1,906 research outputs found
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
Magnetic fields from reionisation
We present a complementary study to a new model for generating magnetic
fields of cosmological interest. The driving mechanism is the photoionisation
process by photons provided by the first luminous sources. Investigating the
transient regime at the onset of inhomogeneous reionisation, we show that
magnetic field amplitudes as high as Gauss can be obtained
within a source lifetime. Photons with energies above the ionisation threshold
accelerate electrons, inducing magnetic fields outside the Stroemgren spheres
which surround the ionising sources. Thanks to their mean free path, photons
with higher energies propagate further and lead to magnetic field generation
deeper in the neutral medium. We find that soft X-ray photons could contribute
to a significant premagnetisation of the intergalactic medium at a redshift of
z=15.Comment: accepted for publication in A&
Enhancing the gain by quantum coherence in terahertz quantum cascade lasers
We propose and study GaAs/AlGaAs terahertz frequency quantum cascade lasers in which mid-infrared radiation is used as a coherent drive for enhancing the terahertz gain
Limits on dust emission from z~5 LBGs and their local environments
We present 1.2mm MAMBO-2 observations of a field which is over-dense in Lyman
Break Galaxies (LBGs) at z~5. The field includes seven
spectroscopically-confirmed LBGs contained within a narrow (z=4.95+/-0.08)
redshift range and an eighth at z=5.2. We do not detect any individual source
to a limit of 1.6 mJy/beam (2*rms). When stacking the flux from the positions
of all eight galaxies, we obtain a limit to the average 1.2 mm flux of these
sources of 0.6mJy/beam. This limit is consistent with FIR imaging in other
fields which are over-dense in UV-bright galaxies at z~5. Independently and
combined, these limits constrain the FIR luminosity (8-1000 micron) to a
typical z~5 LBG of LFIR<~3x10^11 Lsun, implying a dust mass of Mdust<~10^8 Msun
(both assuming a grey body at 30K). This LFIR limit is an order of magnitude
fainter than the LFIR of lower redshift sub-mm sources (z~1-3). We see no
emission from any other sources within the field at the above level. While this
is not unexpected given millimetre source counts, the clustered LBGs trace
significantly over-dense large scale structure in the field at z = 4.95. The
lack of any such detection in either this or the previous work, implies that
massive, obscured star-forming galaxies may not always trace the same
structures as over-densities of LBGs, at least on the length scale probed here.
We briefly discuss the implications of these results for future observations
with ALMA.Comment: 10 pages, 6 figures, MNRAS Accepte
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Ex vivo normothermic perfusion of isolated segmental porcine bowel: a novel functional model of the small intestine.
BACKGROUND: There is an unmet need for suitable ex vivo large animal models in experimental gastroenterology and intestinal transplantation. This study details a reliable and effective technique for ex vivo normothermic perfusion (EVNP) of segmental porcine small intestine. METHODS: Segments of small intestine, 1.5-3.0 m in length, were retrieved from terminally anaesthetized pigs. After a period of cold ischaemia, EVNP was performed for 2 h at 37°C with a mean pressure of 80 mmHg using oxygenated autologous blood diluted with Ringer's solution. The duration of EVNP was extended to 4 h for a second set of experiments in which two segments of proximal to mid-ileum (1.5-3.0 m) were retrieved from each animal and reperfused with whole blood (control) or leucocyte-depleted blood to examine the impact of leucocyte depletion on reperfusion injury. RESULTS: After a mean cold ischaemia time of 5 h and 20 min, EVNP was performed in an initial group of four pigs. In the second set of experiments, five pigs were used in each group. In all experiments bowel segments were well perfused and exhibited peristalsis during EVNP. Venous glucose levels significantly increased following luminal glucose stimulation (mean(s.e.m.) basal level 1.8(0.6) mmol/l versus peak 15.5(5.8) mmol/l; P < 0.001) and glucagon-like peptide 1 (GLP-1) levels increased in all experiments, demonstrating intact absorptive and secretory intestinal functions. There were no significant differences between control and leucocyte-depleted animals regarding blood flow, venous glucose, GLP-1 levels or histopathology at the end of 4 h of EVNP. CONCLUSIONS: This novel model is suitable for the investigation of gastrointestinal physiology, pathology and ischaemia reperfusion injury, along with evaluation of potential therapeutic interventions
Whole-exome sequencing gives additional benefits compared to candidate gene sequencing in the molecular diagnosis of children with growth hormone or IGF-1 insensitivity
Ipsen UK!(HLS).
Sandoz Pharmaceutical
Galaxy Formation in Preheated Intergalactic Media
We outline a scenario of galaxy formation in which the gas in galaxy-forming
regions was preheated to high entropy by vigorous energy feedback associated
with the formation of stars in old ellipticals and bulges and with AGN
activity. Such preheating likely occurred at redshifts z ~ 2-3, and can produce
the entropy excess observed today in low-mass clusters of galaxies without
destroying the bulk of the Lyman alpha forest. Subsequent galaxy formation is
affected by the preheating, because the gas no longer follows the dark matter
on galaxy scales. The hot gas around galaxy haloes has very shallow profiles
and emits only weakly in the X-ray. Cooling in a preheated halo is not
inside-out, because the cooling efficiency does not change significantly with
radius. Only part of the gas in a protogalaxy region can cool and be accreted
into the final galaxy halo. The accreted gas is likely in diffuse clouds and so
does not lose angular momentum to the dark matter. Cluster ellipticals are
produced by mergers of stellar systems formed prior to the preheating, while
large galaxy disks form in low-density environments where gas accretion can
continue to the present time.Comment: 11 pages, 7 figures, MNRAS submitte
Simulation of radiation driven wind from disc galaxies
We present 2-D hydrodynamic simulation of rotating galactic winds driven by
radiation. We study the structure and dynamics of the cool and/or warm
component( K) which is mixed with dust. We have taken into
account the total gravity of a galactic system that consists of a disc, a bulge
and a dark matter halo. We find that the combined effect of gravity and
radiation pressure from a realistic disc drives the gas away to a distance of
kpc in Myr for typical galactic parameters. The outflow
speed increases rapidly with the disc Eddington parameter ) for . We find that the rotation speed of
the outflowing gas is km s. The wind is confined in a
cone which mostly consist of low angular momentum gas lifted from the central
region.Comment: 10 pages, 11 figures, Accepted for publication in MNRA
Probing Hot Gas in Galaxy Groups through the Sunyaev-Zeldovich Effect
We investigate the potential of exploiting the Sunyaev-Zeldovich effect (SZE)
to study the properties of hot gas in galaxy groups. It is shown that, with
upcoming SZE surveys, one can stack SZE maps around galaxy groups of similar
halo masses selected from large galaxy redshift surveys to study the hot gas in
halos represented by galaxy groups. We use various models for the hot halo gas
to study how the expected SZE signals are affected by gas fraction, equation of
state, halo concentration, and cosmology. Comparing the model predictions with
the sensitivities expected from the SPT, ACT and Planck surveys shows that a
SPT-like survey can provide stringent constraints on the hot gas properties for
halos with masses M ~> 10^{13} h^{-1}Msun. We also explore the idea of using
the cross correlation between hot gas and galaxies of different luminosity to
probe the hot gas in dark matter halos without identifying galaxy groups to
represent dark halos. Our results show that, with a galaxy survey as large as
the Sloan Digital Sky Survey and with the help of the conditional luminosity
function (CLF) model, one can obtain stringent constraints on the hot gas
properties in halos with masses down to 10^{13} h^{-1}Msun. Thus, the upcoming
SZE surveys should provide a very promising avenue to probe the hot gas in
relatively low-mass halos where the majority of L*-galaxies reside.Comment: 22 pages, 16 figures, accepted for publication on MNRA
Galaxy morphology and evolution from SWAN Adaptive Optics imaging
We present the results from adaptive optics (AO) assisted imaging in the Ks
band of an area of 15 arcmin^2 for SWAN (Survey of a Wide Area with NACO). We
derive the high resolution near-IR morphology of ~400 galaxies up to Ks~23.5 in
the first 21 SWAN fields around bright guide stars, carefully taking into
account the survey selection effects and using an accurate treatment of the
anisoplanatic AO PSF. The detected galaxies are sorted into two morphological
classes according to their Sersic index. The extracted morphological properties
and number counts of the galaxies are compared with the predictions of
different galaxy formation and evolution models, both for the whole galaxy
population and separately for late-type and early-type galaxies. This is one of
the first times such a comparison has been done in the near-IR, as AO
observations and accurate PSF modeling are needed to obtain reliable
morphological classification of faint field galaxies at these wavelengths. For
early-type galaxies we find that a pure luminosity evolution model, without
evidence for relevant number and size evolution, better reproduces the observed
properties of our Ks-selected sample than current semi-analytic models based on
the hierarchical picture of galaxy formation. In particular, we find that the
observed flattening of elliptical galaxy counts at Ks~20 is quantitatively in
good agreement with the prediction of the pure luminosity evolution model that
was calculated prior to the observation. For late-type galaxies, while both
models are able to reproduce the number counts, we find some hints of a
possible size growth. These results demonstrate the unique power of AO
observations to derive high resolution details of faint galaxies' morphology in
the near-IR and drive studies of galaxy evolution.Comment: 15 pages, 10 figures. A&A, in press. Final version with corrected
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