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Matsumoto, Naoko,Hirota, Tomoya,Sugiyama, Koichiro,Kim, Kee-Tae,Kim, Mikyoung,Byun, Do-Young,Jung, Taehyun,Chibueze, James O.,Honma, Mareki,Kameya, Osamu,Kim, Jongsoo,Lyo, A-Ran,Motogi, Kazuhito,Oh, C IOP Publishing 2014 ASTROPHYSICAL JOURNAL LETTERS - Vol.789 No.1
<P>We have carried out the first very long baseline interferometry (VLBI) imaging of a 44 GHz class I methanol maser (70-61A(+)) associated with a millimeter core MM2 in a massive star-forming region IRAS 18151-1208 with KaVA (KVN and VERA Array), which is a newly combined array of KVN (Korean VLBI Network) and VERA (VLBI Exploration of Radio Astrometry). We have succeeded in imaging compact maser features with a synthesized beam size of 2.7 milliarcseconds x 1.5 milliarcseconds (mas). These features are detected at a limited number of baselines within the length of shorter than approximate to 650 km corresponding to 100 M. in the uv-coverage. The central velocity and the velocity width of the 44 GHz methanol maser are consistent with those of the quiescent gas rather than the outflow traced by the SiO thermal line. The minimum component size among the maser features is similar to 5 mas x 2 mas, which corresponds to the linear size of similar to 15 AU x 6 AU assuming a distance of 3 kpc. The brightness temperatures of these features range from similar to 3.5 x 10(8) to 1.0 x 10(10) K, which are higher than the estimated lower limit from a previous Very Large Array observation with the highest spatial resolution of similar to 50 mas. The 44 GHz class I methanol maser in IRAS 18151-1208 is found to be associated with the MM2 core, which is thought to be less evolved than another millimeter core MM1 associated with the 6.7 GHz class II methanol maser.</P>
Akiko Kuwabara,Naoko Tsugawa,Hiroshi Kondo,Misora Ao,Hitomi Fujiwara,Natsuki Hosokawa,Shiho Matsumoto,Kiyoshi Tanaka,Tetsuo Nakano 대한골다공증학회 2017 Osteoporosis and Sarcopenia Vol.3 No.1
Objectives: One of the important risk factors of falling is decreased muscle mass and muscle strength. Recently, there has been an increasing concern on the role of vitamin D in muscle strength and physical activity. Aim of our study is to examine the relationships between vitamin D status and muscle mass and muscle strength in middle-aged healthy adults. Methods: Subjects were 40 healthy volunteers aged 42.0 ± 10.6 years old. Evaluation was made for serum vitamin D3 metabolites including 25- hydroxyvitamin D3 [25(OH)D3] and 24,25-dihydroxyvitamin D3 [24,25(OH)2D3] concentrations, lower limb muscle strength, and dietary intake by food frequency questionnaire. Body composition was measured by dual-energy X-ray absorptiometry (DXA), and appendicular skeletal mass index (ASMI) was calculated as skeletal muscle mass/squared height. Results: 70% of the subjects had vitamin D insufficiency/deficiency (serum total 25(OH)D < 20 ng/mL), and female subjects had significantly lower serum total 25(OH)D level compared with males. Vitamin D insufficiency/deficiency group had significantly higher body fat, lower SMI and muscle strength, probably reflecting higher percentage of female subjects. Serum vitamin D3 metabolites levels were significantly correlated with whole and site-specific ASMI, and lower limb muscle strength, except for the correlation between serum 24,25(OH)2D3 concentration and lower limb muscle strength. In addition, serum 25(OH)D3 level was a positive significant predictor for both ASMI and lower limb muscle strength, while serum 24,25(OH)2D3 level was not their significant predictor. Conclusions: Serum 25(OH)D3 level was significantly correlated with both skeletal muscle mass and lower limb muscle strength.
ALMA BAND 8 CONTINUUM EMISSION FROM ORION SOURCE I
Hirota, Tomoya,Machida, Masahiro N.,Matsushita, Yuko,Motogi, Kazuhito,Matsumoto, Naoko,Kim, Mi Kyoung,Burns, Ross A.,Honma, Mareki American Astronomical Society 2016 The Astrophysical journal Vol.833 No.2
<P>We have measured continuum flux densities of a high-mass protostar candidate, a radio source. I in the Orion. KL region (Orion Source I) using the Atacama Large Millimeter/Submillimeter Array (ALMA) at band. 8 with an angular resolution of 0 ''.1. The continuum emission at 430, 460, and 490 GHz associated with Source. I shows an elongated structure along the northwest-southeast direction perpendicular to the so-called low-velocity bipolar outflow. The deconvolved size of the continuum source, 90 au x 20 au, is consistent with those reported previously at other millimeter/submillimeter wavelengths. The flux density can be well fitted to the optically thick blackbody spectral energy distribution, and the brightness temperature is evaluated to be 700-800 K. It is much lower than that in the case of proton-electron or H-free-free radiations. Our data are consistent with the latest ALMA results by Plambeck & Wright, in which the continuum emission was proposed to arise from the edge-on circumstellar disk via thermal dust emission, unless the continuum source consists of an unresolved structure with a smaller beam filling factor.</P>
THE VLBI MONITORING PROJECT FOR 6.7 GHz METHANOL MASERS USING THE JVN/EAVN
SUGIYAMA, KOICHIRO,FUJISAWA, KENTA,HACHISUKA, KAZUYA,YONEKURA, YOSHINORI,MOTOGI, KAZUHITO,SAWADA-SATOH, SATOKO,MATSUMOTO, NAOKO,SAITO, YU,HIRANO, DAIKI,HAYASHI, KYONOSUKE,SHEN, ZHIQIANG,HONMA, MAREKI The Korean Astronomical Society 2015 天文學論叢 Vol.30 No.2
We have initiated a Very Long Baseline Interferometer (VLBI) monitoring project of 36 methanol maser sources at 6.7 GHz using the Japanese VLBI Network (JVN) and East-Asian VLBI Network (EAVN), starting in August 2010. The purpose of this project is to systematically reveal 3-dimensional (3-D) kine-matics of rotating disks around forming high-mass protostars. As an initial result, we present proper mo- tion detections for two methanol maser sources showing an elliptical spatial morphology, G 002.53+00.19 and G 006.79-00.25, which could be the best candidates associated with the disk. The detected proper motions indicate a simple rotation in G 002.53+00.19 and rotation with expansion in G 006.79-00.25, respectively, on the basis of disk model fits with rotating and expanding components. The expanding motions might be caused by the magnetic-centrifugal wind on the disk.
SiO MASERS AROUND WX PSC MAPPED WITH THE KVN AND VERA ARRAY (KaVA)
Yun, Youngjoo,Cho, Se-Hyung,Imai, Hiroshi,Kim, Jaeheon,Asaki, Yoshiharu,Chibueze, James O.,Choi, Yoon Kyung,Dodson, Richard,Kim, Dong-Jin,Kusuno, Kozue,Matsumoto, Naoko,Min, Cheulhong,Oyadomari, Miyak American Astronomical Society 2016 The Astrophysical journal Vol.822 No.1
<P>We present the first images of the v = 1 and v = 2 J = 1 -> 0 SiO maser lines taken with KaVA, i.e., the combined array of the Korean Very Long Baseline Interferometry (VLBI) Network and the VLBI Exploration of Radio Astrometry ( VERA), toward the OH/IR star WX Psc. The combination of long and short antenna baselines enabled us to detect a large number of maser spots, which exhibit a typical ring-like structure in both the v. =. 1 and v = 2 J = 1 -> 0 SiO masers as those that have been found in previous VLBI observational results of WX Psc. The relative alignment of the v = 1 and v = 2 SiO maser spots are precisely derived from astrometric analysis, due. to the absolute coordinates of the reference maser spot that were well determined in an independent astrometric observation with VERA. The superposition of the v = 1 and v = 2 maser spot maps shows a good spatial correlation between the v = 1 and v = 2 SiO maser features. Nevertheless, it is also shown that the v = 2 SiO maser spot is distributed in an inner region compared to the v - 1 SiO maser by about 0.5 mas on average. These results provide good support for the recent theoretical studies of the SiO maser pumping, in which both the collisional and the radiative pumping predict the strong spatial correlation and the small spatial discrepancy between the v = 1 and v = 2 SiO maser.</P>