Read the case of Foster v. Chatman. Analyze the types of racism prosecutors could deploy in jury selection.
Given the decision in Foster, discuss whether you think a Batson hearing is sufficient to prevent all of these
types of racism from happening.
Molecular clouds are dark, cold, dense regions of high extinction within the ISM. They confine the majority of the mass in the ISM and these clouds are the primary sites of star formation within the galaxy. Molecular clouds have a characteristic filamentary structure that is omnipresent across the ISM within both star forming regions and quiescent clouds, and these filaments share a high degree of universality in their properties. This however has not always been the case, as before the launch of the Herschel space telescope (1970-2010), Molecular clouds were thought to exhibit a discrete clump and core substructure. Filamentary properties had been observed in molecular clouds as early as the 1970’s, however, filamentary structure was not thought to be the fundamental morphology of the cold ISM; the pervading theory was one of hierarchical cloud structure, from clouds to clumps to cores. The formation of molecular clouds, their observed morphology and star forming regions is attributed to a number of factors in addition to their self-gravitating nature. Magnetic fields, like filaments, are known to be ubiquitous across the ISM and magnetism plays a fundamental role within the molecular ISM in both the formation of clouds and filaments and their subsequent evolution into clumped/star forming regions. Introduction Molecular clouds (MC’s) were first discovered in 1970 through spectroscopic observations of CO in the 2.6mm band in the Orion Cluster (Williams 1970) and the Lyman resonance-absorption bands of interstellar molecular hydrogen (H2) in Perseus (Carruthers 1970); observations of these star forming regions highlighted a hierarchical structure within the interstellar medium (ISM) that was first thought to comprise of cores embedded within clumps that were embedded within the larger MC’s. Clumps are an intermediate substructure with higher column densities than the parent MC, and cores are localised high column density structures within clumps. In recent decades, advances in spatial resolution has highlighted a filamentary substructure of MC’s that has redefined the morphology of gas in the ISM, irrespective of the presence of star forming regimes within them. The unprecedented discovery of the ubiquitous nature of filaments by the Herschel Space Telescope suggests there is an important connection between the structure within the ISM and the formation of pre-stellar cores and protostars, and that the formation of filaments is the first stage of the process of galactic stellar evolution. (Arzoumanian & Andre 2011) The presence of interstellar filaments and prestellar cores represent 2 two fundamental steps in the star formati>GET ANSWER