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Eden McCaffrey,Samuel Chang,Geraldine Farrelly,Abdul Rahman,Blair Ritchie,Roxanne Goldade,David Cawthorpe 대한신경정신의학회 2021 PSYCHIATRY INVESTIGATION Vol.18 No.7
Objective This paper presents a review of the current state of child and adolescent mental health literacy and provides current evidence of the economic impact of a pediatric mental health literacy (MHL) training program. Methods Employing a case-series-comparison design, physician referrals to urgent and specialized mental health services were linked with patient-specific information comparing referrals from MHL participants and non-participating physicians. The economic impact analysis was based on changes in the admitted referral frequency and lengths of stay for the MHL group, compared to themselves pretraining, and over the same time period compared to non-participating physicians. Results Average scheduled ambulatory admission rates per physician remained constant for trained and untrained pre-post groups. Average scheduled ambulatory admission wait time and length of stay reduced significantly post-training for MHL-trained physicians compared to pre-training and untrained physicians. In addition to reductions in length of stay, the total bed costs saving for emergency/inpatients admission deferrals was $2,932,112 or about $20,000 per MHL-trained physician. Conclusion The estimated economic impact of the MHL training shows a substantial return on investment and supports wider implementation. The MHL training program should be a key feature of mental health reform strategies, as well as continuing and undergraduate medical education.
Accuracy of combination rules and individual effect correlation: MDOF vs SDOF systems
Alfredo Reyes-Salazar,Federico Valenzuela-Beltran,David de Leon-Escobedo,Eden Bojorquez,Arturo López-Barraza 국제구조공학회 2012 Steel and Composite Structures, An International J Vol.12 No.4
The accuracy of the 30% and SRSS rules, commonly used to estimate the combined response of structures, and some related issues, are studied. For complex systems and earthquake loading, the principal components give the maximum seismic response. Both rules underestimate the axial load by about 10% and the COV of the underestimation is about 20%. Both rules overestimate the base shear by about 10%. The uncertainty in the estimation is much larger for axial load than for base shear, and, for axial load, it is much larger for inelastic than for elastic behavior. The effect of individual components may be highly correlated, not only for normal components, but also for totally uncorrelated components. The rules are not always inaccurate for large values of correlation coefficients of the individual effects, and small values of such coefficients are not always related to an accurate estimation of the response. Only for perfectly uncorrelated harmonic excitations and elastic analysis of SDOF systems, the individual effects of the components are uncorrelated and the rules accurately estimate the combined response. In the general case, the level of underestimation or overestimation depends on the degree of correlation of the components, the type of structural system, the response parameter, the location of the structural member and the level of structural deformation. The codes should be more specific regarding the application of these rules. If the percentage rule is used for MDOF systems and earthquake loading, at least a value of 45% should be used for the combination factor.
<i>Herschel</i> and SCUBA-2 observations of dust emission in a sample of <i>Planck</i> cold clumps
Juvela, Mika,He, Jinhua,Pattle, Katherine,Liu, Tie,Bendo, George,Eden, David J.,Fehé,r, Orsolya,Michel, Fich,Fuller, Gary,Hirano, Naomi,Kim, Kee-Tae,Li, Di,Liu, Sheng-Yuan,Malinen, Johanna,Marsh Springer-Verlag 2018 Astronomy and astrophysics Vol.612 No.-
<P><I>Context.</I> Analysis of all-sky <I>Planck</I> submillimetre observations and the IRAS 100 <I>μ</I>m data has led to the detection of a population of Galactic cold clumps. The clumps can be used to study star formation and dust properties in a wide range of Galactic environments.</P><P><I>Aims.</I> Our aim is to measure dust spectral energy distribution (SED) variations as a function of the spatial scale and the wavelength.</P><P><I>Methods.</I> We examined the SEDs at large scales using IRAS, <I>Planck</I>, and <I>Herschel</I> data. At smaller scales, we compared JCMT/SCUBA-2 850 <I>μ</I>m maps with <I>Herschel</I> data that were filtered using the SCUBA-2 pipeline. Clumps were extracted using the Fellwalker method, and their spectra were modelled as modified blackbody functions.</P><P><I>Results.</I> According to IRAS and <I>Planck</I> data, most fields have dust colour temperatures <I>T</I>C ~ 14-18 K and opacity spectral index values of <I>β</I> = 1.5-1.9. The clumps and cores identified in SCUBA-2 maps have <I>T</I> ~ 13 K and similar <I>β</I> values. There are some indications of the dust emission spectrum becoming flatter at wavelengths longer than 500 <I>μ</I>m. In fits involving <I>Planck</I> data, the significance is limited by the uncertainty of the corrections for CO line contamination. The fits to the SPIRE data give a median <I>β</I> value that is slightly above 1.8. In the joint SPIRE and SCUBA-2 850 <I>μ</I>m fits, the value decreases to <I>β</I> ~ 1.6. Most of the observed <I>T</I>-<I>β</I> anticorrelation can be explained by noise.</P><P><I>Conclusions.</I> The typical submillimetre opacity spectral index <I>β</I> of cold clumps is found to be ~1.7. This is above the values of diffuse clouds, but lower than in some previous studies of dense clumps. There is only tentative evidence of a <I>T</I>-<I>β</I> anticorrelation and <I>β</I> decreasing at millimetre wavelengths.</P>
Planck Cold Clumps in the <i>λ</i> Orionis Complex. II. Environmental Effects on Core Formation
Yi, Hee-Weon,Lee, Jeong-Eun,Liu, Tie,Kim, Kee-Tae,Choi, Minho,Eden, David,II, Neal J. Evans,Francesco, James Di,Fuller, Gary,Hirano, N.,Juvela, Mika,Kang, Sung-ju,Kim, Gwanjeong,M. Koch, Patrick,Lee, American Astronomical Society 2018 The Astrophysical journal, Supplement series Vol.236 No.2
<P>Based on the 850 mu m dust continuum data from SCUBA-2 at James Clerk Maxwell Telescope (JCMT), we compare overall properties of Planck Galactic Cold Clumps (PGCCs) in the lambda Orionis cloud to those of PGCCs in the Orion A and B clouds. The Orion A and B clouds are well-known active star-forming regions, while the A Orionis cloud has a different environment as a consequence of the interaction with a prominent OB association and a giant H-II region. PGCCs in the lambda Orionis cloud have higher dust temperatures (T-d = 16.13 +/- 0.15 K) and lower values of dust emissivity spectral index (beta = 1.65 +/- 0.02) than PGCCs in the Orion A (T-d = 13.79 +/- 0.21 K, beta = 2.07 +/- 0.03) and Orion B (T-d = 13.82 +/- 0.19 K, beta =1.96 +/- 0.02) clouds. We find 119 substructures within the 40 detected PGCCs and identify them as cores. Out of a total of 119 cores, 15 cores are discovered in the lambda Orionis cloud, while 74 and 30 cores are found in the Orion A and B clouds, respectively. The cores in the lambda Orionis cloud show much lower mean values of size R = 0.08 pc, column density N(H-2) (9.5 +/- 1.2) x 10(22)cm(-2) , number density n(H-2) - (2.9 +/- 0.4) x 10 5 CM -3 , and mass M-core = 1.0 +/- 0.3 M(circle dot)compared to the cores in the Orion A [R = 0.11 pc, N(H-2) = (2.3 +/- 0.3) x 10(23) cm(-2), n(H-2) = (3.8 +/- 0.5) x 10(5)cm(-3) , and M-core = 2.4 +/- 0.3 M-circle dot] and Orion B [R = 0.16 pc, N(H-2) (3.8 +/- 0.4) x 10(23) cm(-2), n(H-2) = (15.6 +/- 1.8) x 10(5) cm(-3) , and M-core = 2.7 +/- 0.3 M-circle dot] clouds. These core properties in the A Orionis cloud can be attributed to the photodissociation and external heating by the nearby H rr region, which may prevent the PGCCs from forming gravitationally bound structures and eventually disperse them. These results support the idea of negative stellar feedback on core formation.</P>
Zhang, Chuan-Peng,Liu, Tie,Yuan, Jinghua,Sanhueza, Patricio,Traficante, Alessio,Li, Guang-Xing,Li, Di,Tatematsu, Ken’ichi,Wang, Ke,Lee, Chang Won,Samal, Manash R.,Eden, David,Marston, Anthony,Liu, Xia American Astronomical Society 2018 The Astrophysical journal Supplement series Vol.236 No.2
<P>In order to understand the initial conditions and early evolution of star formation in a wide range of Galactic environments, we carried out an investigation of 64 Planck Galactic cold clumps (PGCCs) in the second quadrant of the Milky Way. Using the (CO)-C-13 and (CO)-O-18 J = 1-0 lines and 850 mu m continuum observations, we investigated cloud fragmentation and evolution associated with star formation. We extracted 468 clumps and 117 cores from the (CO)-C-13 line and 850 mu m continuum maps, respectively. We made use of the Bayesian distance calculator and derived the distances of all 64 PGCCs. We found that in general, the mass-size plane follows a relation of m similar to r(1.67). At a given scale, the masses of our objects are around 1/10 of that of typical Galactic massive star-forming regions. Analysis of the clump and core masses, virial parameters, densities, and mass-size relation suggests that the PGCCs in our sample have a low core formation efficiency (similar to 3.0%), and most PGCCs are likely low-mass star-forming candidates. Statistical study indicates that the 850 mu m cores are more turbulent, more optically thick, and denser than the (CO)-C-13 clumps for star formation candidates, suggesting that the 850 mu m cores are likely more appropriate future star formation candidates than the (CO)-C-13 clumps.</P>
Liu, Tie,Kim, Kee-Tae,Juvela, Mika,Wang, Ke,Tatematsu, Ken’ichi,Francesco, James Di,Liu, Sheng-Yuan,Wu, Yuefang,Thompson, Mark,Fuller, Gary,Eden, David,Li, Di,Ristorcelli, I.,Kang, Sung-ju,Lin, Yuxin Published by the University of Chicago Press for t 2018 The Astrophysical journal Supplement series Vol.234 No.2
<P>The low dust temperatures (< 14 K) of Planck Galactic cold clumps (PGCCs) make them ideal targets to probe the initial conditions and very early phase of star formation. 'TOP-SCOPE' is a joint survey program targeting similar to 2000 PGCCs in J = 1-0 transitions of CO isotopologues and similar to 1000 PGCCs in 850 mu m continuum emission. The objective of the 'TOP-SCOPE' survey and the joint surveys (SMT 10 m, KVN 21 m, and NRO 45 m) is to statistically study the initial conditions occurring during star formation and the evolution of molecular clouds, across a wide range of environments. The observations, data analysis, and example science cases for these surveys are introduced with an exemplar source, PGCC G26.53+0.17 (G26), which is a filamentary infrared dark cloud (IRDC). The total mass, length, and mean line mass (M/L) of the G26 filament are similar to 6200 M-circle dot, similar to 12 pc, and similar to 500 M-circle dot pc(-1), respectively. Ten massive clumps, including eight starless ones, are found along the filament. The most massive clump as a whole may still be in global collapse, while its denser part seems to be undergoing expansion owing to outflow feedback. The fragmentation in the G26 filament from cloud scale to clump scale is in agreement with gravitational fragmentation of an isothermal, nonmagnetized, and turbulent supported cylinder. A bimodal behavior in dust emissivity spectral index (beta) distribution is found in G26, suggesting grain growth along the filament. The G26 filament may be formed owing to large-scale compression flows evidenced by the temperature and velocity gradients across its natal cloud.</P>