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We constructed a far ultraviolet (FUV) all sky map based on observations from the Far Ultraviolet Imaging Spectrograph (FIMS) aboard the Korean microsatellite STSAT-1. For the ~20% of the sky not covered by FIMS observations, predictions from a deep artificial neural network were used. Seven datasets were chosen for input parameters, including five all sky maps of H-alpha, E(B-V), N(HI), and two X-ray bands, with Galactic longitudes and latitudes. 70% of the pixels of the observed FIMS dataset were randomly selected for training as target parameters and the remaining 30% were used for validation. A simple four-layer neural network architecture, which consisted of three convolution layers and a dense layer at the end, was adopted, with an individual activation function for each convolution layer; each convolution layer was followed by a dropout layer. The predicted FUV intensities exhibited good agreement with Galaxy Evolution Explorer (GALEX) observations made in a similar FUV wavelength band for high Galactic latitudes. As a sample application of the constructed map, a dust scattering simulation was conducted with model optical parameters and a Galactic dust model for a region that included observed and predicted pixels. Overall, FUV intensities in the observed and predicted regions were reproduced well., Comment: 10 pages, 12 figures

We study the galaxy merger fraction and its dependence on star formation mode in the5.4 square degrees of the North Ecliptic Pole-Wide field. We select 6352 galaxies withAKARI 9{\mu}m detections, and identify mergers among them using the Gini coefficientand M20derived from the Subaru/HSC optical images. We obtain the total infraredluminosity and star formation rate of galaxies using the spectral energy distributiontemplates based on one band, AKARI 9{\mu}m. We classify galaxies into three differentstar formation modes (i.e. starbursts, main sequence, and quiescent galaxies) andcalculate the merger fractions for each. We find that the merger fractions of galaxiesincrease with redshift atz, Comment: 13 pages, 11 figures, Accepted for publication by MNRAS

We present all-sky maps of two major FUV cooling lines, C IV and O VI, of highly ionized gas to investigate the nature of the transition-temperature gas. From the extinction-corrected line intensities of C IV and O VI, we calculated the gas temperature and the emission measure of the transition-temperature gas assuming isothermal plasma in the collisional ionization equilibrium. The gas temperature was found to be more or less uniform throughout the Galaxy with a value of (1.89 $\pm$ 0.06) $\times$ $10^5$ K. The emission measure of the transition-temperature gas is described well by a disk-like model in which the scale height of the electron density is $z_0=6_{-2}^{+3}$ kpc. The total mass of the transition-temperature gas is estimated to be approximately $6.4_{-2.8}^{+5.2}\times10^9 M_{\bigodot}$. We also calculated the volume-filling fraction of the transition-temperature gas, which was estimated to be $f=0.26\pm0.09$, and varies from $f\sim0.37$ in the inner Galaxy to $f\sim0.18$ in the outer Galaxy. The spatial distribution of C IV and O VI cannot be explained by a simple supernova remnant model or a three-phase model. The combined effects of supernova remnants and turbulent mixing layers can explain the intensity ratio of C IV and O VI. Thermal conduction front models and high-velocity cloud models are also consistent with our observation., Comment: 20 pages, 16 figures, Accepted to the Astrophysical Journal Supplement Series

We compare vertical profiles of the extraplanar H$\alpha$ emission to those of the UV emission for 38 nearby edge-on late-type galaxies. It is found that detection of the "diffuse" extraplanar dust (eDust), traced by the vertically extended, scattered UV starlight, always coincides with the presence of the extraplanar H$\alpha$ emission. A strong correlation between the scale heights of the extraplanar H$\alpha$ and UV emissions is also found; the scale height at H$\alpha$ is found to be $\sim0.74$ of the scale height at FUV. Our results may indicate the multiphase nature of the diffuse ionized gas and dust in the galactic halos. The existence of eDust in galaxies where the extraplanar H$\alpha$ emission is detected suggests that a larger portion of the extraplanar H$\alpha$ emission than that predicted in previous studies may be caused by H$\alpha$ photons that originate from H II regions in the galactic plane and are subsequently scattered by the eDust. This possibility raise a in studying the eDIG. We also find that the scale heights of the extraplanar emissions normalized to the galaxy size correlate well with the star formation rate surface density of the galaxies. The properties of eDust in our galaxies is on a continuation line of that found through previous observations of the extraplanar polycyclic aromatic hydrocarbons emission in more active galaxies known to have galactic winds., Comment: 25 pages; 6 figures; It was accepted for publication in The Astrophysical Journal at June 7, 2018

To investigate the inhibitory effect of acteoside on the process of exocytosis induced by melittin, we measured Ca(2+) mobilization, arachidonic acid (AA) release and catecholamine exocytosis in PC12 chromaffin cells. Melittin significantly increased the intracellular Ca(2+) mobilization via receptor-operated calcium channel but not the intracellular Ca(2+) release. It caused AA release via activation of Ca(2+)-dependent phospholipase A2 (PLA2) and catecholamine secretion in a dose-dependent manner. Acteoside dose-dependently inhibited the release of AA and intracellular Ca(2+) mobilization induced by melittin. Acteoside reduced the catecholamine release and raised the amount of intracellular chromogranin A which is co-released with catecholamine from melittin-stimulated PC12 cells. Taken together, our results suggest that acteoside could suppress the exocytosis via inhibition of Ca(2+)-dependent PLA2 and extracellular Ca(2+) influx in PC12 cells stimulated by melittin.

To investigate the underlying mechanisms of C18 fatty acids (stearic acid, oleic acid, linoleic acid and α-linolenic acid) on mast cells, we measured the effect of C18 fatty acids on intracellular Ca(2+) mobilization and histamine release in RBL-2H3 mast cells. Stearic acid rapidly increased initial peak of intracellular Ca(2+) mobilization, whereas linoleic acid and α-linolenic acid gradually increased this mobilization. In the absence of extracellular Ca(2+), stearic acid (100 µM) did not cause any increase of intracellular Ca(2+) mobilization. Both linoleic acid and α-linolenic acid increased intracellular Ca(2+) mobilization, but the increase was smaller than that in the presence of extracellular Ca(2+). These results suggest that C18 fatty acid-induced intracellular Ca(2+) mobilization is mainly dependent on extracellular Ca(2+) influx. Verapamil dose-dependently inhibited stearic acid-induced intracellular Ca(2+) mobilization, but did not affect both linoleic acid and α-linolenic acid-induced intracellular Ca(2+) mobilization. These data suggest that the underlying mechanism of stearic acid, linoleic acid and α-linolenic acid on intracellular Ca(2+) mobilization may differ. Linoleic acid and α-linolenic acid significantly increased histamine release. Linoleic acid (C18:2: ω-6)-induced intracellular Ca(2+) mobilization and histamine release were more prominent than α-linolenic acid (C18:3: ω-3). These data support the view that the intake of more α-linolenic acid than linoleic acid is useful in preventing inflammation.

This study was performed to investigate the effects of acteoside on various cellular functions such as, intracellular Ca(2+) mobilization, phospholipase C activity, and exocytosis induced by melittin. Melittin (0.1-1 μM) dose-dependently increased intracellular Ca(2+) mobilization in the presence of extracellular Ca(2+), but was not affected by 1 μM U73122, a specific PLC inhibitor. In the absence of extracellular Ca(2+), melittin (1 μM) did not induce a change in intracellular Ca(2+) mobilization, which suggests that melittin-induced intracellular Ca(2+) mobilization may be dependent on the influx of extracellular Ca(2+) rather than on the release of intracellular Ca(2+) storage. Acteoside (10 μM) significantly inhibited 1 μM melittin-induced Ca(2+) mobilization by 33 %. In [(3)H]inositol-labeled cells, 1 μM melittin did not increase inositol phosphate formation, but more than 5 μM melittin significantly increased inositol phosphate formation, which was significantly inhibited by acteoside. Melittin (1 μM) significantly increased histamine release from RBL 2H3 cells in the presence or absence of extracellular Ca(2+). Acteoside significantly inhibited 1-μM-melittin-induced histamine release by 74 % in the presence of extracellular Ca(2+) and by 71 % in the absence of extracellular Ca(2+). These data suggest that the inhibitory effect of acteoside on 1 μM-melittin-induced histamine release may be related to blockage of the calcium-independent pathway. Taken together, these data suggest that melittin has an influence on cellular functions such as intracellular Ca(2+) mobilization, the PLC pathway, and exocytosis via various independent signalling pathways in RBL-2H3 cells, and was significantly inhibited by acteoside.

Given operators X and Y acting on a Hilbert space , an interpolating operator is a bounded operator A such that AX = Y. In this article, the following is proved: Let be a subspace lattice on and let X and Y be operators acting on a Hilbert space H. Let P be the projection onto the . If PE = EP for each E , then the following are equivalent: (1) sup , and there is a bounded operator T acting on such that =, = for all f and gin and = 0 for h . (2) There is a normal operator A in AlgL such that AX = Y and Ag = 0 for all g in range .

Given operators X and Y acting on a Hilbert space , an interpolating operator is a bounded operator A such that AX = Y. In this article, we showed the following : Let be a subspace lattice acting on a Hilbert space and let X and Y be operators in . Let P be the projection onto . If FE = EF for every , then the following are equivalent: (1) , , and = for any f and g in . (2) There exists a self-adjoint operator A in Alg such that AX = Y.

Let L be a subspace lattice on a Hilbert space H and X and Y be operators acting on a Hilbert space H. Let P be the projection onto , where RX is the range of X. If PE = EP for each , then there exists an operator A in AlgL such that AX = Y if and only if $$sup\{{\parallel}E^{\bot}Yf{\parallel}/{\parallel}E^{\bot}Xf{\parallel}\;:\;f{\in}H,\; E{\in}L}=K\; Let x and y be vectors in H and let be the projection onto the singlely generated space by x. If for each , then the assertion that there exists an operator A in AlgL such that Ax = y is equivalent to the condition $$K_0\;:\;=\;sup\{{\parallel}E^{\bot}y{\parallel}/{\parallel}E^{\bot}x\;:\;E{\in}L}= whose norm is under this case.

We discuss a certain geometric property X of dual algebras generated by a polynomially bounded operator and property (, , =) these are central to the study of -systems of simultaneous equations of weak-continuous linear functionals on a dual algebra. In particular, we prove that if T satisfies a certain sequential property, then T (H) if and only if the algebra A has property X, which is an improvement of Li-Pearcy theorem in [8].

Let X and Y be operators acting on a Hilbert space and let (equation omitted) be a subspace lattice of orthogonal projections on the space containing 0 and I. We investigate normal interpolation problems in Alg(equation omitted): Given operators X and Y acting on a Hilbert space, when does there exist a normal operator A in Alg(equation omitted) such that AX

In this article, we investigate invertible interpolation problems in Alg(equation omitted) : Let(equation omitted) be a subspace lattice on a Hilbert space H and let X and Y be operators acting on H. When does there exist an invertible operator A in Alg(equation omitted) such that AX = Y?

In this paper we obtained the following : Let H be a Hilbert space and L be a subspace lattice on H. Let X and Y be operators acting on H. If the range of X is dense in H, then the following are equivalent: (1) there exists an operator A in AlgL such that AX = Y , (2) sup ‰ kE ? Y fk kE ? Xfk : f 2 H; E 2 L ae = K < 1: Moreover, if condition (2) holds, we may choose the operator A such that kAk = K.

Given vectors x and y in a Hilbert space, an inter- polating operator is a bounded operator T such that Tx = y. An interpolating operator for n vectors satisfies the equation Txi = yi, for i = 1;2;¢¢¢ ;n. In this article, we investigate compact interpo- lation problems in tridiagonal algebra : Given vectors x and y in a Hilbert space, when is there a compact operator A in a tridiagonal algebra such that Ax = y ?

Given vectors x and y in a Hilbert space, an interpo- lating operator is a bounded operator T such that Tx = y. An interpolating operator for n-vectors satisfies the equation Axi = yi for i = 1;2;¢¢¢ ;n. In this article, we investigate unitary interpo- lation problems in CSL-Algebra AlgL : Let L be a commutative subspace lattice on a Hilbert space H. Let x and y be vectors in H. When does there exist a unitary operator A in AlgL such that Ax = y ?

In this paper, we present a catalogue of the spectra of bright stars observed during the sky survey using the Far-Ultraviolet Imaging Spectrograph (FIMS), which was designed primarily to observe diffuse emissions. By carefully eliminating the contamination from the diffuse background, we obtain the spectra of 70 bright stars observed for the first time with a spectral resolution of 2--3 {\AA} over the wavelength of 1370--1710 {\AA}. The far-ultraviolet spectra of an additional 139 stars are also extracted with a better spectral resolution and/or higher reliability than those of the previous observations. The stellar spectral type of the stars presented in the catalogue spans from O9 to A3. The method of spectral extraction of the bright stars is validated by comparing the spectra of 323 stars with those of the International Ultraviolet Explorer (IUE) observations., Comment: 15 pages, 12 figure, 2 tables accepted 2015 November 11 in MNRAS

Given operators X and Y acting on a Hilbert space H, an interpolating operator is a bounded operator A such that AX = Y. An interpolating operator for n-operators satisfies the equation = for i/ = 1,2,…, n. In this article, we obtained the following : Let X ＝ ( and Y ＝ ( be operators in B(H) such that for all i. Then the following statements are equivalent. (1) There exists an operator A in Alg L such that AX = Y, every E in L reduces A and A is a self-adjoint operator. (2) sup and is real for all i = 1,2, ....

Given operators X and Y acting on a Hilbert space H, an interpolating operator is a bounded operator A such that AX = Y. An interpolating operator for the n-operators satisfies the equation AXi/ : Yi/, for i = 1, 2 …, n. In this article, we obtained the following : Let X = (xij/) and Y = (yij/) be operators acting on H such that i (i)/ 0 for all i. Then the following statements are equivalent. (1) There exists a unitary operator A in Alg(equation omitted) such that AX = Y and every E in (equation omitted) reduces A. (2) sup{(equation omitted)} and (equation omitted) = 1 for all i = 1, 2, ….

Given vectors x and y in a Hilbert space, an inter- polating operator is a bounded operator T such that Tx = y. An interpolating operator for n vectors satisfies the equation Txi = yi, for i = 1;2;¢¢¢ ;n. In this article, we obtained the following : Let x = (xi) and y = (yi) be two vectors in H such that xi 6 0 for all i = 1;2;¢¢¢. Then the following statements are equivalent. (1) There exists an operator A in AlgL such that Ax = y, A is a trace-class operator and every E in L reduces A. (2) sup ( k P l=1 fikEkyk k P l=1 fikEkxk : l 2 N;fik 2C and Ek 2 L ) < 1

We present the far-ultraviolet (FUV) fluorescent molecular hydrogen (H_2) emission map of the Milky Way Galaxy obtained with FIMS/SPEAR covering ~76% of the sky. The extinction-corrected intensity of the fluorescent H_2 emission has a strong linear correlation with the well-known tracers of the cold interstellar medium (ISM), including color excess E(B-V), neutral hydrogen column density N(H I), and H_alpha emission. The all-sky H_2 column density map was also obtained using a simple photodissociation region model and interstellar radiation fields derived from UV star catalogs. We estimated the fraction of H2 (f_H2) and the gas-to-dust ratio (GDR) of the diffuse ISM. The f_H2 gradually increases from, 24 pages, 15 figures, This is accepted for publication in ApJS at July 16, 2017

Spatially resolved laser-induced breakdown spectrometry (LIBS) was investigated to evaluate the feasibility as a quick and simple method to analyze trace elemental concentrations in starch-based flour samples. A Nd∶YAG laser beam (λ = 1064 nm, 30 mJ pulse−1) has been used for generation of laser-induced plasma on sample surface under reduced pressure of argon atmosphere. A series of starch powder samples containing different concentrations of Sr, Mg, Al, Cu, Cr, K, Mn, Rb, Cd, and Pb were used to construct the calibration curves and estimate detection limits of measurements. The calibration graphs for all elements show good linearity (correlation coefficient, r > 0.99) in the range 0–160 µg g−1 or within three orders of magnitude. Detection limits achieved were below 18 µg g−1 for all elements studied in this work. The lowest detection limit (0.3 µg g−1) was obtained from Sr measurement. Precision (%RSD) for the selected analysis was in the range 2–10%. The standard addition method was applied to assess the accuracy of LIBS using a NIES standard rice sample. The concentrations of Mg and Mn in NIES standard rice sample determined by spatially resolved LIBS technique have good agreements with those of certified value within an error range. The results indicate that spatially resolved LIBS has been shown to be an accurate technique for determining trace elements of ppm (µg g−1) level in starch-based food samples directly with an acceptable precision without any tedious digestion and dilution procedure.

We report the analysis results of far ultraviolet (FUV) observations, made for a broad region around $\alpha$ Vir (Spica) including the interaction zone of Loop I and the Local Bubble. The whole region was optically thin and a general correlation was seen between the FUV continuum intensity and the dust extinction, except in the neighborhood of the bright central star, indicating the dust scattering nature of the FUV continuum. We performed Monte-Carlo radiative transfer simulations to obtain the optical parameters related to the dust scattering as well as the geometrical structure of the region. The albedo and asymmetry factor were found to be 0.38$\pm$0.06 and 0.46$\pm$0.06, respectively, in good agreement with the Milky Way dust grain models. The distance to and the thickness of the interaction zone were estimated to be 70$^{+4}_{-8}$ pc and 40$^{+8}_{-10}$ pc, respectively. The diffuse FUV continuum in the northern region above Spica was mostly the result of scattering of the starlight from Spica, while that in the southern region was mainly due to the background stars. The \ion{C}{4} $\lambda\lambda$1548, 1551 emission was found throughout the whole region, in contrast to the \ion{Si}{2}* $\lambda$1532 emission which was bright only within the \ion{H}{2} region. This indicates that the \ion{C}{4} line arises mostly at the shell boundaries of the bubbles, with a larger portion likely from the Loop I than from the Local Bubble side, whereas the \ion{Si}{2}* line is from the photoionized Spica nebula., Comment: total 8pages,8 figures

We present the results of dust scattering simulations carried out for the Orion Eridanus Superbubble region by comparing them with observations made in the far-ultraviolet. The albedo and the phase function asymmetry factor (g-factor) of interstellar grains were estimated, as were the distance and thickness of the dust layers. The results are as follows: 0.43$^{+0.02}_{-0.04}$ for the albedo and 0.45$^{+0.2}_{-0.2}$ for the g-factor, in good agreement with previous determinations and theoretical predictions. The distance of the assumed single dust layer, modeled for the Orion Molecular Cloud Complex, was estimated to be ~110 pc and the thickness ranged from ~130 at the core to ~50 pc at the boundary for the region of the present interest, implying that the dust cloud is located in front of the superbubble. The simulation result also indicates that a thin (~10 pc) dust shell surrounds the inner X-ray cavities of hot gas at a distance of ~70-90 pc., 7 pages, 5 figures, 1 table

In this paper we will investigate the isomorphisms of A2n(n) which is defined in the introduction.

We have analyzed the archival data of FUV observations for the region of GSH 006-15+7, a large shell-like structure discovered by Moss et al. (2012) from the Hi velocity maps. FUV emission is seen to be enhanced in the lower supershell region. The FUV emission is considered to come mainly from the scattering of interstellar photons by dust grains. A corresponding Monte Carlo simulation indicates that the distance to the supershell is 1300 ± 800 pc, which is similar to the previous estimation of 1500 ± 500 pc based on kinematic considerations. The spectrum at lower Galactic latitudes of the supershell exhibits molecular hydrogen fluorescence lines; a simulation model for this candidate photodissociation region (PDR) yields an H2 column density of N(H2) = 10 18.0−20.0 cm −2 with a rather high total hydrogen density of nH � 30 cm −3 . Subject headings: ISM: supershell — ISM: dust, extinction — ISM: individual (GSH 006-15+7) — ISM: structure — ultraviolet: ISM

The dust cloud around ? Orionis is observed to be circularly symmetric with a large angular extent (?8?). However, whether the three-dimensional (3D) structure of the cloud is shell- or ring-like has not yet been fully resolved. We study the 3D structure using a new approach that combines a 3D Monte Carlo radiative transfer model for ultraviolet (UV) scattered light and an inverse Abel transform, which gives a detailed 3D radial density profile from a two-dimensional column density map of a spherically symmetric cloud. By comparing the radiative transfer models for a spherical shell cloud and that for a ring cloud, we find that only the shell model can reproduce the radial profile of the scattered UV light, observed using the S2/68 UV observation, suggesting a dust shell structure. However, the inverse Abel transform applied to the column density data from the Pan-STARRS1 dust reddening map results in negative values at a certain radius range of the density profile, indicating the existence of additional, non-spherical clouds near the nebular boundary. The additional cloud component is assumed to be of toroidal ring shape; we subtracted from the column density to obtain a positive, radial density profile using the inverse Abel transform. The resulting density structure, composed of a toroidal ring and a spherical shell, is also found to give a good fit to the UV scattered light profile. We therefore conclude that the cloud around ? Ori is composed of both ring and shell structures.

Given vectors x and y in a Hilbert space, an interpolating operator is a bounded operator T such that Tx = y. In this paper we obtained a necessary and sufficient condition for the existence of a solution A which is in CSL-algebra AlgL.

We investigated the antihypertensive effect of lutein on N(G) -nitro-L-arginine methyl ester hydrochloride (L-NAME)-induced hypertensive rats. Daily oral administration of L-NAME (40 mg/kg)-induced a rapid progressive increase in mean arterial pressure (MAP). L-NAME significantly increased MAP from the first week compared to that in the control and reached 193.3±9.6 mmHg at the end of treatment. MAP in the lutein groups was dose-dependently lower than that in the L-NAME group. Similar results were observed for systolic and diastolic blood pressure of L-NAME-induced hypertensive rats. The control group showed little change in heart rate for 3 weeks, whereas L-NAME significantly reduced heart rate from 434±26 to 376±33 beats/min. Lutein (2 mg/kg) significantly prevented the reduced heart rate induced by L-NAME. L-NAME caused hypertrophy of heart and kidney, and increased plasma lipid peroxidation four-fold but significantly reduced plasma nitrite and glutathione concentrations, which were significantly prevented by lutein in a dose-dependent manner. These findings suggest that lutein affords significant antihypertensive and antioxidant effects against L-NAME-induced hypertension in rats.

Let $A_{2n}^{(m)}$ be a generalization of a tridiagonal algebra which is defined in the introduction. In this paper it is proved that if $\varphi;A_{2n}^{(m)}\rightarrow A_{2n}^{(m)}$ is a surjective isometry, then there exists a unitary operator $U$ such that $\varphi(A)=U^{*}AU$ for all $A$ in $A_{2n}^{(m)}$ or a unitary operator $W$ such that $\varphi(A)=W^{l}AW^{*}$ for all $A$ in $A_{2n}^{(m)}$, where ${}^{t}A$ is the transpose matrix of $A$.

The far-ultraviolet (FUV) continuum and spectral images of C IV and H{sub 2} emission lines for the region of the Orion-Eridanus Superbubble are hereby presented and compared with maps obtained in other wavelengths. While the region shows complex structures, consisting of hot gases and cold dust, a close examination reveals that the FUV emission in this region can be understood reasonably as the result of their interactions. We confirm the origin of most diffuse FUV continuum to be starlight scattered by dust, but we also find that ionized gas contributes 50%-70% of the total FUV intensity in the regions of H{alpha} arcs. We note the bright diffuse FUV continuum in the eastern part of the northern region, which has a lot of dust, and attribute it to a greater abundance of bright, early-type stars in this region than in the west, as the amount of dust itself does not seem to be much different across 'arc A', which separates the two regions. In addition, two P Cygni-type stars are identified in this eastern region and their peculiar spectral profiles around the C IV emission line are manifested in the scattered diffuse spectrum. Besides this, the C IV emission is generallymore » enhanced at the boundaries of the hot X-ray cavities where thin dust regions are located, confirming the thermal interface nature of the origin of this cooling emission line. The morphology of the H{sub 2} emission shows a general correlation with dust extinction features but its intensity peaks are located in thin dust areas, rather than the peak dust regions. Furthermore, H{sub 2} emission is weak in the arc A region even though the arc passes through the center of the dust-rich area. Hence, the H{sub 2} emission and dust features, together with those of X-ray and ion line emissions, show the stratified structure of arc A quite well, again confirming its thermal interface nature.« less