Abstract A potential link between chronic kidney disease (CKD) and non-alcoholic fatty liver disease (NAFLD) has been suggested. We investigated the relationship between fatty liver index (FLI), a noninvasive and simple predictor of NAFLD, and the development of CKD defined as estimated glomerular filtration rate < 60 mL/min/1.73 m 2 or positive for urinary protein during a 10-year follow-up period in subjects who received annual health examinations (n = 28,890). After exclusion of CKD at baseline, a total of 14,163 subjects (male/female: 9077/5086) were recruited. During the 10-year period, 1458 males (16.1%) and 737 females (14.5%) had new onset of CKD. Multivariable Cox proportional hazard models with a restricted cubic spline showed that hazard ratios (HRs) of CKD development increased with a higher FLI at baseline in both males and females after adjustment of confounders. When divided by tertiles of FLI level at baseline (T1 ~ T3), the adjusted risk of CKD development in the T3 group (HR [95% confidence interval], male/female: 1.33 [1.16–1.54]/1.33 [1.08–1.63]) was significantly higher than that in both sexes in the T1 group as the reference. The addition of FLI into traditional risk factors significantly improved the discriminatory capability for predicting CKD. In conclusion, a high level of FLI predicts the development of CKD in both sexes in a general population.
Two lines of Japanese quail were divergently selected for high and low antibody responses after being twice injected at 4 and 6 weeks of age with inactivated Newcastle disease virus antigen. After seven generations of selection, the serum antibody level in the high line was 24% greater than the level in the unselected control lines, whereas the low line antibody level was approximately 37% less than that in the control line. The estimated heritability (H2S+D) was approximately .12 ± .50. The realized h2, calculated from coefficient of regression formula on seven generations (G3 to G9), was .07.
A 25-year-old woman presented with fever, arthralgia and proteinuria exhibiting leukopenia, hypocomplementemia, increased serum IgG and IgG4, and positive antinuclear and anti-double-stranded DNA antibodies. Renal biopsy revealed membranous nephropathy with tubulointerstitial nephritis. IgG subclass immunofluorescence revealed intense IgG4 expression in glomeruli, but no expression of IgG2. Observations resembled membranous lupus nephritis with tubulointerstitial nephritis; however, elevated IgG4, low titers of antinuclear and anti-double-stranded DNA antibodies, IgG4-bearing cell infiltration, and characteristic IgG subclass deposition in glomeruli prompted diagnosis of IgG4-related tubulointerstitial nephritis with membranous nephropathy. It is challenging but important to distinguish lupus nephritis from IgG4-related kidney disease.
We present ALMA CO ($J$=2--1) and 1.3 mm continuum observations of the high-velocity jet associated with the FIR 6b protostar located in the Orion Molecular Cloud-2. We detect a velocity gradient along the short axis of the jet in both the red- and blue-shifted components. The position-velocity diagrams along the short axis of the red-shifted jet show a typical characteristic of a rotating cylinder. We attribute the velocity gradient in the red-shifted component to rotation of the jet. The rotation velocity ($>20\,\ \rm{km s^{-1}}$) and specific angular momentum ($>10^{22}\, \rm{cm^{2}\, s^{-1}}$) of the jet around FIR 6b are the largest among all jets in which rotation has been observed. By combining disk wind theory with our observations, the jet launching radius is estimated to be in the range of $2.18-2.96$\,au. The rapid rotation, large specific angular momentum, and a launching radius far from the central protostar can be explained by a magnetohydrodynamic disk wind that contributes to the angular momentum transfer in the late stages of protostellar accretion.
ObsMode is a yearly process which aims at preparing capabilities for future ALMA Observing cycles. The process has been running for a number of years tied to each ALMA observing cycle, with various leaderships. This document specifically summarizes the ObsMode2020 process (April- October 2020) with a new scheme led by the Joint ALMA Observatory. In the ObsMode2020 process, seven capabilities are identified as high priority items, for which it was originally aimed to be ready for Cycle 9. However, because of the observatory shutdown due to the covid-19 pandemic, we were forced to delay the test plan by one year. While no new data sets were obtained during the observatory shutdown, verifications using the existing data allowed us to offer the 7m-array polarization capability (in ACA standalone mode, single field) for Cycle 8 starting from October, 2021. In addition, subsystem readiness and policy-side preparations for the phased array observing mode were improved for Cycle 8. Other high priority items were decided to be carried over to the ObsMode2021 process.
Abstract We have conducted millimeter interferometric observations of the Orion Molecular Cloud-2 (OMC-2) FIR 6 region at an angular resolution of $\sim$ 4${}^{\prime\prime}$–7${}^{\prime\prime}$ with the Nobeyama Millimeter Array (NMA). In the 3.3-mm continuum emission we detected dusty core counterparts of previously identified FIR sources (FIR 6a, 6b, 6c, and 6d), and moreover resolved FIR 6a into three dusty cores. The size and mass of these cores are estimated to be 1100–5900 AU and 0.19–5.5$ M_{\odot}$, respectively. We found that in the $^{12}$CO ($J$$=$ 1–0) emission FIR 6b, 6c, and 6d eject molecular outflow, and that the FIR 6c outflow also exhibits at least two collimated jet-like components in SiO ($J$$=$ 2–1) emission. At the tip of one of the SiO components there appears an abrupt increase in the SiO line width ($\sim$ 15 km s$^{-1}$), where the three resolved cores in FIR 6a seem to delineate the tip. These results imply the presence of the interaction and a bowshock front between the FIR 6c molecular outflow and FIR 6a. If the interaction occurred after the formation of the FIR 6a cores, the influence of the FIR 6c outflow on the FIR 6a cores would be minimal, since the total gravitational force in the FIR 6a cores (1.0–7.7 $\times$ 10$^{-4} M_{\odot} $km s$^{-1}$yr$^{-1}$) is much larger than the outflow momentum flux (2.4 $\times$ 10$^{-5} M_{\odot} $km s$^{-1}$yr$^{-1}$). On the other hand, it is also possible that the interaction caused the gravitational instability in FIR 6a, and triggered the fragmentation into three cores, since the separation among these cores ($\sim$ 2.0 $\times$ 10$^{3} $AU) is on the same order of the Jeans length ($\sim$ 5.0–8.4 $\times$ 10$^{3} $AU). In either case, FIR 6a cores, with a mass of 0.18–1.6$ M_{\odot}$ and a density of 0.2–5.8 $\times$ 10$^{7} $cm$^{-3}$, might be potential formation sites of the next generation of cluster members.
We present subarcsecond resolution HCN (4–3) and CO (3–2) observations made with the Submillimeter Array, toward an extremely young intermediate-mass protostellar core, MMS 6-main, located in the Orion Molecular Cloud 3 region (OMC-3). We have successfully imaged a compact molecular outflow lobe (≈1000 AU) associated with MMS 6-main, which is also the smallest molecular outflow ever found in the intermediate-mass protostellar cores. The dynamical timescale of this outflow is estimated to be ⩽100 yr. The line width dramatically increases downstream at the end of the molecular outflow (Δv ∼ 25 km s−1) and clearly shows the bow-shock-type velocity structure. The estimated outflow mass (≈10−4 M☉) and outflow size are approximately two to four orders and one to three orders of magnitude smaller, respectively, while the outflow force (≈10−4 M☉ km s−1 yr−1) is similar, compared to the other molecular outflows studied in OMC-2/3. These results show that MMS 6-main is a protostellar core at the earliest evolutionary stage, most likely shortly after the second core formation.
Both high- and low-velocity outflows are occasionally observed around a protostar by molecular line emission. The high-velocity component is called `Extremely High-Velocity (EHV) flow,' while the low-velocity component is simply referred as `(molecular) outflow.' This study reports a newly found EHV flow and outflow around MMS $5$ in the Orion Molecular Cloud 3 observed with ALMA. In the observation, CO $J$=2--1 emission traces both the EHV flow ($|v_{\rm{LSR}} - v_{\rm{sys}}|$ $\simeq$ 50--100 $\rm{km\ s^{-1}}$) and outflow ($|v_{\rm{LSR}} - v_{\rm{sys}}|$ $\simeq$ 10--50 $\rm{km\ s^{-1}}$). On the other hand, SiO $J$=5--4 emission only traces the EHV flow. The EHV flow is collimated and located at the root of the V-shaped outflow. The CO outflow extends up to $\sim$ 14,000\,AU with a position angle (P.A.) of $\sim79^\circ$ and the CO redshifted EHV flow extends to $\sim$11,000 AU with P.A. $\sim96^\circ$. The EHV flow is smaller than the outflow, and the dynamical timescale of the EHV flow is shorter than that of the outflow by a factor of $\sim 3$. The flow driving mechanism is discussed based on the size, time scale, axis difference between the EHV flow and outflow, and the periodicity of the knots. Our results are consistent with the nested wind scenario, although the jet entrainment scenario could not completely be ruled out.
Blood type without the Gregory (Gya) antigen, a high frequency antigen, is extremely rare. A woman showing Gy (a-) received anti-Gya antibody during pregnancy. Two infants born to the woman developed hemolytic disease. There has been no previous report of hemolytic disease in infants born to mothers with anti-Gya antibody. In the present case, the results of a positive direct anti-globulin test on cord blood cells differed from those reported previously. Furthermore, there have been no previous reports describing the IgG subclass in Gy (a-) subjects (IgG1, and IgG4 in the present case). During perinatal care of a pregnant woman with anti-Gya antibody, it is important to provide compatible blood; the present case suggests that transfusion management in these women should consider the possibility of hemolytic disease occurring in the newborn.
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