436 research outputs found
Restricted-Use Pesticide Recordkeeping Rules for Certified Private Applicators
This is a collection of frequently asked questions to help certified private pesticide applicators understand the recordkeeping regulations.https://lib.dr.iastate.edu/extension_ag_pubs/1183/thumbnail.jp
Dynamical robustness of biological networks with hierarchical distribution of time scales
We propose the concepts of distributed robustness and r-robustness, well
adapted to functional genetics. Then we discuss the robustness of the
relaxation time using a chemical reaction description of genetic and signalling
networks. First, we obtain the following result for linear networks: for large
multiscale systems with hierarchical distribution of time scales the variance
of the inverse relaxation time (as well as the variance of the stationary rate)
is much lower than the variance of the separate constants. Moreover, it can
tend to 0 faster than 1/n, where n is the number of reactions. We argue that
similar phenomena are valid in the nonlinear case as well. As a numerical
illustration we use a model of signalling network that can be applied to
important transcription factors such as NFkB
The two states of Sgr A* in the near-infrared: bright episodic flares on top of low-level continuous variability
In this paper we examine properties of the variable source Sgr A* in the
near-infrared (NIR) using a very extensive Ks-band data set from NACO/VLT
observations taken 2004 to 2009. We investigate the variability of Sgr A* with
two different photometric methods and analyze its flux distribution. We find
Sgr A* is continuously emitting and continuously variable in the near-infrared,
with some variability occurring on timescales as long as weeks. The flux
distribution can be described by a lognormal distribution at low intrinsic
fluxes (<~5 mJy, dereddened with A_{Ks}=2.5). The lognormal distribution has a
median flux of approximately 1.1 mJy, but above 5 mJy the flux distribution is
significantly flatter (high flux events are more common) than expected for the
extrapolation of the lognormal distribution to high fluxes. We make a general
identification of the low level emission above 5 mJy as flaring emission and of
the low level emission as the quiescent state. We also report here the
brightest Ks-band flare ever observed (from August 5th, 2008) which reached an
intrinsic Ks-band flux of 27.5 mJy (m_{Ks}=13.5). This flare was a factor 27
increase over the median flux of Sgr A*, close to double the brightness of the
star S2, and 40% brighter than the next brightest flare ever observed from
Sgr~A*.Comment: 14 pages, 6 figures, accepted for publication in Ap
A New Lecture-Tutorial for Teaching about Molecular Excitations and Synchrotron Radiation
Light and spectroscopy are among the most important and frequently taught
topics in introductory, college-level, general education astronomy courses.
This is due to the fact that the vast majority of observational data studied by
astronomers arrives at Earth in the form of light. While there are many
processes by which matter can emit and absorb light, Astro 101 courses
typically limit their instruction to the Bohr model of the atom and electron
energy level transitions. In this paper, we report on the development of a new
Lecture-Tutorial to help students learn about other processes that are
responsible for the emission and absorption of light, namely molecular
rotations, molecular vibrations, and the acceleration of charged particles by
magnetic fields.Comment: 13 pages, 7 figures Accepted for publication in The Physics Teache
Evidence for X-ray synchrotron emission from simultaneous mid-IR to X-ray observations of a strong Sgr A* flare
This paper reports measurements of Sgr A* made with NACO in L' -band (3.80
um), Ks-band (2.12 um) and H-band (1.66 um) and with VISIR in N-band (11.88 um)
at the ESO VLT, as well as with XMM-Newton at X-ray (2-10 keV) wavelengths. On
4 April, 2007, a very bright flare was observed from Sgr A* simultaneously at
L'-band and X-ray wavelengths. No emission was detected using VISIR. The
resulting SED has a blue slope (beta > 0 for nuL_nu ~ nu^beta, consistent with
nuL_nu ~ nu^0.4) between 12 micron and 3.8 micron.
For the first time our high quality data allow a detailed comparison of
infrared and X-ray light curves with a resolution of a few minutes. The IR and
X-ray flares are simultaneous to within 3 minutes. However the IR flare lasts
significantly longer than the X-ray flare (both before and after the X-ray
peak) and prominent substructures in the 3.8 micron light curve are clearly not
seen in the X-ray data. From the shortest timescale variations in the L'-band
lightcurve we find that the flaring region must be no more than 1.2 R_S in
size.
The high X-ray to infrared flux ratio, blue nuL_nu slope MIR to L' -band, and
the soft nuL_nu spectral index of the X-ray flare together place strong
constraints on possible flare emission mechanisms. We find that it is
quantitatively difficult to explain this bright X-ray flare with inverse
Compton processes. A synchrotron emission scenario from an electron
distribution with a cooling break is a more viable scenario.Comment: ApJ, 49 pages, 9 figure
An Inverse Compton Scattering Origin of X-ray Flares from Sgr A*
The X-ray and near-IR emission from Sgr A* is dominated by flaring, while a
quiescent component dominates the emission at radio and sub-mm wavelengths. The
spectral energy distribution of the quiescent emission from Sgr A* peaks at
sub-mm wavelengths and is modeled as synchrotron radiation from a thermal
population of electrons in the accretion flow, with electron temperatures
ranging up to \,MeV. Here we investigate the mechanism by which
X-ray flare emission is produced through the interaction of the quiescent and
flaring components of Sgr A*. The X-ray flare emission has been interpreted as
inverse Compton, self-synchrotron-Compton, or synchrotron emission. We present
results of simultaneous X-ray and near-IR observations and show evidence that
X-ray peak flare emission lags behind near-IR flare emission with a time delay
ranging from a few to tens of minutes. Our Inverse Compton scattering modeling
places constraints on the electron density and temperature distributions of the
accretion flow and on the locations where flares are produced. In the context
of this model, the strong X-ray counterparts to near-IR flares arising from the
inner disk should show no significant time delay, whereas near-IR flares in the
outer disk should show a broadened and delayed X-ray flare.Comment: 22 pages, 6 figures, 2 tables, AJ (in press
X-ray and Radio Variability of M31*, The Andromeda Galaxy Nuclear Supermassive Black Hole
We confirm our earlier tentative detection of M31* in X-rays and measure its
light-curve and spectrum. Observations in 2004-2005 find M31* rather quiescent
in the X-ray and radio. However, X-ray observations in 2006-2007 and radio
observations in 2002 show M31* to be highly variable at times. A separate
variable X-ray source is found near P1, the brighter of the two optical nuclei.
The apparent angular Bondi radius of M31* is the largest of any black hole, and
large enough to be well resolved with Chandra. The diffuse emission within this
Bondi radius is found to have an X-ray temperature ~0.3 keV and density 0.1
cm-3, indistinguishable from the hot gas in the surrounding regions of the
bulge given the statistics allowed by the current observations. The X-ray
source at the location of M31* is consistent with a point source and a power
law spectrum with energy slope 0.9+/-0.2. Our identification of this X-ray
source with M31* is based solely on positional coincidence.Comment: 25 pages, 8 figures, submitted to Ap
What is limiting near-infrared astrometry in the Galactic Center?
We systematically investigate the error sources for high-precision astrometry
from adaptive optics based near-infrared imaging data. We focus on the
application in the crowded stellar field in the Galactic Center. We show that
at the level of <=100 micro-arcseconds a number of effects are limiting the
accuracy. Most important are the imperfectly subtracted seeing halos of
neighboring stars, residual image distortions and unrecognized confusion of the
target source with fainter sources in the background. Further contributors to
the error budget are the uncertainty in estimating the point spread function,
the signal-to-noise ratio induced statistical uncertainty, coordinate
transformation errors, the chromaticity of refraction in Earth's atmosphere,
the post adaptive optics differential tilt jitter and anisoplanatism. For stars
as bright as mK=14, residual image distortions limit the astrometry, for
fainter stars the limitation is set by the seeing halos of the surrounding
stars. In order to improve the astrometry substantially at the current
generation of telescopes, an adaptive optics system with high performance and
weak seeing halos over a relatively small field (r<=3") is suited best.
Furthermore, techniques to estimate or reconstruct the seeing halo could be
promising.Comment: accepted by MNRAS, 13 pages, 14 figure
Simultaneous NIR/sub-mm observation of flare emission from SgrA*
We report on a successful, simultaneous observation and modeling of the
sub-millimeter to near-infrared flare emission of the Sgr A* counterpart
associated with the super-massive black hole at the Galactic center. Our
modeling is based on simultaneous observations that have been carried out on 03
June, 2008 using the NACO adaptive optics (AO) instrument at the ESO VLT and
the LABOCA bolometer at the APEX telescope. Inspection and modeling of the
light curves show that the sub-mm follows the NIR emission with a delay of
1.5+/-0.5 hours. We explain the flare emission delay by an adiabatic expansion
of the source components.Comment: 12 pages, 9 figures, 3 tables, in press with A&
Passives and Se Constructions
In this chapter we discuss some of the main properties of constructions involving participial passives, passive se, and impersonal se in Portuguese, focusing on its two main varieties, European and Brazilian Portuguese (henceforth EP and BP, respectively).1 When the two dialects differ, we will provide the relevant judgments each dialect assigns to the data under discussion by using the abbreviations EP and BP.
The chapter is organized in five sections. Section 2 deals with participial passives, distinguishing between adjectival and verbal passives and between the participial forms of passives and compound tenses. Section 3 focuses on passive se and impersonal se constructions, comparing them with verbal passives when appropriate. Section 4 concludes the paper.info:eu-repo/semantics/publishedVersio
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