Millimeter- and Submillimeter-Wave Observations of the OMC-2/3 Region; I. Dispersing and Rotating Core around an Intermediate-mass Protostar MMS 7

We report the results of H13CO+(1-0), CO(1-0), and 3.3 mm dust continuum observations toward one of the strongest mm-wave sources in OMC-3, MMS 7, with the Nobeyama Millimeter Array (NMA) and the Nobeyama 45 m telescope. With the NMA, we detected centrally-condensed 3.3 mm dust-continuum emission which coincides with the MIR source and the free-free jet. Our combined H13CO+ observations have revealed a disk-like envelope. The size and the mass of the disk-like envelope are 0.15 times 0.11 pc and 5.1 - 9.1 M_sun, respectively. The combined map also shows that the outer portion of the disk-like envelope has a fan-shaped structure which delineates the rim of the CO(1-0) outflow observed with the NMA. The position-velocity (P-V) diagrams in the H13CO+ (1-0) emission show that the velocity field in the disk-like envelope is composed of a dispersing gas motion and a possible rigid-like rotation. The mass dispersing rate is estimated to be (3.4 - 6.0) times 10^-5 M_sun/yr, which implies that MMS 7 has an ability to disperse ~10 M_sun during the protostellar evolutional time of a few times 10^5 yr. The specific angular momentum of the possible rotation in the disk-like envelope is nearly two orders of magnitude larger than that in low-mass cores. The turn-over point of the power law of the angular momentum distribution in the disk-like envelope (< 0.007 pc), which is likely to be related to the outer radius of the central mass accretion, is similar to the size of the 3.3 mm dust condensation. The intermediate-mass protostar MMS 7 is in the last stage of the main accretion phase and that the substantial portion of the outer gas has already been dispersed, while the mass accretion may still be on-going at the innermost region traced by the dusty condensation.Comment: 19 pages, 9 figures, ApJ accepted pape

Millimeter- and Submillimeter-Wave Observations of the OMC-2/3 Region. II. Observational Evidence for Outflow-Triggered Star Formation in the OMC-2 FIR 3/4 Region

We have carried out the observations of the OMC-2 FIR 3/4 region with the NMA and ASTE in the H$^{13}$CO$^{+}$ (1--0), $^{12}$CO (3--2, 1--0), SiO ($v$=0, $J$=2--1), CS (2--1), and CH$_3$OH ($J_K$=7$_K$--6$_K$) lines and in the 3.3 mm continuum emission. Our NMA observations in the H$^{13}$CO$^{+}$ emission have revealed 0.07 pc-scale dense gas associated with FIR 4. The $^{12}$CO (3--2,1--0) emission shows high-velocity blue and red shifted components at the both north-east and south-west of FIR 3, suggesting a molecular outflow nearly along the plane of the sky driven by FIR 3. The SiO and the CH$_{3}$OH emission are detected around the interface between the outflow and the dense gas. Furthermore, the $^{12}$CO (1--0) emission shows an L-shaped structure in the P-V diagram. These results imply presence of the shock due to the interaction between the molecular outflow driven by FIR 3 and the dense gas associated with FIR 4. Moreover, our high angular-resolution observations of FIR 4 in the 3.3 mm continuum emission have first found that FIR 4 consists of eleven dusty cores. The separation among these cores is on the same order of the Jeans length, suggesting that the fragmentation into these cores has been caused by the gravitational instability. The time scale of the fragmentation is similar to the time scale of the interaction between the molecular outflow and the dense gas. We suggest that the interaction between the molecular outflow from FIR 3 and the dense gas associated with FIR 4 triggered the fragmentation into these dusty cores, and hence the next generation the cluster formation.Comment: 13 pages, 9 figures. Accepted by Ap

Millimeter- and Submillimeter-Wave Observations of the OMC-2/3 Region. III. An Extensive Survey for Molecular Outflows

Using the ASTE 10 m submillimeter telescope and the 1.4 m Infrared Survey Facility (IRSF), we performed an extensive outflow survey in the Orion Molecular Cloud -2 and -3 region. Our survey, which includes 41 potential star-forming sites, has been newly compiled using multi-wavelength data based on millimeter- and submillimeter-continuum observations as well as radio continuum observations. From the CO (3-2) observations performed with the ASTE 10 m telescope, we detected 14 CO molecular outflows, seven of which were newly identified. This higher detection rate, as compared to previous CO (1-0) results in the same region, suggests that CO (3-2) may be a better outflow tracer. Physical properties of these outflows and their possible driving sources were derived. Derived parameters were compared with those of CO outflows in low- and high-mass starforming regions. We show that the CO outflow momentum correlates with the bolometric luminosity of the driving source and with the envelope mass, regardless of the mass of the driving sources. In addition to these CO outflows, seven sources having NIR features suggestive of outflows were also identified.Comment: Accepted to Astrophysical Journal, high resolution images at http://www.asiaa.sinica.edu.tw/~satoko_t/papers/ms.ST.pd

Evolutionary Status of Brightest and Youngest Source in the Orion Molecular Cloud-3 Region

The brightest continuum source in the Orion Molecular Cloud-3 region (OMC-3), MMS 6, was observed with the Very Large Array (VLA), the Nobeyama Millimeter Array (NMA), and the Submillimeter Array (SMA). Our data were supplemented by near- to mid-infrared archival data taken by Spitzer Space Telescope. The compact continuum source, MMS 6-main, was detected with an H_2 mass of 3.0 Msun with a size of 510 AU. Despite its compact and well condensed appearance, neither clear CO outflow, radio jet, nor infrared sources (at a wave-length shorter than 8 um) were detected at MMS 6-main even with the present high-spatial resolution and high-sensitivity observations. The derived H_2 column density, 2.6x10^25 cm^-2, corresponds to a visual extinction of A_v~15000 mag., and the derived number density is at least two orders of magnitude higher than for the other OMC-2/3 continuum sources. The volume density profile of the source was estimated to have a power-law index of 2 or steeper down to a radius of ~450 AU. The time scale to form a protostar at the center or the time scale elapsed after its formation is estimated to be 830 to 7600 yr. This is much shorter than the typical lifetime of the Class 0/I protostars, which is ~10^(4-5) yr, suggesting that MMS 6-main is probably in either the earliest stage of the proto-stellar core or in the latest stage of the pre-stellar phase.Comment: 34 pages, 7 figures, accepted to Ap

介護福祉士養成における在宅介護実習の位置づけ

本研究は，在宅介護実習（介護実習Ⅲ）で獲得した在宅支援の視点が，施設をフィールドとし，介護過程の展開実習となる施設介護実習（介護実習Ⅳ）において，個別ケアを実践できる利用者本位の介護への実現にどの程度効果を発揮しているかを明らかにすることを目的としたものである．医療介護福祉科2年次生で介護実習Ⅲ及び介護実習Ⅳを終了した学生を対象に質問紙調査及びインタビュー調査を行った．その結果は，①介護実習Ⅲの学びとなる利用者の在宅への想いや物理的環境への意識の高まり，すなわち利用者本位に向かうアセスメントの視点が介護実習Ⅳへとつながっていること，②利用者との良好な関係形成を築くためのコミュニケーション力が介護実習Ⅳで発揮されていることが説明できた．介護実習Ⅲは，介護実習Ⅳで個別ケアを実践できる利用者本位の介護への実現に活かされていた

<Original Paper>Simultaneous Determination of Sodium Benzoate and p-Hydroxybenzoate Esters Using High-performance Capillary Electrophoresis

A rapid and simple capillary zone electrophoresis (CZE) method was developed for the simultaneous determination of sodium benzoate, potassium sorbate, sodium dehydroacetate, and the parabens, i.e. ethyl, n-propyl, and n-butyl p-hydroxybenzoic esters, which are used in several processed foods as preservatives. The compounds were well separated from each other on a fused silica capillary utilizing a 20 mM sodium tetraborate buffer (pH 9.65) and UV detection at 200 nm. The total analysis time was less than seven minutes per sample. Furthermore, sodium benzoate and the five parabens, i.e. ethyl, isopropyl, n-propyl, isobutyl and n-butyl p-hydroxybenzoic esters, permitted as food preservatives in Japan were well separated from each other in less than eight minutes using a micellar electrokinetic capillary electrophoresis (MEKC) method. Concentrations of sodium benzoate and n-butyl paraben in several soft drinks were determined using the CZE method and the levels of sodium benzoate and n-butyl paraben in the samples were in good agreement with those determined by the HPLC procedure