Resource selection by black bears on U.S. Marine Corps Base Camp Lejeune

In 1992, U.S. Marine Corps Base Camp Lejeune (Camp Lejeune) purchased the 16,691-ha Greater Sandy Run Acquisition (GSRA) in Onslow County, North Carolina. Development and use of the GSRA for live-weapons firing and other military training has steadily increased since the land purchase. Resource managers at Camp Lejeune are interested in assessing the combined effects of military activities, forest management, roads, and the importance of natural vegetation types on black bear habitat use. My objectives were to determine black bear home range and habitat use in relation to those factors, and then synthesize spatial use patterns into a geographic information system-based habitat model. Between 2000-2001, field personnel captured 26 bears and collected 2,119 locations on 20 radio-collared bears (10 M: 10 F). Based on the 95% probability fixed kernel method, the mean annual home range was 37.2 km2 for males (n = 11) and 27.8 km2 for females (n = 12). I used 1,934 telemetry locations collected from 17 bears (7 M: 10 F) to assess habitat use with the multinomial logit form of discrete choice analysis. I compared the resource attributes of selected habitats (telemetry locations) with those available (random locations) within a spatially and temporally defined circle (i.e., choice set ). I investigated habitat use at a daily movements scale (7-km2 choice sets) and at a more local scale (1-km2 choice sets). The analysis was based on 5 primary habitat variables (land-cover type, forest management, bum history, paved road density, and land-cover diversity) and 5 interaction terms (year, season, sex, age, and firing range activity). I used Akaike\u27s information criterion to select the best model and used the parameter estimates to create a map of bear habitat utility values for the study area. The resource selection models performed well at both analysis scales based on model testing with independent data. Both models were robust to the effects of telemetry error. Resource selection varied depending on the spatial analysis scale. Although the importance of variables was relatively consistent for both models, parameters were more significant in the 7-km2 model. Bears selected areas with greater diversity of land-cover types only in the 7-km2 model. Land-cover was the most influential variable in both habitat models. Bottomland hardwoods exerted the greatest positive influence on bear habitat selection, followed closely by pocosin. Current levels of firing range activity did not have a measurable effect on black bear habitat selection, however, bears seemed to avoid the open land-cover type associated with the firing ranges. The density of paved roads and areas burned within 5 years had a strong negative influence on black bear habitat use at both spatial scales. I was unable to analyze the effects of forest management on black bear habitat selection because most forest stands available to bears were in the same age class. Conservation and management of pocosin and bottomland hardwoods is crucial to maintain the black bear population on the GSRA. Infrastructure development, increases in traffic volumes, and development in surrounding areas are likely to affect bear habitat use in the future; careful land-use planning and consideration of these factors will be critical for bear management on the GSRA. Although current levels of firing range activity did not influence black bear habitat use, substantial increases in the number of firing ranges and subsequent firing activities would require further examination to determine the effects on bear habitat use

Human–Black Bear Interactions and Public Attitudinal Changes in an Urban Ordinance Zone

Human–bear (Ursus spp.) interactions (HBI) commonly occur in residential areas throughout North America. Negative HBI can be alleviated by using bear-resistant garbage cans (BRC) and by securing other bear attractants (e.g., bird feeders). Since the early 2000s, human and Florida black bear (U. americanus floridanus) densities have increased substantially throughout Florida, USA, concurrently producing an increase in HBI. In central Florida, an area with high densities of humans and black bears, we surveyed 2 neighborhoods that occurred in an urban ordinance zone established in 2016 that required residents to secure anthropogenic food sources. Residents were supplied with BRC in 2017, and our surveys in 2017 and 2018 assessed the changes in HBI in the year before and after receiving BRC as well as the attitudes of residents toward ordinance measures and the perceived effectiveness of BRC. We found that a combination of preventive measures practiced by residents along with use of BRC effectively reduced HBI by 54%, especially bears eating garbage (reduced to 0%). Consequently, residents spent more time outdoors in their neighborhoods and experienced an elevated quality of life because fear of HBI lessened. We also analyzed public calls to the Florida Fish and Wildlife Conservation Commission concerning HBI. Public calls declined during the 5 years after the ordinance was established compared to 5 years prior. A reduction in HBI (especially conflicts) and public acceptance of using BRC is a long-term goal for management of black bears in Florida

Crystalline Silicate Emission in the Protostellar Binary Serpens--SVS20

We present spatially resolved mid-infrared spectroscopy of the class I/flat-spectrum protostellar binary system SVS20 in the Serpens cloud core. The spectra were obtained with the mid-infrared instrument T-ReCS on Gemini-South. SVS20-South, the more luminous of the two sources, exhibits a mid-infrared emission spectrum peaking near 11.3 \micron, while SVS20-North exhibits a shallow amorphous silicate absorption spectrum with a peak optical depth of $\tau \sim 0.3$. After removal of the the line-of-sight extinction by the molecular common envelope, the ``protostar-only'' spectra are found to be dominated by strong amorphous olivine emission peaking near 10 \micron. We also find evidence for emission from crystalline forsterite and enstatite associated with both SVS20-S and SVS20-N. The presence of crystalline silicate in such a young binary system indicates that the grain processing found in more evolved HAeBe and T Tauri pre-main sequence stars likely begins at a relatively young evolutionary stage, while mass accretion is still ongoing.Comment: Accepted for publication by The Astrophysical Journa

Training of Instrumentalists and Development of New Technologies on SOFIA

This white paper is submitted to the Astronomy and Astrophysics 2010 Decadal Survey (Astro2010)1 Committee on the State of the Profession to emphasize the potential of the Stratospheric Observatory for Infrared Astronomy (SOFIA) to contribute to the training of instrumentalists and observers, and to related technology developments. This potential goes beyond the primary mission of SOFIA, which is to carry out unique, high priority astronomical research. SOFIA is a Boeing 747SP aircraft with a 2.5 meter telescope. It will enable astronomical observations anywhere, any time, and at most wavelengths between 0.3 microns and 1.6 mm not accessible from ground-based observatories. These attributes, accruing from the mobility and flight altitude of SOFIA, guarantee a wealth of scientific return. Its instrument teams (nine in the first generation) and guest investigators will do suborbital astronomy in a shirt-sleeve environment. The project will invest $10M per year in science instrument development over a lifetime of 20 years. This, frequent flight opportunities, and operation that enables rapid changes of science instruments and hands-on in-flight access to the instruments, assure a unique and extensive potential - both for training young instrumentalists and for encouraging and deploying nascent technologies. Novel instruments covering optical, infrared, and submillimeter bands can be developed for and tested on SOFIA by their developers (including apprentices) for their own observations and for those of guest observers, to validate technologies and maximize observational effectiveness.Comment: 10 pages, no figures, White Paper for Astro 2010 Survey Committee on State of the Professio

Mid-Infrared Imaging of Candidate Vega-Like Systems

We have conducted deep mid-infrared imaging of a relatively nearby sample of candidate Vega-like stars using the OSCIR instrument on the CTIO 4-meter and Keck II 10-meter telescopes. Our discovery of a spatially-resolved disk around HR 4796A has already been reported (Jayawardhana et al. 1998). Here we present imaging observations of the other members of the sample, including the discovery that only the primary in the HD 35187 binary system appears to harbor a substantial circumstellar disk and the possible detection of extended disk emission around 49 Ceti. We derive global properties of the dust disks, place constraints on their sizes, and discuss several interesting cases in detail. Although our targets are believed to be main sequence stars, we note that several have large infrared excesses compared to prototype Vega-like systems, and may therefore be somewhat younger. The disk size constraints we derive, in many cases, imply emission from relatively large ($\gtrsim$ 10$\mu$m) particles at mid-infrared wavelengths.Comment: 15 pages and 2 PostScript figures, accepted for publication in The Astronomical Journa

Star Formation and Dynamics in the Galactic Centre

The centre of our Galaxy is one of the most studied and yet enigmatic places in the Universe. At a distance of about 8 kpc from our Sun, the Galactic centre (GC) is the ideal environment to study the extreme processes that take place in the vicinity of a supermassive black hole (SMBH). Despite the hostile environment, several tens of early-type stars populate the central parsec of our Galaxy. A fraction of them lie in a thin ring with mild eccentricity and inner radius ~0.04 pc, while the S-stars, i.e. the ~30 stars closest to the SMBH (<0.04 pc), have randomly oriented and highly eccentric orbits. The formation of such early-type stars has been a puzzle for a long time: molecular clouds should be tidally disrupted by the SMBH before they can fragment into stars. We review the main scenarios proposed to explain the formation and the dynamical evolution of the early-type stars in the GC. In particular, we discuss the most popular in situ scenarios (accretion disc fragmentation and molecular cloud disruption) and migration scenarios (star cluster inspiral and Hills mechanism). We focus on the most pressing challenges that must be faced to shed light on the process of star formation in the vicinity of a SMBH.Comment: 68 pages, 35 figures; invited review chapter, to be published in expanded form in Haardt, F., Gorini, V., Moschella, U. and Treves, A., 'Astrophysical Black Holes'. Lecture Notes in Physics. Springer 201

GTC/CanariCam Deep Mid-infrared Imaging Survey of Northern Stars within 5 pc

© 2021. The Author(s). Published by the American Astronomical Society. This is an open access article distributed under the Creative Commons Attribution License, to view a copy of the license, see: https://creativecommons.org/licenses/by/4.0/In this work we present the results of a direct imaging survey for brown dwarf companions around the nearest stars at the mid-infrared 10 micron range (λ c = 8.7 μm, Δλ = 1.1 μm) using the CanariCam instrument on the 10.4 m Gran Telescopio Canarias (GTC). We imaged the 25 nearest stellar systems within 5 pc of the Sun at declinations δ > −25° (at least half have planets from radial-velocity studies), reaching a mean detection limit of 11.3 ± 0.2 mag (1.5 mJy) in the Si-2 8.7 μm band over a range of angular separations from 1″ to 10″. This would have allowed us to uncover substellar companions at projected orbital separations between ∼2 and 50 au, with effective temperatures down to 600 K and masses greater than 30 M Jup assuming an average age of 5 Gyr and masses down to the deuterium-burning mass limit for objects with ages <1 Gyr. From the nondetection of such companions, we determined upper limits on their occurrence rate at depths and orbital separations yet unexplored by deep imaging programs. For the M dwarfs, the main component of our sample, we found with a 90% confidence level that fewer than 20% of these low-mass stars have L- and T-type brown dwarf companions with m ≳ 30 MJup and Teff ≳ 600 K at ∼3.5–35 au projected orbital separations.Peer reviewedFinal Published versio