Guyasuta: Warrior, Estate, and Home to Boy Scouts

For nearly a century, Camp Guyasuta has been “an ideal place for Boy Scouts to live out their Handbook, to dream and be inspired and become good Americans.” Situated on roughly 130 acres in a deep valley between Aspinwall and Sharpsburg, Guyasuta is the primary camp for the Boy Scouts of America (BSA) in the newly formed Laurel Highlands Council. But before Guyasuta was established in 1918, the land was home to multiple generations of a prominent Pittsburgh family. It also served as the burial ground for a famous Native American. It has hosted lively parties, protected wildlife as a sanctuary, and was the center of a contentious battle between the mighty Pennsylvania Railroad and a “silver-haired old woman.

Standing on the Shoulders of Giants: The Cleft Palate-Craniofacial Journal (1964-1989)Electronic Archive

Current research and clinical practice in cleft palate and craniofacial disorders “stands on the shoulders of giants” who came before us. To enable thirty years of seminal research articles to become digitally available to a worldwide community of students, scholars, and clinicians, a collaboration was forged in 2004 between University of Pittsburgh’s Digital Research Library (DRL) and ACPA, (with the agreement of Allen Press), to create an electronic archive of the first thirty years of the Cleft Palate Craniofacial Journal . The work was performed pro bono, by all parties

BIONOMER PILOT PLANT

The purpose of this project is to develop a pilot-scale process for the bacterial production of methacrylic acid (MAA) and methyl ethyl ketone (MEK) from biomass feedstocks and the subsequent purification steps. The pilot plant will also be located on site at a sugar cane refinery in Brazil where the feedstock should be inexpensive and readily available. Although these sugar cane refineries only operate for 9 months each year, molasses can be stored so that the pilot plant runs year-round. To obtain useful information about the feasibility and scalability of the process, 30 M kg/yr of each product will be produced. The products will be tested for purity and samples will be sent out to consumers to demonstrate the quality of the product. The MAA and MEK must be of the same purity generated by current commercial processes. The pilot plant will be designed in three major parts. The first part consists of the bacterial fermentors that are used to produce and scale up MAA and MEK production. Relatively little is currently known about the efficiency of production of MAA and MEK by E. coli and this part of the plant will provide critical data about conditions required for the bacteria as well as production rates. The second part of the plant consists of the MAA purification process. Many options will be considered for the purification steps, many of which will have to be modeled in ASPEN because MAA is usually not produced in the aqueous phase. The final section of the plant will be used for MEK purification. To reduce plant costs, the design will try to share equipment between the two purification processes. The main goal of the plant is to obtain data and demonstrate feasibility, not to demonstrate sustainable profitability. Estimates for total capital investment and show that the plant will not be profitable for the first five years of operation, but the valuable data gained from the operation will be used to design the larger, more efficient, full-scale plant. The total capital investment required for the plant is approximately $ 6.33 million. Returns generated from sales are minimal compared to the capital investment and operating costs. A full scale plant is expected to be profitable over time because of economies of scale and the price of inputs and outputs of the process

Discovery of a High-Latitude Accreting Millisecond Pulsar in an Ultracompact Binary

We have identified the third known accretion-powered millisecond pulsar, XTE J0929-314, with the Rossi X-Ray Timing Explorer. The source is a faint, high-Galactic-latitude X-ray transient (d >~ 5 kpc) that was in outburst during 2002 April-June. The 185 Hz (5.4 ms) pulsation had a fractional rms amplitude of 3-7% and was generally broad and sinusoidal, although occasionally double-peaked. The hard X-ray pulses arrived up to 770 microseconds earlier than the soft X-ray pulses. The pulsar was spinning down at an average rate of -(9.2 +/- 0.4) * 10^-14 Hz/s; the spin-down torque may arise from magnetic coupling to the accretion disk, a magnetohydrodynamic wind, or gravitational radiation from the rapidly spinning pulsar. The pulsations were modulated by a 43.6 min ultracompact binary orbit, yielding the smallest measured mass function (2.7 * 10^-7 M_sun) of any stellar binary. The binary parameters imply an approximately 0.01 M_sun white dwarf donor and a moderately high inclination. We note that all three known accreting millisecond pulsars are X-ray transients in very close binaries with extremely low mass transfer rates. This is an important clue to the physics governing whether or not persistent millisecond pulsations are detected in low-mass X-ray binaries.Comment: 5 pages, 3 figures; accepted by ApJ Letters. Revised distance lower limit and added a figure showing pulse profile

Design of 280 GHz feedhorn-coupled TES arrays for the balloon-borne polarimeter SPIDER

We describe 280 GHz bolometric detector arrays that instrument the balloon-borne polarimeter SPIDER. A primary science goal of SPIDER is to measure the large-scale B-mode polarization of the cosmic microwave background in search of the cosmic-inflation, gravitational-wave signature. 280 GHz channels aid this science goal by constraining the level of B-mode contamination from galactic dust emission. We present the focal plane unit design, which consists of a 16$\times$16 array of conical, corrugated feedhorns coupled to a monolithic detector array fabricated on a 150 mm diameter silicon wafer. Detector arrays are capable of polarimetric sensing via waveguide probe-coupling to a multiplexed array of transition-edge-sensor (TES) bolometers. The SPIDER receiver has three focal plane units at 280 GHz, which in total contains 765 spatial pixels and 1,530 polarization sensitive bolometers. By fabrication and measurement of single feedhorns, we demonstrate 14.7$^{\circ}$ FHWM Gaussian-shaped beams with $<$1% ellipticity in a 30% fractional bandwidth centered at 280 GHz. We present electromagnetic simulations of the detection circuit, which show 94% band-averaged, single-polarization coupling efficiency, 3% reflection and 3% radiative loss. Lastly, we demonstrate a low thermal conductance bolometer, which is well-described by a simple TES model and exhibits an electrical noise equivalent power (NEP) = 2.6 $\times$ 10$^{-17}$ W/$\sqrt{\mathrm{Hz}}$, consistent with the phonon noise prediction.Comment: Proceedings of SPIE Astronomical Telescopes + Instrumentation 201

Towards a Paperless Choral Classroom

The objective of the “Towards A Paperless Choral Classroom” Interactive Qualifying Project is to integrate music and technology and to provide a template for a paperless choral conference. Students in this project prepared months in advance to assist in the Eastern Division Conference for the American Choral Directors Association. The students explored the many possibilities with which modern technology can benefit the music world. This report suggests technological alternatives to routine choral practices, and can serve as a guide for future choral conferences