2,094 research outputs found
I Know Where You are and What You are Sharing: Exploiting P2P Communications to Invade Users' Privacy
In this paper, we show how to exploit real-time communication applications to
determine the IP address of a targeted user. We focus our study on Skype,
although other real-time communication applications may have similar privacy
issues. We first design a scheme that calls an identified targeted user
inconspicuously to find his IP address, which can be done even if he is behind
a NAT. By calling the user periodically, we can then observe the mobility of
the user. We show how to scale the scheme to observe the mobility patterns of
tens of thousands of users. We also consider the linkability threat, in which
the identified user is linked to his Internet usage. We illustrate this threat
by combining Skype and BitTorrent to show that it is possible to determine the
file-sharing usage of identified users. We devise a scheme based on the
identification field of the IP datagrams to verify with high accuracy whether
the identified user is participating in specific torrents. We conclude that any
Internet user can leverage Skype, and potentially other real-time communication
systems, to observe the mobility and file-sharing usage of tens of millions of
identified users.Comment: This is the authors' version of the ACM/USENIX Internet Measurement
Conference (IMC) 2011 pape
Calibrated Stochastic Dynamic Models for Resource Management
In this paper we develop a positive calibrated approach to stochastic dynamic programming. Risk aversion, discount rate, and intertemporal substitution preferences of the decision-maker are calibrated by a procedure that minimizes the mean squared error from data on past decisions. We apply this framework to managing stochastic water supplies from Oroville Reservoir, located in Northern California. The calibrated positive SDP closely reproduces the historical storage and releases from the dam and shows sensitivity of optimal decisions to a decision-maker's risk aversion and intertemporal preferences. The calibrated model has average prediction errors that are substantially lower than those from the model with an expected net present value objective.Resource /Energy Economics and Policy,
Handbook of X-Ray Astronomy
X-ray astronomy was born in the aftermath of World War II as military rockets were repurposed to lift radiation detectors above the atmosphere for a few minutes at a time. These early flights detected and studied X-ray emission from the Solar corona. The first sources beyond the Solar System were detected during a rocket flight in 1962 by a team headed by Riccardo Giaccom at American Science and Engineering, a company founded by physicists from MIT. The rocket used Geiger counters with a system designed to reduce non-X-ray backgrounds and collimators limiting the region of sky seen by the counters. As the rocket spun, the field of view (FOV) happened to pass over what was later found to be the brightest non-Solar X-ray source; later designated See X-1. It also detected a uniform background glow which could not be resolved into individual sources. A follow-up campaign using X-ray detectors with better spatial resolution and optical telescopes identified See X-1 as an interacting binary with a compact (neutron star) primary. This success led to further suborbital rocket flights by a number of groups. More X-ray binaries were discovered, as well as X-ray emission from supernova remnants, the radio galaxies M87 and Cygnus-A, and the Coma cluster. Detectors were improved and Geiger counters were replaced by proportional counters, which provided information about energy spectra of the sources. A constant challenge was determining precise positions of sources as only collimators were available
Advances in the RXTE Proportional Counter Array Calibration: Nearing the Statistical Limit
During its 16 years of service the Rossi X-ray Timing Explorer (RXTE) mission
has provided an extensive archive of data, which will serve as a primary source
of high cadence observations of variable X-ray sources for fast timing studies.
It is, therefore, very important to have the most reliable calibration of RXTE
instruments. The Proportional Counter Array (PCA) is the primary instrument
on-board RXTE which provides data in 3-50 keV energy range with sub-millisecond
time resolution in up to 256 energy channels. In 2009 the RXTE team revised the
response residual minimization method used to derive the parameters of the PCA
physical model. The procedure is based on the residual minimization between the
model spectrum for Crab nebula emission and a calibration data set consisting
of a number of spectra from the Crab and the on-board Am241 calibration source,
uniformly covering the whole RXTE mission operation period. The new method led
to a much more effective model convergence and allowed for better understanding
of the PCA energy-to-channel relationship. It greatly improved the response
matrix performance. We describe the new version of the RXTE/PCA response
generator PCARMF v11.7 (HEASOFT Release 6.7) along with the corresponding
energy-to-channel conversion table (verson e05v04) and their difference from
the previous releases of PCA calibration. The new PCA response adequately
represents the spectrum of the calibration sources and successfully predicts
the energy of the narrow iron emission line in Cas-A throughout the RXTE
mission.Comment: 8 pages, 4 figures, accepted for publication in Ap
High-Energy Astrophysics in the 2020s and Beyond
With each passing decade, we gain new appreciation for the dynamic,
connected, and often violent nature of the Universe. This reality necessarily
places the study of high-energy processes at the very heart of modern
astrophysics. This White Paper illustrates the central role of high-energy
astrophysics to some of the most pressing astrophysical problems of our time,
the formation/evolution of galaxies, the origin of the heavy elements, star and
planet formation, the emergence of life on exoplanets, and the search for new
physics. We also highlight the new connections that are growing between
astrophysicists and plasma physicists. We end with a discussion of the
challenges that must be addressed to realize the potential of these
connections, including the need for integrated planning across physics and
astronomy programs in multiple agencies, and the need to foster the creativity
and career aspirations of individual scientists in this era of large projects.Comment: Astro2020 White Paper submissio
A Chandra X-ray Study of Cygnus A - II. The Nucleus
We report Chandra ACIS and quasi-simultaneous RXTE observations of the
nearby, powerful radio galaxy Cygnus A, with the present paper focusing on the
properties of the active nucleus. In the Chandra observation, the hard (> a few
keV) X-ray emission is spatially unresolved with a size \approxlt 1 arcsec (1.5
kpc, H_0 = 50 km s^-1 Mpc^-1) and coincides with the radio and near infrared
nuclei. In contrast, the soft (< 2 keV) emission exhibits a bi-polar nebulosity
that aligns with the optical bi-polar continuum and emission-line structures
and approximately with the radio jet. In particular, the soft X-ray emission
corresponds very well with the [O III] \lambda 5007 and H\alpha + [N II]
\lambda\lambda 6548, 6583 nebulosity imaged with HST. At the location of the
nucleus there is only weak soft X-ray emission, an effect that may be intrinsic
or result from a dust lane that crosses the nucleus perpendicular to the source
axis. The spectra of the various X-ray components have been obtained by
simultaneous fits to the 6 detectors. The compact nucleus is detected to 100
keV and is well described by a heavily absorbed power law spectrum with
\Gamma_h = 1.52^{+0.12}_{-0.12} (similar to other narrow line radio galaxies)
and equivalent hydrogen column N_H (nuc) = 2.0^{+0.1}_{-0.2} \times 10^{23}
cm^-2.
(Abstract truncated).Comment: To be published in the Astrophysical Journal, v564 January 1, 2002
issue; 34 pages, 11 figures (1 color
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