#STARS BEYOND CONTACT VERIFICATION#

Joeckel was notified that his contract renewal was suspended pending further inquiry into a parent complaint that his unit on racial justice constituted “indoctrination.” He has been teaching at the university for over twenty years and claims that the racial justice unit had been a part of his syllabus for twelve years without complaint. doi/10.1126/science.The indirect effect of DeSantis’ rhetoric on race and higher education has also surrounded recent disciplinary action leveled against Samuel Joeckel, a professor of English at Palm Beach Atlantic University, a private Christian college in West Palm Beach, Florida. Grains that have O isotopic compositions that deviate from solar compositions by at least 3σ are identified as stardust. Final isotopic ratios and uncertainties were determined according to standard procedures. The standard deviations of the isotopic compositions of these “standard subgrains” were taken into account in the determination of the final measurement uncertainty. The data were corrected for discrimination (which is dominated by the varying sensitivities of the detectors) layer by layer for each subgrain, taking the weighted mean oxygen isotopic ratios of the subgrains as the solar values ( 16O/ 17O = 2610, 16O/ 18O = 498.7). However, within a small field of view (20 μm), the variations in the measured isotopic compositions of standard materials are not substantially greater than is expected from counting error. In similar measurements of solar materials (μm-sized Burma spinel grains, enstatite grains, and Murchison matrix), we have found that in some cases the instrumental mass discrimination is sensitive to the sample stage position for given tuning conditions. Thin sections were coated with 50 Å of Au or C to avoid sample charging. The magnetic field was controlled with a nuclear magnetic resonance probe, which kept peak positions stable to ΔM/M < 5 ppm. Image acquisition times ranged from 3 to 10 hours, consuming 30 to 100 nm of surface material. High-mass-resolution scans were acquired on each sample before analysis in order to ensure that the contribution of 16OH – to the 17O – peak was less than 1‰, with a mass-resolving power of at least 9000 (Cameca definition), or ∼6000 in the conventional definition.

#STARS BEYOND CONTACT VERIFICATION#

Multiple (5 to 20) image scans were acquired for each sample in order to provide verification of any apparent anomalies. In most cases, the images were acquired by rastering a ∼2-pA 16-KeV Cs + primary ion beam over areas ∼10 × 10 μm, while simultaneously acquiring 16,17,18O –, 28Si –, and 24Mg 16O – secondary ion counts with five electron multipliers. The nomenclature refers to the large area collector number (e.g., L2005), followed by the cluster IDP number (e.g., C13 = cluster 13).

Stars beyond contact