637 research outputs found
Letter from Frank G. Muench, May 25, 1942
No full textAnnotated form letter from Frank G. Muench regarding the fact that Lincoln Christian Center in Sacramento, California helped their Japanese friends move safely to Walerga camp [= Sacramento Assembly Center] about 10 miles from Sacramento.The Japanese American Archival Collection documents the people, places, and daily life of Japanese Americans, primarily those who lived in the once thriving community of pre-war Florin in the Sacramento region, as well as the conditions in American incarceration camps during World War II. The approximately 7,000 original items include personal and official letters, photographs, diaries, arts and crafts, newsletters, textiles, camps artifacts, yearbooks and other publications
A Comparison of Leaves of Quercus Coccinea Muench. and Betula Lenta L. from Heath Bald and Mesphytic Ravine Habitats
No full textAn ecological study of the leaves of Quercus coccinea Muench. and Betula lenta L. was undertaken by the writer during the summer of 1945 at the Mountain Lake Biological Station of the University of Virginia in Giles County, Virginia. The writer wishes to express his appreciation to Dr. I. F. Lewis, Director of the Mountain Lake Biological Station, and Mr. Ruskin S. Freer of the Department of Biology of Lynchburg College, Lynchburg, Virginia, for their invaluable aid in the pursuance of this problem
Characterization of the flexibility of the peripheral stalk of prokaryotic rotary A-ATPases by atomistic simulations
No full textRotary ATPases are involved in numerous physiological processes, with the three distinct types (F/A/V-ATPases) sharing functional properties and structural features. The basic mechanism involves the counter rotation of two motors, a soluble ATP hydrolyzing/synthesizing domain and a membrane-embedded ion pump connected through a central rotor axle and a stator complex. Within the A/V-ATPase family conformational flexibility of the EG stators has been shown to accommodate catalytic cycling and is considered to be important to function. For the A-ATPase three EG structures have been reported, thought to represent conformational states of the stator during different stages of rotary catalysis. Here we use long, detailed atomistic simulations to show that those structures are conformers explored through thermal fluctuations, but do not represent highly populated states of the EG stator in solution. We show that the coiled coil tail domain has a high persistence length (∼100 nm), but retains the ability to adapt to different conformational states through the presence of two hinge regions. Moreover, the stator network of the related V-ATPase has been suggested to adapt to subunit interactions in the collar region in addition to the nucleotide occupancy of the catalytic domain. The MD simulations reported here, reinforce this observation showing that the EG stators have enough flexibility to adapt to significantly different structural re-arrangements and accommodate structural changes in the catalytic domain whilst resisting the large torque generated by catalytic cycling. These results are important to understand the role the stators play in the rotary-ATPase mechanism. Proteins 2016; 84:1203–1212. © 2016 The Authors. Proteins: Structure, Function, and Bioinformatics Published by Wiley Periodicals, Inc
The nature of the dense core population in the Pipe Nebula : a survey of NH3, CCS, and HC5N molecular line emission
No full textRecent extinction studies of the Pipe Nebula (d=130 pc) reveal many cores spanning a range in mass from 0.2 to 20.4 Msolar. These dense cores were identified via their high extinction and comprise a starless population in a very early stage of development. Here we present a survey of NH3 (1,1), NH3 (2,2), CCS (21-10), and HC5N (9,8) emission toward 46 of these cores. An atlas of the 2MASS extinction maps is also presented. In total, we detect 63% of the cores in NH3 (1,1), 22% in NH 3 (2,2), 28% in CCS, and 9% in HC5N emission. We find the cores are associated with dense gas (~104 cm-3) with 9.5 K<=TK<=17 K. Compared to C18O, we find the NH3 line widths are systematically narrower, implying that the NH3 is tracing the dense component of the gas and that these cores are relatively quiescent. We find no correlation between core line width and size. The derived properties of the Pipe cores are similar to cores within other low-mass star-forming regions: the only differences are that the Pipe cores have weaker NH 3 emission and most show no current star formation as evidenced by the lack of embedded infrared sources. Such weak NH3 emission could arise due to low column densities and abundances or reduced excitation due to relatively low core volume densities. Either alternative implies that the cores are relatively young. Thus, the Pipe cores represent an excellent sample of dense cores in which to study the initial conditions for star formation and the earliest stages of core formation and evolution
The nature of the dense core population in the Pipe Nebula : core and cloud kinematics from C18O observations
No full textWe present molecular line observations of 94 dark cloud cores identified in the Pipe nebula through near-IR extinction mapping. Using the Arizona Radio Observatory 12m telescope, we obtained spectra of these cores in the J = 1-0 transition of (CO)-O-18. We used the measured core parameters, T-R*, Delta(v), v(lsr,) radius, and mass, to explore the internal kinematics of the cores, as well as their radial motions through the larger molecular cloud. We find that the vast majority of the dark extinction cores are true cloud cores, rather than the superposition of unrelated filaments. While we identify no significant correlations between the cores' internal gas motions and their other physical parameters, we identify spatially correlated radial velocity variations that outline two main kinematic components of the cloud. The largest is a 15 pc long filament that is surprisingly narrow both in spatial dimensions and in radial velocity. Beginning in the "Stem'' of the Pipe, this filament displays uniformly small (CO)-O-18 line widths (Delta v similar to 0.4 km s(-1)), as well as core-to-core motions only slightly in excess of the gas sound speed. The second component outlines what appears to be part of a large (2 pc; 10(3)M(circle dot)) ringlike structure. Cores associated with this component display both larger line widths and core-to-core motions than cores in the main cloud. The Pipe molecular ring may represent a primordial structure related to the formation of this cloud
Muench, Mary (Death, 1896-02-20)
No full textAddress: City Hospital 1414 Clay St.Age at death: 38442/Pg 21/1896/F W M/Ellen F. Mccarthy, M.D./Von Seelin & U./St. Marys Cem.Original record filed in drawer labeled 'MUELLER-MULLER'
Muench, Rose (Birth, 1907-02-12)
No full textAddress: 2582 W. McMicken856/Pg 78/1907/F W/Hungary/Hungary/Dr. F. TheissOriginal record filed in drawer labeled 'MUELLER-MULLER'
Muench, Adeline (Death, 1897-03-15)
No full textAddress: 1507 Race St.Age at death: 46 yrs.Pg 26/1897/276/F W M/City/Dr. G. F. Sudhoff/A. Schraffenberger/St.Mary'sOriginal record filed in drawer labeled 'MUELLER-MULLER'
Dense Cores in The Pipe Nebula: An Improved Core Mass Function
No full textIn this paper, we derive an improved core mass function (CMF) for the Pipe Nebula from a detailed comparison between measurements of visual extinction and molecular-line emission. We have compiled a refined sample of 201 dense cores toward the Pipe Nebula using a two-dimensional threshold identification algorithm informed by recent simulations of dense core populations. Measurements of radial velocities using complimentary C18O (1-0) observations enable us to cull out from this sample those 43 extinction peaks that are either not associated with dense gas or are not physically associated with the Pipe Nebula. Moreover, we use the derived C18O central velocities to differentiate between single cores with internal structure and blends of two or more physically distinct cores, superposed along the same line of sight. We then are able to produce a more robust dense core sample for future follow-up studies and a more reliable CMF than was possible previously. We confirm earlier indications that the CMF for the Pipe Nebula departs from a single power-law-like form with a break or knee at M ~ 2.7 ± 1.3 M sun. Moreover, we also confirm that the CMF exhibits a similar shape to the stellar initial mass function (IMF), but is scaled to higher masses by a factor of ~4.5. We interpret this difference in scaling to be a measure of the star formation efficiency (22% ± 8%). This supports earlier suggestions that the stellar IMF may originate more or less directly from the CMF
View of construction of Alondra Park
No full textConstruction of Alondra Park; "F2.1-12-F" at lower left
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