2,932 research outputs found
Validation of magnetophonon spectroscopy as a tool for analyzing hot-electron effects in devices
It is shown that very high precision hot-electron magnetophonon experiments made on n+nân+-GaAs sandwich device structures which are customized for magnetoresistance measurements can be very accurately modeled by a new Monte Carlo technique. The latter takes account of the Landau quantization and device architecture as well as material parameters. It is proposed that this combination of experiment and modeling yields a quantitative tool for the direct analysis of spatially localized very nonequilibrium electron distributions in small devices and low dimensional structures
A Training Framework and Follow-Up Observations for Multiculturally Inclusive Teaching: Is Believing That We are Emphasizing Diversity Enough?
The authors present a theoretically and empirically grounded training for multiculturally inclusive teaching for new instructors. After implementing this training, qualitative data were gathered from instructors to identify their experience of the training and concerns related to incorporating issues of diversity into their classrooms (Study 1). At the end of the semester immediately following the training, quantitative data were gathered from instructors and their students to examine the interaction between studentsâ and instructorsâ perceived diversity emphasis (Study 2). When allowed to choose the extent to which they incorporated issues of diversity in their classes, the instructors differentially reported emphasizing diversity in class. In addition, results from multi-level linear modeling analyses demonstrated that instructorsâ reported emphasis on diversity in the classroom did not predict studentsâ perceptions of the inclusion of issues of diversity. The authors discuss implications for the development of multiculturally supportive programs of learning at universities
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Distribution ofWater Vapor in Molecular Clouds
We report the results of a large-area study of water vapor along the Orion Molecular Cloud ridge, the purpose of which was to determine the depth-dependent distribution of gas-phase water in dense molecular clouds. We find that the water vapor measured toward 77 spatial positions along the face-on Orion ridge, excluding positions surrounding the outflow associated with BN/KL and IRc2, display integrated intensities that correlate strongly with known cloud surface tracers such as CN, C2H, 13CO J = 5-4, and HCN, and less well with the volume tracer N2H+. Moreover, at total column densities corresponding to A V\u3c 15 mag, the ratio of H2O to C18O integrated intensities shows a clear rise approaching the cloud surface. We show that this behavior cannot be accounted for by either optical depth or excitation effects, but suggests that gas-phase water abundances fall at large A V. These results are important as they affect measures of the true water-vapor abundance in molecular clouds by highlighting the limitations of comparing measured water-vapor column densities with such traditional cloud tracers as 13CO or C18O. These results also support cloud models that incorporate freeze out of molecules as a critical component in determining the depth-dependent abundance of water vapor
First Passage Properties of the Erdos-Renyi Random Graph
We study the mean time for a random walk to traverse between two arbitrary
sites of the Erdos-Renyi random graph. We develop an effective medium
approximation that predicts that the mean first-passage time between pairs of
nodes, as well as all moments of this first-passage time, are insensitive to
the fraction p of occupied links. This prediction qualitatively agrees with
numerical simulations away from the percolation threshold. Near the percolation
threshold, the statistically meaningful quantity is the mean transit rate,
namely, the inverse of the first-passage time. This rate varies
non-monotonically with p near the percolation transition. Much of this behavior
can be understood by simple heuristic arguments.Comment: 10 pages, 9 figures, 2-column revtex4 forma
Embedded Stellar Clusters in the W3/W4/W5 Molecular Cloud Complex
We analyze the embedded stellar content in the vicinity of the W3/W4/W5 HII
regions using the FCRAO Outer Galaxy 12CO(J=1-0) Survey, the IRAS Point Source
Catalog, published radio continuum surveys, and new near-infrared and molecular
line observations. Thirty-four IRAS Point Sources are identified that have
far-infrared colors characteristic of embedded star forming regions, and we
have obtained K' mosaics and 13CO(J=1-0) maps for 32 of them. Ten of the IRAS
sources are associated with an OB star and 19 with a stellar cluster, although
three OB stars are not identified with a cluster. Half of the embedded stellar
population identified in the K' images is found in just the 5 richest clusters,
and 61% is contained in IRAS sources associated with an embedded OB star. Thus
rich clusters around OB stars contribute substantially to the stellar
population currently forming in the W3/W4/W5 region. Approximately 39% of the
cluster population is embedded in small clouds with an average mass of ~130 Mo
that are located as far as 100 pc from the W3/W4/W5 cloud complex. We speculate
that these small clouds are fragments of a cloud complex dispersed by previous
episodes of massive star formation. Finally, we find that 4 of the 5 known
embedded massive star forming sites in the W3 molecular cloud are found along
the interface with the W4 HII region despite the fact that most of the
molecular mass is contained in the interior regions of the cloud. These
observations are consistent with the classical notion that the W4 HII region
has triggered massive star formation along the eastern edge of the W3 molecular
cloud.Comment: to appear in ApJS, see http://astro.caltech.edu/~jmc/papers/w
SWAS Observations of Water in Molecular Outflows
We present SWAS detections of the ground-state 1(10)-1(01) transition of
o-H2O at 557 GHz in 18 molecular outflows. These results are combined with
ground-based observations of the J=1-0 transitions of 12CO and 13CO obtained at
the FCRAO and, for a subset of the outflows, data from ISO. Assuming the SWAS
water line emission originates from the same gas traced by CO emission, we find
that the outflowing gas in most outflows has an o-H2O abundance relative to H2
of between 10(-7) and 10(-6). Analysis of the water abundance as a function of
outflow velocity reveals a strong dependence. The water abundance increases
with velocity, and at the highest outflow velocities some outflows have
relative o-H2O abundances of order 10(-4). However the mass of gas with such
elevated water abundances represents less that 1% of the total outflow gas
mass. The ISO LWS observations of high-J rotational lines of CO and the 179.5
micron transition of o-H2O provide evidence for a warmer outflow component than
required to produce either the SWAS or FCRAO lines. The mass associated with
the ISO emission is similar to that responsible for the highest velocity water
emission detected by SWAS. The bulk of the outflowing gas has an abundance of
o-H2O well below what would be expected if the gas has passed through a C-shock
with shock velocities greater than 10 km/s. Gas-phase water can be depleted in
the post-shock gas due to freeze-out onto grain mantles, however the rate of
freeze-out is too slow to explain our results. Therefore we believe that only a
small fraction of the outflowing molecular gas has passed through shocks strong
enough to fully convert the gas-phase oxygen to water. This result has
implications for the acceleration mechanism of the molecular gas in these
outflows.Comment: Accepted for publication in Ap.J., 51 pages including 4 pages of
figure
A Search for Small-Scale Clumpiness in Dense Cores of Molecular Clouds
We have analyzed HCN(1-0) and CS(2-1) line profiles obtained with high
signal-to-noise ratios toward distinct positions in three selected objects in
order to search for small-scale structure in molecular cloud cores associated
with regions of high-mass star formation. In some cases, ripples were detected
in the line profiles, which could be due to the presence of a large number of
unresolved small clumps in the telescope beam. The number of clumps for regions
with linear scales of ~0.2-0.5 pc is determined using an analytical model and
detailed calculations for a clumpy cloud model; this number varies in the
range: ~2 10^4-3 10^5, depending on the source. The clump densities range from
~3 10^5-10^6 cm^{-3}, and the sizes and volume filling factors of the clumps
are ~(1-3) 10^{-3} pc and ~0.03-0.12. The clumps are surrounded by inter-clump
gas with densities not lower than ~(2-7) 10^4 cm^{-3}. The internal thermal
energy of the gas in the model clumps is much higher than their gravitational
energy. Their mean lifetimes can depend on the inter-clump collisional rates,
and vary in the range ~10^4-10^5 yr. These structures are probably connected
with density fluctuations due to turbulence in high-mass star-forming regions.Comment: 23 pages including 4 figures and 4 table
Submillimeter Wave Astronomy Satellite observations of comet 9P/Tempel 1 and Deep Impact
On 4 July 2005 at 5:52 UT the Deep Impact mission successfully completed its
goal to hit the nucleus of 9P/Tempel 1 with an impactor, forming a crater on
the nucleus and ejecting material into the coma of the comet. NASA's
Submillimeter Wave Astronomy Satellite (SWAS) observed the 1(10)-1(01)
ortho-water ground-state rotational transition in comet 9P/Tempel 1 before,
during, and after the impact. No excess emission from the impact was detected
by SWAS and we derive an upper limit of 1.8e7 kg on the water ice evaporated by
the impact. However, the water production rate of the comet showed large
natural variations of more than a factor of three during the weeks before and
after the impact. Episodes of increased activity with Q(H2O)~1e28 molecule/s
alternated with periods with low outgassing (Q(H2O)<~5e27 molecule/s). We
estimate that 9P/Tempel 1 vaporized a total of N~4.5e34 water molecules (~1.3e9
kg) during June-September 2005. Our observations indicate that only a small
fraction of the nucleus of Tempel 1 appears to be covered with active areas.
Water vapor is expected to emanate predominantly from topographic features
periodically facing the Sun as the comet rotates. We calculate that appreciable
asymmetries of these features could lead to a spin-down or spin-up of the
nucleus at observable rates.Comment: 38 pages, 2 tables, 7 figures; Icarus, in pres
One-carbon metabolism in cancer
Cells require one-carbon units for nucleotide synthesis, methylation and reductive metabolism, and these pathways support the high proliferative rate of cancer cells. As such, anti-folates, drugs that target one-carbon metabolism, have long been used in the treatment of cancer. Amino acids, such as serine are a major one-carbon source, and cancer cells are particularly susceptible to deprivation of one-carbon units by serine restriction or inhibition of de novo serine synthesis. Recent work has also begun to decipher the specific pathways and sub-cellular compartments that are important for one-carbon metabolism in cancer cells. In this review we summarise the historical understanding of one-carbon metabolism in cancer, describe the recent findings regarding the generation and usage of one-carbon units and explore possible future therapeutics that could exploit the dependency of cancer cells on one-carbon metabolism
Water Abundance in Molecular Cloud Cores
We present Submillimeter Wave Astronomy Satellite (SWAS) observations of the
1_{10}-1_{01} transition of ortho-water at 557 GHz toward 12 molecular cloud
cores. The water emission was detected in NGC 7538, Rho Oph A, NGC 2024, CRL
2591, W3, W3(OH), Mon R2, and W33, and was not detected in TMC-1, L134N, and
B335. We also present a small map of the water emission in S140. Observations
of the H_2^{18}O line were obtained toward S140 and NGC 7538, but no emission
was detected. The abundance of ortho-water relative to H_2 in the giant
molecular cloud cores was found to vary between 6x10^{-10} and 1x10^{-8}. Five
of the cloud cores in our sample have previous water detections; however, in
all cases the emission is thought to arise from hot cores with small angular
extents. The water abundance estimated for the hot core gas is at least 100
times larger than in the gas probed by SWAS. The most stringent upper limit on
the ortho-water abundance in dark clouds is provided in TMC-1, where the
3-sigma upper limit on the ortho-water fractional abundance is 7x10^{-8}.Comment: 5 pages, 3 Postscript figures, uses aastex.cls, emulateapj5.sty
(included), and apjfonts.sty (included
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