We probe in some depth into the structure of eleven-dimensional, osp(32|1)-based Chern-Simons supergravity, as put forward by Troncoso and Zanelli (TZ) in 1997. Moliner 50, 46100 Burjassot, Valencia (Spain) Rodriguez, Eduardo, E-mail: [Departamento de Matematica y Fisica Aplicadas, Universidad Catolica de la Santisima Concepcion, Alonso de Ribera 2850, 4090541 Concepcion (Chile) (Mexico) Departament de Fisica Teorica, Universitat de Valencia, C/ Dr. Izaurieta, Fernando, E-mail: [Departamento de Matematica y Fisica Aplicadas, Universidad Catolica de la Santisima Concepcion, Alonso de Ribera 2850, 4090541 Concepcion (Chile) Instituto de Matematicas, Universidad Nacional Autonoma de Mexico, Av. On eleven-dimensional supergravity and Chern-Simons theory The eleven-dimensional origin of the resulting non-linear structures is parameterized by the choice of a complex spinor on Y encoding the off-shell 4D N = 1 subalgebra of the eleven-dimensional super-Poincaré algebra. In this paper, we compute the O(Ψ) action to all orders in the remaining fields. These terms are those of lowest order in a superspace Noether expansion in seven N = 1 conformal gravitino superfields Ψ. This chiral field is part of a tensor hierarchy giving rise to a superspace Chern-Simons action and its real field strength defines a lifting of the Hitchin functional on Y to the G 2 superspace X Ã- Y. The eleven-dimensional 3-form and the stable 3-form on Y define the lowest component of a gauge superfield on X Ã- Y that is chiral as a superfield on X. N = 1 supercurrents of eleven-dimensional supergravityīecker, Katrin Becker, Melanie Butter, Daniel Linch, William D.Įleven-dimensional supergravity can be formulated in superspaces locally of the form X Ã- Y where X is 4D N = 1 conformal superspace and Y is an arbitrary 7-manifold admitting a G 2-structure. International Nuclear Information System (INIS) The population of blue stragglers and blue horizontal branch stars varies along the stream and is a potential probe of the distribution of stellar populations in the Sagittarius dwarf galaxy prior to disruption. Great circle counts and comparisons with theoretical models suggest that the Sagittarius stream comprises 10%-17% of the halo stars in the HVS sample. Applying our method to halo stars in the Hypervelocity Star (HVS) survey, we detect the Sagittarius stream at high significance. The radial velocities enable construction of a more powerful joint statistical test for identifying star streams in the Milky Way halo. Comparisons between the radial velocity distribution within a great circle and the radial velocity distribution of the entire sample also measure the statistical significance of potential streams. Within a great circle, departures of the observed spatial distribution from random provide a measure of the likelihood of a potential star stream. We develop statistical methods for identifying star streams in the halo of the Milky Way that exploit observed spatial and radial velocity distributions. Kenyon, Scott J., E-mail: E-mail: E-mail: E-mail: [Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138 (United States) IDENTIFYING STAR STREAMS IN THE MILKY WAY HALOĮnergy Technology Data Exchange (ETDEWEB)
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