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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>
Koch, Robert H.,Wolf, George W.,Hull, Anthony B.,Elias, Nicholas M. II,Holenstein, Bruce D.,Mitchell, Richard J. 한국우주과학회 2012 Journal of Astronomy and Space Sciences Vol.29 No.1
This report describes the inception, development and extensive use over 30 years of elliptical polarimeters at the Uni\-versity of Pennsylvania. The initial Mark I polarimeter design utilized oriented retarder plates and a calcite Foster-Clarke prism as the analyzer. The Mark I polarimeter was used on the Kitt Peak 0.9 m in 1969-70 to accomplish a survey of ap\-proximately 70 objects before the device was relocated to the 0.72 m reflector at the Flower and Cook Observatory. Suc\-cessive generations of automation and improvements included the early-80’s optical redesign to utilize a photoelastic modulated wave plate and an Ithaco lock-in amplifier-the photoelastic modulating polarimeter. The final design in 2000 concluded with a fully remote operable device. The legacy of the polarimetric programs includes studies of close binaries, pulsating hot stars, and luminous late-type variables.
Robert H. Koch,George W. Wolf,Anthony B. Hull,Nicholas M. Elias II,Bruce D. Holenstei,Richard J. Mitchell 한국우주과학회 2012 Journal of Astronomy and Space Sciences Vol.29 No.1
This report describes the inception, development and extensive use over 30 years of elliptical polarimeters at the University of Pennsylvania. The initial Mark I polarimeter design utilized oriented retarder plates and a calcite Foster-Clarke prism as the analyzer. The Mark I polarimeter was used on the Kitt Peak 0.9 m in 1969-70 to accomplish a survey of approximately 70 objects before the device was relocated to the 0.72 m reflector at the Flower and Cook Observatory. Successive generations of automation and improvements included the early-80’s optical redesign to utilize a photoelastic modulated wave plate and an Ithaco lock-in amplifier–the photoelastic modulating polarimeter. The final design in 2000 concluded with a fully remote operable device. The legacy of the polarimetric programs includes studies of close binaries, pulsating hot stars, and luminous late-type variables.
LaBonte, Melissa J.,Yang, Dongyun,Zhang, Wu,Wilson, Peter M.,Nagarwala, Yasir M.,Koch, Kevin M.,Briner, Colleen,Kaneko, Tomomi,Rha, Sun-Young,Gladkov, Oleg,Urba, Susan G.,Sakaeva, Dina,Pishvaian, Mich American Association for Cancer Research 2016 Molecular Cancer Therapeutics Vol.15 No.9
<P>An exploratory phase II biomarker-embedded trial (LPT109747; NCT00526669) designed to determine the association of lapatinib-induced fluoropyrimidine gene changes with efficacy of lapatinib plus capecitabine as first-line treatment for advanced gastric cancer or gastroesophageal junction adenocarcinoma-independent of tumor HER2 status. Tumor biopsies obtained before and after 7- day lapatinib (1,250 mg) to analyze changes in gene expression, followed by a 14-day course of capecitabine (1,000 mg/m(2) twice daily, 14/21 days) plus lapatinib 1,250 mg daily. Blood samples were acquired for pharmacokinetic analysis. Primary clinical objectives were response rate (RR) and 5-month progression-free survival (PFS). Secondary objectives were overall survival (OS), PFS, time to response, duration of response, toxicity, and identification of associations between lapatinib pharmacokinetics and biomarker endpoints. Primary biomarker objectives were modulation of 5FU- pathway genes by lapatinib, effects of germline SNPs on treatment outcome, and trough steady-state plasma lapatinib concentrations. Sixty-eight patients were enrolled; (75% gastric cancer, 25% gastroesophageal junction). Twelve patients (17.9%) had confirmed partial response, 31 (46.3%) had stable disease, and 16 (23.9%) had progressive disease. Median PFS and OS were 3.3 and 6.3 months, respectively. Frequent adverse events included diarrhea (45%), decreased appetite (39%), nausea (36%), and fatigue (36%). Lapatinib induced no changes in gene expression from baseline and no significant associations were found for SNPs analyzed. Elevated baseline HER3 mRNA expression was associated with a higher RR (33% vs. 0%; P = 0.008). Lapatinib plus capecitabine was well tolerated, demonstrating modest antitumor activity in patients with advanced gastric cancer. The association of elevated HER3 and RR warrants further investigation as an important player for HER-targeted regimens in combination with capecitabine. (C)2016 AACR.</P>
The JCMT BISTRO Survey: The Magnetic Field Strength in the Orion A Filament
Pattle, Kate,Ward-Thompson, Derek,Berry, David,Hatchell, Jennifer,Chen, Huei-Ru,Pon, Andy,Koch, Patrick M.,Kwon, Woojin,Kim, Jongsoo,Bastien, Pierre,Cho, Jungyeon,Coudé,, Simon,Di Francesco, Jam American Astronomical Society 2017 The Astrophysical journal Vol.846 No.2
<P>We determine the magnetic field strength in the OMC. 1 region of the Orion A filament via a new implementation of the Chandrasekhar-Fermi method using observations performed as part of the James Clerk Maxwell Telescope (JCMT) B-Fields In Star-forming Region Observations (BISTRO) survey with the POL-2 instrument. We combine BISTRO data with archival SCUBA-2 and HARP observations to find a plane-of-sky magnetic field strength in OMC. 1 of B-pos= 6.6 +/- 4.7 mG, where delta B-pos = 4.7 mG represents a predominantly systematic uncertainty. We develop a new method for measuring angular dispersion, analogous to unsharp masking. We find a magnetic energy density of similar to 1.7 x 10(-7) J m(-3) in OMC. 1, comparable both to the gravitational potential energy density of OMC 1 (similar to 10(-7) J m(-3)) and to the energy density in the Orion BN/KL outflow (similar to 10(-7) J m(-3)). We find that neither the Alfven velocity in OMC. 1 nor the velocity of the super-Alfvenic outflow ejecta is sufficiently large for the BN/KL outflow to have caused large-scale distortion of the local magnetic field in the similar to 500 yr lifetime of the outflow. Hence, we propose that the hourglass field morphology in OMC. 1 is caused by the distortion of a primordial cylindrically symmetric magnetic field by the gravitational fragmentation of the filament and/or the gravitational interaction of the BN/KL and S clumps. We find that OMC. 1 is currently in or near magnetically supported equilibrium, and that the current large-scale morphology of the BN/KL outflow is regulated by the geometry of the magnetic field in OMC 1, and not vice versa.</P>
Metabolic Crosstalk between the Heart and Fat
Kimberly M. Ferrero,Walter J. Koch 대한심장학회 2020 Korean Circulation Journal Vol.50 No.5
It is now recognized that the heart can behave as a true endocrine organ, which can modulate the function of other tissues. Emerging evidence has shown that visceral fat is one such distant organ the heart communicates with. In fact, it appears that bi-directional crosstalk between adipose tissue and the myocardium is crucial to maintenance of normal function in both organs. In particular, factors secreted from the heart are now known to influence the metabolic activity of adipose tissue and other organs, as well as modulate the release of metabolic substrates and signaling molecules from the periphery. This review summarizes current knowledge regarding primary cardiokines and adipokines involved in heart-fat crosstalk, as well as implications of their dysregulation for cardiovascular health.
Final report on key comparison CCAUV.U-K3.1
Haller, J,Koch, C,Costa-Felix, R P B,Dubey, P K,Durando, G,KIM, Y T,Yoshioka, M BUREAU INTERNATIONAL DES POIDS ET MESURES 2016 METROLOGIA -BERLIN- Vol.53 No.-
<P></P> <P>The CCAUV.U-K3.1 is a follow-up of the comparison CCAUV.U-K3 which was the third key comparison in the ultrasound branch organised under the auspices of the Consultative Committee for Acoustics, Ultrasound and Vibration (CCAUV) of the BIPM. It was necessary to allow participants with discrepant values and additional laboratories to have another possibility to take part in an international comparison and to test their measurement facilities. The comparison dealt with power measurement in the frequency range 2 to 10.5 MHz and a power range between 10 mW and 15 W. The parameter range covered is of particular importance for medical applications of ultrasound.</P> <H2>Main text</H2> <P> To reach the main text of this paper, click on <A HREF='http://www.bipm.org/utils/common/pdf/final_reports/AUV/U-K3/CCAUV.U-K3.1_Final_Report.pdf'>Final Report</A>. Note that this text is that which appears in Appendix B of the BIPM key comparison database <A HREF='http://kcdb.bipm.org/'>kcdb.bipm.org/</A>.</P> <P>The final report has been peer-reviewed and approved for publication by the CCAUV, according to the provisions of the CIPM Mutual Recognition Arrangement (CIPM MRA).</P>