Showing papers by "University of Hertfordshire published in 2012"
TL;DR: The distinction between personal identity and self-conception is a well-honed distinction between who we are (call it our ontological self) and who we think we are, and this too seems to work at its best once you drop it as mentioned in this paper.
Abstract: Some time ago, I met a very bright and lively graduate, who registered with Facebook during the academic year 2003–2004, when she was a student at Harvard. Her Facebook ID number was 246. Impressive. A bit like being the 246th person to land on a new continent. Such Facebook ID numbers no longer exist. In a few years, that continent has become rather crowded, as she has been joined by several hundreds of million users worldwide. Half a billion was reached in July 2010. It is a good reminder of how more and more people spend an increasing amount of time ‘onlife’, interacting with and within an infosphere that is neither entirely virtual nor only physical. It is also a good reminder of how influential information and communication technologies are becoming in shaping our personal identities, as technologies of the self. In the philosophy of mind, there is a well-honed distinction between personal identity and self-conception or more simply between who we are (call it our ontological self) and who we think we are (call it our epistemological self). Like many other handy distinctions, this too seems to work at its best once you drop it. Like a Wittgensteinian ladder, it helps you to reach a better perspective, as long as you do not get stuck on it. Of course, there is a difference between being and believing to be. However, it is equally obvious that, in healthy individuals, the ontological and the epistemological selves flourish only if they support each other in a symbiotic relationship. Not only our self-conceptions should be close to who we really are. Our ontological selves are also sufficiently malleable to be significantly influenced by who we think we are or would like to be. And such epistemological selves in turn are sufficiently ductile to be shaped by who we are told to be. Enter the social self:
1,675 citations
TL;DR: The aim of this work is to provoke a more systematic analysis of the causes of the decline in R&D efficiency, and discusses four factors that it considers to be primary causes: the 'better than the Beatles' problem; the 'cautious regulator' problem'; the 'throw money at it' tendency; and the 'basic research–brute force' bias.
Abstract: The past 60 years have seen huge advances in many of the scientific, technological and managerial factors that should tend to raise the efficiency of commercial drug research and development (RD). Yet the number of new drugs approved per billion US dollars spent on RD has halved roughly every 9 years since 1950, falling around 80-fold in inflation-adjusted terms. There have been many proposed solutions to the problem of declining RD efficiency. However, their apparent lack of impact so far and the contrast between improving inputs and declining output in terms of the number of new drugs make it sensible to ask whether the underlying problems have been correctly diagnosed. Here, we discuss four factors that we consider to be primary causes, which we call the 'better than the Beatles' problem; the 'cautious regulator' problem; the 'throw money at it' tendency; and the 'basic research-brute force' bias. Our aim is to provoke a more systematic analysis of the causes of the decline in RD efficiency.
1,565 citations
San Jose State University1, Ames Research Center2, Las Cumbres Observatory Global Telescope Network3, Harvard University4, University of California, Berkeley5, University of Florida6, Pennsylvania State University7, Georgia State University8, NASA Exoplanet Science Institute9, California Institute of Technology10, Carnegie Institution for Science11, University of Copenhagen12, Aarhus University13, University of Texas at Austin14, Massachusetts Institute of Technology15, Search for extraterrestrial intelligence16, Lawrence Hall of Science17, University of Hertfordshire18, Villanova University19, Fermilab20, Princeton University21, San Diego State University22
TL;DR: In this paper, the authors used the noise-weighted robust averaging of multi-quarter photo-center offsets derived from difference image analysis, which identifies likely background eclipsing binaries.
Abstract: New transiting planet candidates are identified in sixteen months (May 2009 - September 2010) of data from the Kepler spacecraft. Nearly five thousand periodic transit-like signals are vetted against astrophysical and instrumental false positives yielding 1,091 viable new planet candidates, bringing the total count up to over 2,300. Improved vetting metrics are employed, contributing to higher catalog reliability. Most notable is the noise-weighted robust averaging of multi-quarter photo-center offsets derived from difference image analysis which identifies likely background eclipsing binaries. Twenty-two months of photometry are used for the purpose of characterizing each of the new candidates. Ephemerides (transit epoch, T_0, and orbital period, P) are tabulated as well as the products of light curve modeling: reduced radius (Rp/R*), reduced semi-major axis (d/R*), and impact parameter (b). The largest fractional increases are seen for the smallest planet candidates (197% for candidates smaller than 2Re compared to 52% for candidates larger than 2Re) and those at longer orbital periods (123% for candidates outside of 50-day orbits versus 85% for candidates inside of 50-day orbits). The gains are larger than expected from increasing the observing window from thirteen months (Quarter 1-- Quarter 5) to sixteen months (Quarter 1 -- Quarter 6). This demonstrates the benefit of continued development of pipeline analysis software. The fraction of all host stars with multiple candidates has grown from 17% to 20%, and the paucity of short-period giant planets in multiple systems is still evident. The progression toward smaller planets at longer orbital periods with each new catalog release suggests that Earth-size planets in the Habitable Zone are forthcoming if, indeed, such planets are abundant.
1,162 citations
University of California, Berkeley1, Ames Research Center2, San Jose State University3, Lowell Observatory4, Jet Propulsion Laboratory5, University of Texas at Austin6, Harvard University7, Las Cumbres Observatory Global Telescope Network8, Space Telescope Science Institute9, Niels Bohr Institute10, Aarhus University11, National Center for Atmospheric Research12, NASA Exoplanet Science Institute13, Massachusetts Institute of Technology14, Fermilab15, University of California, Santa Cruz16, Yale University17, University of Florida18, California Institute of Technology19, University of California, Santa Barbara20, University of Hertfordshire21, San Diego State University22, Carnegie Institution for Science23, Lawrence Hall of Science24, Villanova University25
TL;DR: In this paper, the authors report the distribution of planets as a function of planet radius, orbital period, and stellar effective temperature for orbital periods less than 50 days around solar-type (GK) stars.
Abstract: We report the distribution of planets as a function of planet radius, orbital period, and stellar effective temperature for orbital periods less than 50 days around solar-type (GK) stars. These results are based on the 1235 planets (formally "planet candidates") from the Kepler mission that include a nearly complete set of detected planets as small as 2 R_⊕. For each of the 156,000 target stars, we assess the detectability of planets as a function of planet radius, R_p, and orbital period, P, using a measure of the detection efficiency for each star. We also correct for the geometric probability of transit, R_*/a. We consider first Kepler target stars within the "solar subset" having T_eff = 4100-6100 K, log g = 4.0-4.9, and Kepler magnitude K_p 2 R_⊕ we measure an occurrence of less than 0.001 planets per star. For all planets with orbital periods less than 50 days, we measure occurrence of 0.130 ± 0.008, 0.023 ± 0.003, and 0.013 ± 0.002 planets per star for planets with radii 2-4, 4-8, and 8-32 R_⊕, in agreement with Doppler surveys. We fit occurrence as a function of P to a power-law model with an exponential cutoff below a critical period P_0. For smaller planets, P_0 has larger values, suggesting that the "parking distance" for migrating planets moves outward with decreasing planet size. We also measured planet occurrence over a broader stellar T_eff range of 3600-7100 K, spanning M0 to F2 dwarfs. Over this range, the occurrence of 2-4 R_⊕ planets in the Kepler field increases with decreasing T_eff, with these small planets being seven times more abundant around cool stars (3600-4100 K) than the hottest stars in our sample (6600-7100 K).
1,159 citations
TL;DR: Although there are a set of fault prediction studies in which confidence is possible, more studies are needed that use a reliable methodology and which report their context, methodology, and performance comprehensively.
Abstract: Background: The accurate prediction of where faults are likely to occur in code can help direct test effort, reduce costs, and improve the quality of software. Objective: We investigate how the context of models, the independent variables used, and the modeling techniques applied influence the performance of fault prediction models. Method: We used a systematic literature review to identify 208 fault prediction studies published from January 2000 to December 2010. We synthesize the quantitative and qualitative results of 36 studies which report sufficient contextual and methodological information according to the criteria we develop and apply. Results: The models that perform well tend to be based on simple modeling techniques such as Naive Bayes or Logistic Regression. Combinations of independent variables have been used by models that perform well. Feature selection has been applied to these combinations when models are performing particularly well. Conclusion: The methodology used to build models seems to be influential to predictive performance. Although there are a set of fault prediction studies in which confidence is possible, more studies are needed that use a reliable methodology and which report their context, methodology, and performance comprehensively.
1,012 citations
University of Sussex1, Jet Propulsion Laboratory2, California Institute of Technology3, European Space Agency4, Ames Research Center5, University of Edinburgh6, Paris Diderot University7, Imperial College London8, University of Paris-Sud9, Aix-Marseille University10, Cornell University11, University of La Laguna12, Spanish National Research Council13, Complutense University of Madrid14, UK Astronomy Technology Centre15, University of Colorado Boulder16, University of California, Irvine17, Goddard Space Flight Center18, University of Nottingham19, Cardiff University20, University of Padua21, Institut d'Astrophysique de Paris22, University of Cambridge23, University of British Columbia24, European Space Research and Technology Centre25, University of Manchester26, University College London27, Rutherford Appleton Laboratory28, University of Lethbridge29, University of Oxford30, Commonwealth Scientific and Industrial Research Organisation31, University of Hertfordshire32, Harvard University33
TL;DR: The Herschel Multi-tiered Extragalactic Survey (HerMES) is a legacy program designed to map a set of nested fields totalling ∼380deg^2 as mentioned in this paper.
Abstract: The Herschel Multi-tiered Extragalactic Survey (HerMES) is a legacy programme designed to map a set of nested fields totalling ∼380 deg^2. Fields range in size from 0.01 to ∼20 deg^2, using the Herschel-Spectral and Photometric Imaging Receiver (SPIRE) (at 250, 350 and 500 μm) and the Herschel-Photodetector Array Camera and Spectrometer (PACS) (at 100 and 160 μm), with an additional wider component of 270 deg^2 with SPIRE alone. These bands cover the peak of the redshifted thermal spectral energy distribution from interstellar dust and thus capture the reprocessed optical and ultraviolet radiation from star formation that has been absorbed by dust, and are critical for forming a complete multiwavelength understanding of galaxy formation and evolution.
The survey will detect of the order of 100 000 galaxies at 5σ in some of the best-studied fields in the sky. Additionally, HerMES is closely coordinated with the PACS Evolutionary Probe survey. Making maximum use of the full spectrum of ancillary data, from radio to X-ray wavelengths, it is designed to facilitate redshift determination, rapidly identify unusual objects and understand the relationships between thermal emission from dust and other processes. Scientific questions HerMES will be used to answer include the total infrared emission of galaxies, the evolution of the luminosity function, the clustering properties of dusty galaxies and the properties of populations of galaxies which lie below the confusion limit through lensing and statistical techniques.
This paper defines the survey observations and data products, outlines the primary scientific goals of the HerMES team, and reviews some of the early results.
852 citations
University of Copenhagen1, Harvard University2, Lund University3, Ames Research Center4, San Jose State University5, University of Texas at Austin6, California Institute of Technology7, University of Florida8, Space Telescope Science Institute9, University of California, Berkeley10, Bowling Green State University11, University of Hertfordshire12, Rensselaer Polytechnic Institute13, University of California, Santa Barbara14, Las Cumbres Observatory Global Telescope Network15
TL;DR: Spectroscopic metallicities of the host stars of 226 small exoplanet candidates discovered by NASA's Kepler mission are reported, finding that planets with radii less than four Earth radii form around host stars with a wide range of metallicities (but on average a metallicity close to that of the Sun), whereas large planets preferentially form around stars with higher metallicities.
Abstract: The abundance of heavy elements (metallicity) in the photospheres of stars similar to the Sun provides a 'fossil' record of the chemical composition of the initial protoplanetary disk. Metal-rich stars are much more likely to harbour gas giant planets(1-4), supporting the model that planets form by accumulation of dust and ice particles(5). Recent ground-based surveys suggest that this correlation is weakened for Neptunian-sized planets(4,6-9). However, how the relationship between size and metallicity extends into the regime of terrestrial-sized exoplanets is unknown. Here we report spectroscopic metallicities of the host stars of 226 small exoplanet candidates discovered by NASA's Kepler mission(10), including objects that are comparable in size to the terrestrial planets in the Solar System. We find that planets with radii less than four Earth radii form around host stars with a wide range of metallicities (but on average a metallicity close to that of the Sun), whereas large planets preferentially form around stars with higher metallicities. This observation suggests that terrestrial planets may be widespread in the disk of the Galaxy, with no special requirement of enhanced metallicity for their formation.
743 citations
University of Sussex1, Jet Propulsion Laboratory2, California Institute of Technology3, European Space Agency4, Ames Research Center5, University of Edinburgh6, Paris Diderot University7, Imperial College London8, Aix-Marseille University9, Cornell University10, University of La Laguna11, Spanish National Research Council12, Complutense University of Madrid13, UK Astronomy Technology Centre14, University of Colorado Boulder15, University of California, Irvine16, Goddard Space Flight Center17, University of Nottingham18, Cardiff University19, University of Padua20, Institut d'Astrophysique de Paris21, University of Cambridge22, University of British Columbia23, European Space Research and Technology Centre24, University of Manchester25, University College London26, University of Lethbridge27, Rutherford Appleton Laboratory28, University of Oxford29, Commonwealth Scientific and Industrial Research Organisation30, University of Hertfordshire31, Harvard University32
TL;DR: The Herschel Multi-tiered Extragalactic Survey (HerMES) is a legacy program designed to map a set of nested fields totalling ~380 deg^2 as mentioned in this paper.
Abstract: The Herschel Multi-tiered Extragalactic Survey, HerMES, is a legacy program designed to map a set of nested fields totalling ~380 deg^2. Fields range in size from 0.01 to ~20 deg^2, using Herschel-SPIRE (at 250, 350 and 500 \mu m), and Herschel-PACS (at 100 and 160 \mu m), with an additional wider component of 270 deg^2 with SPIRE alone. These bands cover the peak of the redshifted thermal spectral energy distribution from interstellar dust and thus capture the re-processed optical and ultra-violet radiation from star formation that has been absorbed by dust, and are critical for forming a complete multi-wavelength understanding of galaxy formation and evolution.
The survey will detect of order 100,000 galaxies at 5\sigma in some of the best studied fields in the sky. Additionally, HerMES is closely coordinated with the PACS Evolutionary Probe survey. Making maximum use of the full spectrum of ancillary data, from radio to X-ray wavelengths, it is designed to: facilitate redshift determination; rapidly identify unusual objects; and understand the relationships between thermal emission from dust and other processes. Scientific questions HerMES will be used to answer include: the total infrared emission of galaxies; the evolution of the luminosity function; the clustering properties of dusty galaxies; and the properties of populations of galaxies which lie below the confusion limit through lensing and statistical techniques.
This paper defines the survey observations and data products, outlines the primary scientific goals of the HerMES team, and reviews some of the early results.
707 citations
Book•
14 Dec 2012TL;DR: Hutto and Myin this article defend the counter-thesis that there can be intentionality and phenomenal experience without content, and demonstrate the advantages of their approach for thinking about scaffolded minds and consciousness.
Abstract: Most of what humans do and experience is best understood in terms of dynamically unfolding interactions with the environment. Many philosophers and cognitive scientists now acknowledge the critical importance of situated, environment-involving embodied engagements as a means of understanding basic minds -- including basic forms of human mentality. Yet many of these same theorists hold fast to the view that basic minds are necessarily or essentially contentful -- that they represent conditions the world might be in. In this book, Daniel Hutto and Erik Myin promote the cause of a radically enactive, embodied approach to cognition that holds that some kinds of minds -- basic minds -- are neither best explained by processes involving the manipulation of contents nor inherently contentful. Hutto and Myin oppose the widely endorsed thesis that cognition always and everywhere involves content. They defend the counter-thesis that there can be intentionality and phenomenal experience without content, and demonstrate the advantages of their approach for thinking about scaffolded minds and consciousness
688 citations
University of Oxford1, University of California, Berkeley2, Centre national de la recherche scientifique3, Paris Diderot University4, University of Massachusetts Amherst5, European Southern Observatory6, Leiden University7, École Normale Supérieure8, University of Lyon9, Max Planck Society10, ASTRON11, Kapteyn Astronomical Institute12, University of Hertfordshire13, Swinburne University of Technology14, University of Toronto15
TL;DR: A study of the two-dimensional stellar kinematics for the large representative ATLAS3D sample of nearby early- type galaxies spanning two orders of magnitude in stellar mass, using detailed dynamical models finds a strong systematic variation in IMF in early-type galaxies as a function of their stellar mass-to-light ratios, implying that a galaxy’s IMF depends intimately on the galaxy's formation history.
Abstract: Much of our knowledge of galaxies comes from analysing the radiation emitted by their stars, which depends on the present number of each type of star in the galaxy. The present number depends on the stellar initial mass function (IMF), which describes the distribution of stellar masses when the population formed, and knowledge of it is critical to almost every aspect of galaxy evolution. More than 50 years after the first IMF determination, no consensus has emerged on whether it is universal among different types of galaxies. Previous studies indicated that the IMF and the dark matter fraction in galaxy centres cannot both be universal, but they could not convincingly discriminate between the two possibilities. Only recently were indications found that massive elliptical galaxies may not have the same IMF as the Milky Way. Here we report a study of the two-dimensional stellar kinematics for the large representative ATLAS(3D) sample of nearby early-type galaxies spanning two orders of magnitude in stellar mass, using detailed dynamical models. We find a strong systematic variation in IMF in early-type galaxies as a function of their stellar mass-to-light ratios, producing differences of a factor of up to three in galactic stellar mass. This implies that a galaxy's IMF depends intimately on the galaxy's formation history
639 citations
TL;DR: The meta-analysis estimated the population effect sizes of 25 potential risk factors for PTSD in children and adolescents aged 6-18 years and supports the cognitive model of PTSD as a way of understanding its development and guiding interventions to reduce symptoms.
Leibniz Institute for Astrophysics Potsdam1, Max Planck Society2, Durham University3, University of Maryland, College Park4, University of Victoria5, Heidelberg University6, Heidelberg Institute for Theoretical Studies7, University of Zurich8, University of Washington9, McMaster University10, Leiden University11, Swinburne University of Technology12, University of Hertfordshire13, Australian National University14, INAF15, University of Trieste16, University of Tsukuba17, University of Antwerp18
TL;DR: In this article, the authors compare the results of various cosmological gas-dynamical codes used to simulate the formation of a galaxy in the Λ cold dark matter structure formation paradigm.
Abstract: We compare the results of various cosmological gas-dynamical codes used to simulate the formation of a galaxy in the Λ cold dark matter structure formation paradigm. The various runs (13 in total) differ in their numerical hydrodynamical treatment [smoothed particle hydrodynamics (SPH), moving mesh and adaptive mesh refinement] but share the same initial conditions and adopt in each case their latest published model of gas cooling, star formation and feedback. Despite the common halo assembly history, we find large code-to-code variations in the stellar mass, size, morphology and gas content of the galaxy at z= 0, due mainly to the different implementations of star formation and feedback. Compared with observation, most codes tend to produce an overly massive galaxy, smaller and less gas rich than typical spirals, with a massive bulge and a declining rotation curve. A stellar disc is discernible in most simulations, although its prominence varies widely from code to code. There is a well-defined trend between the effects of feedback and the severity of the disagreement with observed spirals. In general, models that are more effective at limiting the baryonic mass of the galaxy come closer to matching observed galaxy scaling laws, but often to the detriment of the disc component. Although numerical convergence is not particularly good for any of the codes, our conclusions hold at two different numerical resolutions. Some differences can also be traced to the different numerical techniques; for example, more gas seems able to cool and become available for star formation in grid-based codes than in SPH. However, this effect is small compared to the variations induced by different feedback prescriptions. We conclude that state-of-the-art simulations cannot yet uniquely predict the properties of the baryonic component of a galaxy, even when the assembly history of its host halo is fully specified. Developing feedback algorithms that can effectively regulate the mass of a galaxy without hindering the formation of high angular momentum stellar discs remains a challenge.
TL;DR: A review of the emerging international literature in this area, and linked to a wider conceptual review undertaken as part of a major project researching recovery practice in the UK, can be found in this paper.
Abstract: Although there is now increasing evidence as to the role played by social factors in contributing to the onset of mental health difficulties, there has been little systematic examination of the role that social factors can play in enabling (or impeding) recovery. This paper provides a review of the emerging international literature in this area, and is linked to a wider conceptual review undertaken as part of a major project researching recovery practice in the UK. Research findings are explored in detail in relation to three areas that had been identified by the wider review as central to recovery: empowerment and control over one's life; connectedness (including both inter-personal relationships and social inclusion); and rebuilding positive identities (often within the context of stigma and discrimination). Out of this emerges a clearer picture of the importance of particular social factors, which starts to define a more broad-based and proactive agenda for mental health social work—with an emphasis not just on working with individuals, but also on engaging with families and communities. However, there is a need for further research and development work in order to determine how to intervene most effectively in order to influence specific social factors.
Pontifical Catholic University of Chile1, Princeton University2, University of Hertfordshire3, European Southern Observatory4, Atacama Large Millimeter Submillimeter Array5, University of Cambridge6, University of Edinburgh7, University of Manchester8, Queen Mary University of London9, University of La Serena10, University of Lisbon11, Instituto de Astronomía Teórica y Experimental12, INAF13, University of Warsaw14, University of Concepción15, Valparaiso University16, National University of Cordoba17, University of Florida18, National Scientific and Technical Research Council19, University of São Paulo20, National University of La Plata21, University of Padua22, University of Wisconsin–Whitewater23, Universidade Federal do Rio Grande do Sul24, University of Chile25, Kyung Hee University26, Peking University27, Max Planck Society28, University of Alicante29, University College London30, University of Cincinnati31, University of Leeds32, Ames Research Center33, UK Astronomy Technology Centre34, Spanish National Research Council35, University of La Laguna36, University of Southampton37, Saint Mary's University38, Australian Astronomical Observatory39, Macquarie University40, Andrés Bello National University41, Hartebeesthoek Radio Astronomy Observatory42, Aryabhatta Research Institute of Observational Sciences43, University of Kent44
TL;DR: The ESO VISTA public survey VISTA variables in the V�a L�ctea (VVV) started in 2010 and is expected to run for about five years.
Abstract: Context The ESO public survey VISTA variables in the V�a L�ctea (VVV) started in 2010 VVV targets 562 sq deg in the Galactic bulge and an adjacent plane region and is expected to run for about five years Aims: We describe the progress of the survey observations in the first observing season, the observing strategy, and quality of the data obtained Methods: The observations are carried out on the 4-m VISTA telescope in the ZYJHK s filters In addition to the multi-band imaging the variability monitoring campaign in the K s filter has started Data reduction is carried out using the pipeline at the Cambridge Astronomical Survey Unit The photometric and astrometric calibration is performed via the numerous 2MASS sources observed in each pointing Results: The first data release contains the aperture photometry and astrometric catalogues for 348 individual pointings in the ZYJHK s filters taken in the 2010 observing season The typical image quality is 09 arcsec {-10 arcsec} The stringent photometric and image quality requirements of the survey are satisfied in 100% of the JHK s images in the disk area and 90% of the JHK s images in the bulge area The completeness in the Z and Y images is 84% in the disk, and 40% in the bulge The first season catalogues contain 128 � 10 8 stellar sources in the bulge and 168 � 10 8 in the disk area detected in at least one of the photometric bands The combined, multi-band catalogues contain more than 163 � 10 8 stellar sources About 10% of these are double detections because of overlapping adjacent pointings These overlapping multiple detections are used to characterise the quality of the data The images in the JHK s bands extend typically 4 mag deeper than 2MASS The magnitude limit and photometric quality depend strongly on crowding in the inner Galactic regions The astrometry for K s = 15-18 mag has rms 35-175 mas Conclusions: The VVV Survey data products offer a unique dataset to map the stellar populations in the Galactic bulge and the adjacent plane and provide an exciting new tool for the study of the structure, content, and star-formation history of our Galaxy, as well as for investigations of the newly discovered star clusters, star-forming regions in the disk, high proper motion stars, asteroids, planetary nebulae, and other interesting objects Based on observations taken within the ESO VISTA Public Survey VVV, Programme ID 179B-2002
TL;DR: The principle that dual targeting may be achieved using genetically targeted T-cells is demonstrated and paved the way for testing of this strategy in vivo.
Abstract: Chimeric antigen receptor (CAR) engineered T-cells occupy an increasing niche in cancer immunotherapy. In this context, CAR-mediated CD3ζ signaling is sufficient to elicit cytotoxicity and interferon-γ production while the additional provision of CD28-mediated signal 2 promotes T-cell proliferation and interleukin (IL)-2 production. This compartmentalisation of signaling opens the possibility that complementary CARs could be used to focus T-cell activation within the tumor microenvironment. Here, we have tested this principle by co-expressing an ErbB2- and MUC1-specific CAR that signal using CD3ζ and CD28 respectively. Stoichiometric co-expression of transgenes was achieved using the SFG retroviral vector containing an intervening Thosea asigna peptide. We found that “dual-targeted” T-cells kill ErbB2+ tumor cells efficiently and proliferate in a manner that requires co-expression of MUC1 and ErbB2 by target cells. Notably, however, IL-2 production was modest when compared to control CAR-engineered T-cells in which signaling is delivered by a fused CD28 + CD3ζ endodomain. These findings demonstrate the principle that dual targeting may be achieved using genetically targeted T-cells and pave the way for testing of this strategy in vivo.
ASTRON1, Kapteyn Astronomical Institute2, University of California, Berkeley3, École normale supérieure de Lyon4, European Southern Observatory5, Paris Diderot University6, University of Oxford7, University of Massachusetts Amherst8, Leiden University9, Max Planck Society10, University of Hertfordshire11, University of Toronto12, New Mexico Institute of Mining and Technology13
Abstract: We present the ATLAS3D H i survey of a volume-limited, complete sample of 166 nearby early-type galaxies (ETGs) brighter than MK=-21.5. The survey is mostly based on data taken with the Westerbork Synthesis Radio Telescope, which enables us to detect H i down to 5 x 1065 x 107 M? within the survey volume. We detect similar to 40 per cent of all ETGs outside the Virgo galaxy cluster and similar to 10 per cent of all ETGs inside it. This demonstrates that it is common for non-cluster ETGs to host H i. The morphology of the detected gas varies in a continuous way from regular, settled H i discs and rings to unsettled gas distributions (including tidal or accretion tails) and systems of clouds scattered around the galaxy. The majority of the detections consist of H i discs or rings (1/4 of all ETGs outside Virgo) so that if H i is detected in an ETG it is most likely distributed on a settled configuration. These systems come in two main types: small discs [ M?], which are confined within the stellar body and share the same kinematics of the stars; and large discs/rings [M(H i) up to 5 x 109 M?], which extend to tens of kpc from the host galaxy and are in half of the cases kinematically decoupled from the stars. Neutral hydrogen seems to provide material for star formation in ETGs. Galaxies containing H i within similar to 1Re exhibit signatures of on-going star formation in similar to 70 per cent of the cases, approximately five times more frequently than galaxies without central H i. The interstellar medium (ISM) in the centre of these galaxies is dominated by molecular gas, and in ETGs with a small gas disc the conversion of H i into H2 is as efficient as in spirals. The ETG H i mass function is characterized by M*similar to 2 x 109 M? and by a slope a similar to-0.7. Compared to spirals, ETGs host much less H i as a family. However, a significant fraction of all ETGs are as H i-rich as spiral galaxies. The main difference between ETGs and spirals is that the former lack the high-column-density H i typical of the bright stellar disc of the latter. The ETG H i properties vary with environment density in a more continuous way than suggested by the known Virgo versus non-Virgo dichotomy. We find an envelope of decreasing M(H i) and M(H i)/LK with increasing environment density. The gas-richest galaxies live in the poorest environments (as found also with CO observations), where the detection rate of star formation signatures is higher. Galaxies in the centre of Virgo have the lowest H i content, while galaxies at the outskirts of Virgo represent a transition region and can contain significant amounts of H i, indicating that at least a fraction of them has joined the cluster only recently after pre-processing in groups. Finally, we find an H i morphologydensity relation such that at low environment density (measured on a local scale) the detected H i is mostly distributed on large, regular discs and rings, while more disturbed H i morphologies dominate environment densities typical of rich groups. This confirms the importance of processes occurring on a galaxy-group scale for the evolution of ETGs.
Book•
17 Aug 2012TL;DR: In this paper, the authors present a survey of the UHRA's work in the field of computer vision and artificial intelligence, focusing on the use of data from the Internet.
Abstract: Original book is available at : http://books.google.com/ [Full text of this book is not available in the UHRA]
TL;DR: The results provide an initial molecular framework for the integration with BRs of additional pathways that control plant development and provide biochemical evidence, both in vitro and in vivo, that GAI inactivates the transcriptional regulatory activity of BZR1 upon their interaction by inhibiting the ability of BzR1 to bind to target promoters.
Abstract: Plant development is modulated by the convergence of multiple environmental and endogenous signals, and the mechanisms that allow the integration of different signaling pathways is currently being unveiled. A paradigmatic case is the concurrence of brassinosteroid (BR) and gibberellin (GA) signaling in the control of cell expansion during photomorphogenesis, which is supported by physiological observations in several plants but for which no molecular mechanism has been proposed. In this work, we show that the integration of these two signaling pathways occurs through the physical interaction between the DELLA protein GAI, which is a major negative regulator of the GA pathway, and BRASSINAZOLE RESISTANT1 (BZR1), a transcription factor that broadly regulates gene expression in response to BRs. We provide biochemical evidence, both in vitro and in vivo, indicating that GAI inactivates the transcriptional regulatory activity of BZR1 upon their interaction by inhibiting the ability of BZR1 to bind to target promoters. The physiological relevance of this interaction was confirmed by the observation that the dominant gai-1 allele interferes with BR-regulated gene expression, whereas the bzr1-1D allele displays enhanced resistance to DELLA accumulation during hypocotyl elongation. Because DELLA proteins mediate the response to multiple environmental signals, our results provide an initial molecular framework for the integration with BRs of additional pathways that control plant development.
TL;DR: In vivo pharmacokinetic and efficacy data for compound 4k are presented, demonstrating the potential of this series of compounds for the treatment of Parkinson’s disease.
Abstract: Potent, ligand efficient, selective, and orally efficacious 1,2,4-triazine derivatives have been identified using structure based drug design approaches as antagonists of the adenosine A2A receptor. The X-ray crystal structures of compounds 4e and 4g bound to the GPCR illustrate that the molecules bind deeply inside the orthosteric binding cavity. In vivo pharmacokinetic and efficacy data for compound 4k are presented, demonstrating the potential of this series of compounds for the treatment of Parkinson’s disease.
TL;DR: Applying associative transcriptomics, which uses transcriptome sequencing to identify and score molecular markers representing variation in both gene sequences and gene expression, and correlate this with trait variation, facilitates the application of association genetics in a broad range of crops, even those with complex genomes.
Abstract: Sequencing a genome and identifying genetic markers lays the groundwork for genome-wide association studies, but can be difficult to achieve for polyploid species. Harper et al. present an approach for performing association studies using genetic maps and markers generated from transcriptome sequencing data alone and apply it to the polyploid crop Brassica napus.
Finnish Meteorological Institute1, University of Helsinki2, University of Manchester3, Danish Meteorological Institute4, Swedish Meteorological and Hydrological Institute5, University of Aveiro6, Central Institution for Meteorology and Geodynamics7, European Centre for Medium-Range Weather Forecasts8, Aristotle University of Thessaloniki9, University of Hertfordshire10, University of Eastern Finland11, Technical University of Madrid12, The Cyprus Institute13, National and Kapodistrian University of Athens14, Free University of Berlin15, University of Cologne16, Academy of Sciences of the Czech Republic17
TL;DR: In this article, chemical weather forecasting models are described and compared on regional and continental scales in Europe, and the most prominent gaps of knowledge are highlighted for the following selected focus areas: emission inventories, the integration of numerical weather prediction and atmospheric chemical transport models, boundary conditions and nesting of models, data assimilation of the various chemical species, improved understanding and parameterization of physical processes, better evaluation of models against data and the construction of model ensembles.
Abstract: Numerical models that combine weather forecasting and atmospheric chemistry are here referred to as chemical weather forecasting models. Eighteen operational chemical weather forecasting models on regional and continental scales in Europe are described and compared in this article. Topics discussed in this article include how weather forecasting and atmospheric chemistry models are integrated into chemical weather forecasting systems, how physical processes are incorporated into the models through parameterization schemes, how the model architecture affects the predicted variables, and how air chemistry and aerosol processes are formulated. In addition, we discuss sensitivity analysis and evaluation of the models, user operational requirements, such as model availability and documentation, and output availability and dissemination. In this manner, this article allows for the evaluation of the relative strengths and weaknesses of the various modelling systems and modelling approaches. Finally, this article highlights the most prominent gaps of knowledge for chemical weather forecasting models and suggests potential priorities for future research directions, for the following selected focus areas: emission inventories, the integration of numerical weather prediction and atmospheric chemical transport models, boundary conditions and nesting of models, data assimilation of the various chemical species, improved understanding and parameterization of physical processes, better evaluation of models against data and the construction of model ensembles. © 2012 Author(s).
TL;DR: In this paper, the authors used stacking techniques to perform the first sensitive search for CO emission in dwarf galaxies outside the Local Group ranging from individual lines of sight, stacking over IR-bright regions of embedded star formation, and stacking over the entire galaxy.
Abstract: We present maps of {sup 12}COJ = 2-1 emission covering the entire star-forming disks of 16 nearby dwarf galaxies observed by the IRAM HERACLES survey. The data have 13'' angular resolution, {approx}250 pc at our average distance of D = 4 Mpc, and sample the galaxies by 10-1000 resolution elements. We apply stacking techniques to perform the first sensitive search for CO emission in dwarf galaxies outside the Local Group ranging from individual lines of sight, stacking over IR-bright regions of embedded star formation, and stacking over the entire galaxy. We detect five galaxies in CO with total CO luminosities of L{sub CO2-1} = (3-28) Multiplication-Sign 10{sup 6} K km s{sup -1} pc{sup 2}. The other 11 galaxies remain undetected in CO even in the stacked images and have L{sub CO2-1} {approx}< (0.4-8) Multiplication-Sign 10{sup 6} K km s{sup -1} pc{sup 2}. We combine our sample of dwarf galaxies with a large sample of spiral galaxies from the literature to study scaling relations of L{sub CO} with M{sub B} and metallicity. We find that dwarf galaxies with metallicities of Z Almost-Equal-To 1/2-1/10 Z{sub Sun} have L{sub CO} of 2-4 orders of magnitude smaller than massive spiral galaxies and that theirmore » L{sub CO} per unit L{sub B} is 1-2 orders of magnitude smaller. A comparison with tracers of star formation (FUV and 24 {mu}m) shows that L{sub CO} per unit star formation rate (SFR) is 1-2 orders of magnitude smaller in dwarf galaxies. One possible interpretation is that dwarf galaxies form stars much more efficiently: we argue that the low L{sub CO}/SFR ratio is due to the fact that the CO-to-H{sub 2} conversion factor, {alpha}{sub CO}, changes significantly in low-metallicity environments. Assuming that a constant H{sub 2} depletion time of {tau}{sub dep} = 1.8 Gyr holds in dwarf galaxies (as found for a large sample of nearby spirals) implies {alpha}{sub CO} values for dwarf galaxies with Z Almost-Equal-To 1/2-1/10 Z{sub Sun} that are more than one order of magnitude higher than those found in solar metallicity spiral galaxies. Such a significant increase of {alpha}{sub CO} at low metallicity is consistent with previous studies, in particular those of Local Group dwarf galaxies that model dust emission to constrain H{sub 2} masses. Even though it is difficult to parameterize the dependence of {alpha}{sub CO} on metallicity given the currently available data, the results suggest that CO is increasingly difficult to detect at lower metallicities. This has direct consequences for the detectability of star-forming galaxies at high redshift, which presumably have on average sub-solar metallicity.« less
University of California, Santa Cruz1, University of Florida2, Fermilab3, Ames Research Center4, Search for extraterrestrial intelligence5, Harvard University6, San Jose State University7, University of Copenhagen8, University of Texas at Austin9, Yale University10, San Francisco State University11, University of Hertfordshire12, University of California, Berkeley13, Tel Aviv University14, University of California, Santa Barbara15, Las Cumbres Observatory Global Telescope Network16
TL;DR: In this article, the authors present four sets of light curves from the Kepler spacecraft, each of which shows multiple planets transiting the same star, and report dynamical fits to the transit times, yielding possible values for the planets' masses and eccentricities.
Abstract: Eighty planetary systems of two or more planets are known to orbit stars other than the Sun. For most, the data can be sufficiently explained by non-interacting Keplerian orbits, so the dynamical interactions of these systems have not been observed. Here we present four sets of light curves from the Kepler spacecraft, each which of shows multiple planets transiting the same star. Departure of the timing of these transits from strict periodicity indicates that the planets are perturbing each other: the observed timing variations match the forcing frequency of the other planet. This confirms that these objects are in the same system. Next we limit their masses to the planetary regime by requiring the system remain stable for astronomical timescales. Finally, we report dynamical fits to the transit times, yielding possible values for the planets' masses and eccentricities. As the timespan of timing data increases, dynamical fits may allow detailed constraints on the systems' architectures, even in cases for which high-precision Doppler follow-up is impractical.
TL;DR: There is no evidence that one colloid solution is more effective or safe than any other, although the confidence intervals are wide and do not exclude clinically significant differences between colloids.
Abstract: Original article can be found at: http://www3.interscience.wiley.com Copyright John Wiley and Sons. ‘This review is published as a Cochrane Review in the Cochrane Database of Systematic Reviews 2003, Issue 1. Cochrane Reviews are regularly updated as new evidence emerges and in response to comments and criticisms, and the Cochrane Database of Systematic Reviews should be consulted for the most recent version of the Review.’ Bunn, F. , Alderson, P. and Hawkins, V. (2003) 'Colloid solutions for fluid resuscitation'. Cochrane Database of Systematic Reviews (1) CD001319 DOI: 10.1002/14651858.CD001319
Ames Research Center1, University of Edinburgh2, University of Leicester3, Spanish National Research Council4, Complutense University of Madrid5, California Institute of Technology6, University of Sussex7, Goddard Space Flight Center8, University of Nottingham9, Cardiff University10, University of Padua11, UK Astronomy Technology Centre12, European Space Research and Technology Centre13, University of Manchester14, Institut d'Astrophysique de Paris15, University of British Columbia16, University of Hertfordshire17, Harvard University18
TL;DR: Submillimetre and X-rays observations show that rapid star formation was common in the host galaxies of AGN when the Universe was 2–6 billion years old, but that the most vigorous star formation is not observed around black holes above an X-ray luminosity of 1044 ergs per second.
Abstract: The old, red stars that constitute the bulges of galaxies, and the massive black holes at their centres, are the relics of a period in cosmic history when galaxies formed stars at remarkable rates and active galactic nuclei (AGN) shone brightly as a result of accretion onto black holes. It is widely suspected, but unproved, that the tight correlation between the mass of the black hole and the mass of the stellar bulge1 results from the AGN quenching the surrounding star formation as it approaches its peak luminosity2, 3, 4. X-rays trace emission from AGN unambiguously5, whereas powerful star-forming galaxies are usually dust-obscured and are brightest at infrared and submillimetre wavelengths6. Here we report submillimetre and X-ray observations that show that rapid star formation was common in the host galaxies of AGN when the Universe was 2-6 billion years old, but that the most vigorous star formation is not observed around black holes above an X-ray luminosity of 1044 ergs per second. This suppression of star formation in the host galaxy of a powerful AGN is a key prediction of models in which the AGN drives an outflow7, 8, 9, expelling the interstellar medium of its host and transforming the galaxy's properties in a brief period of cosmic time
TL;DR: A meta-analysis of neurocognitive data from 15 studies revealed a consistent male advantage on verbal and visuospatial tasks and tests of episodic and semantic memory, and it was shown that age, education level, and dementia severity did not significantly predict the male advantage.
Abstract: Studies reporting on the cognitive abilities of men and women with Alzheimer's disease (AD) are surprisingly rare. We carried out a meta-analysis of neurocognitive data from 15 studies (n = 828 men; 1,238 women), which revealed a consistent male advantage on verbal and visuospatial tasks and tests of episodic and semantic memory. Moderator regression analyses showed that age, education level, and dementia severity did not significantly predict the male advantage. Reasons posited for this advantage include a reduction of estrogen in postmenopausal women, sex differences in AD pathology, and greater cognitive reserve in men.
TL;DR: A systematic review of qualitative studies conducted by Frances Bunn and colleagues identifies and describes the experiences of patients and caregivers on receiving and adapting to a diagnosis of dementia.
Abstract: Background
Early diagnosis and intervention for people with dementia is increasingly considered a priority, but practitioners are concerned with the effects of earlier diagnosis and interventions on patients and caregivers. This systematic review evaluates the qualitative evidence about how people accommodate and adapt to the diagnosis of dementia and its immediate consequences, to guide practice.
Methods and Findings
We systematically reviewed qualitative studies exploring experiences of community-dwelling individuals with dementia, and their carers, around diagnosis and the transition to becoming a person with dementia. We searched PubMed, PsychINFO, Embase, CINAHL, and the British Nursing Index (all searched in May 2010 with no date restrictions; PubMed search updated in February 2012), checked reference lists, and undertook citation searches in PubMed and Google Scholar (ongoing to September 2011). We used thematic synthesis to identify key themes, commonalities, barriers to earlier diagnosis, and support identified as helpful. We identified 126 papers reporting 102 studies including a total of 3,095 participants. Three overarching themes emerged from our analysis: (1) pathways through diagnosis, including its impact on identity, roles, and relationships; (2) resolving conflicts to accommodate a diagnosis, including the acceptability of support, focusing on the present or the future, and the use or avoidance of knowledge; and (3) strategies and support to minimise the impact of dementia. Consistent barriers to diagnosis include stigma, normalisation of symptoms, and lack of knowledge. Studies report a lack of specialist support particularly post-diagnosis.
Conclusions
There is an extensive body of qualitative literature on the experiences of community-dwelling individuals with dementia on receiving and adapting to a diagnosis of dementia. We present a thematic analysis that could be useful to professionals working with people with dementia. We suggest that research emphasis should shift towards the development and evaluation of interventions, particularly those providing support after diagnosis.
Please see later in the article for the Editors' Summary.
TL;DR: In this article, a physically motivated IR spectral energy distribution-based approach is presented to account for possible contributions to 24 µm emission not associated with recent star formation, and the authors compare a large suite of SFR estimates and find that the intrinsic uncertainty in H{alpha-and FUV-based SFRs is approximately 0.3 and 0.5 dex.
Abstract: Using combinations of H{alpha}, ultraviolet (UV), and infrared (IR) emission, we estimate the star formation rate (SFR) surface density, {Sigma}{sub SFR}, at 1 kpc resolution for 30 disk galaxies that are targets of the IRAM HERACLES CO survey. We present a new physically motivated IR spectral-energy-distribution-based approach to account for possible contributions to 24 {mu}m emission not associated with recent star formation. Considering a variety of 'reference' SFRs from the literature, we revisit the calibration of the 24 {mu}m term in hybrid (UV+IR or H{alpha}+IR) tracers. We show that the overall calibration of this term remains uncertain at the factor of two level because of the lack of wide-field, robust reference SFR estimates. Within this uncertainty, published calibrations represent a reasonable starting point for 1 kpc-wide areas of star-forming disk galaxies, but we re-derive and refine the calibration of the IR term in these tracers to match our resolution and approach to 24 {mu}m emission. We compare a large suite of {Sigma}{sub SFR} estimates and find that above {Sigma}{sub SFR} {approx} 10{sup -3} M{sub Sun} yr{sup -1} kpc{sup -2} the systematic differences among tracers are less than a factor of two across two orders of magnitude dynamic range. We cautionmore » that methodology and data both become serious issues below this level. We note from simple model considerations that when focusing on a part of a galaxy dominated by a single stellar population, the intrinsic uncertainty in H{alpha}- and FUV-based SFRs is {approx}0.3 and {approx}0.5 dex.« less
TL;DR: Although a high number of novel psychoactive substances have been identified in the 2-year duration of the project, not all have become trends that needed public health response and it is recommended that these monitoring activities are to be continued.
Abstract: Background This paper presents the outcomes of the 2-year European Union funded Psychonaut Web Mapping Project which aimed at developing and implementing an integrated web mapping system to promptly identify and learn about novel psychoactive substances (NPS; “legal highs”) through the regular monitoring of the Internet. Methods More than 200 discussion forums, social media, online shops, websites and other Internet resources (e.g. YouTube, eBay, Google, Google Insight) have been extensively and regularly monitored in 7 European countries (UK, Finland, Norway, Belgium, Germany, Italy and Spain) for emerging trends of NPS throughout the period of the study. Results Key online resources have been identified as “leading edge” which have provided accurate and timely information on novel emerging compounds. In total more than 400 substances/products have been recorded. NPS have been noted online before reaching wider audiences. Discussion Although a high number of novel psychoactive substances have been identified in the 2-year duration of the project, not all have become trends that needed public health response. Conversely, new recreational drug phenomena such as “spice drugs,” mephedrone and naphyrone were all identified as emerging trends in forums and websites. In addition, it has been possible for the first time to collate detailed information on these and several more compounds even though no or limited scientific publications were available. It is therefore recommended that these monitoring activities are to be continued, that more countries, researchers and health professionals are involved, and that the findings are widely shared with all the relevant agencies, health professionals and future research projects. Implications, advantages and limitations of using the Internet as primary source for identifying emerging trends are also discussed.
Argonne National Laboratory1, University of Chicago2, Lawrence Berkeley National Laboratory3, University of Illinois at Urbana–Champaign4, Fermilab5, University of the Western Cape6, University of Hertfordshire7, University of Sussex8, Federal University of Rio de Janeiro9, University of Pennsylvania10, University of Oxford11
TL;DR: In this article, the authors present an analysis of supernova light curves simulated for the upcoming DES supernova search using a code suite that generates and fits realistic light curves in order to obtain distance modulus/redshift pairs that are passed to a cosmology fitter.
Abstract: We present an analysis of supernova light curves simulated for the upcoming Dark Energy Survey (DES) supernova search. The simulations employ a code suite that generates and fits realistic light curves in order to obtain distance modulus/redshift pairs that are passed to a cosmology fitter. We investigated several different survey strategies including field selection, supernova selection biases, and photometric redshift measurements. Using the results of this study, we chose a 30 deg2 search area in the griz filter set. We forecast (1) that this survey will provide a homogeneous sample of up to 4000 Type Ia supernovae in the redshift range 0.05