Investigation of Material Supply Strategies to Increase Resilience in Matrix Production Systems

In order to design a resilient production system, individual system elements have to be flexible and adapt towards changing requirements. In contrast to the prevailing paradigm that complexity in production systems is reduced by standardisation or cycle production, complexity in resilient production systems offers great potential in terms of adaptiveness, robustness and anticipation. Within production control, matrix production is seen as a resilient and versatile system. Flexible routing between work-stations makes it possible to compensate for failures more quickly in the event of a malfunction, flexible logistics and control processes allow the workstations to be controlled and used in a job-specific manner. In this paper, challenges and operating principles of material supply strategies are investigated that have the biggest influence on the design of resilient processes in matrix production. Using a simulation model and scenarios from the automotive sector, the potentials, requirements and parameters for describing resilience are specified

Investigation of Material Supply Strategies to Increase Resilience in Matrix Production Systems

In order to design a resilient production system, individual system elements have to be flexible and adapt towards changing requirements. In contrast to the prevailing paradigm that complexity in production systems is reduced by standardisation or cycle production, complexity in resilient production systems offers great potential in terms of adaptiveness, robustness and anticipation. Within production control, matrix production is seen as a resilient and versatile system. Flexible routing between work-stations makes it possible to compensate for failures more quickly in the event of a malfunction, flexible logistics and control processes allow the workstations to be controlled and used in a job-specific manner. In this paper, challenges and operating principles of material supply strategies are investigated that have the biggest influence on the design of resilient processes in matrix production. Using a simulation model and scenarios from the automotive sector, the potentials, requirements and parameters for describing resilience are specified

Guided sparse camera pose estimation

In this paper, we present an idea for a sparse approach to calculate camera poses from RGB images and laser distance measurements to perform subsequent facade reconstruction. The core idea is to guide the image recording process by choosing distinctive features with the laser range finder, e.g. building or window corners. From these distinctive features, we can establish correspondences between views to compute metrically accurate camera poses from just a few precise measurements. In our experiments, we achieve reasonable results in building facade reconstruction with only a fraction of features compared to standard structure from motion

The X-ray Size-Temperature Relation for Intermediate Redshift Galaxy Clusters

We present the first measurements of the X-ray size-temperature (ST) relation in intermediate redshift (z~0.30) galaxy clusters. We interpret the local ST relation (z~0.06) in terms of underlying scaling relations in the cluster dark matter properties, and then we use standard models for the redshift evolution of those dark matter properties to show that the ST relation does not evolve with redshift. We then use ROSAT HRI observations of 11 clusters to examine the intermediate redshift ST relation; for currently favored cosmological parameters, the intermediate redshift ST relation is consistent with that of local clusters. Finally, we use the ST relation and our evolution model to measure angular diameter distances; with these 11 distances we evaluate constraints on Omega_M and Omega_L which are consistent with those derived from studies of Type Ia supernovae. The data rule out a model with Omega_M=1 and Omega_L=0 with 2.5 sigma confidence. When limited to models where Omega_M+Omega_L=1, these data are inconsistent with Omega_M=1 with 3 sigma confidence.Comment: ApJ: submitted April 7, accepted June 28, to appear Dec 1 (vol 544

[μ-1,3-Bis(diphenyl­phosphino)propane-κ2 P:P′]bis­[bromidogold(I)]

The title compound, [Au2Br2(C27H26P2)], features linearly coordinated AuI atoms within P,Br-donor sets. The central portion of the mol­ecule is practically planar as quanti­fied by the Br–Au⋯Au–Br torsion angle of −169.9 (2)°. The P—Au—Br chromophores are twisted with respect to each other [dihedral angle = 52.3 (6)°]. The benzene rings on each P atom lie on either side of this plane. The Au atoms are positioned at the periphery of the mol­ecule, which facilitates the formation of Au⋯Au inter­actions [3.2575 (11) Å] that result in the formation of supra­molecular chains along the b-axis direction. The Au⋯Au inter­actions are responsible for the deviations from the ideal linear geometry for each Au atom

Cooling flow bulk motion corrections to the Sunyaev Zel'dovich effect

We study the influence of converging cooling flow bulk motions on the Sunyaev-Zel'dovich (SZ) effect. To that purpose we derive a modified Kompaneets equation which takes into account the contribution of the accelerated electron media of the cooling flow inside the cluster frame. The additional term is different from the usual kinematic SZ-effect, which depends linearly on the velocity, whereas the contribution described here is quadratic in the macroscopic electron fluid velocity, as measured in the cluster frame. For clusters with a large cooling flow mass deposition rate and/or a small central electron density, it turns out that this effect becomes relevant.Comment: accepted for publication in New Astronom

A Photometric and Kinematic Study of AWM 7

We have measured redshifts and Kron-Cousins R-band magnitudes for a sample of galaxies in the poor cluster AWM 7. We have measured redshifts for 172 galaxies; 106 of these are cluster members. We determine the luminosity function from a photometric survey of the central 1.2 h^{-1} x 1.2 h^{-1} Mpc. The LF has a bump at the bright end and a faint-end slope of \alpha = -1.37+-0.16, populated almost exclusively by absorption-line galaxies. The cluster velocity dispersion is lower in the core (\sim 530 km/s) than at the outskirts (\sim 680 km/s), consistent with the cooling flow seen in the X-ray. The cold core extends \sim 150 h^{-1} kpc from the cluster center. The Kron-Cousins R-band mass-to-light ratio of the system is 650+-170 h M_\odot/L_\odot, substantially lower than previous optical determinations, but consistent with most previous X-ray determinations. We adopt H_0 = 100 h km/s/Mpc throughout this paper; at the mean cluster redshift, (5247+-76 km/s), 1 h^{-1} Mpc subtends 65\farcm5.Comment: 37 pages, LaTeX, including 12 Figures and 1 Table. Accepted for publication in the Astronomical Journa

[μ-1,1′-Bis(diphenyl­phosphino)ferro­cene-κ2 P:P′]bis­[chloridogold(I)]–chloro­form–hexane (2/2/1)

In the title mixed solvate, [Au2Fe(C17H14P)2Cl2]·CHCl3·0.5CH3(CH2)4CH3, the hexane solvent mol­ecule is disposed about an inversion centre. The Au atoms exist within nearly ideal linear coordination defined by P,Cl-donor sets, and when viewed down the P⋯P axis the Au atoms are gauche to each other. In the crystal structure, the chloro­form solvent mol­ecule is associated with the complex via a C—H⋯Cl contact, and the hexane solvent mol­ecules occupy voids defined by the remaining components of the structure

Improved constraints on dark energy from Chandra X-ray observations of the largest relaxed galaxy clusters

We present constraints on the mean matter density, Omega_m, dark energy density, Omega_de, and the dark energy equation of state parameter, w, using Chandra measurements of the X-ray gas mass fraction (fgas) in 42 hot (kT>5keV), X-ray luminous, dynamically relaxed galaxy clusters spanning the redshift range 0.05<z<1.1. Using only the fgas data for the 6 lowest redshift clusters at z<0.15, for which dark energy has a negligible effect on the measurements, we measure Omega_m=0.28+-0.06 (68% confidence, using standard priors on the Hubble Constant, H_0, and mean baryon density, Omega_bh^2). Analyzing the data for all 42 clusters, employing only weak priors on H_0 and Omega_bh^2, we obtain a similar result on Omega_m and detect the effects of dark energy on the distances to the clusters at ~99.99% confidence, with Omega_de=0.86+-0.21 for a non-flat LCDM model. The detection of dark energy is comparable in significance to recent SNIa studies and represents strong, independent evidence for cosmic acceleration. Systematic scatter remains undetected in the fgas data, despite a weighted mean statistical scatter in the distance measurements of only ~5%. For a flat cosmology with constant w, we measure Omega_m=0.28+-0.06 and w=-1.14+-0.31. Combining the fgas data with independent constraints from CMB and SNIa studies removes the need for priors on Omega_bh^2 and H_0 and leads to tighter constraints: Omega_m=0.253+-0.021 and w=-0.98+-0.07 for the same constant-w model. More general analyses in which we relax the assumption of flatness and/or allow evolution in w remain consistent with the cosmological constant paradigm. Our analysis includes conservative allowances for systematic uncertainties. The small systematic scatter and tight constraints bode well for future dark energy studies using the fgas method. (Abridged)Comment: Published in MNRAS. 20 pages, 11 figures. The data and analysis code (in the form of a patch to CosmoMC) are now available at http://www.stanford.edu/~drapetti/fgas_module