4,381 research outputs found
The Luminous Starburst Ring in NGC 7771: Sequential Star Formation?
Only two of the twenty highly luminous starburst galaxies analyzed by Smith
et al. exhibit circumnuclear rings of star formation. These galaxies provide a
link between 10^11 L_sun systems and classical, less-luminous ringed systems.
We report the discovery of a near-infrared counterpart to the nuclear ring of
radio emission in NGC 7771. A displacement between the ~10 radio bright clumps
and the ~10 near-infrared bright clumps indicates the presence of multiple
generations of star formation. The estimated thermal emission from each radio
source is equivalent to that of ~35000 O6 stars. Each near-infrared bright knot
contains ~5000 red supergiants, on average. The stellar mass of each knot is
estimated to be ~10^7 M_sun. The implied time-averaged star formation rate is
\~40 M_sun per yr. Several similarities are found between the properties of
this system and other ringed and non-ringed starbursts. Morphological
differences between NGC 7771 and the starburst + Seyfert 1 galaxy NGC 7469
suggest that NGC 7771 may not be old enough to fuel an AGN, or may not be
capable of fueling an AGN. Alternatively, the differences may be unrelated to
the presence or absence of an AGN and may simply reflect the possibility that
star formation in rings is episodic.Comment: accepted for publication in The Astrophysical Journal (10 January
1999); 48 pages including 13 figures; AAS LaTe
Smart Focal Plane Technologies for VLT Instruments
As we move towards the era of ELTs, it is timely to think about the future
role of the 8-m class telescopes. Under the OPTICON programme, novel
technologies have been developed that are intended for use in multi-object and
integral-field spectrographs. To date, these have been targeted at instrument
concepts for the European ELT, but there are also significant possibilities for
their inclusion in new VLT instruments, ensuring the continued success and
productivity of these unique telescopes.Comment: 5 pages, to appear in the proceedings of the ESO Workshop "Science
with the VLT in the ELT era
On the Origins of Starburst and Post-Starburst Galaxies in Nearby Clusters
HST WFPC2 images in B (F450W) and I (F814W) have been obtained for three
starburst (SB) and two post-starburst (PSB) galaxies in the Coma cluster, and
for three such galaxies in the cluster DC2048-52. V (F555W) and I images for an
additional PSB galaxy in Coma have been extracted from the archive. Seven of
these galaxies were previously classified as E/S0 on the basis of ground-based
images, one as Sa, and the other as an irregular.
The HST images reveal these SB/PSB galaxies to be heterogeneous in
morphology. Nevertheless a common theme is that many of them, especially the SB
galaxies, tend to have centralized spiral structure that appears simply as a
bright ``bulge''on ground-based images. In addition, while some PSB galaxies
exhibit distinct spiral structure, on the whole they have smoother morphologies
than the SB galaxies. The morphologies and luminosity profiles are generally
consistent with substantial starbursts in the form of centralized spiral
structure (the SB galaxies) which fade into smoother morphologies (the PSB
galaxies), with lingering spectroscopic evidence for past central starbursts.
An important point is that the PSB galaxies retain disks, i.e, they have not
evolved into spheroidal systems.Comment: 32 pages, 10 figures including 3 jpg images. To appear in the January
1999 Astronomical Journa
Chemical Analysis of Five Red Giants in the Globular Cluster M10 (NGC 6254)
We have determined Al, , Fe-peak, and neutron capture elemental
abundances for five red giant branch (RGB) stars in the Galactic globular
cluster M10. Abundances were determined using equivalent width analyses of
moderate resolution (R15,000) spectra obtained with the Hydra multifiber
positioner and bench spectrograph on the WIYN telescope. The data sample the
upper RGB from the luminosity level near the horizontal branch to about 0.5 mag
below the RGB tip. We find in agreement with previous studies that M10 is
moderately metal-poor with [Fe/H]=-1.45 (=0.04). All stars appear
enhanced in Al with =+0.33 ($\sigma$=0.19), but no stars have
[Al/Fe]$\ga$+0.55. We find the $\alpha$ elements to be enhanced by +0.20 to
+0.40 dex and the Fe--peak elements to have [el/Fe]$\sim$0, which are
consistent with predictions from type II SN ejecta. Additionally, the cluster
appears to be r-process rich with =+0.41.Comment: 16 Pages; 3 Figures; 3 Tables; Accepted for publication in PAS
Planck pre-launch status: HFI beam expectations from the optical optimisation of the focal plane
Planck is a European Space Agency (ESA) satellite, launched in May 2009, which will map the cosmic microwave background anisotropies in intensity and polarisation with unprecedented detail and sensitivity. It will also provide full-sky maps of astrophysical foregrounds. An accurate knowledge of the telescope beam patterns is an essential element for a correct analysis of the acquired astrophysical data. We present a detailed description of the optical design of the High Frequency Instrument (HFI) together with some of the optical performances measured during the calibration campaigns. We report on the evolution of the knowledge of the pre-launch HFI beam patterns when coupled to ideal telescope elements, and on their significance for the HFI data analysis procedure
The ALFALFA "Almost Darks" Campaign: Pilot VLA HI Observations of Five High Mass-to-Light Ratio Systems
We present VLA HI spectral line imaging of 5 sources discovered by ALFALFA.
These targets are drawn from a larger sample of systems that were not uniquely
identified with optical counterparts during ALFALFA processing, and as such
have unusually high HI mass to light ratios. These candidate "Almost Dark"
objects fall into 4 categories: 1) objects with nearby HI neighbors that are
likely of tidal origin; 2) objects that appear to be part of a system of
multiple HI sources, but which may not be tidal in origin; 3) objects isolated
from nearby ALFALFA HI detections, but located near a gas-poor early-type
galaxy; 4) apparently isolated sources, with no object of coincident redshift
within ~400 kpc. Roughly 75% of the 200 objects without identified counterparts
in the .40 database (Haynes et al. 2011) fall into category 1. This
pilot sample contains the first five sources observed as part of a larger
effort to characterize HI sources with no readily identifiable optical
counterpart at single dish resolution. These objects span a range of HI mass
[7.41 < log(M) < 9.51] and HI mass to B-band luminosity ratios (3 <
M/L < 9). We compare the HI total intensity and velocity
fields to SDSS optical imaging and to archival GALEX UV imaging. Four of the
sources with uncertain or no optical counterpart in the ALFALFA data are
identified with low surface brightness optical counterparts in SDSS imaging
when compared with VLA HI intensity maps, and appear to be galaxies with clear
signs of ordered rotation. One source (AGC 208602) is likely tidal in nature.
We find no "dark galaxies" in this limited sample. The present observations
reveal complex sources with suppressed star formation, highlighting both the
observational difficulties and the necessity of synthesis follow-up
observations to understand these extreme objects. (abridged)Comment: Astronomical Journal, in pres
The Low Surface Brightness Extent of the Fornax Cluster
We have used a large format CCD camera to survey the nearby Fornax cluster
and its immediate environment for low luminosity low surface brightness
galaxies. Recent observations indicate that these are the most dark matter
dominated galaxies known and so they are likely to be a good tracer of the dark
matter in clusters. We have identified large numbers of these galaxies
consistent with a steep faint end slope of the luminosity function (alpha~ -2)
down to MB ~ -12. These galaxies contribute almost the same amount to the total
cluster light as the brighter galaxies and they have a spatial extent that is
some four times larger. They satisfy two of the important predictions of N-body
hierarchical simulations of structure formation using dark halos. The
luminosity (mass ?) function is steep and the mass distribution is more
extended than that defined by the brighter galaxies. We also find a large
concentration of low surface brightness galaxies around the nearby galaxy
NGC1291.Comment: 16 pages, 6 figure
On the Lagrangian Dynamics of Atmospheric Zonal Jets and the Permeability of the Stratospheric Polar Vortex
The Lagrangian dynamics of zonal jets in the atmosphere are considered, with
particular attention paid to explaining why, under commonly encountered
conditions, zonal jets serve as barriers to meridional transport. The velocity
field is assumed to be two-dimensional and incompressible, and composed of a
steady zonal flow with an isolated maximum (a zonal jet) on which two or more
travelling Rossby waves are superimposed. The associated Lagrangian motion is
studied with the aid of KAM (Kolmogorov--Arnold--Moser) theory, including
nontrivial extensions of well-known results. These extensions include
applicability of the theory when the usual statements of nondegeneracy are
violated, and applicability of the theory to multiply periodic systems,
including the absence of Arnold diffusion in such systems. These results,
together with numerical simulations based on a model system, provide an
explanation of the mechanism by which zonal jets serve as barriers to
meridional transport of passive tracers under commonly encountered conditions.
Causes for the breakdown of such a barrier are discussed. It is argued that a
barrier of this type accounts for the sharp boundary of the Antarctic ozone
hole at the perimeter of the stratospheric polar vortex in the austral spring.Comment: Submitted to Journal of the Atmospheric Science
Smooth-filamental transition of active tracer fields stirred by chaotic advection
The spatial distribution of interacting chemical fields is investigated in
the non-diffusive limit. The evolution of fluid parcels is described by
independent dynamical systems driven by chaotic advection. The distribution can
be filamental or smooth depending on the relative strength of the dispersion
due to chaotic advection and the stability of the chemical dynamics. We give
the condition for the smooth-filamental transition and relate the H\"older
exponent of the filamental structure to the Lyapunov exponents. Theoretical
findings are illustrated by numerical experiments.Comment: 4 pages, 3 figure
Explosive Particle Dispersion in Plasma Turbulence
Particle dynamics are investigated in plasma turbulence, using
self-consistent kinetic simulations, in two dimensions. In steady state, the
trajectories of single protons and proton-pairs are studied, at different
values of plasma "beta" (ratio between kinetic and magnetic pressure). For
single-particle displacements, results are consistent with fluids and magnetic
field line dynamics, where particles undergo normal diffusion for very long
times, with higher "beta" being more diffusive. In an intermediate time range,
with separations lying in the inertial range, particles experience an explosive
dispersion in time, consistent with the Richardson prediction. These results,
obtained for the first time with a self-consistent kinetic model, are relevant
for astrophysical and laboratory plasmas, where turbulence is crucial for
heating, mixing and acceleration processes
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