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Fire suppression, combined with lack of forest thinning and short-rotation, monodominant management, has drastically altered the landscape in the southeastern U.S., leading to the loss of open pine ecosystems and associated avian species. Management of open pine ecosystems is a common practice; yet, there remains uncertainty regarding how vegetation structure impacts priority species. Using empirical data, I assessed changes in species abundance and associated vegetation characteristics before and after management. I also sought to identify vegetation characteristics that influence home range establishment and microhabitat selection of Bachman’s Sparrows. Priority species were negatively associated with hardwood midstory and abundance per site increased following management. Home range establishment of Bachman’s Sparrows was influenced by disturbance, canopy cover, and slope, while microhabitat selection was influenced by pine basal area, available perching options, vegetation density, and herbaceous groundcover. Understanding how vegetation structure impacts priority species may be helpful in guiding conservation and management efforts.

Duration tuning in the mammalian inferior colliculus (IC) is created by the interaction of excitatory and inhibitory synaptic inputs. We used extracellular recording and paired-tone stimulation to measure the strength and time-course of the contralateral inhibition and offset-evoked excitation underlying duration-tuned neurons (DTNs) in the IC of the awake bat. The onset time of a short, best duration (BD), excitatory probe tone was varied relative to the onset of a longer-duration, non-excitatory (NE) suppressor tone. Spikes evoked by the roving BD tone were suppressed or facilitated when the stationary NE tone was varied in frequency or amplitude. When the NE tone frequency was presented away from the cell’s best excitatory frequency (BEF) or at lower SPLs, the onset of inhibition was relatively constant whereas the offset and duration of inhibition decreased. Excitatory and inhibitory frequency response areas were measured and best inhibitory frequencies matched best excitatory frequencies; however, inhibitory bandwidths were broader than excitatory bandwidths. Excitatory rate-level and inhibitory suppression-level functions were also measured and the dynamic ranges and inflection points were similar, which is hypothesized to play a role in the level tolerance of responses measured from DTNs. We compared the latency of offset-locked facilitation to the onset or offset of inhibition as a function of frequency and amplitude; we found that the facilitation was more related to the onset of inhibition. Moreover, facilitation typically preceded the offset of inhibition – suggesting that it is a separate excitatory input to DTNs and not a rebound from inhibition. We conclude that DTNs receive inputs that generate and preserve temporal selectivity. / Dissertation / Doctor of Philosophy (PhD)

Les naines brunes sont définies comme des objets généralement plus massifs que les planètes géantes, mais qui demeurent moins massifs que les plus petites étoiles. Étant incapables de fusionner de l’hydrogène en hélium comme les étoiles de la séquence principale en raison de leur faible masse, les naines brunes rayonnent seulement leur chaleur initiale de formation et se refroidissent continuellement au fil du temps. Cette perpétuelle diminution en luminosité introduit une dégénérescence entre leurs propriétés physiques, car il devient impossible de distinguer par sa seule luminosité une jeune naine brune massive de celle d’une vielle naine brune moins massive. Une modélisation atmosphérique et évolutive devient donc nécessaire pour contraindre les propriétés physiques (masse, rayon, âge, température effective, métallicité) des naines brunes sans compagnons, où seulement la luminosité peut être mesurée directement. Le flux émergeant de ces modèles semble bien reproduire ceux des naines brunes observées jusqu’à présent. Cependant, les paramètres physiques qu’ils prédisent demeurent sans calibration empirique, car il n’existe pas suffisamment de mesures indépendantes de ces paramètres venant de naines brunes observées qui permettrait de vérifier les prédictions des modèles. L’étude de naines brunes binaires éclipsant une étoile ouvre la possibilité de prendre des mesures directes de ses caractéristiques physiques via des analyses de vitesses radiales, de transits et d’éclipses secondaires, le tout de manière indépendante des modèles. Ce mémoire porte sur l’étude d’une naine brune binaire éclipsante découverte en 2011 via photométrie de transit par le télescope Kepler: LHS 6343 C. Des observations de transit (Kepler) en plus d’observations de vitesses radiales (Keck/HIRES) et d’éclipses secondaires (Kepler, HST, Spitzer) permettent la mesure directe de tous ses paramètres physiques importants sauf l’âge. Ce mémoire apporte une première analyse des données d’éclipse secondaire HST pour obtenir un spectre d’émission de la naine brune dans la bande passante WFC3-G141 (1.1 à 1.7 µm), permettant d’identifier un type spectrale de T1.5. De plus, ce mémoire met à jour la masse et le rayon de LHS 6343 C en utilisant une distance Gaia DR3 et des relations stellaires empiriques. Ce nouvel ensemble de paramètres est ensuite comparé à ceux prédits par des modèles atmosphériques, où l’on trouve que ceux en déséquilibre chimique reproduisent mieux les données comparés à ceux en équilibre chimique. Finalement, des modèles d’évolution sont utilisés pour déterminer l’âge de la naine brune. / Brown dwarfs are defined as substellar objects that are generally more massive than giant planets, but which remain less massive than the smallest stars. Being unable to fuse hydrogen into helium like main-sequence stars due to their low mass, brown dwarfs do not have access to a long-term energy source. They therefore radiate only their initial heat of formation and cool continuously over time. This perpetual decrease in luminosity introduces a degeneracy between their physical properties, making it impossible to distinguish a young massive brown dwarf from an older less massive one based on their luminosity and spectra alone. Therefore, atmospheric and evolutionary modelling becomes necessary to obtain other properties (e.g. mass, radius, age, effective temperature) of field brown dwarfs, since only their luminosity can be measured directly. Fortunately, the luminosities and spectra of the best models reproduce observations well. However, the physical parameters they predict (i.e. mass, radius, effective temperature, metallicity) lack an empirical calibration; i.e. there are not enough independent measurements of these parameters to meaningfully confirm the predictive power of models. One of the scenarios allowing the direct measurement of several physical characteristics is provided by brown dwarf eclipsing binaries (BDEB), i.e. a brown dwarf orbiting a star. With radial velocity, transit, and secondary eclipse analyses, all but the age of a BDEB can be determined independently of models. This thesis pertains to the study of a minimally irradiated BDEB, LHS 6343 C, discovered in 2011 via transit photometry by the Kepler telescope. Since its discovery, a greater amount of transit (Kepler) observations in addition to radial velocity (Keck/HIRES) and secondary eclipse (Kepler, HST, Spitzer) observations allow for everything but an age measurement to be obtained. This thesis provides a first analysis of the HST secondary eclipse data to obtain a brown dwarf emission spectrum in the WFC3-G141 filter (1.1 to 1.7 µm), identifying it as a T1.5 dwarf. In addition, this thesis updates the physical parameters of previous studies using a Gaia DR3 distance and empirical stellar relations. This new set of parameters is then compared to those predicted by atmospheric models, where those in chemical nonequilibrium reproduce the observed flux better than chemical equilibrium or cloud models. Finally, evolutionary models are used to determine the age of the brown dwarf.