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The interannual El Niño-Southern Oscillation (ENSO) triggers extreme climate events worldwide. Geochemical proxies in coral skeletons from the eastern equatorial Pacific (EP) track ENSO conditions, constraining its long-term variance and response to forcing. Multiproxy analysis of three subfossil colonies from the EP Galápagos Islands finds ENSO variability ~4000 years before present (BP) was similar to that from 1959-1979 CE. These mid-Holocene results exhibit stronger ENSO variability than that over the preindustrial last millennium, but weaker than that between 1986-2016 CE. Whereas positively skewed instrumental and reconstructed temperatures reveal the predominance of warm ENSO events in the modern EP, the corals from 4000 BP record negatively skewed variance reflecting stronger cold events. The Galápagos results contrast with central equatorial Pacific (CP) coral records identifying minimal ENSO variance from 5000-3000 BP. Stronger cold events in the EP likely limited CP ENSO variability, creating spatially diverse ENSO signals at 4000 BP. 

As science fields enter the Big Data revolution, open-access repositories are essential for addressing larger-scale questions than are possible for single researchers by making data findable, accessible, interoperable, and reusable (FAIR). Furthermore, transparent data and code are increasingly important for reproducible research, especially for data types that inherently require subjective human interpretations. These ideas are applicable to coral sclerochronology, as the field has long been characterized by individual researchers collecting and analyzing coral skeletal cores from their study sites without substantial data sharing or archiving of the core images to meet FAIR principles. Here, we present CoralCache, a virtual coral core repository that not only archives image datasets (i.e., digitized X-rays and computed tomography scans), but also observer interpretations of the density banding patterns. CoralCache is linked to a graphical user interface, CoralCT, which together offer a way forward for coral growth rate analysis that is reproducible and collaborative. The data organization systems presented here could also be readily applied to related archives such as tree rings or bivalve shells. 

Context.Superluminous supernovae (SLSNe) are a rare class of transients with peak luminosities 10–100 times greater than those of standard core-collapse supernovae (SNe). The mechanisms powering their extreme brightness remain debated, with circumstellar medium (CSM) interaction, or energy injection from a central engine like a magnetar wind nebula being the most plausible scenarios. While the optical properties of SLSNe are extensively studied, theirγ-ray signatures remain poorly constrained. Aims.To further constrain the underlying mechanism, we carried out a systematic search for giga-electronvoltγ-ray emission using theFermiLarge Area Telescope (LAT) from a sample of nearby hydrogen-poor (Type I) and hydrogen-rich (Type II) SLSNe over the past 16 years. Our objective is to test predictions from CSM and magnetar models, and to assess the prospects for future detections with the Cherenkov Telescope Array Observatory (CTAO). Methods.For the six targets of this sample, we studied the time variability of a putativeγ-ray signal at the optical position of the SLSN on a six-month timescale, and in the case of SN 2017egm, we further investigated variability on 15-day intervals and applied a Bayesian block algorithm to characterize the time variability of the signal. We then compared the temporal evolution and spectral properties to the predictions from a magnetar and CSM interaction model. Results.Among the sample, only SN 2017egm shows significantγ-ray emission, with likelihood test statistic (TS) values of 26–33 (i.e., > 5σ) depending on the adopted time window. The signal arises between 50 and 160 days after explosion and is well described by a power-law spectrum with index Γ = 2.17 ± 0.23. The emission is consistent both in terms of its light curve and its spectrum, with predictions from magnetar models requiring either low nebular magnetization or faster spin-down than dipole losses. The CSM shell interaction scenario can reproduce the observed flux level but not the observed timing of theγ-ray signal. In addition, the observed ratio,L_γ/L_opt ∼ 1, is inconsistent with theoretical expectations and not in line with ratio measurements in other interacting CSM-dominated objects (e.g., novae or SNe) where this ratio is less than 10⁻². Conclusions.Our study strongly suggests that a central engine like a magnetar plays a key role in this SLSN and could explain the bulk of the optical andγ-ray light curves properties. In order to explain the observed late-time bumps in the optical light curve of SN 2017egm, we require either: a hybrid picture combining magnetar and multiple CSM shells for the optical bumps or a pure magnetar model with infalling matter on an accretion disk. Finally, simulations of 50 hours of CTAO observations indicate that a SN 2017egm-like event would be detectable up to ∼140 Mpc in the magnetar model but not in the CSM model due to strongγ − γabsorption. 

The STEM Center at Sam Houston State University (SHSU) has received funding from the National Science Foundation (NSF - IUSE) and was established in 2017. The STEM Center seeks to increase the number and quality of STEM graduates by establishing a strong foundation for learning using innovative teaching practices, supporting students in finding research and internship opportunities, and building lifelong skills needed for advancement and leadership in STEM careers. The center is in one of the STEM buildings with two fully equipped classrooms and office space for full-time staff members. The center staff collaborates with university-wide programs to promote STEM education and contribute to the university’s quality enhancement plan (QEP). The paper shares details regarding faculty and student involvement, the development of preparatory courses, institution-wide resources, and student outcomes from the project with the academic community. 

Abstract One of the most poorly understood aspects of low-mass star formation is how multiple-star systems are formed. Here we present the results of Atacama Large Millimeter/submillimeter Array (ALMA) Band 6 observations toward a forming quadruple protostellar system, G206.93-16.61E2, in the Orion B molecular cloud. ALMA 1.3 mm continuum emission reveals four compact objects, of which two are Class I young stellar objects and the other two are likely in prestellar phase. The 1.3 mm continuum emission also shows three asymmetric ribbon-like structures that are connected to the four objects, with lengths ranging from ∼500 to ∼2200 au. By comparing our data with magnetohydrodynamic simulations, we suggest that these ribbons trace accretion flows and also function as gas bridges connecting the member protostars. Additionally, ALMA CO J = 2−1 line emission reveals a complicated molecular outflow associated with G206.93-16.61E2, with arc-like structures suggestive of an outflow cavity viewed pole-on.