The youngest low-mass protostars are known to be chemically rich, accreting matter most vigorously, and producing the most powerful outflows. Molecules are unique tracers of these phenomena. We use ALMA to study several outflow sources in the Serpens Main region. The most luminous source, Ser-SMM1, shows the richest chemical composition, but some complex molecules are also present in S68N. No emission from complex organics is detected toward Ser-emb 8N, which is the least luminous in the sample. We discuss whether these differences reflect an evolutionary effect or whether they are due to different physical structures. We also analyze the outflow structure from these young protostars by comparing emission of CO and SiO. EHV molecular jets originating from SMM1-a,b and Ser-emb 8N contrast with no such activity from S68N, which on the other hand presents a complex outflow structure.

Due to the wide bandgap and other key materials properties of 4H-SiC, SiC MOSFETs offer performance advantages over competing Si-based power devices. For example, SiC can more easily be used to fabricate MOSFETs with very high voltage ratings, and with lower switching losses. Silicon carbide power MOSFET development has progressed rapidly since the market release of Cree’s 1200V 4H-SiC power MOSFET in 2011. This is due to continued advancements in SiC substrate quality, epitaxial growth capabilities, and device processing. For example, high-quality epitaxial growth of thick, low-doped SiC has enabled the fabrication of SiC MOSFETs capable of blocking extremely high voltages (up to 15kV); while dopant control for thin highly-doped epitaxial layers has helped enable low on-resistance 900V SiC MOSFET production. Device design and processing improvements have resulted in lower MOSFET specific on-resistance for each successive device generation. SiC MOSFETs have been shown to have a long device lifetime, based on the results of accelerated lifetime testing, such as high-temperature reverse-bias (HTRB) stress and time-dependent dielectric breakdown (TDDB).

An integrated experimental – simulation – control theory approach designed to enable adaptive control of microstructural evolution in polycrystalline metals is described. A micro-heater array, containing ten addressable channels, is used to create desired temperature profiles across thin polycrystalline films in situ to a scanning electron microscope (SEM). The goal is that on heating with controlled temperature profiles, the evolution of grain growth within the film can be continuously monitored and compared to Monte Carlo simulations of trajectories towards a desired microstructure. Feed-forward and feedback control strategies are then used to guide the microstructure along the desired trajectory.

The Milky Way appears as a typical barred spiral, and comparisons can be made between its nuclear region and those of structurally similar nearby spirals. Maffei 2, M83, IC 342 and NGC 253 are nearby systems whose nuclear region properties contrast with those of the Milky Way. Stellar masses derived from NIR photometery, molecular gas masses and star formation rates allow us to assess the evolutionary states of this set of nuclear regions. These data suggest similarities between nuclear regions in terms of their stellar content while highlighting significant differences in current star formation rates. In particular current star formation rates appear to cover a larger range than expected based on the molecular gas masses. This behavior is consistent with nuclear region star formation experiencing episodic variations. Under this hypothesis the Milky Way's nuclear region currently may be in a low star formation rate phase.

Recent excavations at two sites located along the coastal margin of the Los Angeles basin revealed three features created as a result of communal mourning ritual during the Intermediate Period (ca. 3000–1000 cal B.P.). Detailed analysis of constituents, structure, and context indicates that formation of these dense concentrations of ground stone implements, unmodified cobbles, other artifacts, and cremated human remains involved deliberate equipment production, sequential implement fragmentation and treatment including burning and pigmentation of items, and secondary interment of incomplete objects and bodies in pits within locales often used for this purpose over many generations. The large size and evident manipulation of objects as part of communal mourning ritual indicates that actions would have been readily visible to a gathered assembly. Thus, while the meaning and significance of these practices remains to be thoroughly explored, the data suggest that communal mourning ritual may have played a significant role in community-building and the maintenance of identity within a region with a dynamic population history.

Starting from first principles, we construct a simple model for the evolution of energetic particles produced by supernovae in the starburst galaxy M82. The supernova rate, geometry, and properties of the interstellar medium are all well observed in this nearby galaxy. Assuming a uniform interstellar medium and constant cosmic-ray injection rate, we estimate the cosmic-ray proton and primary & secondary electron/positron populations. From these particle spectra, we predict the gamma ray flux and the radio synchrotron spectrum. The model is then compared to the observed radio and gamma-ray spectra of M82 as well as previous models by Torres (2004), Persic et al. (2008), and de Cea del Pozo et al. (2009). Through this project, we aim to build a better understanding of the calorimeter model, in which energetic particle fluxes reflect supernova rates, and a better understanding of the radio-FIR correlation in galaxies.