1,261 research outputs found
Geant4 Simulation of a filtered X-ray Source for Radiation Damage Studies
Geant4 low energy extensions have been used to simulate the X-ray spectra of
industrial X-ray tubes with filters for removing the uncertain low energy part
of the spectrum in a controlled way. The results are compared with precisely
measured X-ray spectra using a silicon drift detector. Furthermore, this paper
shows how the different dose rates in silicon and silicon dioxide layers of an
electronic device can be deduced from the simulations
Tendency of spherically imploding plasma liners formed by merging plasma jets to evolve toward spherical symmetry
Three dimensional hydrodynamic simulations have been performed using smoothed
particle hydrodynamics (SPH) in order to study the effects of discrete jets on
the processes of plasma liner formation, implosion on vacuum, and expansion.
The pressure history of the inner portion of the liner was qualitatively and
quantitatively similar from peak compression through the complete stagnation of
the liner among simulation results from two one dimensional
radiationhydrodynamic codes, 3D SPH with a uniform liner, and 3D SPH with 30
discrete plasma jets. Two dimensional slices of the pressure show that the
discrete jet SPH case evolves towards a profile that is almost
indistinguishable from the SPH case with a uniform liner, showing that
non-uniformities due to discrete jets are smeared out by late stages of the
implosion. Liner formation and implosion on vacuum was also shown to be robust
to Rayleigh-Taylor instability growth. Interparticle mixing for a liner
imploding on vacuum was investigated. The mixing rate was very small until
after peak compression for the 30 jet simulation.Comment: 28 pages, 16 figures, submitted to Physics of Plasmas (2012
The Ultraviolet-to-Mid-Infrared Spectral Energy Distribution of Weak Emission Line Quasars
We present Spitzer Space Telescope photometry of 18 Sloan Digital Sky Survey
(SDSS) quasars at 2.7 <= z <= 5.9 which have weak or undetectable
high-ionization emission lines in their rest-frame ultraviolet (UV) spectra
(hereafter weak-lined quasars, or WLQs). The Spitzer data are combined with
SDSS spectra and ground-based, near-infrared (IR) photometry of these sources
to produce a large inventory of spectral energy distributions (SEDs) of WLQs
across the rest-frame ~0.1-5 mum spectral band. The SEDs of our sources are
inconsistent with those of BL Lacertae objects which are dominated by
synchrotron emission due to a jet aligned close to our line-of-sight, but are
consistent with the SED of ordinary quasars with similar luminosities and
redshifts that exhibit a near-to-mid-IR 'bump', characteristic of hot dust
emission. This indicates that broad emission lines in WLQs are intrinsically
weak, rather than suffering continuum dilution from a jet, and that such
sources cannot be selected efficiently from traditional photometric surveys.Comment: 10 pages (emulateapj), 4 figures. Accepted for publication in Ap
On acoustic scattering by a shell-covered seafloor
Author Posting. © Acoustical Society of America, 2000. This article is posted here by permission of Acoustical Society of America for personal use, not for redistribution. The definitive version was published in Journal of the Acoustical Society of America 108 (2000): 551-555, doi:10.1121/1.429585.Acoustic scattering by the seafloor is sometimes influenced, if not dominated, by the presence of discrete volumetric objects such as shells. A series of measurements of target strength of a type of benthic shelled animal and associated scattering modeling have recently been completed (Stanton et al., "Acoustic scattering by benthic and planktonic shelled animals," J. Acoust. Soc. Am., this issue). The results of that study are used herein to estimate the scattering by the seafloor with a covering of shells at high acoustic frequencies. A simple formulation is derived that expresses the area scattering strength of the seafloor in terms of the average reduced target strength or material properties of the discrete scatterers and their packing factor (where the reduced target strength is the target strength normalized by the geometric cross section of the scatterers and the averaging is done over orientation and/or a narrow range of size or frequency). The formula shows that, to first order, the backscattering at high acoustic frequencies by a layer of shells (or other discrete bodies such as rocks) depends principally upon material properties of the objects and packing factor and is independent of size and acoustic frequency. Estimates of area scattering strength using this formula and measured values of the target strength of shelled bodies from Stanton et al. (this issue) are close to or consistent with observed area scattering strengths due to shell-covered seafloors published in other papers.This research was
supported by the U.S. Office of Naval Research Grant No.
N00014-95-1-0287
X-ray Insights into the Nature of Weak Emission-Line Quasars at High Redshift
We present Chandra observations of nine high-redshift quasars (z=2.7-5.9)
discovered by the Sloan Digital Sky Survey with weak or undetectable
high-ionization emission lines in their UV spectra (WLQs). Adding archival
X-ray observations of six additional sources of this class has enabled us to
place the strongest constraints yet on the X-ray properties of this remarkable
class of AGNs. Although our data cannot rule out the possibility that the
emission lines are overwhelmed by a relativistically boosted continuum, as
manifested by BL Lac objects, we find that WLQs are considerably weaker in the
X-ray and radio bands than the majority of BL Lacs found at much lower
redshifts. If WLQs are high-redshift BL Lacs, then it is difficult to explain
the lack of a large parent population of X-ray and radio bright weak-lined
sources at high redshift. We also consider the possibility that WLQs are
quasars with extreme properties, and in particular that the emission lines are
suppressed by high accretion rates. Using joint spectral fitting of the X-ray
spectra of 11 WLQs we find that the mean photon index in the hard X-ray band is
consistent with those observed in typical radio-quiet AGNs with no hint of an
unusually steep hard-X-ray spectrum. This result poses a challenge to the
hypothesis that WLQs have extremely high accretion rates, and we discuss
additional observations required to test this idea.Comment: 13 pages (emulateapj), 7 figures. Accepted for publication in Ap
Disentangling AGN and Star Formation in Soft X-rays
We have explored the interplay of star formation and AGN activity in soft
X-rays (0.5-2 keV) in two samples of Seyfert 2 galaxies (Sy2s). Using a
combination of low resolution CCD spectra from Chandra and XMM-Newton, we
modeled the soft emission of 34 Sy2s using power law and thermal models. For
the 11 sources with high signal-to-noise Chandra imaging of the diffuse host
galaxy emission, we estimate the luminosity due to star formation by removing
the AGN, fitting the residual emission. The AGN and star formation
contributions to the soft X-ray luminosity (i.e. L and L)
for the remaining 24 Sy2s were estimated from the power law and thermal
luminosities derived from spectral fitting. These luminosities were scaled
based on a template derived from XSINGS analysis of normal star forming
galaxies. To account for errors in the luminosities derived from spectral
fitting and the spread in the scaling factor, we estimated L and
L from Monte Carlo simulations. These simulated luminosities agree
with L and L derived from Chandra imaging analysis within a
3\sigma\ confidence level. Using the infrared [NeII]12.8\mu m and [OIV]26\mu m
lines as a proxy of star formation and AGN activity, respectively, we
independently disentangle the contributions of these two processes to the total
soft X-ray emission. This decomposition generally agrees with L and
L at the 3\sigma\ level. In the absence of resolvable nuclear
emission, our decomposition method provides a reasonable estimate of emission
due to star formation in galaxies hosting type 2 AGN.Comment: accepted for publication in ApJ; 34 pages, 9 tables, 4 figure
The challenges of harmonising anti-doping policy implementation
The policy-implementation gap conceptualises how policy intentions and outcomes often differ due to a failure to consider the realities of implementation. The World Anti-Doping Agency (WADA) directs Olympic anti-doping policy, seeking to harmonise anti-doping policy globally; however, the realisation of consistent implementation has proven challenging. A major cause of inconsistent policy implementation is inter-signatory variation, but the mechanisms of variation are poorly understood. WADA provides an excellent example to explore why policy gaps occur in international sport governance. Consequently, we aimed to analyse the different types of inter-signatory variation in anti-doping policy and identify practical solutions to address inter-signatory variation in anti-doping. Data were collected from the Regional Anti-Doping Programme (RADO), a group of organisations tasked with increasing the capacity of NADOs globally. Semi-structured interviews were conducted with 22 RADO staff and board members who were sampled as key informants to discuss how inter-signatory variation affects anti-doping policy compliance. Following reflexive thematic analysis, we identified four thematic categories explaining inter-signatory variation in anti-doping implementation: (1) socio-geographic, (2) political, (3) organisational, and (4) human resources. Based on our analysis, we theorise why the policy-implementation gap occurs and provide recommendations to improve anti-doping policy implementation
On the acoustic diffraction by the edges of benthic shells
Author Posting. © Acoustical Society of America, 2004. This article is posted here by permission of Acoustical Society of America for personal use, not for redistribution. The definitive version was published in Journal of the Acoustical Society of America 116 (2004): 239-244, doi:10.1121/1.1675813.Recent laboratory measurements of acoustic backscattering by individual benthic shells have isolated the edge-diffracted echo from echoes due to the surface of the main body of the shell. The data indicate that the echo near broadside incidence is generally the strongest for all orientations and is due principally to the surface of the main body. At angles well away from broadside, the echo levels are lower and are due primarily to the diffraction from the edge of the shell. The decrease in echo levels from broadside incidence to well off broadside is shown to be reasonably consistent with the decrease in acoustic backscattering from normal incidence to well off normal incidence by a shell-covered seafloor. The results suggest the importance of the edge of the shell in off-normal-incidence backscattering by a shell-covered seafloor. Furthermore, when considering bistatic diffraction by edges, there are implications that the edge of the shell (lying on the seafloor) can cause significant scattering in many directions, including at subcritical angles.This research was supported by the U.S. Office of Naval
Research (Grant No. N00014-02-1-0095) and the Woods
Hole Oceanographic Institution (WHOI), Woods Hole, MA
The Lick AGN Monitoring Project 2011: Spectroscopic Campaign and Emission-Line Light Curves
In the Spring of 2011 we carried out a 2.5 month reverberation mapping
campaign using the 3 m Shane telescope at Lick Observatory, monitoring 15
low-redshift Seyfert 1 galaxies. This paper describes the observations,
reductions and measurements, and data products from the spectroscopic campaign.
The reduced spectra were fitted with a multicomponent model in order to isolate
the contributions of various continuum and emission-line components. We present
light curves of broad emission lines and the AGN continuum, and measurements of
the broad H-beta line widths in mean and root-mean square (rms) spectra. For
the most highly variable AGNs we also measured broad H-beta line widths and
velocity centroids from the nightly spectra. In four AGNs exhibiting the
highest variability amplitudes, we detect anticorrelations between broad H-beta
width and luminosity, demonstrating that the broad-line region "breathes" on
short timescales of days to weeks in response to continuum variations. We also
find that broad H-beta velocity centroids can undergo substantial changes in
response to continuum variations; in NGC 4593 the broad H-beta velocity shifted
by ~250 km/s over a one-month duration. This reverberation-induced velocity
shift effect is likely to contribute a significant source of confusion noise to
binary black hole searches that use multi-epoch quasar spectroscopy to detect
binary orbital motion. We also present results from simulations that examine
biases that can occur in measurement of broad-line widths from rms spectra due
to the contributions of continuum variations and photon-counting noise.Comment: 33 pages, 28 figures, accepted for publication in ApJ Supplement
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