391 research outputs found
Posterior maxillary alveolar vertical distraction osteogenesis by bi-directional distractor
AbstractA patient with severe posterior maxillary hypoplasia was simulated using a 3-dimensional model by rapid prototyping, and segmental vertical distraction osteogenesis was planned to advance the posterior maxillary segment. The bi-directional distractor was adapted to the alveolar ridge and zygomatic buttress. After a 7-day latency period, we started distraction at a rate of 0.35mm every 12h. 12mm of advancement of the posterior maxillary segment was achieved. This distraction osteogenesis using a bi-directional distractor with proper therapeutic planning and good surgical technique will help ensure adequate vector control to predictably regenerate the hard and soft tissues during alveolar distraction
Metallicity of the Fossil Group NGC 1550 Observed with Suzaku
We studied the temperature and metal abundance distributions of the
intra-cluster medium (ICM) in a group of galaxies NGC 1550 observed with
Suzaku. The NGC 1550 is classified as a fossil group, which have few bright
member galaxies except for the central galaxy. Thus, such a type of galaxy is
important to investigate how the metals are enriched to the ICM. With the
Suzaku XIS instruments, we directly measured not only Si, S, and Fe lines but
also O and Mg lines and obtained those abundances to an outer region of ~0.5
r_180 for the first time, and confirmed that the metals in the ICM of such a
fossil group are indeed extending to a large radius. We found steeper gradients
for Mg, Si, S, and Fe abundances, while O showed almost flat abundance
distribution. Abundance ratios of alpha-elements to Fe were similar to those of
the other groups and poor clusters. We calculated the number ratio of type II
to type Ia supernovae for the ICM enrichment to be 2.9 +- 0.5 within 0.1 r_180,
and the value was consistent with those for the other groups and poor clusters
observed with Suzaku. We also calculated metal mass-to-light ratios (MLRs) for
Fe, O and Mg with B-band and K-band luminosities of the member galaxies of NGC
1550. The derived MLRs were comparable to those of NGC 5044 group in the r<0.1
r_180 region, while those of NGC 1550 are slightly higher than those of NGC
5044 in the outer region.Comment: 11 pages, 7 figures, accepted for publication in PAS
Suzaku and XMM-Newton Observations of the Fornax cluster: Temperature and Metallicity Distribution
Suzaku observed a central region and five offset regions within 0.2 r180 in
the Fornax cluster, a nearby poor cluster, and XMM-Newton mapped the cluster
with 15 pointings out to 0.3 r180. The distributions of O, Mg, Si, S, and Fe in
the intracluster medium (ICM) were studied with Suzaku, and those of Fe and
temperature were studied with XMM. The temperature of the ICM gradually
decreases with radius from 1.3 keV at 0.04 r180 to 1 keV at 0.2-0.3 r180. If
the new solar abundances of Lodders et al. (2003) and a single-temperature
plasma model are adopted, O, Mg, Si, S, and Fe show similar abundances: 0.4-0.6
solar within 0.02-0.2 r180. This Fe abundance is similar to those at 0.1-0.2
r180 in rich clusters and other groups of galaxies. At 0.2-0.3 r180, the Fe
abundance becomes 0.2-0.3 solar. A two-temperature plasma model yields ICM
abundances that are higher by a factor of 1.2-1.5, but gives similar abundance
ratios among O, Mg, Si, S, and Fe. The northern region has a lower ICM
temperature and higher brightness and Fe abundance, whereas the southern region
has a higher ICM temperature and lower brightness and Fe abundance. These
results indicate that the cD galaxy may have traveled from the north because of
recent dynamical evolution. The cumulative oxygen- and iron-mass-to-light
ratios within 0.3 r180 are more than an order of magnitude lower than those of
rich clusters and some relaxed groups of galaxies. Past dynamical evolution
might have hindered the strong concentration of hot gas in the Fornax cluster's
central region. Scatter in the IMLR and similarity in the element abundances in
the ICM of groups and clusters of galaxies indicate early metal synthesis.Comment: 15 pages, 13 figures, accepted for publication in PAS
Combining course- and program-level outcomes assessments through embedded performance assessments at key courses: A proposal based on the experience from a Japanese dental education program
This paper addresses how to combine the course- and program-level assessments and presents a new method illustrated by a case of dental education program in Japan. Performance assessments are considered effective for evaluating knowledge integration and higher-order skills, while placing a burden on faculty, hence their feasibility as the program-level assessment is regarded lower than standardized tests or questionnaire surveys. We have developed several performance assessments at the course level, such as Modified Triple Jump for the PBL course. Based on this experience, we propose Pivotal Embedded Performance Assessment (PEPA) as a method for combining assessment at the course and program levels. The method limits the range of performance assessment to key courses directly linked to program goals and placed at the critical juncture points of curriculum, while entrusting the assessment of other courses to expert judgment of individual teachers. PEPA consists of the following procedures: systematization of curriculum and selection of key courses; design and implementation of performance assessments by a faculty team; setting passing criteria with incorporating the function of formative assessment; certifying the completion of the degree program. PEPA thus enables maintaining assessment feasibility and compatibility with a credit system, while ensuring assessment validity and reliability.Received: 27 September 2018Accepted: 13 November 2018Published online: 29 November 2018</p
Detection of Excess Hard X-ray Emission from the Group of Galaxies HCG62
From the group of galaxies HCG62, we detected an excess hard X-ray emission
in energies above keV with \A SCA. The excess emission is spatially
extended up to from the group center, and somewhat enhanced toward
north. Its spectrum can be represented by either a power-law of photon index
0.8-2.7, or a Bremsstrahlung of temperature keV. In the 2-10 keV range,
the observed hard X-ray flux, erg cm
s, implies a luminosity of erg s for a
Hubble constant of 50 km s Mpc. The emission is thus too luminous
to be attributed to X-ray binaries in the memb er galaxies. We discuss possible
origin of the hard X-ray emission.Comment: 6 pages, 3 Postscript figures, uses emulateapj.sty. Accepted for
publication in the Astrophysical Journal Letter
Effectiveness of Lignin-Removal in Simultaneous Saccharification and Fermentation for Ethanol Production from Napiergrass, Rice Straw, Silvergrass, and Bamboo with Different Lignin-Contents
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