Hydrogen in Type Ic Supernovae?

By definition, a Type Ic supernova (SN Ic) does not have conspicuous lines of hydrogen or helium in its optical spectrum. SNe Ic usually are modelled in terms of the gravitational collapse of bare carbon-oxygen cores. We consider the possibility that the spectra of ordinary (SN 1994I-like) SNe Ic have been misinterpreted, and that SNe Ic eject hydrogen. An absorption feature usually attributed to a blend of Si II 6355 and C II 6580 may be produced by H-alpha. If SN 1994I-like SNe Ic eject hydrogen, the possibility that hypernova (SN 1998bw-like) SNe Ic, some of which are associated with gamma-ray bursts, also eject hydrogen should be considered. The implications of hydrogen for SN Ic progenitors and explosion models are briefly discussed.Comment: Accepted by PASP. Several significant changes including one additional figur

Submillimeter Atmospheric Transparency at Maunakea, at the South Pole, and at Chajnantor

For a systematic assessment of submillimeter observing conditions at different sites, we constructed tipping radiometers to measure the broad band atmospheric transparency in the window around 350 $\mu$m wavelength. The tippers were deployed on Maunakea, Hawaii, at the South Pole, and in the vicinity of Cerro Chajnantor in northern Chile. Identical instruments permit direct comparison of these sites. Observing conditions at the South Pole and in the Chajnantor area are better than on Maunakea. Simultaneous measurements with two tippers demonstrate conditions at the summit of Cerro Chajnantor are significantly better than on the Chajnantor plateau.Comment: Accepted by PAS

Cousins Photometry and Temperatures for the Hyades, Coma, NGC 752, Praesepe, and M67

In this paper, new Cousins VRI data are presented for NGC 752 and Praesepe, and new and extant data are combined into an augmented database for M67. For those three clusters, catalogs containing Cousins VRI photometry, reddening-corrected values of (V -K)(J), and temperatures are produced. The same is done for Coma by using both previously published and newly derived Cousins photometry. An extant set of catalogs for the Hyades is updated to include V magnitudes and values of (R -I)(C) that were published after the original catalogs appeared. Finally, M67 V magnitudes published previously by Sandquist are corrected for an effect that depends on location on the face of the cluster. The corrected data and values of (V -I)(C) given by Sandquist are then set out in a supplementary catalog. Data files containing all of these catalogs are deposited in the CDS archives. To assess the quality of the data in the catalogs, the consistency of extant Cousins VRI databases is tested by performing analyses with the following features: (1) quantities as small as a few millimags are regarded as meaningful; (2) statistical analysis is applied; (3) no use is made of data other than VRI measurements and comparable results; (4) no inferences are drawn from color-magnitude comparisons; (5) pertinent data that have not been included previously are analyzed; and (6) results based on direct comparisons of stellar groups at the telescope are featured. In this way, it is found that our updated M67 color data and those of Sandquist are on the E region zero point. In contrast, values of (V -I)(C) from Montgomery and collaborators are found to be too red by 27 +/- 3 mmag, with an even larger offset being likely for unpublished data from Richer and his collaborators. Zero-point tests of our Cousins VRI colors for Coma, Praesepe, and NGC 752 are also satisfactory. Scale factor tests of the M67 colors are performed, and a likely scale factor error in the Montgomery et al. colors is found. However, it appears at present that the scale factors of our M67 colors and those of Sandquist are satisfactory. For the most part, zero-point tests of the assembled V magnitudes are also satisfactory, although it is found that further work on the V magnitudes for Praesepe and M67 would be useful. To put these results in perspective, it is pointed out that photometric tests that are satisfactory at the few-millimag level have been published for some two decades and so are not appearing for the first time in this paper.Astronom

Neural network identification of keystream generators

Applications such as stream ciphers and spread spectra require the generation of binary keystreams to implement, and the simulation of such keystreams to break. Most cryptanalytic attacks are of the known generator type, that is, they assume knowledge of the method used to generate the keystream. We show that a neural network can be used to identify the generator, and in some cases to simulate the keystream.http://archive.org/details/neuralnetworkide00leadApproved for public release; distribution is unlimited

The Competitive Behaviors of Small Retailers: Examining the Strategies of Local Merchants in Rural America

Mass merchandisers, discount  chain  stores,  category  killers,  and e-commerce  are  changing the retail industry through innovations in marketing and service. Driven by increased competition and discriminating  customers,  small,  local  retailers  are  searching for  ways  to gain and sustain competitive advantage. This study examines the competitive behaviors and performances of 236 retailers located in rural Nebraska. The findings indicate that retailers which adopted competitive behaviors with a goal of low cost/low price leadership were most successful. However, retailers using a combination or value-oriented strategy were also successful. Retailers which adopted competitive behaviors that constitute solely a differentiation strategy and those which had no clearly defined strategy were the worst performers. These findings suggest that in order to achieve competitive advantage,  rural retailers should follow a value-oriented strategy, being effective at both cost reduction and competitive pricing  while  offering  unique products  and services

Optimal Population Codes for Space: Grid Cells Outperform Place Cells

Rodents use two distinct neuronal coordinate systems to estimate their position: place fields in the hippocampus and grid fields in the entorhinal cortex. Whereas place cells spike at only one particular spatial location, grid cells fire at multiple sites that correspond to the points of an imaginary hexagonal lattice. We study how to best construct place and grid codes, taking the probabilistic nature of neural spiking into account. Which spatial encoding properties of individual neurons confer the highest resolution when decoding the animal’s position from the neuronal population response? A priori, estimating a spatial position from a grid code could be ambiguous, as regular periodic lattices possess translational symmetry. The solution to this problem requires lattices for grid cells with different spacings; the spatial resolution crucially depends on choosing the right ratios of these spacings across the population. We compute the expected error in estimating the position in both the asymptotic limit, using Fisher information, and for low spike counts, using maximum likelihood estimation. Achieving high spatial resolution and covering a large range of space in a grid code leads to a trade-off: the best grid code for spatial resolution is built of nested modules with different spatial periods, one inside the other, whereas maximizing the spatial range requires distinct spatial periods that are pairwisely incommensurate. Optimizing the spatial resolution predicts two grid cell properties that have been experimentally observed. First, short lattice spacings should outnumber long lattice spacings. Second, the grid code should be self-similar across different lattice spacings, so that the grid field always covers a fixed fraction of the lattice period. If these conditions are satisfied and the spatial “tuning curves” for each neuron span the same range of firing rates, then the resolution of the grid code easily exceeds that of the best possible place code with the same number of neurons

Archaeological Excavation of the Priest Quarters, Mission San Francisco de la Espada, 41BX4, San Antonio, Texas

The following report is the result of two projects completed by the Center for Archaeological Research, of The University of Texas at San Antonio for San Francisco de la Espada/Catholic Diocese of San Antonio and J. T. Michel, Inc., under Texas Historical Commission Permit Number 2076. The investigations were conducted at Mission San Francisco de la Espada, San Antonio, Bexar County, Texas (41BX4). The initial investigation was conducted in November 1998, prior to the planned installation of electrical lines along the southwest corner of the Convento (complex of structures grouped around a patio area), while the additional excavations of July and August 1999, were conducted to coincide with restoration work being conducted on the Chapel and Priest Quarters. Additional investigations were also conducted in July and August 1999, along the southern-most walls of the Priest Quarters prior to the installation of new foundation piers and beams designed to stabilize the existing wall foundations. The excavations affected the exterior walls of the Convento; an area 1 m wide by 1 m deep, and 25.2 m long. The monitoring portion conducted in October and November 1999, focused on unexcavated areas along walls that were exposed during the stabilization work. During the course of the investigations exposed foundations and features were documented, with specific attention to mode of construction and condition. The excavations resulted in the recovery of a variety of Colonial and post-Colonial artifacts including ceramics, lithics, glass, metal, and animal bone. These excavations which supplied the opportunity for the recovery of valuable cultural data, also revealed noticeable differences in wall foundation construction and reconstruction, which strongly suggest at least two distinct construction sequences

New Techniques to Determine Ages of Open Clusters Using White Dwarfs

Currently there are two main techniques for independently determining the ages of stellar populations: main-sequence evolution theory (via cluster isochrones) and white dwarf cooling theory. Open clusters provide the ideal environment for the calibration of these two clocks. Because current techniques to derive cluster ages from white dwarfs are observationally challenging, we discuss the feasibility of determining white dwarf ages from the brighter white dwarfs alone. This would eliminate the requirement of observing the coolest (i.e., faintest) white dwarfs. We discuss our method for testing this new idea, as well as the required photometric precision and prior constraints on metallicity, distance, and reddening. We employ a new Bayesian statistical technique to obtain and interpret results