33 research outputs found
Temperature response of the cell cycle of Haplopappus gracilis in suspension culture and its significance to the G1 transition probability model
Pharmacokinetics in early drug discovery. The report recommendations of ECVAM Workshop 22.
Galaxy kinematics and mass calibration in massive SZE-selected galaxy clusters to z = 1.3
The galaxy phase-space distribution in galaxy clusters provides insights into the formation and evolution of cluster galaxies, and it can also be used to measure cluster mass profiles. We present a dynamical study based on 3c3000 passive, non-emission-line cluster galaxies drawn from 110 galaxy clusters. The galaxy clusters were selected using the Sunyaev-Zel'dovich effect (SZE) in the 2500 deg2 South Pole Telescope (SPT)-SZ survey and cover the redshift range 0.2 < z < 1.3. We model the clusters using the Jeans equation, while adopting NFW mass profiles and a broad range of velocity dispersion anisotropy profiles. The data prefer velocity dispersion anisotropy profiles that are approximately isotropic near the centre and increasingly radial toward the cluster virial radius, and this is true for all redshifts and masses we study. The pseudo-phase-space density profile of the passive galaxies is consistent with expectations for dark matter particles and subhaloes from cosmological N-body simulations. The dynamical mass constraints are in good agreement with external mass estimates of the SPT cluster sample from either weak lensing, velocity dispersions, or X-ray YX measurements. However, the dynamical masses are lower (at the 2.2\u3c3 level) when compared to the mass calibration favoured when fitting the SPT cluster data to a \u39bcold dark matter model with external cosmological priors, including cosmic microwave background anisotropy data from Planck. The discrepancy grows with redshift, where in the highest redshift bin the ratio of dynamical to SPT + Planck masses is \u3b7 = 0.63^{+0.13}_{-0.08}\ub1 0.06 (statistical and systematic), corresponding to a 2.6\u3c3 discrepancy
Variation in isomeric products of a phosphodiesterase from the chloroplasts of **Phaseolus vulgaris** in response to cations
Effects of annealing temperature on the alloying behavior of the AuGe-GaAs?100? interface
Water Chemistry Impact on Autogenous Metallic Pipe Leak Repair in Simulated Potable Water Systems
Deep Chandra, HST-COS, and Megacam Observations of the Phoenix Cluster: Extreme Star Formation and AGN Feedback on Hundred Kiloparsec Scales
We present new ultraviolet, optical, and X-ray data on the Phoenix galaxy cluster (SPT-CLJ2344-4243). Deep optical imaging reveals previously undetected filaments of star formation, extending to radii of ~50â100 kpc in multiple directions. Combined UV-optical spectroscopy of the central galaxy reveals a massive (2 Ă 109 Mâ), young (~4.5 Myr) population of stars, consistent with a time-averaged star formation rate of 610 ± 50 Mâ yrâ1. We report a strong detection of O vi λλ1032,1038, which appears to originate primarily in shock-heated gas, but may contain a substantial contribution (>1000 Mâ yrâ1) from the cooling intracluster medium (ICM). We confirm the presence of deep X-ray cavities in the inner ~10 kpc, which are among the most extreme examples of radio-mode feedback detected to date, implying jet powers of 2â7 Ă 1045 erg sâ1. We provide evidence that the active galactic nucleus inflating these cavities may have only recently transitioned from "quasar-mode" to "radio-mode," and may currently be insufficient to completely offset cooling. A model-subtracted residual X-ray image reveals evidence for prior episodes of strong radio-mode feedback at radii of ~100 kpc, with extended "ghost" cavities indicating a prior epoch of feedback roughly 100 Myr ago. This residual image also exhibits significant asymmetry in the inner ~200 kpc (0.15R500), reminiscent of infalling cool clouds, either due to minor mergers or fragmentation of the cooling ICM. Taken together, these data reveal a rapidly evolving cool core which is rich with structure (both spatially and in temperature), is subject to a variety of highly energetic processes, and yet is cooling rapidly and forming stars along thin, narrow filaments