SZE Observables, Pressure Profiles and Center Offsets in Magneticum Simulation Galaxy Clusters

We present a detailed study of the galaxy cluster thermal \ac{sze} signal $Y$ and pressure profiles using {\it Magneticum} Pathfinder hydrodynamical simulations. With a sample of 50,000 galaxy clusters ($M_{\rm 500c}>1.4\times10^{14} \rm M_{\odot}$) out to $z=2$, we find significant variations in the shape of the pressure profile with mass and redshift and present a new generalized NFW model that follows these trends. We show that the thermal pressure at $R_{\rm 500c}$ accounts for only 80~percent of the pressure required to maintain hydrostatic equilibrium, and therefore even idealized hydrostatic mass estimates would be biased at the 20~percent level. We compare the cluster \ac{sze} signal extracted from a sphere with different virial-like radii, a virial cylinder within a narrow redshift slice and the full light cone, confirming small scatter ($\sigma_{\ln Y}\simeq 0.087$) in the sphere and showing that structure immediately surrounding clusters increases the scatter and strengthens non self-similar redshift evolution in the cylinder. Uncorrelated large scale structure along the line of sight leads to an increase in the \ac{sze} signal and scatter that is more pronounced for low mass clusters, resulting in non self-similar trends in both mass and redshift and a mass dependent scatter that is $\sim0.16$ at low masses. The scatter distribution is consistent with log-normal in all cases. We present a model of the offsets between the center of the gravitational potential and the \ac{sze} center that follows the variations with cluster mass and redshift.Comment: 20 pages, 15 figures, submitted to MNRA

They\u27re Wearing \u27Em Higher in Hawaii (Higher-Higher-Higher)

https://digitalcommons.library.umaine.edu/mmb-vp/6270/thumbnail.jp

Paul Revere : Won\u27t You Ride For Us Again?

https://digitalcommons.library.umaine.edu/mmb-vp/5508/thumbnail.jp

Lookout Mountain

https://digitalcommons.library.umaine.edu/mmb-vp/4352/thumbnail.jp

Liberty Bell : It\u27s Time To Ring Again

https://digitalcommons.library.umaine.edu/mmb-vp/1980/thumbnail.jp

Liberty Bell

[Verse 1] You have rested, Liberty Bell, For a hundred years and more, End your slumbers, Liberty Bell, Ring as you did before, It’s time to wake ‘em up, It’s time to shake ‘em up, It’s a cause worth ringing for: [Chorus] Liberty Bell, It’s time to ring again, Liberty Bell, It’s time to swing again, We’re in the same sort of fix We were in Seventy six And we are ready to mix and rally ‘round you Like we did before, Oh! Liberty Bell, Your voice is needed now, Liberty Bell, We’ll hear your call one and all, Though you’re old and there’s a crack in you Don’t forget Old Glory’s backin’ you Oh! Liberty Bell, it’s time to ring again. [Verse 2] Once you rang out, Liberty Bell, As we watched Old Glory wave, You have made us, Liberty Bell, Land of the free and brave It’s time to sing again, It’s time to ring again For the cause you’ve got to save: [Chorus

The Lifetime and Powers of FR IIs in Galaxy Clusters

We have identified and studied a sample of 151 FR IIs found in brightest cluster galaxies (BCGs) in the MaxBCG cluster catalog with data from FIRST and NVSS. We have compared the radio luminosities and projected lengths of these FR IIs to the projected length distribution of a range of mock catalogs generated by an FR II model and estimate the FR II lifetime to be 1.9 x 10^8 yr. The uncertainty in the lifetime calculation is a factor of two, due primarily to uncertainties in the ICM density and the FR II axial ratio. We furthermore measure the jet power distribution of FR IIs in BCGs and find that it is well described by a log-normal distribution with a median power of 1.1 x 10^37 W and a coefficient of variation of 2.2. These jet powers are nearly linearly related to the observed luminosities, and this relation is steeper than many other estimates, although it is dependent on the jet model. We investigate correlations between FR II and cluster properties and find that galaxy luminosity is correlated with jet power. This implies that jet power is also correlated with black hole mass, as the stellar luminosity of a BCG should be a good proxy for its spheroid mass and therefore the black hole mass. Jet power, however, is not correlated with cluster richness, nor is FR II lifetime strongly correlated with any cluster properties. We calculate the enthalpy of the lobes to examine the impact of the FR IIs on the ICM and find that heating due to adiabatic expansion is too small to offset radiative cooling by a factor of at least six. In contrast, the jet power is approximately an order of magnitude larger than required to counteract cooling. We conclude that if feedback from FR IIs offsets cooling of the ICM, then heating must be primarily due to another mechanism associated with FR II expansion.Comment: 22 pages, 20 figures. Accepted to ApJ. Added minor clarifications throughout the paper and restructured section 6.2 in response to the referee. A brief video explaining the paper can be found at http://youtu.be/DOq85qUSU-

Dynamic Line Rating Oncor Electric Delivery Smart Grid Program

Electric transmission lines are the lifeline of the electric utility industry, delivering its product from source to consumer. This critical infrastructure is often constrained such that there is inadequate capacity on existing transmission lines to efficiently deliver the power to meet demand in certain areas or to transport energy from high-generation areas to high-consumption regions. When this happens, the cost of the energy rises; more costly sources of power are used to meet the demand or the system operates less reliably. These economic impacts are known as congestion, and they can amount to substantial dollars for any time frame of reference: hour, day or year. There are several solutions to the transmission constraint problem, including: construction of new generation, construction of new transmission facilities, rebuilding and reconductoring of existing transmission assets, and Dynamic Line Rating (DLR). All of these options except DLR are capital intensive, have long lead times and often experience strong public and regulatory opposition. The Smart Grid Demonstration Program (SGDP) project co-funded by the Department of Energy (DOE) and Oncor Electric Delivery Company developed and deployed the most extensive and advanced DLR installation to demonstrate that DLR technology is capable of resolving many transmission capacity constraint problems with a system that is reliable, safe and very cost competitive. The SGDP DLR deployment is the first application of DLR technology to feed transmission line real-time dynamic ratings directly into the system operation’s State Estimator and load dispatch program, which optimizes the matching of generation with load demand on a security, reliability and economic basis. The integrated Dynamic Line Rating (iDLR)1 collects transmission line parameters at remote locations on the lines, calculates the real-time line rating based on the equivalent conductor temperature, ambient temperature and influence of wind and solar radiation on the stringing section, transmits the data to the Transmission Energy Management System, validates its integrity and passes it on to Oncor and ERCOT (Electric Reliability Council of Texas) respective system operations. The iDLR system is automatic and transparent to ERCOT System Operations, i.e., it operates in parallel with all other system status telemetry collected through Supervisory Control and Data Acquisition (SCADA) employed across the company

ECSGS Management Plan

Version 0.9 reviewed by ESA at the Euclid SGS Preliminary Requirements Review (2013) Version 1.9 reviewed by ESA at the Euclid SGS System Requirements Review (2015)The ECSGS Management Plan is focused on the following topics: ECSGS organisation, responsibilities, reporting; ECSGS costing, manpower, effort tracking; ECSGS logistic (when relevant); organisation of individual OUs and SDCs under ECSGS coordination. Sections 9 and 10 contain global and local organisation details, and the names of responsible staff. The management principles expressed in this document are a coherent extension of those described in the ECSGS Science Implementation Plan. The document is compliant with the ECSS standards, as tailored for the Euclid SGS

Differential cross section measurements for the production of a W boson in association with jets in proton–proton collisions at √s = 7 TeV

Measurements are reported of differential cross sections for the production of a W boson, which decays into a muon and a neutrino, in association with jets, as a function of several variables, including the transverse momenta (pT) and pseudorapidities of the four leading jets, the scalar sum of jet transverse momenta (HT), and the difference in azimuthal angle between the directions of each jet and the muon. The data sample of pp collisions at a centre-of-mass energy of 7 TeV was collected with the CMS detector at the LHC and corresponds to an integrated luminosity of 5.0 fb[superscript −1]. The measured cross sections are compared to predictions from Monte Carlo generators, MadGraph + pythia and sherpa, and to next-to-leading-order calculations from BlackHat + sherpa. The differential cross sections are found to be in agreement with the predictions, apart from the pT distributions of the leading jets at high pT values, the distributions of the HT at high-HT and low jet multiplicity, and the distribution of the difference in azimuthal angle between the leading jet and the muon at low values.United States. Dept. of EnergyNational Science Foundation (U.S.)Alfred P. Sloan Foundatio