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  • 1
    Publication Date: 2012-10-26
    Description: The interrelationship between brown adipose tissue (BAT) and white adipose tissue (WAT) is emerging as an important factor in obesity, but the effect of impairing non-shivering thermogenesis in BAT on lipid storage in WAT remains unclear. To address this, we have characterized the metabolic phenotype of a mouse model for Costeff syndrome, in which a point mutation in the mitochondrial membrane protein Opa3 impairs mitochondrial activity. Opa3 L122P mice displayed an 80% reduction in insulin-like growth factor 1, postnatal growth retardation and hepatic steatosis. A 90% reduction in uncoupling protein 1 (UCP1) expression in interscapular BAT was accompanied by a marked reduction in surface body temperature, with a 2.5-fold elevation in interscapular BAT mass and lipid storage. The sequestration of circulating lipid into BAT resulted in profound reductions in epididymal and retroperitoneal WAT mass, without affecting subcutaneous WAT. The histological appearance and intense mitochondrial staining in intra-abdominal WAT suggest significant ‘browning’, but with UCP1 expression in WAT of Opa3 L122P mice only 62% of that in wild-type littermates, any precursor differentiation does not appear to result in thermogenically active beige adipocytes. Thus, we have identified Opa3 as a novel regulator of lipid metabolism, coupling lipid uptake with lipid processing in liver and with thermogenesis in BAT. These findings indicate that skeletal and metabolic impairment in Costeff syndrome may be more significant than previously thought and that uncoupling lipid uptake from lipid metabolism in BAT may represent a novel approach to controlling WAT mass in obesity.
    Print ISSN: 0964-6906
    Electronic ISSN: 1460-2083
    Topics: Biology , Medicine
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  • 2
  • 3
    Publication Date: 2020-09-18
    Description: Summary The relatively short duration of the early stages of subduction results in a poor geological record, limiting our understanding of this critical stage. Here, we utilize a 2D numerical model of incipient subduction, that is the stage after a plate margin has formed with a slab tip that extends to a shallow depth and address the conditions under which subduction continues or fails. We assess energy budgets during the evolution from incipient subduction to either a failed or successful state, showing how the growth of potential energy, and slab pull, is resisted by the viscous dissipation within the lithosphere and the mantle. The role of rheology is also investigated, as deformation mechanisms operating in the crust and mantle facilitate subduction. In all models, the onset of subduction is characterized by high lithospheric viscous dissipation and low convergence velocities, whilst successful subduction sees the mantle become the main area of viscous dissipation. In contrast, failed subduction is defined by the lithospheric viscous dissipation exceeding the lithospheric potential energy release rate and velocities tend towards zero. We show that development of a subduction zone depends on the convergence rate, required to overcome thermal diffusion and to localise deformation along the margin. The results propose a minimum convergence rate of ∼ 0.5 cm yr−1 is required to reach a successful state, with 100 km of convergence over 20 Myr, emphasizing the critical role of the incipient stage.
    Print ISSN: 0956-540X
    Electronic ISSN: 1365-246X
    Topics: Geosciences
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  • 4
    Publication Date: 2016-08-03
    Description: In most studies of dust in galaxies, dust is only detected from its emission to approximately the optical radius of the galaxy. By combining the signal of 110 spiral galaxies observed as part of the Herschel Reference Survey, we are able to improve our sensitivity by an order of magnitude over that for a single object. Here we report the direct detection of dust from its emission that extends out to at least twice the optical radius. We find that the distribution of dust is consistent with an exponential at all radii with a gradient of ~–1.7 dex  $R_{25}^{-1}$ . Our dust temperature declines linearly from ~25 K in the centre to 15 K at R 25 from where it remains constant out to ~2.0  R 25 . The surface density of dust declines with radius at a similar rate to the surface density of stars but more slowly than the surface density of the star-formation rate. Studies based on dust extinction and reddening of high-redshift quasars have concluded that there are substantial amounts of dust in intergalactic space. By combining our results with the number counts and angular correlation function from the SDSS, we show that with Milky Way-type dust we can explain the reddening of the quasars by the dust within galactic discs alone. Given the uncertainties in the properties of any intergalactic dust, we cannot rule out its existence, but our results show that statistical investigations of the dust in galactic haloes that use the reddening of high-redshift objects must take account of the dust in galactic discs.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
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  • 5
    Publication Date: 2016-07-17
    Description: The existence of long (〉100 kpc) H i streams and small (〈20 kpc) free-floating H i clouds is well known. While the formation of the streams has been investigated extensively, and the isolated clouds are often purported to be interaction debris, little research has been done on the formation of optically dark H i clouds that are not part of a larger stream. One possibility is that such features result from the fragmentation of more extended streams, while another idea is that they are primordial, optically dark galaxies. We test the validity of the fragmentation scenario (via harassment) using numerical simulations. In order to compare our numerical models with observations, we present catalogues of both the known long H i streams (42 objects) and free-floating H i clouds suggested as dark galaxy candidates (51 objects). In particular, we investigate whether it is possible to form compact features with high velocity widths (〉100 km s –1 ), similar to observed clouds which are otherwise intriguing dark galaxy candidates. We find that producing such features is possible but extremely unlikely, occurring no more than 0.2% of the time in our simulations. In contrast, we find that genuine dark galaxies could be extremely stable to harassment and remain detectable even after 5 Gyr in the cluster environment (with the important caveat that our simulations only explore harassment and do not yet include the intracluster medium, heating and cooling, or star formation). We also discuss the possibility that such objects could be the progenitors of recently discovered ultra diffuse galaxies.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
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  • 6
    Publication Date: 2015-12-26
    Description: We have used data from the Next Generation Virgo Survey to investigate the dwarf galaxy population of the Virgo cluster. We mask and smooth the data, and then use the object detection algorithm SE xtractor to make our initial dwarf galaxy selection. All candidates are then visually inspected to remove artefacts and duplicates. We derive parameters to best select low surface brightness galaxies using central surface brightness values of $22.5 \le \mu ^{g}_{0} \le 26.0$ μg and exponential scale lengths of 3.0 ≤ h ≤ 10.0 arcsec to identify 443 cluster dwarf galaxies – 303 of which are new detections, with a surface density that decreases with radius from the cluster centre. We also apply our selection algorithm to ‘background’, non-cluster, fields and find zero detections. In combination, this leads us to believe that we have isolated a cluster dwarf galaxy population. The range of objects we detect is limited because smaller scale sized galaxies are confused with the background, while larger galaxies are split into numerous smaller objects by the detection algorithm. Combining our data with that from other surveys, we find a faint-end slope to the luminosity function of –1.35 ± 0.03, which is not significantly different to what has previously been found, but is a little steeper than the slope for field galaxies. There is no evidence for a faint-end slope steep enough to correspond with galaxy formation models, unless those models invoke either strong feedback processes or use warm dark matter.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
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  • 7
    Publication Date: 2016-03-09
    Description: We describe a far-infrared survey of the Coma cluster and the galaxy filament it resides within. Our survey covers an area of ~150 deg 2 observed by Herschel H-ATLAS ( Herschel Astrophysical Terahertz Large Area Survey) in five bands at 100, 160, 250, 350 and 500 μm. The SDSS spectroscopic survey ( m r ≤ 17.8) is used to define an area (within the virial radius) and redshift selected (4268 〈 v 〈 9700 km s –1 ) sample of 744 Coma cluster galaxies – the Coma Cluster Catalogue. For comparison, we also define a sample of 951 galaxies in the connecting filament – the Coma Filament Catalogue. The optical positions and parameters are used to define appropriate apertures to measure each galaxy's far-infrared emission. We have detected 99 of 744 (13 per cent) and 422 of 951 (44 per cent) of the cluster and filament galaxies in the SPIRE 250 μm band. We consider the relative detection rates of galaxies of different morphological types finding that it is only the S0/Sa population that shows clear differences between the cluster and filament. We find no differences between the dust masses and temperatures of cluster and filament galaxies with the exception of early-type galaxy dust temperatures, which are significantly hotter in the cluster than in the filament (X-ray heating?). From a chemical evolution model, we find no evidence for different evolutionary processes (gas loss or infall) between galaxies in the cluster and filament.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
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  • 8
    Publication Date: 2016-01-07
    Description: The IUPHAR/BPS Guide to PHARMACOLOGY (GtoPdb, http://www.guidetopharmacology.org ) provides expert-curated molecular interactions between successful and potential drugs and their targets in the human genome. Developed by the International Union of Basic and Clinical Pharmacology (IUPHAR) and the British Pharmacological Society (BPS), this resource, and its earlier incarnation as IUPHAR-DB, is described in our 2014 publication. This update incorporates changes over the intervening seven database releases. The unique model of content capture is based on established and new target class subcommittees collaborating with in-house curators. Most information comes from journal articles, but we now also index kinase cross-screening panels. Targets are specified by UniProtKB IDs. Small molecules are defined by PubChem Compound Identifiers (CIDs); ligand capture also includes peptides and clinical antibodies. We have extended the capture of ligands and targets linked via published quantitative binding data (e.g. K i , IC 50 or K d ). The resulting pharmacological relationship network now defines a data-supported druggable genome encompassing 7% of human proteins. The database also provides an expanded substrate for the biennially published compendium, the Concise Guide to PHARMACOLOGY . This article covers content increase, entity analysis, revised curation strategies, new website features and expanded download options.
    Print ISSN: 0305-1048
    Electronic ISSN: 1362-4962
    Topics: Biology
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  • 9
    Publication Date: 2015-12-20
    Description: As part of the H i Arecibo Galaxy Environment Survey (AGES), we have observed 5 x 4 deg of sky centred on M33, reaching a limiting column density of ~1.5 x 10 17  cm –2 (line width of 10 km s –1 and resolution 3.5 arcmin). We particularly investigate the absence of optically detected dwarf galaxies around M33, something that is contrary to galaxy formation models. We identify 22 discrete H i clouds, 11 of which are new detections. The number of objects detected and their internal velocity dispersion distribution is consistent with expectations from standard galaxy formation models. However, the issue remains open as to whether the observed velocity dispersions can be used as a measure of the H i clouds total mass, i.e. are the velocities indicative of virialized structures or have they been influenced by tidal interactions with other structures in the Local Group? We identify one particularly interesting H i cloud, AGESM33-31, that has many of the characteristics of H i distributed in the disc of a galaxy, yet there is no known optical counterpart associated with it. This object has a total H i mass of 1.22 x 10 7 M and a diameter of 18 kpc if at the distance of M33 ( D M33 = 840 kpc). However, we also find that there are numerous other H i clouds in this region of sky that have very similar velocities and so it is plausible that all these clouds are actually associated with debris from the Magellanic stream.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
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  • 10
    Publication Date: 2015-12-02
    Description: We have used the Arecibo L -band Feed Array (ALFA) to map three regions, each of 5 deg 2 , around the isolated galaxies NGC 1156, UGC 2082, and NGC 5523. In the vicinity of these galaxies we have detected two dwarf companions: one near UGC 2082, previously discovered by the Arecibo Legacy Fast ALFA (ALFALFA) survey, and one near NGC 1156, discovered by this project and reported in an earlier paper. This is significantly fewer than the $15.4^{+1.7}_{-1.5}$ that would be expected from the field H i mass function from ALFALFA or the 8.9 ± 1.2 expected if the H i mass function from the Local Group applied in these regions. The number of dwarf companions detected is, however, consistent with a flat or declining H i mass function as seen by a previous, shallower, H i search for companions to isolated galaxies. We attribute this difference in H i mass functions to the different environments in which they are measured. This agrees with the general observation that lower ratios of dwarf to giant galaxies are found in lower density environments.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
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