338 research outputs found
A bright radio HH object with large proper motions in the massive star-forming region W75N
We analyze radio continuum and line observations from the archives of the
Very Large Array, as well as X-ray observations from the \emph{Chandra} archive
of the region of massive star formation W75N. Five radio continuum sources are
detected: VLA 1, VLA 2, VLA 3, Bc, and VLA 4. VLA 3 appears to be a radio jet;
we detect J=1-0, v=0 SiO emission towards it, probably tracing the inner parts
of a molecular outflow. The radio continuum source Bc, previously believed to
be tracing an independent star, is found to exhibit important changes in total
flux density, morphology, and position. These results suggest that source Bc is
actually a radio Herbig-Haro object, one of the brightest known, powered by the
VLA~3 jet source. VLA 4 is a new radio continuum component, located a few
arcsec to the south of the group of previously known radio sources. Strong and
broad (1,1) and (2,2) ammonia emission is detected from the region containing
the radio sources VLA~1, VLA~2, and VLA~3. Finally, the 2-10 keV emission seen
in the \emph{Chandra}/ACIS image shows two regions that could be the
termination shocks of the outflows from the multiple sources observed in W75N.Comment: 26 pages, 7 figure
Risk Factors, Dynamics, and Clinical Consequences of Aortic Neck Dilatation after Standard Endovascular Aneurysm Repair
Objective: Aortic neck dilatation (AND) occurs after endovascular aneurysm repair (EVAR) with self expanding stent grafts (SESs). Whether it continues, ultimately exceeding the endograft diameter leading to abdominal aortic aneurysm (AAA) rupture, remains uncertain. Dynamics, risk factors, and clinical relevance of AND were investigated after EVAR with standard SESs.
Methods: All intact EVAR patients treated from 2000 to 2015 at a tertiary institution were included. Demographic, anatomical, and device related characteristics were investigated as risk factors for AND. Outer to outer diameters were measured at a single standardised aortic level on reconstructed computed tomography (CT) images.
Results: A total of 460 patients were included (median follow up 5.2 years, interquartile range [IQR] 3.0, 7.7 years; CT imaging follow up 3.3 years, IQR 1.3, 5.4). Baseline neck diameter was 24 mm (IQR 22, 26) and increased 11.1% (IQR 1.5%, 21.9%) at last CT imaging. Endograft oversizing was 20.0% (IQR 13.6, 28.0). AND was greater during the first year (5.2% [IQR 0, 11.7]) decreasing subsequently (two to four years to 1.4%/year [IQR 0.0, 4.5%], p ≤ .001) and was associated with suprarenal fixation endografts (t value = 7.9, p 5 mm (HR 3.1, 95% CI 1.4 - 6.9).
Conclusion: AND after EVAR with SES is associated with endograft oversizing and radial force but decelerates after the first post-operative year. Baseline aortic neck diameter and suprarenal stent bearing endografts were associated with an increased risk of AND beyond nominal stent graft diameter. However, it remains unclear whether patient selection, differences in endograft radial force or the suprarenal stent are accountable for this difference.info:eu-repo/semantics/publishedVersio
Large Silicon Abundance in Photodissociation Regions
We have made one-dimensional raster-scan observations of the rho Oph and
sigma Sco star-forming regions with two spectrometers (SWS and LWS) on board
the ISO. In the rho Oph region, [SiII] 35um, [OI] 63um, 146um, [CII] 158um, and
the H2 pure rotational transition lines S(0) to S(3) are detected, and the PDR
properties are derived as the radiation field scaled by the solar neighborhood
value G_0~30-500, the gas density n~250--2500 /cc, and the surface temperature
T~100-400 K. The ratio of [SiII] 35um to [OI] 146um indicates that silicon of
10--20% of the solar abundance must be in the gaseous form in the
photodissociation region (PDR), suggesting that efficient dust destruction is
undergoing even in the PDR and that part of silicon atoms may be contained in
volatile forms in dust grains. The [OI] 63um and [CII] 158um emissions are too
weak relative to [OI] 146um to be accounted for by standard PDR models. We
propose a simple model, in which overlapping PDR clouds along the line of sight
absorb the [OI] 63um and [CII] 158um emissions, and show that the proposed
model reproduces the observed line intensities fairly well. In the sigma Sco
region, we have detected 3 fine-structure lines, [OI] 63um, [NII] 122um, and
[CII] 158um, and derived that 30-80% of the [CII] emission comes from the
ionized gas. The upper limit of the [SiII] 35um is compatible with the solar
abundance relative to nitrogen and no useful constraint on the gaseous Si is
obtained for the sigma Sco region.Comment: 25 pages with 7 figures, accepted in Astrophysical Journa
Observations of Massive Star Forming Regions with Water Masers: Mid-Infrared Imaging
We present here a mid-infrared imaging survey of 26 sites of water maser
emission. Observations were obtained at the InfraRed Telescope Facility 3-m
telescope with the University of Florida mid-infrared imager/spectrometer
OSCIR, and the JPL mid-infrared camera MIRLIN. The main purpose of the survey
was to explore the relationship between water masers and the massive star
formation process. It is generally believed that water masers predominantly
trace outflows and embedded massive stellar objects, but may also exist in
circumstellar disks around young stars. We investigate each of these
possibilities in light of our mid-infrared imaging. We find that mid-infrared
emission seems to be more closely associated with water and OH maser emission
than cm radio continuum emission from UC HII regions. We also find from the
sample of sources in our survey that, like groups of methanol masers, both
water and OH masers have a proclivity for grouping into linear or elongated
distributions. We conclude that the vast majority of linearly distributed
masers are not tracing circumstellar disks, but outflows and shocks instead.Comment: 49 pages; 23 figures; To appear in February 2005 ApJS; To download a
version with better quality figures, go to
http://www.ctio.noao.edu/~debuizer
Clustered Star Formation in W75 N
We present 2" to 7" resolution 3 mm continuum and CO(J=1-0) line emission and
near infrared Ks, H2, and [FeII] images toward the massive star forming region
W75 N. The CO emission uncovers a complex morphology of multiple, overlapping
outflows. A total flow mass of greater than 255 Msun extends 3 pc from
end-to-end and is being driven by at least four late to early-B protostars.
More than 10% of the molecular cloud has been accelerated to high velocities by
the molecular flows (> 5.2 km/s relative to v{LSR}) and the mechanical energy
in the outflowing gas is roughly half the gravitational binding energy of the
cloud. The W75 N cluster members represent a range of evolutionary stages, from
stars with no apparent circumstellar material to deeply embedded protostars
that are actively powering massive outflows. Nine cores of
millimeter-wavelength emission highlight the locations of embedded protostars
in W75 N. The total mass of gas & dust associated with the millimeter cores
ranges from 340 Msun to 11 Msun. The infrared reflection nebula and shocked H2
emission have multiple peaks and extensions which, again, suggests the presence
of several outflows. Diffuse H2 emission extends about 0.6 parsecs beyond the
outer boundaries of the CO emission while the [FeII] emission is only detected
close to the protostars. The infrared line emission morphology suggests that
only slow, non-dissociative J-type shocks exist throughout the pc-scale
outflows. Fast, dissociative shocks, common in jet-driven low-mass outflows,
are absent in W75 N. Thus, the energetics of the outflows from the late to
early B protostars in W75 N differ from their low-mass counterparts -- they do
not appear to be simply scaled-up versions of low-mass outflows.Comment: Astrophysical Journal, in press. 23 pages plus 10 figures (jpg
format). See http://www.aoc.nrao.edu/~dshepher/science.shtml for reprint with
full resolution figure
Polarization Observations of 1720 MHz OH Masers toward the Three Supernova Remnants W28, W44, and IC443
(abridged) - We present arcsecond resolution observations from the VLA of the
satellite line of the hydroxyl molecule (OH) at 1720.53 MHz toward three
Galactic supernova remnants: W28, W44 and IC443. All of our observations are
consistent with a model in which the OH(1720 MHz) is collisionally excited by
H2 molecules in the postshock gas heated by a non-dissociative shock. Supernova
remnants with OH(1720 MHz) maser emission may be promising candidates to
conduct high energy searches for the sites of cosmic ray acceleration.Comment: ApJ Let (accepted). Hardcopies available from [email protected]
Interstellar Hydroxyl Masers in the Galaxy. II. Zeeman Pairs and the Galactic Magnetic Field
We have identified and classified Zeeman pairs in the survey by Argon, Reid,
& Menten of massive star-forming regions with 18 cm (2 Pi 3/2, J = 3/2) OH
maser emission. We have found a total of more than 100 Zeeman pairs in more
than 50 massive star-forming regions. The magnetic field deduced from the
Zeeman splitting has allowed us to assign an overall line-of-sight magnetic
field direction to many of the massive star-forming regions. Combining these
data with other data sets obtained from OH Zeeman splitting, we have looked for
correlations of magnetic field directions between star-forming regions
scattered throughout the Galaxy. Our data do not support a uniform,
Galactic-scale field direction, nor do we find any strong evidence of magnetic
field correlations within spiral arms. However, our data suggest that in the
Solar neighborhood the magnetic field outside the Solar circle is oriented
clockwise as viewed from the North Galactic Pole, while inside the Solar circle
it is oriented counterclockwise. This pattern, including the magnetic field
reversal near the Sun, is in agreement with results obtained from pulsar
rotation measures.Comment: 37 pages AASTeX, including 6 figures, to appear in Ap
Mr. Meteo: Providing climate information for the unconnected
A majority of the world remain unconnected to the World Wide Web due to issues like low literacy and relevant information. This study presents Mr. Meteo, a system that provides weather information via voice calls in local languages to rural farmers in Ghana. The study used an interdisciplinary approach to identify relevant informational needs and socio-economic implications, and early end-user and stakeholder involvement. Mr. Meteo was deployed in Bolgatanga, Ghana and represents a novel design in terms of actual web data access to rural areas. The positive feedback from farmers, and stakeholder’s interest in continuity, shows this approach to be an appropriate method of development and implementation of information systems for rural areas; successful due to end-user and stakeholder involvement, focus on existing technologies, the use of voice technologies to mitigate the problem of illiteracy, and information relevance to end-users. This paper presents the methodology and results of this novel, practical, local-context ICT4D project,that has produced a viable information system for rural communities
Si and Fe depletion in Galactic star-forming regions observed by the Spitzer Space Telescope
We report the results of the mid-infrared spectroscopy of 14 Galactic
star-forming regions with the high-resolution modules of the Infrared
Spectrograph (IRS) on board the Spitzer Space Telescope. We detected [SiII]
35um, [FeII] 26um, and [FeIII] 23um as well as [SIII] 33um and H2 S(0) 28um
emission lines. Using the intensity of [NII] 122um or 205um and [OI] 146um or
63um reported by previous observations in four regions, we derived the ionic
abundance Si+/N+ and Fe+/N+ in the ionized gas and Si+/O0 and Fe+/O0 in the
photodissociation gas. For all the targets, we derived the ionic abundance of
Si+/S2+ and Fe2+/S2+ for the ionized gas. Based on photodissociation and HII
region models the gas-phase Si and Fe abundance are suggested to be 3-100% and
<8% of the solar abundance, respectively, for the ionized gas and 16-100% and
2-22% of the solar abundance, respectively, for the photodissociation region
gas. Since the [FeII] 26um and [FeIII] 23um emissions are weak, the high
sensitivity of the IRS enables to derive the gas-phase Fe abundance widely in
star-forming regions. The derived gas-phase Si abundance is much larger than
that in cool interstellar clouds and that of Fe. The present study indicates
that 3-100% of Si atoms and <22% of Fe atoms are included in dust grains which
are destroyed easily in HII regions, probably by the UV radiation. We discuss
possible mechanisms to account for the observed trend; mantles which are
photodesorbed by UV photons, organometallic complexes, or small grains.Comment: 43 pages with 7 figures, accepted in Astrophysical Journa
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