Small Mammals in Prairie Wetlands: Habitat Use and the Effects of Wetland Modifications

Although well documented for other habitat types, small mammal habitat use patterns in prairie wetlands are poorly understood. The distribution of the mammal fauna of South Dakota is also not well known. Because of the lack of information in these areas, evaluation of the impacts of wetland modifications on the resident mammal community is not possible. The objectives of this study were (1) to document the species composition and abundance of small mammal communities inhabiting prairie wetland basins, (2) to determine the effects of small scale habitat modification on small mammals, (3) and to explain local species distribution patterns using habitat measurements. This study was conducted during the summers of 1981 and 1982. Meadow voles (Microtus pennsylvanicus) were the most common small mammal in prairie wetlands, followed by deer mice (Peromyscus spp.), masked shrews (Sorex cinereous), meadow jumping mice (Zapus hudsonius) and northern short-tailed shrews (Blarina brevicauda). Deer mine were more common in modified habitats within wetland basins than in undisturbed habitat. Modification of wetlands tended to reduce the species diversity of small mammals I the modified areas. Local distributions of species seemed to be largely determined by soil moisture. Meadow voles used the wettest habitats and deer mice used the driest. Both species of shrew seemed to use habitats intermediate in terms of moisture between wetlands and uplands

Infrared reflection nebulae in Orion molecular cloud 2

New obervations of Orion Molecular Cloud-2 have been made from 1-100 microns using the NASA Infrared Telescope Facility and the Kuiper Airborne Observatory. An extensive program of polarimetry, photometry and spectrophotometry has shown that the extended emission regions associated with two of the previously known near infrared sources, IRS1 and IRS4, are infrared reflection nebulae, and that the compact sources IRS1 and IRS4 are the main luminosity sources in the cloud. The constraints from the far infrared observations and an analysis of the scattered light from the IRS1 nebula show that OMC-2/IRS1 can be characterized by L less than or equal to 500 Solar luminosities and T approx. 1000 K. The near infrared (1-5) micron albedo of the grains in the IRS1 nebula is greater than 0.08

The Statistics of the BATSE Spectral Features

The absence of a BATSE line detection in a gamma-ray burst spectrum during the mission's first six years has led to a statistical analysis of the occurrence of lines in the BATSE burst database; this statistical analysis will still be relevant if lines are detected. We review our methodology, and present new simulations of line detectability as a function of the line parameters. We also discuss the calculation of the number of ``trials'' in the BATSE database, which is necessary for our line detection criteria.Comment: 5 pages, 2 figures, AIPPROC LaTeX, to appear in "Gamma-Ray Bursts, 4th Huntsville Symposium," eds. C. Meegan, R. Preece and T. Koshu

Terdiurnal Oscillations in OH Meinel Rotational Temperatures for Fall Conditions at Northern Mid-latitude Sites

High‐precision (∼0.5 K) measurements of OH Meinel (M) (6,2) rotational temperatures above the Bear Lake Observatory, UT (42°N, 112°W) during October 1996 have revealed an interesting and unexpected mean nocturnal pattern. Ten quality nights (\u3e100 h) of data have been used to form a mean night for autumnal, near‐equinoctial conditions. The mean temperature and RMS variability associated with this mean night were 203 ± 5 K and 2.4 K, respectively, and compare very favorably with expectations based on Na‐lidar measurements of mean tidal temperature perturbations over Urbana, IL (40°N, 88°W) during the fall 1996. Furthermore, this comparison shows that the 8‐h tide was the dominant source of the mean nocturnal temperature variability in the OH M region during this period. Additional data, obtained at Fort Collins, CO (41°N, 105°W) in November 1997, illustrate the occurrence of an 8‐h component of OH temperature variability about two months after the equinox and show that daily amplitudes as high as ≅15 K are possible