Educational Procedures In This Development Of Agricultural Cooperatives At The Sabine Farms, Harrison County, Texas

Purposes of the Study The purposes of this study are, first, to determine the educational procedures involved in the organization of the Sabine Farms Agricultural Cooperatives, and second, to present certain facts that may be applied to similar situations in other communities where there is a possibility of the organization of agricultural cooperatives through educational procedures in such channels as creating desires on the part of farmers to work cooperatively for increased economic, social, and educational advantages. It Is hoped that professional agricultural leaders, as well as laymen, will find this information practical and helpful. Statement of the Problem Under the present economic conditions in America, it is a fundamental principle that successful business organization among farmers must be founded for those enterprises engaged in by the farmers. Up to the present time, it has not been a general, but rather, it has been a rare practice for the average or small farmers to organize themselves for business purposes. One cannot say why this laxity exists the rarity of the organization of farmers for economic purposes. Whether the farmers are lazy, lack information as to the importance of such organizations, or whether the farmers do not have the necessary guiding forces in the form of information or individuals cannot be determined. At any rate, the problem exists. A solution for this problem is gravely needed. Scope. Sources, and Methods of Obtaining Data In this paper, the writer is concerned with the Sabine Farms Cooperatives only. The materials used in compiling this work were obtained from the W. R, Banks Library, Consumers Cooperative Association, Cooperative League of the United States of America, Cooperative Publishers Association, the Organization and Cooperative Marketing Specialist of the Texas Agricultural and Mechanical College Extension Service, National Cooperative Incorporated, and numerous inquiry forms carried to the Supervisor of the Sabine Farms and to the Manager of the Sabine Farms Agricultural Cooperatives

Characterization of the LIGO detectors during their sixth science run

In 2009-2010, the Laser Interferometer Gravitational-Wave Observatory (LIGO) operated together with international partners Virgo and GEO600 as a network to search for gravitational waves (GWs) of astrophysical origin. The sensitivity of these detectors was limited by a combination of noise sources inherent to the instrumental design and its environment, often localized in time or frequency, that couple into the GW readout. Here we review the performance of the LIGO instruments during this epoch, the work done to characterize the detectors and their data, and the effect that transient and continuous noise artefacts have on the sensitivity of LIGO to a variety of astrophysical sources

Multi-messenger Observations of a Binary Neutron Star Merger

International audienceOn 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of $\sim 1.7\,{\rm{s}}$ with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg(2) at a luminosity distance of ${40}_{-8}^{+8}$ Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 $\,{M}_{\odot }$. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at $\sim 40\,{\rm{Mpc}}$) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ∼10 days. Following early non-detections, X-ray and radio emission were discovered at the transient’s position $\sim 9$ and $\sim 16$ days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC 4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta