Search NASA⌕ Search

SEARCH · Search NASA

Results for “upsilon”

Search indexed NASA NTRS and DOE OSTI research on propulsion, heat transfer, battery materials and energy systems. Follow report and document links to the original sources.

Quote a phrase for an exact phrase match. Source license links do not imply unrestricted reuse.

171 records · Page 10
All sourcesNASA NTRSDOE OSTI
NASA NTRS2006

Comprehensive Analysis of RXTE Data from Cyg X-1. Spectral Index-Quasi-Periodic Oscillation Frequency-Luminosity Correlations

We present timing and spectral analysis of approx. 2.2 Ms of Rossi X-ray Time Explorer (RXTE) archival data from Cyg X-1. Using the generic Comptonization model we reveal that the spectrum of Cyg X-1 consists of three components: a thermal seed photon spectrum, a Comptonized part of the seed photon spectrum and the iron line. We find a strong correlation between 0.1-20 Hz frequencies of quasiperiodic oscillations (QPOs) and the spectral power-law index. Presence of two spectral phases (states) are clearly seen in the data when the spectral indices saturate at low and high values of QPO frequencies. This saturation effect was discovered earlier in a number of black hole candidate (BHC) sources and now we strongly confirm this phenomenon in Cyg X-1. In the soft state this index- QPO frequency correlation shows a saturation of the photon index Gamma approx. 2.1 at high values of the low frequency upsilon(sub L). The saturation level of Gamma approx. 2.1 is the lowest value found yet in BHCs. The bolometric luminosity does not show clear correlation with the index. We also show that Fe K(sub alpha) emission line strength (equivalent width, EW) correlates with the QPO frequency. EW increases from 200 eV in the low/hard state to 1.5 keV in the high/soft state. The revealed observational correlations allow us to propose a scenario for the spectral transition and iron line formation which occur in BHC sources. We also present the spectral state (the power-law index) evolution for eight years of Cyg X-1 observations by RXTE.

Shaposhnikov, Nickolai↗
NASA NTRS2007

Radio Sources Toward Galaxy Clusters at 30 GHz

Extra-galactic radio sources are a significant contaminant in cosmic microwave background and Sunyaev-Zeldovich effect experiments. Deep interferometric observations with the BIMA and OVRO arrays are used to characterize the spatial, spectral, and flux distributions of radio sources toward massive galaxy clusters at 28.5 GHz. We compute counts of mJy source fluxes from 89 fields centered on known massive galaxy clusters and 8 non-cluster fields. We find that source counts in the inner regions of the cluster fields (within 0.5 arcmin of the cluster center) are a factor of 8.9 (+4.2 to -3.8) times higher than counts in the outer regions of the cluster fields (radius greater than 0.5 arcmin). Counts in the outer regions of the cluster fields are in turn a factor of 3.3 (+4.1 -1.8) greater than those in the noncluster fields. Counts in the non-cluster fields are consistent with extrapolations from the results of other surveys. We compute spectral indices of mJy sources in cluster fields between 1.4 and 28.5 GHz and find a mean spectral index of al[ja = 0.66 with an rms dispersion of 0.36, where flux S varies as upsilon(sup -alpha). The distribution is skewed, with a median spectral index of 0.72 and 25th and 75th percentiles of 0.51 and 0.92, respectively. This is steeper than the spectral indices of stronger field sources measured by other surveys.

Coble, K.↗
NASA NTRS2012

Constraints on Cosmic Rays, Magnetic Fields, and Dark Matter from Gamma-ray Observations of the Coma Cluster of Galaxies with VERITAS and FERMI

Observations of radio halos and relics in galaxy clusters indicate efficient electron acceleration. Protons should likewise be accelerated and, on account of weak energy losses, can accumulate, suggesting that clusters may also be sources of very high energy (VHE; E greater than100 GeV) gamma-ray emission. We report here on VHE gamma-ray observations of the Coma galaxy cluster with the VERITAS array of imaging Cerenkov telescopes, with complementing Fermi Large Area Telescope observations at GeV energies. No significant gamma-ray emission from the Coma Cluster was detected. Integral flux upper limits at the 99 confidence level were measured to be on the order of (2-5) x 10(sup -8) photons m(sup -2) s(sup -1) (VERITAS,greater than 220 GeV) and approximately 2 x 10(sup -6) photons m(sup -2) s(sup -1) (Fermi, 1-3 GeV), respectively. We use the gamma-ray upper limits to constrain cosmic rays (CRs) and magnetic fields in Coma. Using an analytical approach, the CR-to-thermal pressure ratio is constrained to be less than 16% from VERITAS data and less than 1.7% from Fermi data (averaged within the virial radius). These upper limits are starting to constrain the CR physics in self-consistent cosmological cluster simulations and cap the maximum CR acceleration efficiency at structure formation shocks to be 50. Alternatively, this may argue for non-negligible CR transport processes such as CR streaming and diffusion into the outer cluster regions. Assuming that the radio-emitting electrons of the Coma halo result from hadronic CR interactions, the observations imply a lower limit on the central magnetic field in Coma of approximately (2-5.5)microG, depending on the radial magnetic field profile and on the gamma-ray spectral index. Since these values are below those inferred by Faraday rotation measurements in Coma (for most of the parameter space), this renders the hadronic model a very plausible explanation of the Coma radio halo. Finally, since galaxy clusters are dark matter (DM) dominated, the VERITAS upper limits have been used to place constraints on the thermally averaged product of the total self-annihilation cross section and the relative velocity of the DM particles, (sigma upsilon)

cosmic↗
DOE OSTI2018

QCD Results from the Tevatron

We present results from soft and hard QCD studies at the Tevatron. The recent study of central exclusive $π^+ π^-$ production at $\sqrt{s} =$ 900 and 1960 GeV is discussed, as well as results on multi-parton interaction (MPI) for different final states, including final states consisting of heavy flavor mesons, $J/ψ$ and/or $\Upsilon$. Finally, the measurement of $Z → bb$ jets is presented.

72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS↗
DOE OSTI2017

Υ measurements in p+p, p+Au and Au+Au collisions at $\sqrt{s}$$_ {NN}$ = 200 GeV with the STAR experiment

In these proceedings, we present the latest Υ measurements with the STAR experiment. The production cross-section in p+p and the nuclear modification factor R p A in p+Au collisions at $\sqrt{s}$$_ {NN}$ = 200GeV are obtained via the dielectron channel. These measurements provide a p+p reference with significantly improved precision and quantification of the cold nuclear matter effects for Υ measurements in heavy-ion collisions at RHIC. The nuclear modification factor R AA in Au+Au collisions at $\sqrt{s}$$_ {NN}$ = 200GeV is obtained via both the dimuon and dielectron channels. The centrality and transverse momentum dependences of Υ(1S) and Υ(2S+3S) R AA are reported and compared to those at the LHC and theoretical calculations.

72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS↗
DOE OSTI2017

Υ Production in Heavy-Ion Collisions from the STAR Experiment

In these proceedings, we present recent results of Υ measurements in heavy-ion collisions from the STAR experiment at RHIC. Nuclear modification factors (RAA) for Υ(1S) and Υ(1S+2S+3S) in U+U collisions at s NN = 193  GeV are measured through the di-electron channel and compared to those in Au+Au collisions at s NN = 200 GeV and Pb+Pb collisions at \sqrtsNN\ = 2.76 TeV. The ratio between the Υ(2S+3S) and Υ(1S) yields in Au+Au collisions at s NN = 200 GeV is measured in the di-muon channel and compared to those in p+p collisions and in Pb+Pb collisions at s NN = 2.76 TeV . Lastly, prospects for future Υ measurements with the STAR experiment are also discussed.

72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS↗
DOE OSTI2021

Measurement of the azimuthal anisotropy of Υ(1S) and Υ(2S) mesons in PbPb collisions at $\sqrt{s_{NN}}$ = 5.02TeV

The second-order Fourier coefficients ( v 2 ) characterizing the azimuthal distributions of Υ(1S) and Υ(2S) mesons produced in PbPb collisions at s NN = 5.02 TeV are studied. The Υ mesons are reconstructed in their dimuon decay channel, as measured by the CMS detector. The collected data set corresponds to an integrated luminosity of 1.7 nb - 1 . The scalar product method is used to extract the v 2 coefficients of the azimuthal distributions. Results are reported for the rapidity range | y | < 2.4 , in the transverse momentum interval 0 < p T < 50 GeV / c , and in three centrality ranges of 10–30%, 30–50% and 50–90%. In contrast to the J / ψ mesons, the measured v 2 values for the Image 5 mesons are found to be consistent with zero.

5.02 TeV↗
DOE OSTI2025

Gluon saturation effects in exclusive heavy vector meson photoproduction

We study exclusive J/ψ and ϒ photoproduction for proton and Pb targets in the high-energy limit, with the energy dependence computed using the linear Balitsky–Fadin–Kuraev–Lipatov and the nonlinear Balitsky–Kovchegov evolution equations. The difference between these two evolution equations can be directly attributed to gluon saturation physics. We find that for proton targets there is no difference between the two approaches at the energies of the currently available data, while for Pb targets in J/ψ production the data shows a clear preference for the evolution with gluon saturation.

UPC↗
DOE OSTI2018

Where do particle names come from?

One of the most difficult things in learning particle physics for the first time is to understand all of the various names. There are dozens and dozens and sometimes many names can apply to one particle or a single name can apply to many particles. It’s all very confusing. Luckily, Fermilab’s Dr. Don Lincoln made this video to help you sort it all out.

72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS↗