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We performed simultaneous observations of the H2O 6(1,6) - 5(2,3) (22.235080 GHz) and SiO v= 1, 2, J = 1 - 0, SiO v = 1, J = 2 - 1, 3 - 2 (43.122080, 42.820587, 86.243442, and 129.363359 GHz) masers towards the suspected D-type symbiotic star, V627 Cas, using the Korean VLBI Network. Here, we present astrometrically registered maps of the H2O and SiO v = 1, 2, J = 1 - 0, SiO v = 1, J = 2 - 1 masers for five epochs from January 2016 to June 2018. Distributions of the SiO maser spots do not show clear ring-like structures, and those of the H2O maser are biased towards the north-north-west to west with respect to the SiO maser features according to observational epochs. These asymmetric distributions of H2O and SiO masers are discussed based on two scenarios of a bipolar outflow and the presence of the hot companion, a white dwarf, in V627 Cas. We carried out ring fitting of SiO v = 1, and v = 2 masers and estimated the expected position of the cool red giant. The ring radii of the SiO v = 1 maser are slightly larger than those of the SiO v = 2 maser, as previously known. Our assumption for the physical size of the SiO maser ring of V627 Cas to be the typical size of a SiO maser ring radius (\sim4 au) of red giants yields the distance of V627 Cas to be \sim1 kpc., 7 pages, 4 figures, 1 table, Published in MNRAS

We report VLBI monitoring observations of the 22 GHz water (H$_{2}$O) masers around the Mira variable BX Cam, which were carried out as a part of the EAVN Synthesis of Stellar Maser Animations (ESTEMA) project. Data of 37 epochs in total were obtained from 2018 May to 2021 June with a time interval of 3-4 weeks, spanning approximately three stellar pulsation periods ($P= \sim$440 d). In particular, the dual-beam system equipped on the VERA stations was used to measure the kinematics and parallaxes of the H$_{2}$O maser features. The measured parallax, $\pi=1.79\pm 0.08$ mas, is consistent with $Gaia$ EDR3 and previously measured VLBI parallaxes within a 1-$\sigma$ error level. The position of the central star was estimated, based on both the $Gaia$ EDR3 data and the center position of the ring-like 43 GHz silicon-monoxide (SiO) maser distribution imaged with the KVN. The three-dimensional H$_{2}$O maser kinematics indicates that the circumstellar envelope is expanding at a velocity of $13\pm4$ km s$^{-1}$, while there are asymmetries in both the spatial and velocity distributions of the maser features. Furthermore, the H$_{2}$O maser animation achieved by our dense monitoring program manifests the propagation of shock waves in the circumstellar envelope of BX Cam., Comment: 31 pages, 16 figures, accepted by ApJ

AGBs and YSOs often share the same domains in IR color-magnitude or color-color diagrams leading to potential mis-classification. We extracted a list of AGB interlopers from the published YSO catalogues using the periodogram analysis on NEOWISE time series data. YSO IR variability is typically stochastic and linked to episodic mass accretion. Furthermore, most variable YSOs are at an early evolutionary stage, with significant surrounding envelope and/or disk material. In contrast, AGBs are often identified by a well defined sinusoidal variability with periods of a few hundreds days. From our periodogram analysis of all known low mass YSOs in the Gould Belt, we find 85 AGB candidates, out of which 62 were previously classified as late-stage Class III YSOs. Most of these new AGB candidates have similar IR colors to O-rich AGBs. We observed 73 of these AGB candidates in the H2O, CH3OH and SiO maser lines to further reveal their nature. The SiO maser emission was detected in 10 sources, confirming them as AGBs since low mass YSOs, especially Class III YSOs, do not show such maser emission. The H2O and CH3OH maser lines were detected in none of our targets., Comment: Accepted for publication in ApJL

We report on the astrometric registration of VLBI images of the SiO and H2O masers in OH 231.8+4.2, the iconic Proto-Planetary Nebula also known as the Calabash nebula, using the KVN and Source/Frequency Phase Referencing. This, for the first time, robustly confirms the alignment of the SiO masers, close to the AGB star, which drives the bi-lobe structure with the water masers in the out-flow.

The Korean VLBI Network (KVN) is a unique millimeter VLBI system which is consisted of three 21 m telescopes with relatively short baselines. We present the preliminary results of simultaneous monitoring observations of the 22.2 GHz H2O and 43.1/42.8/86.2/129.3 GHz SiO masers based on the KVN Key Science Project (KSP). We obtained the astrometrically registered maps of the H2O and SiO masers toward nine evolved stars using the source frequency phase referencing method (SFPR). The SFPR maps of the H2O and SiO masers enabled us to investigate the spatial structure and kinematics from the SiO to H2O maser regions including the development of an outward motion from the ring-like or elliptical structures of SiO masers to the asymmetric structures of the 22.2 GHz H2O maser features. In particular, the 86.2/129.3 GHz SiO (v=1, J=2–1 and J=3–2) masers were clearly imaged toward several objects for the first time. The SiO v=1, J=3–2 maser shows different distributions compared to those of the SiO v=1, 2, J=1–0 and v=1, J=2–1 masers implying a different physical condition.

H2O (22 GHz) and SiO masers (43, 86, 129 GHz) in the bipolar proto-planetary nebula OH231.8+4.2 were simultaneously monitored using the 21-m antennas of the Korean VLBI Network in 2009-2015. Both species exhibit periodic flux variations that correlate with the central star's optical light curve, with a phase delay of up to 0.15 for the maser flux variations with respect to the optical light curve. The flux densities of SiO v = 2, J = 1-0 and H2O masers decrease with time, implying that they may disappear in 10-20 years. However, there seems to have been a transient episode of intense H2O maser emission around 2010. We also found a systematic behaviour in the velocity profiles of these masers. The velocities of the H2O maser components appear to be remarkably constant, suggesting ballistic motion for the bipolar outflow in this nebula. On the other hand, those of the SiO maser clumps show a systematic radial acceleration of the individual clumps, converging to the outflow velocity of the H2O maser clumps. Measuring the full widths at zero power of the detected lines, we estimated the expansion velocities of the compact bipolar outflow traced by H2O maser and SiO thermal line, and discussed the possibility of the expanding SiO maser region in the equatorial direction. All of our analyses support that the central host star of OH231.8 is close to the tip of the AGB phase, and that the mass-loss rate recently started to decrease because of incipient post-AGB evolution., Comment: 21 pages, 16 figures

We present the jet kinematics of the flat spectrum radio quasar (FSRQ) 4C +21.35 using time-resolved KaVA very long baseline interferometry array radio maps obtained from September 2014 to July 2016. During two out of three observing campaigns, observations were performed bi-weekly at 22 and 43 GHz quasi-simultaneously. At 22 GHz, we identified three jet components near the core with apparent speeds up to (14.4+/-2.1)c. The timing of the ejection of a new component detected in 2016 is consistent with a gamma-ray flare in November 2014. At 43 GHz, we found four inner jet (, 11 pages, 9 figures, 3 tables. To appear in MNRAS (submitted 2018 June 7; accepted 2019 March 28)

Simultaneous monitoring observations of H2O 61,6 − 52,3 and SiO v = 1, 2, J = 1 → 0, v = 1, J = 2 → 1, J = 3 → 2 masers were performed toward the suspected D-type symbiotic star V627 Cas from 2011 October to 2020 March using the Korean Very Long Baseline Interferometry (VLBI) Network (KVN) single-dish telescopes. All spectra of the H2O masers showed highly redshifted emissions with respect to the stellar velocity of −52 km s−1 with high asymmetries. In addition, the spectra of the H2O maser showed three components which varied according to observational dates. On the other hand, the SiO v = 1, 2, J = 1 → 0 and v = 1, J = 2 → 1 masers exhibited a predominantly blueshifted emission in most epochs. The SiO v = 1, J = 3 → 2 maser has arisen around the stellar velocity from 2016 November 19 and shows a predominantly redshifted emission from 2018 June 15. We analyze time variations of the H2O and SiO maser intensities, their intensity ratios, peak and mean velocities, and full width zero power. Based on these analyses, the asymmetries of the H2O and SiO masers’ spectra in V627 Cas and the variation characteristics of the maser properties of the different maser lines are discussed. As a possible cause of asymmetries, the influence of a hot component located at the eastern part of the red giant can be suggested based on the KVN VLBI results. The differences in the variation characteristics of the maser properties may originate from the differences in their locations and excitation conditions.

We observe ten known 22GHz H₂O maser galaxies during February 19–22, 2011 using the 21 m Tamna telescope of the Korean VLBI Network and a new wide-band digital spectrometer. Simultaneously we searched for 43GHz SiO v = 1, 2, J = 1–0 maser emission. We detect H₂O maser emission towards five sources (M 33, NGC 1052, NGC 1068, NGC 4258, M 82), with non-detections towards the remaining sources (UGC 3193, UGC 3789, Antennae H₂O-West, M 51, NGC 6323) likely due to sensitivity. Our 22GHz spectra are consistent with earlier findings. Our simultaneous 43GHz SiO maser search produced non-detections, yielding – for the first time – upper limits on the 43GHz SiO maser emission in these sources at a 3 σ sensitivity level of 0.018K–0.033K (0.24 Jy–0.44 Jy) in a 1.75 km s −1 velocity resolution. Our findings suggest that any 43GHz SiO masers in these sources (some having starburst-associated H₂O kilomasers) must be faint compared to the 22GHz H₂O maser emission.

The supergiant VX Sagittarii is a strong emitter of both H2O and SiO masers. However, previous VLBI observations have been performed separately, which makes it difficult to spatially trace the outward transfer of the material consecutively. Here we present the astrometrically registered, simultaneous maps of 22.2 GHz H2O and 43.1/42.8/86.2/129.3 GHz SiO masers toward VX Sagittarii. The H2O masers detected above the dust-forming layers have an asymmetric distribution. The multi-transition SiO masers are nearly circular ring, suggesting spherically symmetric wind within a few stellar radii. These results provide the clear evidence that the asymmetry in the outflow is enhanced after the smaller molecular gas clump transform into the inhomogeneous dust layers. The 129.3 GHz maser arises from the outermost region compared to that of 43.1/42.8/86.2 GHz SiO masers. The ring size of the 129.3 GHz maser is maximized around the optical maximum, suggesting that radiative pumping is dominant., 7 pages, 4 figures, available complementary data in nature communications web site

We report on the astrometric registration of VLBI images of the SiO and water masers in OH231.8+4.2, the iconic Proto-Planetary Nebula also known as the Calabash nebula, using the KVN and Source/Frequency Phase Referencing. This, for the first time, robustly confirms the alignment of the SiO masers, close to the AGB star, driving the bi-lobe structure with the water masers in the out-flow. We are able to trace the bulk motions for the water masers over the last few decades to be 19 km/s and deduce that the age of this expansion stage is 38$\pm$2 years. The combination of this result with the distance allows a full 3D reconstruction, and confirms that the water masers lie on and expand along the known large-scale symmetry axis and that the outflow is only a few decades old, so mass loss is almost certainly on-going. Therefore we conclude that the SiO emission marks the stellar core of the nebular, the water emission traces the expansion, and that there must be multiple epochs of ejection to drive the macro-scale structure., Figure 6 is 3D

In order to understand the excitation mechanisms of silicon monoxide (SiO) masers around long-period variables (LPVs), we have investigated distributions of the SiO v = 2 and v = 3 J = 1 → 0 masers around 12 LPVs by very long baseline interferometry (VLBI) observations with the VLBI Exploration of Radio Astrometry (VERA) and the Nobeyama 45 m telescopes. VLBI fringes of the v = 3 maser emission were detected for five LPVs. The composite maps of the v = 2 and v = 3 masers were made for T Cep, W Hya, WX Psc, and R Leo using the spectral line phase-referencing technique. The v = 2 maser spots were distributed in a ring-like form around the central stars, while it is difficult to recognize any specific morphology in the v = 3 maser distributions due to the small number of v = 3 spots detected. However in T Cep, we find that the distribution of the v = 3 maser spots correlates well with the v = 2 masers within a few milliarcseconds (0.2-0.3 au) in position and 1 km s-1 in line-of-sight velocity at the light curve phase of θ = 0.28 (θ = 0.0 and 1.0 correspond to the visible light maxima). This correlation implies that the mechanism of line-overlapping between the mid-infrared lines of H2O and SiO molecules works in T Cep at θ = 0.28. We discuss the possibility that the line-overlapping may work at the limited duration from the maximum to the minimum of the stellar light curve. © 2018 The Author(s).

Purpose Healthy, young individuals are known to exhibit circadian variation in urinary functions. However, the effects of chronic circadian disturbance on voiding functions are largely unknown. The present work compared the effects of rotational shifts on the micturition patterns of female nurses to that in female nurses with routine daytime shifts. Methods A total of 19 nurses without lower urinary tract symptoms who worked rotational shifts for an average duration of 2 years were recruited. A voiding diary was kept for 9 consecutive days, and the overactive bladder symptom score (OABSS) questionnaire was completed three times, starting 3 days before their night duties until 3 days after completion of their night duties. For comparison, seven nurses with regular shifts completed a 3-day voiding diary and the OABSS questionnaire. Results Female nurses working rotational shifts had lower overall urine production and had decreased urination frequency and nocturia than female nurses working regular shifts, even when the nurses who worked rotational shifts had a regular night's sleep for at least 7 days. Upon reinitiation of night duty, overall urine production increased significantly, with no significant changes in urgency and frequency. When these nurses returned to daytime duty, the volume of urine decreased but nocturnal urine production remained high, and the incidence of nocturia also increased significantly. However, the effects on OABSS score were not significant under the study design used. Conclusions Long-term rotational shifts resulted in adaptive changes such as decreased urine production and frequency in healthy, young female nurses. In addition, their micturition patterns were significantly affected by abrupt changes in their work schedules. Although working in shifts did not increase urgency or frequency of urination in healthy, young female nurses working rotational shifts for an average 2 years, large-scale studies are needed to systematically analyze the influence of shift work timings on micturition in humans.

Circadian rhythmic(CR) disruption shows adverse effects like fatigue, nocturia, sleep-disturbance, and mood disorder which are common in elderly. We investigate the relationship between CR and water metabolism(WM) and expression of circadian-clock-gene(CCG) in peripheral bladder and central-micturition-centers(CMC).

Recent studies have explored the association between serum lipids and bone mineral density (BMD). However, the results are inconsistent and studies for premenopausal women are very sparse. For the investigation without confounding effects of menopause, we analyzed the data collected from premenopausal women in early 40s and elderly women aged 70 and older, and comprehensive physiologic markers were included. Our Korean study population was consisted of 3,953 premenopausal women (age range 40~44, mean age 42.3 ± 1.3) and 986 elderly women (70~92, 73.8 ± 3.5). BMDs were measured by dual X-ray absorptiometry at lumbar spine (LS), femoral neck (FN), and total hip (TH). Height, percent body fat, and fasting serum measures of total cholesterol (TC), HDL-C, LDL-C, triglyceride, hsCRP, albumin, glucose, gamma-glutamyltransferase (GGT), estradiol, thyroid-stimulating hormone, and estimated GFR were included in the analyses. Multivariate linear regression models were used to examine relationships between BMD (dependent variable) and other variables. After adjusting for covariates, HDL-C was negatively associated with BMD at LS (β = -0.052, p = 0.004), FN (β = -0.064, p = 0.000), and TH (β = -0.073, p = 0.000) in premenopausal women. In elderly women, LDL-C was negatively associated with BMD at LS (β = -0.104, p = 0.001), FN (β = -0.057, p = 0.068), and TH (β = -0.064, p = 0.042). Our results suggest that serum lipids are inversely correlated with BMD and the pattern is different among young and old women.

The circadian clock is a self-sustaining oscillator that controls daily rhythms. For the proper circadian gene expression, dynamic changes in chromatin structure are important. Although chromatin modifiers have been shown to play a role in circadian gene expression, the in vivo role of circadian signal-modulated chromatin modifiers at an organism level remains to be elucidated. Here, we provide evidence that the lysine-specific demethylase 1 (LSD1) is phosphorylated by protein kinase Cα (PKCα) in a circadian manner and the phosphorylated LSD1 forms a complex with CLOCK:BMAL1 to facilitate E-box-mediated transcriptional activation. Knockin mice bearing phosphorylation-defective Lsd1(SA/SA) alleles exhibited altered circadian rhythms in locomotor behavior with attenuation of rhythmic expression of core clock genes and impaired phase resetting of circadian clock. These data demonstrate that LSD1 is a key component of the molecular circadian oscillator, which plays a pivotal role in rhythmicity and phase resetting of the circadian clock.

We recently established an adrenal clock-disrupted transgenic mouse line (BMAS) that exhibits a dampened rhythm of corticosterone secretion and reduced amplitude of day/night activity. Here, we observe that voluntary wheel running increases the robustness and amplitude of both body temperature and home cage activity (HCA) rhythms in wild-type, but not in BMAS mice, but without affecting estrous cycle. Surprisingly, wheel running alters the HCA waveform of BMAS females in a way that preferentially increases the late nighttime (ZT21–ZT24) HCA. These results indicate that adrenal clock disruption causes the animals to respond differently to the voluntary exercise cue in middle-aged female mice.

Glucocorticoid (GC) signaling synchronizes the circadian rhythm of individual peripheral cells and induces the expression of circadian genes, including Period1 (Per1) and Period2 (Per2). However, no GC response element (GRE) has been reported in the Per2 promoter region. Here we report the molecular mechanisms of Per2 induction by GC signaling and its relevance to the regulation of circadian timing. We found that GC prominently induced Per2 expression and delayed the circadian phase. The overlapping GRE and E-box (GE2) region in the proximal Per2 promoter was responsible for GC-mediated Per2 induction. The GRE in the Per2 promoter was unique in that brain and muscle ARNT-like protein-1 (BMAL1) was essential for GC-induced Per2 expression, whereas other GRE-containing promoters, such as Per1 and mouse mammary tumor virus, responded to dexamethasone in the absence of BMAL1. This specialized regulatory mechanism was mediated by BMAL1-dependent binding of the GC receptor to GRE in Per2 promoter. When Per2 induction was abrogated by the mutation of the GRE or E-box, the circadian oscillation phase failed to be delayed compared with that of the wild-type. Therefore, the current study demonstrates that the rapid Per2 induction mediated by GC is crucial for delaying the circadian rhythm.

Most bipolar outflows are associated with individual young stellar objects and have small opening angles. Here we report the discovery of an extremely wide-angle ($\sim$180$\arcdeg$) bipolar outflow ("EWBO") in a cluster forming region AFGL 5142 from low-velocity emission of the HCN (3-2) and HCO$^{+}$ (3-2) lines. This bipolar outflow is along a north-west to south-east direction with a line-of-sight flow velocity of about 3 km~s$^{-1}$ and is spatially connected to the high-velocity jet-like outflows. It seems to be a collection of low-velocity material entrained by the high-velocity outflows due to momentum feedback. The total ejected mass and mass loss rate due to both high velocity jet-like outflows and the "EWBO" are $\sim$24.5 M$_{\sun}$ and $\sim1.7\times10^{-3}$ M$_{\sun}$~yr$^{-1}$, respectively. Global collapse of the clump is revealed by the "blue profile" in the HCO$^{+}$ (1-0) line. A hierarchical network of filaments was identified in NH$_{3}$ (1,1) emission. Clear velocity gradients of the order of 10 km~s$^{-1}$~pc$^{-1}$ are found along filaments, indicating gas inflow along the filaments. The sum of the accretion rate along filaments and mass infall rate along the line of sight is $\sim$3.1$\times10^{-3}$ M$_{\sun}$~yr$^{-1}$, which exceeds the total mass loss rate, indicating that the central cluster is probably still gaining mass. The central cluster is highly fragmented and 22 condensations are identified in 1.1 mm continuum emission. The fragmentation process seems to be determined by thermal pressure and turbulence. The magnetic field may not play an important role in fragmentation., accepted by ApJ

The purpose of this study was to examine whether Phellodendri Cortex extract (PCE) could improve learning and memory impairments caused by lipopolysaccharide (LPS)-induced inflammation in the rat brain. The effect of PCE on modulating pro-inflammatory mediators in the hippocampus and its underlying mechanism were investigated. Injection of LPS into the lateral ventricle caused acute regional inflammation and subsequent deficits in spatial learning ability in the rats. Daily administration of PCE (50, 100, and 200 mg/kg, i.p.) for 21 days markedly improved the LPS-induced learning and memory disabilities in the Morris water maze and passive avoidance test. PCE administration significantly decreased the expression of pro-inflammatory mediators such as tumor necrosis factor-α, interleukin-1β, and cyclooxygenase-2 mRNA in the hippocampus, as assessed by RT-PCR analysis and immunohistochemistry. Together, these findings suggest that PCE significantly attenuated LPS-induced spatial cognitive impairment...

The purpose of this study is to clarify the impact of information contents at online purchase sites of movie merchandise. The results of this study are as follows: 1) Movie-understanding information(synopsis, actors, reviews) has a meaningful influence on information service satisfaction irrespective of consumer involvement; 2) Movie-understanding and movie-going information(time, place, price, purchasing method) are alike in having a meaningful influence on online purchasing intention. However, movie-going information has a meaningful influence in case of lower consumer involvement, while movie-understanding information has a meaningful influence in case of higher consumer involvement.; 3) Information service satisfaction gives a strong influence on online purchasing intention irrespective of the level of consumer involvement. In conclusion, there is a need to improve diversity and quality of movie-understanding information to enhance consumer satisfaction. Also, it will be necessary to improve movie-understanding and movie-going information in order to enhance online purchasing intention. These results are expected to give an insight to build a creative marketing strategy of online purchase sites of movie merchandise.

Depression is one of the most prevalent diseases of alcohol abuse. Brain-derived neurotrophic factor (BDNF) plays a critical role in cell survival in the hippocampus. Phosphorylation of extracellular signal-regulated kinase 1/2 (p-ERK1/2) is induced by BDNF, and it regulates cell proliferation and differentiation in the brain. We investigated the effects of alcohol intake on depression-like behavior, cell proliferation, expressions of BDNF and its downstream molecules in the hippocampus using Mongolian gerbils. The gerbils were divided into four groups: control group, 0.5 g/kg alcohol-treated group, 1 g/kg alcohol-treated group, 2 g/kg alcohol-treated group. Each dose of alcohol was orally administered for 3 weeks. The present results demonstrated that alcohol intake induced depression-like behavior. Both 5-hydroxytryptamine synthesis and its synthesizing enzyme tryptophan hydroxylase expression in the dorsal raphe and cell proliferation in the hippocampal dentate gyrus were decreased by alcohol ...

Hypoxic ischemia injury is a common cause of functional brain damage, resulting from a decrease in cerebral blood flow and oxygen supply to the brain. The main problems associated with hypoxic ischemia to the brain are memory impairment and dopamine dysfunction. Hypothermia has been suggested to ameliorate the neurological impairment induced by various brain insults. In this study, we investigated the effects of hypothermia on memory function and dopamine synthesis following hypoxic ischemia to the brain in rats. For this purpose, a step-down avoidance task, a radial eight-arm maze task, and immunohistochemistry for tyrosine hydroxylase (TH) and 5-bromo-2′-deoxyuridine (BrdU) were performed. The present results indicated that the hypoxic ischemia-induced disturbance of the animal's performances and spatial working memory was associated with a decrement in TH expression in the substantia nigra and striatum, and an increase in cell proliferation in the hippocampal dentate gyrus. Hypothermia treatme...

Stress urinary incontinence (SUI) is a common condition that primarily affects women. Here, we investigate the effects of human adipose-derived stem cells (ADSCs) in a rodent model of SUI. Female Sprague-Dawley rats at 7 weeks of age were randomly divided into three groups (n=8 per group): sham-operation, SUI-induction by transabdominal urethrolysis, and SUI-induction followed by transplantation of human ADSCs into the urethra. The abdominal leak point pressure at 8 weeks after the operation was markedly decreased by transabdominal urethrolysis, confirming successful induction of SUI. Interestingly, transplantation of human ADSCs into the urethra significantly blunted the decrease of abdominal leak point pressure in SUI-induced rats. Accordingly, we observed expression of α-smooth muscle actin in a significant proportion of transplanted ADSCs, indicating differentiation of ADSCs into smooth muscle cells in the urethra. Moreover, the SUI-induced elevations of c-Fos immunoreactivities in the pontin...

Aging leads to functional changes in the hippocampus, and consequently induces cognitive deficits, such as failure of memory. Neurogenesis in the hippocampal dentate gyrus continues throughout life, but steadily declines from early adulthood. Apoptosis occurs under various pathologic and physiologic conditions, and excessive apoptotic cell death can cause a number of functional disorders in humans. Apoptosis in the hippocampus also disturbs cognitive functions. In this study, we examined the effect of treadmill exercise on memory in relation to neurogensis and apoptosis in the hippocampal dentate gyrus of old-aged rats. The present results showed that loss of memory by aging was associated with a decrease in neurogenesis and an increase in apoptosis in the hippocampal dentate gyrus. Treadmill exercise improved short-term and spatial memories by enhancing neurogenesis and suppressing apoptosis in the hippocampal dentate gyrus of old-aged rats. In the present study, we showed that treadmill exercise is a very useful strategy for preventing failure of memory in the elderly.

We present the results of simultaneous observations of both SiO and H2O masers toward 166 known SiO and H2O maser sources using the Korean VLBI Network Yonsei 21 m radio telescope during 2009 June. Both SiO and H2O maser emission were detected from 112 sources giving a detection rate of 67% at one epoch observation. SiO-only maser emission was detected from 42 sources, while H2O-only maser emission was detected from four sources. Most of the SiO masers appear around the stellar velocity, while H2O masers show different characteristics compared with SiO masers. There are more than 20 sources that show a one-way peak or double peaks with respect to the stellar velocity and SiO maser peak velocity. The H2O maser peak and integrated intensity ratios with respect to those of SiO (v = 1) show increasingly larger values from Mira variables, to OH/IR stars, to semi-regular variables. In addition, the IRAS two-color diagram of SiO and H2O maser observational results is discussed.

We have carried out time monitoring observations of the 28SiO v = 0, 1, 2, J = 2 – 1, 28SiO v = 0, 1, 2, J = 3 – 2, and 29SiO v = 0, J = 3 – 2 transitions in Orion KL with the 14 m radio telescope at Taeduk Radio Astronomy Observatory. The pair of J = 2 – 1 and J = 3 – 2 transitions was simultaneously observed from 1999 January to 2001 March. Each transition shows different characteristics. Both the v = 1, J = 2 – 1, and J = 3 – 2 masers show a relatively stable double-peaked profile and little variation in intensity. The 28SiO v = 2, J = 3 – 2 maser presents the most active intensity variations including a disappearance on 2000 February 17 and 2001 February 16. The v = 2, J = 3 – 2 maser may trace the closest region to the central young stellar object and results in the strongest variations of intensity and line profile. The v = 2, J = 2 – 1 maser was not detected in the monitoring. The 28SiO v = 0, J = 3 – 2 lines showed a large variation of peak intensity compared with 28SiO v = 0, J = 2 – 1 that might be due to partial masing. The different observational results of 28SiO v = 0, 1, J = 2 – 1, 28SiO v = 0, 1, 2, J = 3 – 2, and 29SiO v = 0, J = 3 – 2 transitions might reflect that individual transitions trace different portions of gas.

Second observations of SiO v = 1, 2, J = 3-2 transitions, together with SiO v = 1, J = 2-1 transitions, have been performed toward 42 program late-type stars, using the 14 m radio telescope at Taeduk Radio Astronomy Observatory, from 1997 February to 1998 March. The v = 1, J = 3-2 maser was detected from 24 stars giving a detection rate of 57%, which is slightly higher than that of the first observations of 1995-1996. Four of these are new detections. For the v = 2, J = 3-2 maser, the line was detected from six stars including two new detections. The peak velocities and the velocity patterns of the v = 1, J = 3-2 masers are different from those of the v = 1, J = 2-1 indicating a difference in the traced regions. The average total photon flux of the v = 1, J = 3-2 maser is estimated to be 10{sup 42.7}, that of the v = 2, J = 3-2 maser 10{sup 42.2}, and that of the v = 1, J = 2-1 maser 10{sup 43.2} photons s{sup -1}. In addition, we confirm that the v = 2, J = 4-3 masermore » is stronger than the v = 1, J = 4-3.« less

This study aims to investigate the impacts of managerial and technical IT knowledges on firm`s financial performance. Specifically, the study examines the following three effects between IT personnel knowledges and financial performance: (1) direct effect, (2) mediating effect of business process performance, and (3) moderating effect of firm size, between them. An empirical study resulted in the followings. First, both managerial and technical IT knowledges do not have direct influences on financial performance. Second, unlike technical IT knowledge, managerial IT knowledge indirectly affects financial performance through business process performance, confirming the mediating role of business process performance. Third, while technical IT knowledge produce no direct and indirect effect on financial performance regardless of firm size, managerial IT knowledge exerts significant impacts on financial performance although such effects represent some different patterns according to firm size. That is, in the smaller group, the association between managerial IT knowledge and financial performance is partially mediated by business process performance and in the larger group, that relationship fully mediated.

A spectral line survey of the proto-planetary nebula CRL 2688 was carried out in the frequency range of 85-116 GHz with the 14 m radio telescope at the Taeduk Radio Astronomy Observatory. Eight detected molecules are all carbon bearing molecules: HCN, HNC, C2H, HC3N, CS, CCS, CN, and CO, and their isotopic species H13CN and 13CO. A CCS line was newly detected in CRL 2688. The molecular lines detected in CRL 2688 were also compared with those of the proto-typical AGB star IRC +10216. The SiS (J = 5-4, v = 0) molecular line detected in IRC +10216 was not detected in CRL 2688, indicating a lower abundance of the SiS molecule in CRL 2688 than in IRC +10216. Excitation temperatures and column densities of HC3N in both CRL 2688 and IRC +10216 were derived using standard LTE rotational diagram analysis. The HC3N column density of CRL 2688 was found to be lower than that of IRC +10216. This fact, together with the lower abundance of the SiS molecule in CRL 2688, may be related to the chemical evolution of the circumstellar envelope of CRL 2688.

From the simultaneous observations of SiO v = 3, J = 2-1 and J = 3-2 masers, SiO v = 3, J = 2-1 maser emission was detected for the first time toward the S-type Mira variable χ Cyg. The line was a single spike and was redshifted with respect to the stellar velocity. The SiO v = 3, J = 3-2 maser emission was not detected from this star. However, for the O-rich Mira variable TX Cam, SiO v = 3, J = 3-2 maser emission was detected, while v = 3, J = 2-1 maser was not detected. Two possible line overlaps were adopted as an explanation of these observational results.

Metformin is a treatment of choice for patients with type 2 diabetes. Its action involves the phosphorylation of 5'-adenosine monophosphate activated protein kinase (AMPK), leading to inhibition of liver gluconeogenesis. The effects of a novel chemical compound derived from metformin, HL271, on molecular and physiological actions involving AMPK and rhythmically-expressed circadian clock genes were investigated. HL271 potently activated AMPK in a dose-dependent manner, and produced shortening of the circadian period and enhanced degradation of the clock genes PER2 and CRY1. Although the molecular effects of HL271 resembled those of metformin, it produced different physiological effects in mice with diet-induced obesity. HL271 did not elicit glucose-lowering or insulin-sensitizing effects, possibly because of altered regulation of glucose-6-phosphatase and phosphoenolpyruvate carboxykinase 1. This indicated that, although HL271 acted on circadian clock machinery through a similar molecular mechanism to metformin, it differed in its systemic effect on glucose and lipid metabolite regulations.

Simultaneous time monitoring observations of H$_{2}$O and SiO maser lines were performed toward the D-type symbiotic binary system V407 Cyg with the Korean VLBI Network single dish radio telescope. These monitoring observations were carried out from March 2, 2010 (optical phase $\phi$ = 0.0), 8 days before the nova outburst on March 10, 2010 to June 5, 2014 ($\phi$ = 2.13). Eight days before the nova outburst, we detected the SiO $v$ = 1, 2, $J$ = 1--0 maser lines which exhibited values of 0.51 K ($\sim$ 6.70 Jy) and 0.71 K ($\sim$ 9.30 Jy), respectively, while after the outburst we could not detect them on April 2 ($\phi$ = 0.04), May 5 ($\phi$ = 0.09), May 8 ($\phi$ = 0.09), or on June 5, 2010 ($\phi$ = 0.13) within the upper limits of our KVN observations. After restarting our monitoring observations, we detected SiO $v$ = 2, $J$ = 1--0 masers starting on October 20, 2011 ($\phi$ = 0.83) and detected SiO $v$ = 1, $J$ = 1--0 masers starting on December 22, 2011 ($\phi$ = 0.92). These results provide clear evidence of the interaction between the shock from the nova outburst and the SiO maser regions of the Mira envelope. The peak emission of SiO $v$ = 1, 2, $J$ = 1--0 masers always occurred at blueshifted velocities with respect to the stellar velocity except for that of SiO $v$ = 1 at one epoch. These phenomena may be related to the redistribution of SiO maser regions after the outburst. The peak velocity variations of SiO masers associated with stellar pulsation phases show an increasing blueshifted trend during our monitoring interval after the outburst., Comment: 9 pages and 3 figures

The mammalian circadian clock is an endogenous biological timer comprised of transcriptional/translational feedback loops of clock genes. Bmal1 encodes an indispensable transcription factor for the generation of circadian rhythms. Here, we report a new circadian mutant mouse from gene-trapped embryonic stem cells harboring a C-terminus truncated Bmal1 (Bmal1(GT Delta C)) allele. The homozygous mutant (Bmal1(GT Delta C/GT Delta C)) mice immediately lost circadian behavioral rhythms under constant darkness. The heterozygous (Bmal1(+/GT Delta C)) mice displayed a gradual loss of rhythms, in contrast to Bmal1+/-mice where rhythms were sustained. Bmal1(GT Delta C/GT Delta C) mice also showed arrhythmic mRNA and protein expression in the SCN and liver. Lack of circadian reporter oscillation was also observed in cultured fibroblast cells, indicating that the arrhythmicity of Bmal1(GT Delta C/GT Delta C) mice resulted from impaired molecular clock machinery. Expression of clock genes exhibited distinct responses to the mutant allele in Bmal1(+/GT Delta C) and Bmal1(GT Delta C/GT Delta C) mice. Despite normal cellular localization and heterodimerization with CLOCK, overexpressed BMAL1(GT Delta C) was unable to activate transcription of Per1 promoter and BMAL1-dependent CLOCK degradation. These results indicate that the C-terminal region of Bmal1 has pivotal roles in the regulation of circadian rhythms and the Bmal1(GT Delta C) mice constitute a novel model system to evaluate circadian functional mechanism of BMAL1.

Background Patients with Alzheimer’s disease (AD) frequently experience disruption of their circadian rhythms, but whether and how circadian clock molecules are perturbed by AD remains unknown. AD is an age-related neurological disorder and amyloid-β (Aβ) is one of major causative molecules in the pathogenesis of AD. Results In this study, we investigated the role of Aβ in the regulation of clock molecules and circadian rhythm using an AD mouse model. These mice exhibited altered circadian behavior, and altered expression patterns of the circadian clock genes, Bmal1 and Per2. Using cultured cells, we showed that Aβ induces post-translational degradation of the circadian clock regulator CBP, as well as the transcription factor BMAL1, which forms a complex with the master circadian transcription factor CLOCK. Aβ-induced degradation of BMAL1 and CBP correlated with the reduced binding of transcription factors to the Per2 promoter, which in turn resulted in disruptions to PER2 protein expression and the oscillation of Per2 mRNA levels. Conclusions Our results elucidate the underlying mechanisms for disrupted circadian rhythm in AD. Electronic supplementary material The online version of this article (doi:10.1186/s13024-015-0007-x) contains supplementary material, which is available to authorized users.

W49N is a mini-starburst in the Milky Way and thus an ideal laboratory for high-mass star formation studies. Due to its large distance (11.1$_{-0.7}^{+0.9}$ kpc), the kinematics inside and between the dense molecular clumps in W49N are far from well understood. The SMA observations resolved the continuum emission into two clumps. The molecular line observation of SO$_{2}$ (28$_{4,24}$-28$_{3,25}$) suggests that the two clumps have a velocity difference of $\sim$7 km~s$^{-1}$. The eastern clump is very close to two radio sources "G1" and "G2", and the western clump coincides with a radio source "B". The HCN (3-2) line reveals an extremely energetic outflow, which is among the most energetic molecular outflows in the Milky Way. This is the first report of high-velocity molecular outflow detection in W49N. The outflow jet might be in precession, which could account for the distribution, velocity and rotation of water maser spots. Three absorption systems are identified in HCO$^{+}$ (3-2) spectra. The absorption features are blueshifted with respect to the emission of SO$_{2}$ (28$_{4,24}$-28$_{3,25}$) lines, indicating that a cold layer is expanding in front of the warm gas. Further analysis indicates that the expansion is decelerated from the geometric expansion centers., Comment: Accepted to ApJ

We present the results of simultaneous time monitoring observations of SiO J = 2-1 and J = 3-2 maser emission for 10 late-type stars (8 Mira variables, 1 OH/IR star, and 1 supergiant) with the 14 m radio telescope at Taeduk Radio Astronomy Observatory from 1999 January to 2001 February. The SiO v = 1, J = 2-1 and J = 3-2 maser emission was detected at almost all observational epochs. The SiO v = 2, J = 2-1 maser was detected from 4 late-type stars (VY CMa, R Cas, χ Cyg, R Leo) and the v = 2, J = 3-2 maser was detected from 7 stars (R Aqr, TX Cam, R Cas, χ Cyg, W Hya, R Leo, IK Tau). The v = 3, J = 2-1 and J = 3-2 masers were also detected from χ Cyg and TX Cam, respectively. Based on these observational data, line profile and peak velocity variations with respect to stellar velocity, antenna temperatures, and their ratio variations as a function of optical phase of central star were investigated. As main results, the line profile and the peak velocity variation of the v = 1, J = 3-2 maser with pulsation phase was found to differ from the v = 1, J = 2-1 transition. Similarly, the J = 2-1 and J = 3-2 transitions also differ between rovibrational transitions at a given pulsation phase. However, it is difficult to find significant correlations between the peak velocity variation relative to the stellar velocity of either the J = 3-2 or J = 2-1 transitions over pulsation phase, due to limited time sampling in these data. The peak and integrated antenna temperature (PT and IT) ratios among rotational ladders and vibrational states are investigated. These ratios between rotational ladders of the v = 1, J = 2-1, and J = 3-2 masers are averaged to be the peak antenna temperature ratio, PT(v = 1, J = 3-2)/PT(v = 1, J = 2-1) ≈ 0.29, and the integrated antenna temperature ratio, IT(v = 1, J = 3-2)/IT(v = 1, J = 2-1) ≈ 0.21, respectively. In the v = 2 state, these ratios are PT(v = 2, J = 3-2)/PT(v = 2, J = 2-1) ≈ 7.94 and IT(v = 2, J = 3-2)/IT(v = 2, J = 2-1) ≈ 8.50, respectively. The peak and integrated antenna temperature ratios between vibrational states are also averaged to be PT(v = 2, J = 3-2)/PT(v = 1, J = 3-2) ≈ 1.29, IT(v = 2, J = 3-2)/IT(v = 1, J = 3-2) ≈ 1.02, PT(v = 2, J = 2-1)/PT(v = 1, J = 2-1) ≈ 0.06, and IT(v = 2, J = 2-1)/IT(v = 1, J = 2-1) ≈ 0.05, respectively. These intensity ratios for the v = 2, J = 2-1 and v = 2, J = 3-2 masers suggest that line overlaps operating in the v = 2, J = 2-1 transition do not similarly affect the v = 2, J = 3-2 transition.

Simultaneous time monitoring observations of H$_{2}$O $6_{16}-5_{23}$, SiO $J$ = 1--0, 2--1, 3--2, and $^{29}$SiO $v$ = 0, $J$ = 1--0 lines were carried out in the direction of the Mira variable star TX Cam with the Korean VLBI Network single dish radio telescopes. For the first time, the H$_{2}$O maser emission from TX Cam was detected near the stellar velocity at five epochs from April 10, 2013 ($\phi$ = 3.13) to June 4, 2014 ($\phi$ = 3.89) including minimum optical phases. The intensities of H$_{2}$O masers are very weak compared to SiO masers. The variation of peak antenna temperature ratios among SiO $v$ = 1, $J$ = 1--0, $J$ = 2--1, and $J$ = 3--2 masers is investigated according to their phases. The shift of peak velocities of H$_{2}$O and SiO masers with respect to the stellar velocity is also investigated according to observed optical phases. The H$_{2}$O maser emission occurs around the stellar velocity during our monitoring interval. On the other hand, the peak velocities of SiO masers show a spread compared to the stellar velocity. The peak velocities of SiO $J$ = 2--1, and $J$ = 3--2 masers show a smaller spread with respect to the stellar velocity than those of SiO $J$ = 1--0 masers. These simultaneous observations of multi-frequencies will provide a good constraint for maser pumping models and a good probe for investigating the stellar atmosphere and envelope according to their different excitation conditions., Comment: 10 pages

A spectral line survey is performed from 159.7 to 164.7 GHz toward Orion-KL, as an extension of our previous line survey from 138.3 to 150.7 GHz with the same 14 m radio telescope of Taeduk Radio Astronomy Observatory. Typical system temperatures were 260 - 1000 K to achieve a sensitivity of about 0.02 - 0.04 K in TA unit. A total of 63 line spectra are detected in this survey. Among them, 54 lines lines are found to be the first detections towards an astronomical source and only 9 spectral lines have been previously identified from other observations. Forty-eight of 54 lines are believed to be from the known transitions of the known molecules, while 6 lines are `unidentified`. All detected lines are found to be from a total of 10 molecular species and their isotopic variants. The molecular species with most numerous detected transitions are (22), followed by (7), (7), and (6). The LTE rotation diagram analysis using all homogeneous data with those from previous survey gives more reliable determination of physical quantities. The derived values of the rotation temperatures and column densities for , , and are are 75 197 K and , respectively.

Oxygen-rich Asymptotic Giant Branch (AGB) stars can be intense emitters of SiO ($v$=1 and 2, J=1$\rightarrow$0) and H$_2$O maser lines at 43 and 22 GHz, respectively. VLBI observations of the maser emission provide a unique tool to probe the innermost layers of the circumstellar envelopes in AGB stars. Nevertheless, the difficulties in achieving astrometrically aligned \water\ and $v$=1 and $v$=2 SiO maser maps have traditionally limited the physical constraints that can be placed on the SiO maser pumping mechanism. We present phase referenced simultaneous spectral-line VLBI images for the SiO $v$=1 and $v$=2, J=1$\rightarrow$0, and H$_2$O maser emission around the AGB star R\,LMi, obtained from the Korean VLBI Network (KVN). The simultaneous multi-channel receivers of the KVN offer great possibilities for astrometry in the frequency domain. With this facility we have produced images with bona-fide absolute astrometric registration between high frequency maser transitions of different species to provide the positions of the \water\ maser emission, and the centre of the SiO maser emission, and hence reducing the uncertainty in the proper motion for R\,LMi by an order of magnitude over that from Hipparcos. This is the first successful demonstration of source frequency phase referencing for mm-VLBI spectral-line observations and also where the ratio between the frequencies is not an integer., Comment: Accepted in AJ

We present the results of a spectral line survey from 138.3 to 150.7 GHz toward Orion-KL. The observations were made using the 14 m radio telescope of Taeduk Radio Astronomy Observatory. Typical system temperatures were between 500 and 700 K, with the sensitivity between $0.02 - 0.06$ K in units of $\rm T_A^*$. A total of 149 line spectra are detected in this survey. Fifty lines have been previously reported, however we find 99 new detections. Among these new lines, 32 are `unidentified', while 67 are from molecular transitions with known identifications. There is no detection of H or He recombination lines. The identified spectra are from a total of 16 molecular species and their isotopic variants. In the range from 138.3 to 150.7 GHz, the strongest spectral line is the J=3-2 transition of CS molecule, followed by transitions of the $\rm H_2CO$, $\rm CH_3OH$, $\rm CH_3CN$, and $\rm SO_2$. Spectral lines from the large organic molecules such as $\rm CH_3OH$, $\rm CH_3OCH_3$, $\rm HCOOCH_3$, $\rm C_2H_5CN$ and $\rm CH_3CN$ are prominent; with 80 % of the identified lines arising from transitions of these molecules. The rotational temperatures and column densities are derived using the standard rotation diagram analysis for $\rm CH_3OH$ ($\rm ^{13}CH_3OH$), $\rm HCOOCH_3$, $\rm CH_3CN$ and $\rm SO_2$ with $\rm 10\sim 270 K$ and $\rm 0.2\sim 20\times 10^{15} cm^{-2}$. These estimates are fairly comparable to the values for the same molecule in other frequency regions by other studies., Comment: 10 figures, 2 tex files for a manuscript and tables, accepted to ApJ