• Clinics in Shoulder and Elbow
• /
• 제21권2호
• /
• pp.59-66
• /
• 2018

Background: Massive, irreparable rotator cuff tears (RCTs) are a challenging clinical problem in young patients. In recent years, arthroscopic superior capsular reconstruction (ASCR) is a popular treatment in the massive, irreparable RCTs. However, studies reporting clinical results of ASCR are rare in the literature. Methods: Between 2013 and 2015, six patients underwent ASCR. One patient treated with dermal allograft, while five patients with autogenous fascia lata graft. Demographic data, as well as preoperative and last follow-up clinical data including pain, range of motion (ROM), strength, American Shoulder and Elbow Surgeons system, the Constant system, the University of California at Los Angeles system, the Simple Shoulder Test, and the Shoulder Pain and Disability Index system were obtained. Acromiohumeral distances and Hamada classification were measured on standard anteroposterior x-ray. Results: All patients were men, and the average age was $59.5{\pm}4.18years$ (range, 53-65 years).The minimum follow-up was 18 months with a mean follow-up was $27.33{\pm}7.58months$ (range, 18-36). All patients had postoperative improvement in pain scores and functional scores. The ROM and strength did not improve after surgery. The Hamada score progressed of radiographic stage in 2 patients. In the case of dermal allograft, there was graft failure 6 weeks after ASCR. Conclusions: Our results support the ASCR as a viable treatment for surgical salvage in massive, irreparable RCTs. This treatment option may provide patients with decreased pain and increased function. And studying our case of dermal allograft failure provides opportunities to decrease graft failure in ASCR using dermal allograft.

• Imaging Science in Dentistry
• /
• 제44권2호
• /
• pp.89-94
• /
• 2014

Purpose: Vertical root fracture (VRF) is a common complication in endodontically treated teeth. Considering the poor prognosis of VRF, a reliable and valid detection method is necessary. Cone beam computed tomography (CBCT) has been reported to be a reliable tool for the detection of VRF; however, the presence of metallic intracanal posts can decrease the diagnostic values of CBCT systems. This study evaluated and compared the effects of intracanal stainless steel or titanium posts on the sensitivity, specificity, and accuracy of VRF detection using a NewTom VG CBCT system. Materials and Methods: Eighty extracted single-rooted teeth were selected and sectioned at the cemento-enamel junction. The roots were divided into two groups of 40. Root fracture was induced in the test group by using an Instron machine, while the control group was kept intact. Roots were randomly embedded in acrylic blocks and radiographed with the NewTom VG, both with titanium and stainless steel posts and also without posts. Sensitivity, specificity, and accuracy values were calculated as compared to the gold standard. Results: The sensitivity, specificity, and accuracy of VRF diagnosis were significantly lower in teeth with stainless steel and titanium posts than in those without posts. Interobserver agreement was the highest in teeth without posts, followed by stainless steel posts, and then titanium posts. Conclusion: Intracanal posts significantly decreased the VRF diagnostic values of CBCT. The stainless steel posts decreased the diagnostic values more than the titanium posts.

• 천문학회보
• /
• 제42권1호
• /
• pp.45.1-45.1
• /
• 2017

Optical variability is one way to probe the nature of the central engine of AGN at smaller linear scales, and previous studies have shown that optical variability of AGN is more prevalent at longer timescales and at shorter wavelengths. To understand the properties and physical mechanism of variability, we are performing the KMTNet Active Nuclei Variability Survey (KANVaS). Especially, we investigated intra-night variability of AGN with KMTNet data which observed COSMOS field during 3 separate nights from 2015 to 2016 in B, V, R, and I bands. Each night was composed of 5, 9, and 11 epochs with 20-30 min cadence. To find AGN in the COSMOS field, we applied multi-wavelength selection methods. Using X-ray, mid-infrared, and radio selection methods, 50-60, 130-220, 20-40 number of AGN are detected, respectively. Achieving photometric uncertainty ~0.01mag by differential photometry, we employed a standard time-series analysis tool to identify variable AGN, chi-square test. Preliminary results indicate that there is no evidence of intra-night optical variability of AGN. It is possible that previous studies discovered intra-night variability used inappropriate photometric error. However, main reason seems that our targets have fainter magnitude (higher photometric error) than that of previous studies. To discover variability of AGN, we will investigate longer timescale variability of AGN.

• 한국토양비료학회지
• /
• 제33권2호
• /
• pp.127-138
• /
• 2000

일반 밭, 논, 과수원 및 비닐하우스 토양 78점을 채취하여 3반복으로 농촌진흥청 표준분석법과 Soiltek$^{(R)}$ KA-P 분광광도계법으로 유기물, 치환성 K, Ca 및 Mg, CEC, 유효규산 및 질산염 함량을 측정하였다. Soiltek$^{(R)}$ KA-P 분광광도계로 측정한 유기물, 치환성 Ca, 및 Mg 용액의 발색 안정도는 1시간 동안 약 2%정도 낮아졌으며, 치환성 K, CEC및 질산염은 거의 변화가 없었다. Soiltek$^{(R)}$ KA-P 분광광도계로 측정한 분석 절대값은 농촌진흥청 표준분석법으로 측정한 값과 거의 1:1의 관계를 갖고 있었으며, 결정계수($R^2$)는 0.9501 이상이었다. 두 방법으로 측정한 유기물, 치환성 K, Ca 및 Mg, CEC, 유효규산 및 질산염의 표준편차는 각각 ${\pm}1.8gkg^{-1}$, ${\pm}0.05cmol^+kg^{-1}$, ${\pm}0.18cmol^+kg^{-1}$ 및 ${\pm}0.13cmol^+kg^{-1}$, ${\pm}1.0cmol^+kg^{-1}$, ${\pm}5.0mgkg^{-1}$ 및 ${\pm}10.0mgkg^{-1}$ 이하였다. 모든 성분에 대한 분석값은 95% 신뢰수준을 만족시켰으며, 변이계수는 7~17% 이하였다. 따라서, 기기조작의 간편성 저가 기기의 사용, 정확도, 정밀도 등을 고려한다면 Soiltek$^{(R)}$ KA-P 분광광도계에서 제시하는 방법으로 측정하는 것도 유용한 방법이라고 생각된다.

• 지질공학
• /
• 제17권1호
• /
• pp.125-133
• /
• 2007

본 연구에서는 난지도 매립지내 하수슬러지만으로 이루어진 8호 매립장에 대하여 환경 및 지반공학적 특성을 조사한다. 이를 위하여 대상현장에 대하여 시료를 채취하고, 용출시험, 중금속 총량시험 등을 실시하여 환경적인 특성을 조사하였다. 중금속 총량시험결과 Pb, Zn, Cu, Ni, Cd, Cr 등의 성분이 검출되었으며, Cu의 경우 캘리포니아주 규제기준을 초과하므로 하수슬러지 재활용시 함량을 낮추어야 할 것이다 한편, 하수슬러지의 비중, 입도분석, 액소성한계, 다짐, 투수, 전단시험을 실시하여 지반공학적 특성을 조사하였다. 하수슬러지는 모래, 실트 및 점토로 구성되어 있으며, 소성지수는 42.3%로서 압축성이 큰 무기질 실트 혹은 유기질 점토인 것으로 분류된다. 다짐시험결과 건조단위중량이 낮고 다짐곡선이 비교적 평탄한 형태를 보이고 있으므로 함수비 변화에 따른 다짐효과가 비교적 적을 것으로 예상된다. 그리고 직접전단시험결과 점착력은 $0.058kg/cm^2$이고, 내부마찰각은 $14^{\circ}$ 것으로 나타났다. 대상현장의 하수슬러지는 다짐이 잘 되지 않으며, 전단강도도 비교적 낮으므로 매립지의 복토층 등으로 재활용할 경우 여러 가지 문제가 발생될 것으로 예상된다. 그리고 하수슬러지에 포함되어 있는 중금속의 용출에 따른 지하수 오염문제도 예상된다. 따라서 대상현장의 하수슬러지를 재활용하기 위해서는 이에 대한 보완 및 처리방안이 마련되어야 할 것이다.

• 천문학회지
• /
• 제29권spc1호
• /
• pp.63-64
• /
• 1996

The nature of distant faint blue field galaxies remains a mystery, despite the fact that much attention has been devoted to this subject in the last decade. Galaxy counts, particularly those in the optical and near ultraviolet bandpasses, have been demonstrated to be well in excess of those expected in the 'no-evolution' scenario. This has usually been taken to imply that galaxies were brighter in the past, presumably due to a higher rate of star formation. More recently, redshift surveys of galaxies as faint as B$\~$24 have shown that the mean redshift of faint blue galaxies is lower than that predicted by standard evolutionary models (de-signed to fit the galaxy counts). The galaxy number count data and redshift data suggest that evolutionary effects are most prominent at the faint end of the galaxy luminosity function. While these data constrain the form of evolution of the overall luminosity function, they do not constrain evolution in individual galaxies. We are carrying out a series of observations as part of a long-term program aimed at a better understanding of the nature and amount of luminosity evolution in individual galaxies. Our study uses the luminosity-linewidth relation (Tully-Fisher relation) for disk galaxies as a tool to study luminosity evolution. Several studies of a related nature are being carried out by other groups. A specific experiment to test a 'no-evolution' hypothesis is presented here. We have used the AUTOFIB multifibre spectro-graph on the 4-metre Anglo-Australian Telescope (AAT) and the Rutgers Fabry-Perot imager on the Cerro Tolalo lnteramerican Observatory (CTIO) 4-metre tele-scope to measure the internal kinematics of a representative sample of faint blue field galaxies in the red-shift range z = 0.15-0.4. The emission line profiles of [OII] and [OIII] in a typical sample galaxy are significantly broader than the instrumental resolution (100-120 km $s^{-l}$), and it is possible to make a reliable de-termination of the linewidth. Detailed and realistic simulations based on the properties of nearby, low-luminosity spirals are used to convert the measured linewidth into an estimate of the characteristic rotation speed, making statistical corrections for the effects of inclination, non-uniform distribution of ionized gas, rotation curve shape, finite fibre aperture, etc.. The (corrected) mean characteristic rotation speed for our distant galaxy sample is compared to the mean rotation speed of local galaxies of comparable blue luminosity and colour. The typical galaxy in our distant sample has a B-band luminosity of about 0.25 L$\ast$ and a colour that corresponds to the Sb-Sd/Im range of Hub-ble types. Details of the AUTOFIB fibre spectroscopic study are described by Rix et al. (1996). Follow-up deep near infrared imaging with the 10-metre Keck tele-scope+ NIRC combination and high angular resolution imaging with the Hubble Space Telescope's WFPC2 are being used to determine the structural and orientation parameters of galaxies on an individual basis. This information is being combined with the spatially resolved CTIO Fabry-Perot data to study the internal kinematics of distant galaxies (Ing et al. 1996). The two main questions addressed by these (preliminary studies) are: 1. Do galaxies of a given luminosity and colour have the same characteristic rotation speed in the distant and local Universe? The distant galaxies in our AUTOFIB sample have a mean characteristic rotation speed of $\~$70 km $s^{-l}$ after correction for measurement bias (Fig. 1); this is inconsistent with the characteristic rotation speed of local galaxies of comparable photometric proper-ties (105 km $s^{-l}$) at the > $99\%$ significance level (Fig. 2). A straightforward explanation for this discrepancy is that faint blue galaxies were about 1-1.5 mag brighter (in the B band) at z $\~$ 0.25 than their present-day counterparts. 2. What is the nature of the internal kinematics of faint field galaxies? The linewidths of these faint galaxies appear to be dominated by the global disk rotation. The larger galaxies in our sample are about 2"-.5" in diameter so one can get direct insight into the nature of their internal velocity field from the $\~$ I" seeing CTIO Fabry-Perot data. A montage of Fabry-Perot data is shown in Fig. 3. The linewidths are too large (by. $5\sigma$) to be caused by turbulence in giant HII regions.