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Entrepreneurship Support Programs (ESP) in engineering provide education, mentoring, and advising for emerging entrepreneurs and their ventures. The impact of ESPs on engineering students’ professional formation and the acquisition of different attributes—such as creativity, risk-taking, empathy, and curiosity—is largely unknown. Though the social sciences have a strong and robust history of studying many of the attributes, such as creativity and problem-solving, typically associated with entrepreneurship, there has been little connection between this foundational research and the work of ESPs. In fact, two separate systematic reviews have shown that most published work in STEM entrepreneurship education is not theoretically grounded and does not follow standards of quality research approaches in the social sciences. In an effort to bridge the gap between social scientists and engineering entrepreneurship practitioners, the authors are conducting a two-phase study. Phase 1 of the study involves conducting a Delphi study to identify the top entrepreneurial attributes of professionals and researchers who lead ESPs. Phase 2 of the study includes conducting workshops with social scientists who study the attributes and ESP leaders. The goal of the workshops is to identify assessment frameworks grounded in social science theory and literature that will guide the measurement of the attributes. This session will focus on the results of the Delphi phase. Delphi study is a common research technique used to achieve consensus among experts (Hasson, Keeney, and McKenna, 2000). Seventy-three participants who lead or have led an ESP, have conducted research in entrepreneurship education, or act as administrators for relevant entrepreneurship programs were invited to participate in the Delphi study. Of the 73 invited, 14 completed at least two rounds of the Delphi study. All participants were experts in the field of engineering entrepreneurship education. The Delphi Study comprised three rounds- brainstorming, narrowing, and ranking. Each phase of the Delphi asked participants to think about three different sets of attributes: 1) entrepreneurial attributes that they thought were important in the development of an entrepreneur, 2) attributes in becoming a successful professional, and 3) attributes in working in an inclusive workspace. In the brainstorming phase, participants were sent an online questionnaire and were asked to brainstorm as many attributes as they could think of. The results of the brainstorming questionnaire were consolidated and used to develop the narrowing questionnaire, where participants were asked to narrow all attributes to the top 10 key attributes The results from the narrowing questionnaire were then used to develop a ranking questionnaire, where participants were asked to rank the items on a scale of importance with 1 being the most important to 10 being the least important for each set of attributes. The results of the phase 3 questionnaire were analyzed to identify the attributes that were ranked the highest among a majority of the participants. This paper discusses the findings of the Delphi Study and its implications in assessing the impact of ESP on entrepreneur formation. 

Whitepaper for the 2023 NSAC Long Range Plan 

We report the characteristics of collisional plasma shocks formed during interactions between low density (ne≈1015 cm−3), low temperature (Te≈2 eV), high velocity (30 km s−1), plasma jets and stagnant plasma of similar parameters. This investigation seeks to probe the structure of shocks in multi-ion-species plasmas, in particular, the presence of gradient-driven ion species separation at the shock front. The railgun-accelerated jets utilized here have previously been shown to exist in a collisional regime with intra-jet collisional mean-free-path substantially smaller than jet size [Schneider et al., Plasma Sources Sci. Technol. 29, 045013 (2020)]. To induce collisions, a dielectric barrier is located downstream of the railgun to stagnate an initially supersonic plasma jet. Around the time of stagnation, the railgun emits a second jet which shortly collides with the stagnant plasma. The presence of a structure emitting in the UV-visible band is evident in high-speed photographs of the moments immediately following the arrival of the second jet at the stagnant plasma. Analysis of interferometric and spectroscopic data suggests that the observed increase in density from the jet to the post-collision plasma is consistent with the formation of a bow shock structure with a multi-millimeter-scale ion shock layer. 

Abstract Pulsar halos are regions around middle-aged pulsars extending out to tens of parsecs. The large extent of the halos and well-defined central cosmic-ray accelerators make this new class of Galactic sources an ideal laboratory for studying cosmic-ray transport. LHAASO J0621+3755 is a candidate pulsar halo associated with the middle-aged gamma-ray pulsar PSR J0622+3749. We observed LHAASO J0621+3755 with VERITAS and XMM-Newton in the TeV and X-ray bands, respectively. For this work, we developed a novel background estimation technique for imaging atmospheric Cherenkov telescope observations of such extended sources. No halo emission was detected with VERITAS (0.3–10 TeV) or XMM-Newton (2–7 keV) within 1^∘and $10^{\prime }$around PSR J0622+3749, respectively. Combined with the LHAASO Kilometer Square Array (KM2A) and Fermi-LAT data, VERITAS flux upper limits establish a spectral break at  ∼1–10 TeV, a unique feature compared with Geminga, the most studied pulsar halo. We model the gamma-ray spectrum and LHAASO-KM2A surface brightness as inverse Compton emission and find suppressed diffusion around the pulsar, similar to Geminga. A smaller diffusion suppression zone and harder electron injection spectrum than Geminga are necessary to reproduce the spectral cutoff. A magnetic field ≤1μG is required by our XMM-Newton observation and synchrotron spectral modeling, consistent with Geminga. Our findings support slower diffusion and lower magnetic field around pulsar halos than the Galactic averages, hinting at magnetohydrodynamic turbulence around pulsars. Additionally, we report the detection of an X-ray point source spatially coincident with PSR J0622+3749, whose periodicity is consistent with the gamma-ray spin period of 333.2 ms. The soft spectrum of this source suggests a thermal origin. 

Abstract Assuming Galactic cosmic rays originate in supernovae and the winds of massive stars, starburst galaxies should produce very-high-energy (VHE;E > 100 GeV) gamma-ray emission via the interaction of their copious quantities of cosmic rays with the large reservoirs of dense gas within the galaxies. Such VHE emission was detected by VERITAS from the starburst galaxy M82 in 2008–09. An extensive, multiyear campaign followed these initial observations, yielding a total of 254 hr of good-quality VERITAS data on M82. Leveraging modern analysis techniques and the larger exposure, these VERITAS data show a more statistically significant VHE signal (∼6.5 standard deviations,σ). The corresponding photon spectrum is well fit by a power law (Γ = 2.3 ± 0.3_stat ± 0.2_sys), and the observed integral flux isF(>450 GeV) = (3.2 ± 0.6_stat ± 0.6_sys) × 10⁻¹³cm⁻²s⁻¹, or ∼0.4% of the Crab Nebula flux above the same energy threshold. The improved VERITAS measurements, when combined with various multiwavelength data, enable modeling of the underlying emission and transport processes. A purely leptonic scenario is found to be a poor representation of the gamma-ray spectral energy distribution (SED). A lepto-hadronic scenario with cosmic rays following a power-law spectrum in momentum (indexs ≃ 2.25) and with significant bremsstrahlung below 1 GeV provides a good match to the observed SED. The synchrotron emission from the secondary electrons indicates that efficient nonradiative losses of cosmic-ray electrons may be related to advective escape from the starburst core. 

Abstract We present the design and performance of a four-phased radiofrequency (RF) carpet system for ion transport between 200–600 mbar, significantly higher than previously demonstrated RF carpet applications. The RF carpet, designed with a 160 $$\upmu $$ $\mu$m pitch, is applied to the lateral collection of ions in xenon at pressures up to 600 mbar. We demonstrate transport efficiency of caesium ions across varying pressures, and compare with microscopic simulations made in the SIMION package. The novel use of an N-phased RF carpet can achieve ion levitation and controlled lateral motion in a denser environment than is typical for RF ion transport in gases. This feature makes such carpets strong candidates for ion transport to single ion sensors envisaged for future neutrinoless double-beta decay experiments in xenon gas. 

Understanding the nature and identity of dark matter is a key goal in the physics community. In the case that TeV-scale dark matter particles decay or annihilate into standard model particles, very-high-energy (VHE) gamma rays (greater than 100 GeV) will be present in the final state. The Very Energetic Radiation Imaging Telescope Array System (VERITAS) is an imaging atmospheric Cherenkov telescope array that can indirectly detect VHE gamma rays in an energy range of 100 GeV to > 30 TeV. Dwarf spheroidal galaxies (dSphs) are ideal candidates in the search for dark matter due to their high dark matter content, high mass-to-light ratios, and their low gamma-ray fluxes from astrophysical processes. This study uses a legacy data set of 638 hours collected on 17 dSphs, built over 11 years with an observing strategy optimized according to the dark matter content of the targets. The study addresses a broad dark matter particle mass range, extending from 200 GeV to 30 PeV. In the absence of a detection, we set the upper limits on the dark matter velocity-weighted annihilation cross section 

Abstract In 2017 February, the blazar OJ 287 underwent a period of intense multiwavelength activity. It reached a new historic peak in the soft X-ray (0.3–10 keV) band, as measured by the Swift X-ray Telescope. This event coincides with a very-high-energy (VHE)γ-ray outburst that led VERITAS to detect emission above 100 GeV, with a detection significance of 10σ(from 2016 December 9 to 2017 March 31). The time-averaged VHEγ-ray spectrum was consistent with a soft power law (Γ = −3.81 ± 0.26) and an integral flux corresponding to ∼2.4% that of the Crab Nebula above the same energy. Contemporaneous data from multiple instruments across the electromagnetic spectrum reveal a complex flaring behavior, primarily in the soft X-ray and VHE bands. To investigate the possible origin of such an event, our study focuses on three distinct activity states: before, during, and after the 2017 February peak. The spectral energy distributions during these periods suggest the presence of at least two nonthermal emission zones, with the more compact one responsible for the observed flare. Broadband modeling results and observations of a new radio knot in the jet of OJ 287 in 2017 are consistent with a flare originating from a strong recollimation shock outside the radio core.