1,784 research outputs found
Oil and Gas Maps of the Pikeville 30 x 60 Minute Quadrangle, Kentucky
The purpose of these oil and gas maps is to portray the distribution of types of wells in a manner useful to the oil and gas industry and geologists interested in subsurface research. The maps are designed to help geologists better evaluate acreage holdings and exploratory/development potential
A biophysical model of prokaryotic diversity in geothermal hot springs
Recent field investigations of photosynthetic bacteria living in geothermal
hot spring environments have revealed surprisingly complex ecosystems, with an
unexpected level of genetic diversity. One case of particular interest involves
the distribution along hot spring thermal gradients of genetically distinct
bacterial strains that differ in their preferred temperatures for reproduction
and photosynthesis. In such systems, a single variable, temperature, defines
the relevant environmental variation. In spite of this, each region along the
thermal gradient exhibits multiple strains of photosynthetic bacteria adapted
to several distinct thermal optima, rather than the expected single thermal
strain adapted to the local environmental temperature. Here we analyze
microbiology data from several ecological studies to show that the thermal
distribution field data exhibit several universal features independent of
location and specific bacterial strain. These include the distribution of
optimal temperatures of different thermal strains and the functional dependence
of the net population density on temperature. Further, we present a simple
population dynamics model of these systems that is highly constrained by
biophysical data and by physical features of the environment. This model can
explain in detail the observed diversity of different strains of the
photosynthetic bacteria. It also reproduces the observed thermal population
distributions, as well as certain features of population dynamics observed in
laboratory studies of the same organisms
A Detailed Study on the Equal Arrival Time Surface Effect in Gamma-Ray Burst Afterglows
Due to the relativistic motion of gamma-ray burst remnant and its
deceleration in the circumburst medium, the equal arrival time surfaces at any
moment are not spherical, but should be distorted ellipsoids. This will leave
some imprints in the afterglows. In this article, we study the effect of equal
arrival time surfaces numerically under various conditions, i.e., for isotropic
fireballs, collimated jets, density jump conditions, and energy injection
events. For each condition, direct comparison between the two instances when
the effect is and is not included, is presented. For isotropic fireballs and
jets viewed on axis, the effect slightly hardens the spectra and postpones the
peak time of afterglows, but does not change the shapes of the spectra and
light curves significantly. In the cases when a density jump or an energy
injection is involved, the effect smears the variability of the afterglows
markedly.Comment: Accepted for publication in: Chin. J. Astron. Astrophys., 15 pages, 8
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Follow-up observations at 16 and 33 GHz of extragalactic sources from WMAP 3-year data: I - Spectral properties
We present follow-up observations of 97 point sources from the Wilkinson
Microwave Anisotropy Probe (WMAP) 3-year data, contained within the New
Extragalactic WMAP Point Source (NEWPS) catalogue between declinations of -4
and +60 degrees; the sources form a flux-density-limited sample complete to 1.1
Jy (approximately 5 sigma) at 33 GHz. Our observations were made at 16 GHz
using the Arcminute Microkelvin Imager (AMI) and at 33 GHz with the Very Small
Array (VSA). 94 of the sources have reliable, simultaneous -- typically a few
minutes apart -- observations with both telescopes. The spectra between 13.9
and 33.75 GHz are very different from those of bright sources at low frequency:
44 per cent have rising spectra (alpha < 0.0), where flux density is
proportional to frequency^-alpha, and 93 per cent have spectra with alpha <
0.5; the median spectral index is 0.04. For the brighter sources, the agreement
between VSA and WMAP 33-GHz flux densities averaged over sources is very good.
However, for the fainter sources, the VSA tends to measure lower values for the
flux densities than WMAP. We suggest that the main cause of this effect is
Eddington bias arising from variability.Comment: 12 pages, 13 figures, submitted to MNRA
Microwave observations of spinning dust emission in NGC6946
We report new cm-wave measurements at five frequencies between 15 and 18GHz
of the continuum emission from the reportedly anomalous "region 4" of the
nearby galaxy NGC6946. We find that the emission in this frequency range is
significantly in excess of that measured at 8.5GHz, but has a spectrum from
15-18GHz consistent with optically thin free-free emission from a compact HII
region. In combination with previously published data we fit four emission
models containing different continuum components using the Bayesian spectrum
analysis package radiospec. These fits show that, in combination with data at
other frequencies, a model with a spinning dust component is slightly preferred
to those that possess better-established emission mechanisms.Comment: submitted MNRA
CMB observations from the CBI and VSA: A comparison of coincident maps and parameter estimation methods
We present coincident observations of the Cosmic Microwave Background (CMB)
from the Very Small Array (VSA) and Cosmic Background Imager (CBI) telescopes.
The consistency of the full datasets is tested in the map plane and the Fourier
plane, prior to the usual compression of CMB data into flat bandpowers. Of the
three mosaics observed by each group, two are found to be in excellent
agreement. In the third mosaic, there is a 2 sigma discrepancy between the
correlation of the data and the level expected from Monte Carlo simulations.
This is shown to be consistent with increased phase calibration errors on VSA
data during summer observations. We also consider the parameter estimation
method of each group. The key difference is the use of the variance window
function in place of the bandpower window function, an approximation used by
the VSA group. A re-evaluation of the VSA parameter estimates, using bandpower
windows, shows that the two methods yield consistent results.Comment: 10 pages, 6 figures. Final version. Accepted for publication in MNRA
AMI observations of Lynds Dark Nebulae: further evidence for anomalous cm-wave emission
Observations at 14.2 to 17.9 GHz made with the AMI Small Array towards
fourteen Lynds Dark Nebulae with a resolution of 2' are reported. These sources
are selected from the SCUBA observations of Visser et al. (2001) as small
angular diameter clouds well matched to the synthesized beam of the AMI Small
Array. Comparison of the AMI observations with radio observations at lower
frequencies with matched uv-plane coverage is made, in order to search for any
anomalous excess emission which can be attributed to spinning dust. Possible
emission from spinning dust is identified as a source within a 2' radius of the
Scuba position of the Lynds dark nebula, exhibiting an excess with respect to
lower frequency radio emission. We find five sources which show a possible
spinning dust component in their spectra. These sources have rising spectral
indices in the frequency range 14.2--17.9 GHz. Of these five one has already
been reported, L1111, we report one new definite detection, L675, and three new
probable detections (L944, L1103 and L1246). The relative certainty of these
detections is assessed on the basis of three criteria: the extent of the
emission, the coincidence of the emission with the Scuba position and the
likelihood of alternative explanations for the excess. Extended microwave
emission makes the likelihood of the anomalous emission arising as a
consequence of a radio counterpart to a protostar or a proto-planetary disk
unlikely. We use a 2' radius in order to be consistent with the IRAS
identifications of dark nebulae (Parker 1988), and our third criterion is used
in the case of L1103 where a high flux density at 850 microns relative to the
FIR data suggests a more complicated emission spectrum.Comment: submitted MNRA
Somatostatin subtype-2 receptor-targeted metal-based anticancer complexes
Conjugates of a dicarba analogue of octreotide, a potent somatostatin agonist whose receptors are overexpressed on tumor cells, with [PtCl 2(dap)] (dap = 1-(carboxylic acid)-1,2-diaminoethane) (3), [(η 6-bip)Os(4-CO 2-pico)Cl] (bip = biphenyl, pico = picolinate) (4), [(η 6-p-cym)RuCl(dap)] + (p-cym = p-cymene) (5), and [(η 6-p-cym)RuCl(imidazole-CO 2H)(PPh 3)] + (6), were synthesized by using a solid-phase approach. Conjugates 3-5 readily underwent hydrolysis and DNA binding, whereas conjugate 6 was inert to ligand substitution. NMR spectroscopy and molecular dynamics calculations showed that conjugate formation does not perturb the overall peptide structure. Only 6 exhibited antiproliferative activity in human tumor cells (IC 50 = 63 ± 2 μ in MCF-7 cells and IC 50 = 26 ± 3 μ in DU-145 cells) with active participation of somatostatin receptors in cellular uptake. Similar cytotoxic activity was found in a normal cell line (IC 50 = 45 ± 2.6 μ in CHO cells), which can be attributed to a similar level of expression of somatostatin subtype-2 receptor. These studies provide new insights into the effect of receptor-binding peptide conjugation on the activity of metal-based anticancer drugs, and demonstrate the potential of such hybrid compounds to target tumor cells specifically. © 2012 American Chemical Society
Diaryl- and triaryl-pyrrole derivatives:Inhibitors of the MDM2-p53 and MDMX-p53 protein-protein interactions
Screening identified 2-(3-((4,6-dioxo-2-thioxotetrahydropyrimidin-5(2H)-ylidene)methyl)-2,5-dimethyl-1H-pyrrol-1-yl)-4,5,6,7-tetrahydrobenzo[b]thiophene-3-carbonitrile as an MDM2–p53 inhibitor (IC(50) = 12.3 μM). MDM2–p53 and MDMX–p53 activity was seen for 5-((1-(4-chlorophenyl)-2,5-diphenyl-1H-pyrrol-3-yl)methylene)-2-thioxodihydropyrimidine-4,6(1H,5H)-dione (MDM2 IC(50) = 0.11 μM; MDMX IC(50) = 4.2 μM) and 5-((1-(4-nitrophenyl)-2,5-diphenyl-1H-pyrrol-3-yl)methylene)pyrimidine-2,4,6(1H,3H,5H)-trione (MDM2 IC(50) = 0.15 μM; MDMX IC(50) = 4.2 μM), and cellular activity consistent with p53 activation in MDM2 amplified cells. Further SAR studies demonstrated the requirement for the triarylpyrrole moiety for MDMX–p53 activity but not for MDM2–p53 inhibition
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