributions of any celestial x-ray sources, has been developed and tuned based on the results of detailed measurements. The ray-tracing simulation provides results that are consistent within 3% with the real measurement except for large off-axis angles and higher energies. We propose, based on knowledge obtained from all the measurements and simulations, several plans for future developments to improve the performance of the nested thin-foil mirrors.

Characterization of the supermirror hard-x-ray telescope for the InFOCmuS balloon experiment.

A hard-x-ray telescope is successfully produced for balloon observations by making use of depth-graded multilayers, or so-called supermirrors, with platinum-carbon (Pt/C) layer pairs. It consists of four quadrant units assembled in an optical configuration with a diameter of 40 cm and a focal length of 8 m. Each quadrant is made of 510 pieces of coaxially and confocally aligned supermirrors that significantly enhance the sensitivity in an energy range of 20-40 keV. The configuration of the telescope is similar to the x-ray telescope onboard Astro-E, but with a longer focal length. The reflectivity of supermirrors is of the order of 40% in the energy range concerned at a grazing angle of 0.2 deg. The effective area of a fully assembled telescope is 50 cm2 at 30 keV. The angular resolution is 2.37 arc min at half-power diameter 8.0 keV. The field of view is 12.6 arc min in the hard-x-ray region, depending somewhat on x-ray energies. We discuss these characteristics, taking into account the figure errors of reflectors and their optical alignment in the telescope assembly. This hard-x-ray telescope is unanimously afforded in the International Focusing Optics Collaboration for muCrab Sensitivity balloon experiment.