Figure 1: Invariant mass distributions of the reconstructed Bc± → J/ψπ± candidates in 7 TeV data (top) and in 8 TeV data (bottom). The data are represented by the points with error bars (statistical only). The solid line is the projection of the results of the unbinned maximum likelihood fit to all candidates in the mass range 5620–6820 MeV. The dashed line is the projection of the background component of the same fit. [From G. Aad et al.
On November 14, 2014, experts from fields as far-ranging as human cognitive neuroscience and neural computation, animal life science, anthropology and culture, space science, current and future technology, and emergency management converged on Radcliffe’s annual Science Symposium to conduct a broad, cross-disciplinary investigation of navigation and way-finding.
Fig 1: Dusty olivine-bearing chondrules from the Semarkona meteorite. Optical photomicrograph of chondrule DOC4 showing the location of dusty olivine grains. Image taken in reflected light with crossed polarizers. [From: Roger R. Fu, et al., "Solar nebula magnetic fields recorded in the Semarkona meteorite," Science DOI: 10.1126/science.1258022. Reprinted with permission from AAAS.]
Figure 8:An example of a microfabricated array of TES bolometers, an 88 pixel, dual polarization TES bolometer array made at NIST for the SPTpol experiment. TES detectors are micro-machined from thin films deposited on silicon wafer substrates which means TES-based devices are fundamentally fabricated as arrays. [from K.N. Abazajian, et al., "Neutrino physics from the cosmic microwave background and large scale structure," Astroparticle Physics, v. 63.]