8,648 research outputs found
Combined uncertainty factor for sampling and analysis
Measurement uncertainty that arises from primary sampling can be expressed as an uncertainty factor, which recognises its sometimes approximately log-normal probability distribution. By contrast, uncertainty arising from chemical analysis is usually expressed as relative uncertainty, based upon the assumptions of its approximately normal distribution. A new method is proposed that enables uncertainty from these two sources, expressed in these different ways, to be combined to produce an estimate of the total combined uncertainty of the measurement values that result when the measurement process is considered as a whole
The multi-band nonthermal emission from the supernova remnant RX J1713.7-3946
Nonthermal X-rays and very high-energy (VHE) -rays have been detected
from the supernova remnant (SNR) RX J1713.7-3946, and especially the recent
observations with the \textit{Suzaku} satellite clearly reveal a spectral
cutoff in the X-ray spectrum, which directly relates to the cutoff of the
energy spectrum of the parent electrons. However, whether the origin of the VHE
-rays from the SNR is hadronic or leptonic is still in debate. We
studied the multi-band nonthermal emission from RX J1713.7-3946 based on a
semi-analytical approach to the nonlinear shock acceleration process by
including the contribution of the accelerated electrons to the nonthermal
radiation. The results show that the multi-band observations on RX J1713.7-3946
can be well explained in the model with appropriate parameters and the TeV
-rays have hadronic origin, i.e., they are produced via proton-proton
(p-p) interactions as the relativistic protons accelerated at the shock collide
with the ambient matter.Comment: 6 pages, 5 figures, accepted by MNRA
KECK HIRES Spectroscopy of APM 08279+5255
With an optical R-band magnitude of 15.2, the recently discovered z=3.911 BAL
quasar APM 08279+5255 is an exceptionally bright high redshift source. Its
brightness has allowed us to acquire a high signal-to-noise ratio (~100), high
resolution (~6 km/s) spectrum using the HIRES echelle spectrograph on the 10-m
Keck I telescope. Given the quality of the data, these observations provide an
unprecedented view of associated and intervening absorption systems. Here we
announce the availability of this spectrum to the general astronomical
community and present a brief analysis of some of its main features.Comment: 21 pages including 5 figures. Accepted for publication by PAS
Diffusion due to the Beam-Beam Interaction and Fluctuating Fields in Hadron Colliders
Random fluctuations in the tune, beam offsets and beam size in the presence
of the beam-beam interaction are shown to lead to significant particle
diffusion and emittance growth in hadron colliders. We find that far from
resonances high frequency noise causes the most diffusion while near resonances
low frequency noise is responsible for the large emittance growth observed.
Comparison of different fluctuations shows that offset fluctuations between the
beams causes the largest diffusion for particles in the beam core.Comment: 5 pages, 3 postscript figure
Radio emission models of Colliding-Wind Binary Systems
We present calculations of the spatial and spectral distribution of the radio
emission from a wide WR+OB colliding-wind binary system based on
high-resolution hydrodynamical simulations and solutions to the radiative
transfer equation. We account for both thermal and synchrotron radio emission,
free-free absorption in both the unshocked stellar wind envelopes and the
shocked gas, synchrotron self-absorption, and the Razin effect. The
applicability of these calculations to modelling radio images and spectra of
colliding-wind systems is demonstrated with models of the radio emission from
the wide WR+OB binary WR147. Its synchrotron spectrum follows a power-law
between 5 and 15 GHz but turns down to below this at lower and higher
frequencies. We find that while free-free opacity from the circum-binary
stellar winds can potentially account for the low-frequency turnover, models
that also include a combination of synchrotron self-absorption and Razin effect
are favoured. We argue that the high-frequency turn down is a consequence of
inverse-Compton cooling. We present our resulting spectra and intensity
distributions, along with simulated MERLIN observations of these intensity
distributions. From these we argue that the inclination of the WR147 system to
the plane of the sky is low. We summarise by considering extensions of the
current model that are important for models of the emission from closer
colliding wind binaries, in particular the dramatically varying radio emission
of WR140.Comment: 18 pages, 18 figures; Accepted by Astronomy and Astrophysics, July 8,
200
Galaxy mergers moulding the circum-galactic medium - I. The impact of a major merger
Galaxies are surrounded by sizeable gas reservoirs which host a significant
amount of metals: the circum-galactic medium (CGM). The CGM acts as a mediator
between the galaxy and the extra-galactic medium. However, our understanding of
how galaxy mergers, a major evolutionary transformation, impact the CGM remains
deficient. We present a theoretical study of the effect of galaxy mergers on
the CGM. We use hydrodynamical cosmological zoom-in simulations of a major
merger selected from the Illustris project such that the z=0 descendant has a
halo mass and stellar mass comparable to the Milky Way. To study the CGM we
then re-simulated this system at a 40 times better mass resolution, and
included detailed post-processing ionization modelling. Our work demonstrates
the effect the merger has on the characteristic size of the CGM, its
metallicity, and the predicted covering fraction of various commonly observed
gas-phase species, such as H I, C IV, and O VI. We show that merger-induced
outflows can increase the CGM metallicity by 0.2-0.3 dex within 0.5 Gyr
post-merger. These effects last up to 6 Gyr post-merger. While the merger
increases the total metal covering fractions by factors of 2-3, the covering
fractions of commonly observed UV ions decrease due to the hard ionizing
radiation from the active galactic nucleus, which we model explicitly. Our
study of the single simulated major merger presented in this work demonstrates
the significant impact that a galaxy interaction can have on the size,
metallicity, and observed column densities of the CGM
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