681 research outputs found
A Test of the Standard Hypothesis for the Origin of the HI Holes in Holmberg II
The nearby irregular galaxy Holmberg II has been extensively mapped in HI
using the Very Large Array (VLA), revealing intricate structure in its
interstellar gas component (Puche et al. 1992). An analysis of these structures
shows the neutral gas to contain a number of expanding HI holes. The formation
of the HI holes has been attributed to multiple supernova events occurring
within wind-blown shells around young, massive star clusters, with as many as
10-200 supernovae required to produce many of the holes. From the sizes and
expansion velocities of the holes, Puche et al. assigned ages of ~10^7 to 10^8
years. If the supernova scenario for the formation of the HI holes is correct,
it implies the existence of star clusters with a substantial population of
late-B, A and F main sequence stars at the centers of the holes. Many of these
clusters should be detectable in deep ground-based CCD images of the galaxy. In
order to test the supernova hypothesis for the formation of the HI holes, we
have obtained and analyzed deep broad-band BVR and narrow-band H-alpha images
of Ho II. We compare the optical and HI data and search for evidence of the
expected star clusters in and around the HI holes. We also use the HI data to
constrain models of the expected remnant stellar population. We show that in
several of the holes the observed upper limits for the remnant cluster
brightness are strongly inconsistent with the SNe hypothesis described in Puche
et al. Moreover, many of the HI holes are located in regions of very low
optical surface brightness which show no indication of recent star formation.
Here we present our findings and explore possible alternative explanations for
the existence of the HI holes in Ho II, including the suggestion that some of
the holes were produced by Gamma-ray burst events.Comment: 30 pages, including 6 tables and 3 images. To appear in Astron.
Journal (June 1999
Towards integrated urban and horticultural planning in Hanoi and Nanjing
In an international and interdisciplinary research project, partly funded by the European Union, the possibilities were explored of having specialized horticultural production around East Asian cities benefit from urban growth. Anywhere in the world, farmers around cities have to cope with two contradictory trends. The inhabitants of the rapidly expanding cities like Hanoi and Nanjing not only enjoy eating fresh vegetables but also âeat upâ some of the most productive farmland where these vegetables are grown for new housing estates and other urban functions. After analysing and comparing the general speed, directions and mechanisms of physical expansion in both cities over the last decade the research team focused on one pilot area in each city. In these pilot studies it became clear that, next to many farmers who were not able to make much money from agriculture and are therefore quite happy to shift to urban jobs, there is an important group of knowledgeable and ambitious market gardeners, who do make a good living out of horticulture. How could urban planners take the skills and ambitions of these people into consideration and cooperate with agricultural planners, while designing and developing urban growth? Several workshops were held and examples from Europe and other parts of the world were discussed with all stakeholders to see how productive open spaces could become an integral part of the new urban areas. For both pilot areas different scenarios were made to make the stakeholders see the possible effect of combining urban interests with those of sustainable, specialised agricultural production that should be attractive for urban residents to encounter on a daily basis. We conclude that this project has made the planners in both cities aware of the advantages and possibilities of working together in the further expansion of Hanoi and Nanjing towards the integration of highly productive green spaces with serious farmers in the further expansion of Hanoi and Nanjing
An Exploration of the Tully-Fisher Relation for Extreme Late-Type Spiral Galaxies
This paper explores the adherence of 47 extreme late-type galaxies to the B-
and V-band Tully-Fisher relations defined by a sample of local calibrators. In
both bands we find the mean luminosity at a given line width for extreme
late-type spirals to lie below that predicted by standard Tully-Fisher
relations. While many of the extreme late-type spirals do follow the
Tully-Fisher relation to within our observational uncertainties, most of these
galaxies lie below the normal, linear Tully-Fisher relation, and some are
underluminous by more than 2 sigma (i.e. >1.16 magnitudes in V). This suggests
a possible downward curvature of the Tully-Fisher relation for some of the
smallest and faintest rotationally supported disk galaxies. This may be a
consequence of the increasing prevalence of dark matter in these systems. We
find the deviation from the Tully-Fisher relation to increase with decreasing
luminosity and decreasing optical linear size in our sample, implying that the
physically smallest and faintest spirals may be a structurally and
kinematically distinct class of objects.Comment: 32 pages, 13 figures; to appear in the November A
Radio Continuum Emission in Polar-Ring Galaxies
We have used the Very Large Array aperture synthesis telescope to conduct a
radio continuum survey of polar-ring galaxies, at 20cm and 6cm. Forty objects
were observed at 20cm with 5" resolution. Twenty (50%) of the program sources
were detected at 20cm, down to our 5-sigma limit of 0.5 mJy/beam. This
detection rate is similar to those in surveys with comparable sensitivity for
early-type galaxies without polar rings. Sixteen of the objects we detected at
20cm were also observed at 6cm. We show radio continuum maps for the five
objects in our sample that have noticeably extended emission. Our spatial
resolution was sufficient to distinguish between emission originating in the
host galaxy from that in the polar ring. The radio morphology of the extended
sources, as well as the radio to far-infrared flux ratio and the radio spectral
indices of our detected sources, indicate that star formation, not nuclear
activity, is the dominant source of the radio continuum emission in polar-ring
galaxies. However, the implied star-formation rates are modest, and only one of
our sample galaxies will consume its supply of cool gas within 500 Myr.Comment: 21 pages, 7 figures. Produced with AASTeX 5.2 To appear in November
2004 Astronomical Journa
Rational Design of Photoelectrodes for the Fully Integrated Polymer Electrode MembraneâPhotoelectrochemical Water-Splitting System: A Case Study of Bismuth Vanadate
Photoelectrochemical (PEC) reactors based on polymer electrolyte membrane (PEM) electrolyzers are an attractive alternative to improve scalability compared to conventional monolithic devices. To introduce narrow band gap photoabsorbers such as BiVO4 in PEM-PEC system requires cost-effective and scalable deposition techniques beyond those previously demonstrated on monolithic FTO-coated glass substrates, followed by the preparation of membrane electrode assemblies. Herein, we address the significant challenges in coating narrow band gap metal-oxides on porous substrates as suitable photoelectrodes for the PEM-PEC configuration. In particular, we demonstrate the deposition and integration of W-doped BiVO4 on porous conductive substrates by a simple, cost-effective, and scalable deposition based on the SILAR (successive ionic layer adsorption and reaction) technique. The resultant W-doped BiVO4 photoanode exhibits a photocurrent density of 2.1 mA·cmâ2, @1.23V vs RHE, the highest reported so far for the BiVO4 on any porous substrates. Furthermore, we integrated the BiVO4 on the PEM-PEC reactor to demonstrate the solar hydrogen production from ambient air with humidity as the only water source, retaining 1.55 mA·cmâ2, @1.23V vs RHE. The concept provides insights into the features necessary for the successful development of materials suitable for the PEM-PEC tandem configuration reactors and the gas-phase operation of the reactor, which is a promising approach for low-cost, large-scale solar hydrogen production.</p
Neutral Gas Distribution and Kinematics of the Nearly Face-on Spiral Galaxy NGC 1232
We have analyzed high velocity resolution HI synthesis observations of the
nearly face-on Sc galaxy NGC 1232. The neutral gas distribution extends well
beyond the optical extent of the galaxy. As expected, local peaks in the HI
column density are associated with the spiral arms. Further, the HI column
density drops precipitously near the center of the galaxy. Closed contours in
the velocity field suggest either that the system is warped, or that the
rotation curve declines. The velocity dispersion is approximately constant
throughout the system, with a median value of 9.9 +/- 1.8 km/s. When corrected
for rotational broadening, there is no indication of a radial trend in the
neutral gas velocity dispersion in this galaxy.Comment: 14 pages of text, 10 pages of figures. Accepted to the A
The Photometric and Kinematic Structure of Face-On Disk Galaxies. I. Sample Definition, H-alpha Integral Field Spectroscopy, and HI Line-Widths
We present a survey of the photometric and kinematic properties of 39 nearby,
nearly face-on disk galaxies. Our approach exploits echelle-resolution
integral-field spectroscopy of the H-alpha regions, obtained with DensePak on
the WIYN 3.5m telescope Bench Spectrograph. This data is complemented by HI
line-profiles observed with the Nancay radio telescope for 25 of these sample
galaxies. Twelve additional line-widths are available for sample galaxies from
the literature. In this paper, we introduce the goals of this survey, define
the sample selection algorithm, and amass the integral field spectroscopic data
and HI line-widths. We establish spatially-integrated H-alpha line-widths for
the sample. We test the veracity of these spatially-integrated line profiles by
convolving narrow-band imaging data with velocity field information for one of
the sample galaxies, PGC 38268, and also by comparing to HI line profiles. We
find HI and H-alpha line profiles to be similar in width but different in
shape, indicating we are observing different spatial distributions of ionized
and neutral gas in largely axisymmetric systems with flat outer
rotation-curves. We also find vertical velocity dispersions of the ionized disk
gas within several disk scale-lengths have a median value of 18 km/s and an 80%
range of 12-26 km/s. This is only a factor of ~2 larger than what is observed
for neutral atomic and molecular gas. With standard assumptions for intrinsic
and thermal broadening for H-alpha, this translates into a factor of three
range in turbulent velocities, between 8 and 25 km/s.Comment: 29 pages, 20 figures; accepted for publication in ApJ Supplement
Serie
Evidence for tidal interaction and a supergiant HI shell in the Local Group dwarf galaxy NGC 6822
We present a wide-field, high spatial and velocity resolution map of the
entire extended HI distribution of the Local Group dwarf galaxy NGC 6822. The
observations were obtained with the Australia Telescope Compact Array in
mosaicing mode. The interstellar medium of NGC 6822 is shaped by the presence
of numerous H{\sc i} holes and shells, including a supergiant shell, and the
effects of tidal interaction, in the form of a tidal arm and an infalling or
interacting HI complex. The HI shell is situated outside the optical galaxy and
occupies roughly a quarter of the area of the main HI disk. It measures 2.0
times 1.4 kpc, making it one of the largest supergiant HI shells ever found.
The giant hole shows no signs of expansion and no obvious creation mechanism is
evident from our data. If star formation was the cause, an energy equivalent of
\~100 supernovae (10^53 erg) is needed to create the hole. We derive an upper
limit for the age of order 100 Myr. The presence of a possible tidal arm
indicates that NGC 6822 may recently have undergone some interaction. An HI
complex located in the north-west of the galaxy may be the interaction partner.
We argue that it is likely that these features were created about 100 Myr ago
in an event that also enhanced the star formation rateComment: Accepted for publication in Astrophysical Journal Letters (needs
emulateapj5.sty, included
Gas-Phase Oxygen Gradients in Strongly Interacting Galaxies: I. Early-Stage Interactions
A consensus is emerging that interacting galaxies show depressed nuclear gas
metallicities compared to isolated star-forming galaxies. Simulations suggest
that this nuclear underabundance is caused by interaction-induced inflow of
metal-poor gas, and that this inflow concurrently flattens the radial
metallicity gradients in strongly interacting galaxies. We present
metallicities of over 300 HII regions in a sample of 16 spirals that are
members of strongly interacting galaxy pairs with mass ratio near unity. The
deprojected radial gradients in these galaxies are about half of those in a
control sample of isolated, late-type spirals. Detailed comparison of the
gradients with simulations show remarkable agreement in gradient distributions,
the relationship between gradients and nuclear underabundances, and the shape
of profile deviations from a straight line. Taken together, this evidence
conclusively demonstrates that strongly interacting galaxies at the present day
undergo nuclear metal dilution due to gas inflow, as well as significant
flattening of their gas-phase metallicity gradients, and that current
simulations can robustly reproduce this behavior at a statistical level.Comment: Accepted for publication in Ap
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