1,178 research outputs found
A Group of Red, Ly-alpha Emitting, High Redshift Galaxies
We have discovered two new high redshift (z=2.38) galaxies, near the
previously known z=2.38 galaxy 2139-4434 B1 (Francis et al. 1996).
All three galaxies are strong Ly-alpha emitters, and have much redder
continuum colors (I-K about 5) than other optically-selected high redshift
galaxies. We hypothesize that these three galaxies are QSO IIs; radio-quiet
counterparts of high redshift radio galaxies, containing concealed QSO nuclei.
The red colors are most easily modelled by an old (> 0.5 Gyr), massive (> 10E11
solar masses) stellar population. If true, this implies that at least one
galaxy cluster of mass much greater than 3E11 solar masses had collapsed before
redshift five.Comment: 12 pages, 2 figures, uses aaspp4 style file. Accepted for publication
in Astrophysical Journal Letter
Thermal tolerance, climatic variability and latitude
The greater latitudinal extents of occurrence of species towards higher latitudes has been attributed to the broadening of physiological tolerances with latitude as a result of increases in climatic variation. While there is some support for such patterns in climate, the physiological tolerances of species across large latitudinal gradients have seldom been assessed. Here we report findings for insects based on published upper and lower lethal temperature data. The upper thermal limits show little geographical variation. In contrast, the lower bounds of supercooling points and lower lethal temperatures do indeed decline with latitude. However, this is not the case for the upper bounds, leading to an increase in the variation in lower lethal limits with latitude. These results provide some support for the physiological tolerance assumption associated with Rapoport's rule, but highlight the need for coupled data on species tolerances and range size
Galaxy Clusters and Large Scale Structure at High Redshifts
We present a detailed study of a rich galaxy cluster at z=2.38. We
demonstrate that this cluster contains large overdensities of damped Ly-alpha
absorption lines, of Ly-alpha emitting galaxies and of extremely red objects.
The overdensity of extremely red objects in this field demonstrates that many
are high z galaxies.
The huge overdensities we measure for these three classes of object are much
larger than the mass overdensities of typical clusters at this redshift, as
predicted by CDM and related models. We suggest therefore that the distribution
of damped Ly-alpha absorption line systems, of Ly-alpha emitting galaxies and
of extremely red objects are all very strongly biassed, and that somehow a
small overdensity of mass has increased the fraction of baryons in collapsed
objects, in the volume occupied by the cluster, to close to unity (a factor of
~10 increase).
We speculate that some unknown physical process, acting on the volume
occupied by our cluster, caused the normally diffuse ionised inter-galactic
medium to coalesce into small (< 10^8 Solar masses) blobs of neutral hydrogen,
which produce the Ly-alpha absorption-lines. Star formation occurred within
these blobs at z>5, enriching them with metals and producing stars, which after
several mergers and ~ 0.5 Gyr of passive evolution form the extremely red
objects. The Ly-alpha emitting galaxies are probably AGN, triggered perhaps by
mergers of the small blobs.Comment: Invited talk to appear in "The Young Universe", proceedings of Rome
conference, ed. D'Odorico, Fontana and Giallongo. 8 pages, uses paspconf.st
Superflares on Ordinary Solar-Type Stars
Short duration flares are well known to occur on cool main-sequence stars as
well as on many types of `exotic' stars. Ordinary main-sequence stars are
usually pictured as being static on time scales of millions or billions of
years. Our sun has occasional flares involving up to ergs which
produce optical brightenings too small in amplitude to be detected in
disk-integrated brightness. However, we identify nine cases of superflares
involving to ergs on normal solar-type stars. That is,
these stars are on or near the main-sequence, are of spectral class from F8 to
G8, are single (or in very wide binaries), are not rapid rotators, and are not
exceedingly young in age. This class of stars includes many those recently
discovered to have planets as well as our own Sun, and the consequences for any
life on surrounding planets could be profound. For the case of the Sun,
historical records suggest that no superflares have occurred in the last two
millennia.Comment: 16 pages, accepted for publication in Ap
Immunocytochemical demonstration of PTHrP protein in neoplastic tissue of HTLV-1 positive human adult T cell leukaemia/lymphoma: implications for the mechanism of hypercalcaemia.
The infiltrated tissues from seven West Indian patients with HTLV-1 positive adult T cell lymphoma/leukaemia (ATLL) have been analysed by immunocytochemical techniques for the presence of immunoreactive parathyroid hormone-related protein (PTHrP), a hormonal mediator of humoral hypercalcaemia of malignancy. Six of the seven were hypercalcaemic at some stage of the course of their disease. Four of the six evaluable patients showed evidence of specific cellular and extracellular expression of PTHrP protein in neoplastic tissues. This finding suggests that PTHrP may be involved in the production of hypercalcaemia in at least some cases of T cell lymphoma - proof of a causal relationship however must await the demonstration of tissue release of PTHrP resulting in raised circulating hormone levels
The evolution of plasticity of dauer larva developmental arrest in the nematode Caenorhabditis elegans.
Organisms can end up in unfavourable conditions and to survive this they have evolved various strategies. Some organisms, including nematodes, survive unfavourable conditions by undergoing developmental arrest. The model nematode Caenorhabditis elegans has a developmental choice between two larval forms, and it chooses to develop into the arrested dauer larva form in unfavourable conditions (specifically, a lack of food and high population density, indicated by the concentration of a pheromone). Wild C. elegans isolates vary extensively in their dauer larva arrest phenotypes, and this prompts the question of what selective pressures maintain such phenotypic diversity? To investigate this we grew C. elegans in four different environments, consisting of different combinations of cues that can induce dauer larva development: two combinations of food concentration (high and low) in the presence or absence of a dauer larva-inducing pheromone. Five generations of artificial selection of dauer larvae resulted in an overall increase in dauer larva formation in most selection regimes. The presence of pheromone in the environment selected for twice the number of dauer larvae, compared with environments not containing pheromone. Further, only a high food concentration environment containing pheromone increased the plasticity of dauer larva formation. These evolutionary responses also affected the timing of the worms' reproduction. Overall, these results give an insight into the environments that can select for different plasticities of C. elegans dauer larva arrest phenotypes, suggesting that different combinations of environmental cues can select for the diversity of phenotypically plastic responses seen in C. elegans.We would like to thank Henrique Teotonio for the gift of the G140.A population, Louise Hughes and Laura Weldon for technical help, two anonymous reviewers for their comments, and NERC for funding.This is the final published version of the article. It was originally published in Ecology and Evolution (Diaz SA, Viney M, Ecology and Evolution 2015, 5(6), 1343â1353, doi:10.1002/ece3.1436) http://dx.doi.org/10.1002/ece3.143
High Velocity Line Emission in the NLR of NGC 4151
Narrow-band imaging of the nuclear region of NGC 4151 with the Hubble Space
Telescope is presented. The filter bandpasses isolate line emission in various
high velocity ranges in several ions. Slitless and long-slit spectra of the
region with the Space Telescope Imaging Spectrograph also indicate the
locations of high velocity gas. These emission regions are faint and are
interspersed among the bright emission clouds seen in direct images. They have
radial velocities up to 1400 km/s relative to the nucleus, and are found in
both approach and recession on both sides of the nucleus. This contrasts
strongly with the bright emission line clouds which have been discussed
previously as showing bidirectional outflow with velocities within 400 km/s of
the nucleus. We discuss the possible connections of the high velocity material
with the radio jet and the nuclear radiation.Comment: 12 pages plus 6 figures, to be published in A
STIS Echelle Observations of the Seyfert Galaxy NGC 4151: Physical Conditions in the Ultraviolet Absorbers
We have examined the physical conditions in intrinsic UV-absorbing gas in the
Seyfert galaxy NGC 4151, using echelle spectra obtained with the Space
Telescope Imaging Spectrograph (STIS). We confirm the presence of the kinematic
components detected in earlier GHRS observations as well as a new broad
absorption feature at a radial velocity of -1680 km/s. The UV continuum of NGC
4151 decreased by a factor of 4 over the previous two years, and we argue the
changes in the column density of the low ionization absorption lines associated
with the broad component at -490 km/s reflect the decrease in the ionizing
flux. Most of the strong absorption lines (e.g., N V, C IV, Si IV) from this
component are saturated, but show substantial residual flux in their cores,
indicating that the absorber does not fully cover the source of emission. Our
interpretation is that the unocculted light is due to scattering by free
electrons from an extended region, which reflects continuum, emission lines,
and absorption lines. We have been able to constrain the densities for the
kinematic components based on absorption lines from metastable states of C III
and Fe II, and/or the ratios of ground and fine structure lines of O I,C II,
and Si II. We have generated a set of photoionization models which match the
ionic column densities for each component during the present low flux state and
those seen in previous high flux states with the GHRS and STIS, confirming that
the absorbers are photoionized and respond to the changes in the continuum
flux. We have been able to map the relative radial positions of the absorbers,
and find that the gas decreases in density with distance. None of the UV
absorbers is of sufficiently large column density or high enough ionization
state to account for the X-ray absorption.Comment: 46 pages (Latex), 14 figures (postscript), plus a landscape table
(Latex), to appear in the Astrophysical Journa
Flourescent liquid pyrene derivative-in-water mircoemulsions
A fluorescent liquid pyrene derivative with a high fluorescence quantum yield (65%) in the bulk state is reported. With this as the sole oil phase, stable luminescent oil-in-water microemulsions have been prepared. Increasing the loading of liquid pyrene swells the droplets, as detected by small-angle neutron scattering. These larger droplets have a greater proportion of pyrene excimer emission contribution in their photoluminescence spectra, which leads to a red shift in the chromaticity of the emission
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