bluuebunny/crossref_metadata_2025_split huggingface dataset:
High throughput sequencing of the Angiostrongylus cantonensis genome: a parasite spreading worldwide
Authors: MORASSUTTI ALESSANDRA L. , PERELYGIN ANDREY , DE CARVALHO MARCOS O. , LEMOS LEANDRO NASCIMENTO , PINTO PAULO MARCOS , FRACE MIKE , WILKINS PATRICIA P. , GRAEFF-TEIXEIRA CARLOS , DA SILVA ALEXANDRE J. 
Published: July 2013

SUMMARYAngiostrongylus cantonensis is a parasitic nematode of rodents and a leading aetiological agent of eosinophilic meningitis in humans. Definitive diagnosis is difficult, often relying on immunodiagnostic methods which utilize crude antigens. New immunodiagnostic methods based on recombinant proteins are being developed, and ideally these methods would be made available worldwide. Identification of diagnostic targets, as well as studies on the biology of the parasite, are limited by a lack of molecular information on Angiostrongylus spp. available in databases. In this study we present data collected from DNA random high-throughput sequencing together with proteomic analyses and a cDNA walking methodology to identify and obtain the nucleotide or amino acid sequences of unknown immunoreactive proteins. 28 080 putative ORFs were obtained, of which 3371 had homology to other deposited protein sequences. Using the A. cantonensis genomic sequences, 156 putative ORFs, matching peptide sequences obtained from previous proteomic studies, were considered novel, with no homology to existing sequences. Full-length coding sequences of eight antigenic target proteins were obtained. In this study we generated not only the complete nucleotide sequences of the antigenic protein targets but also a large amount of genomic data which may help facilitate future genomic, proteomic, transcriptomic or metabolomic studies on Angiostrongylus.
FACTORS INFLUENCING DECISION MAKING ON THERAPEUTIC INTERVENTIONS
Authors: Lee Sang Moo , Kim Gaeun , Ahn Jeonghoon , Suh Hae Sun , Heo Dae Seog 
Published: July 2013

Objectives: The aim of this study was to explore factors that influenced decision making in the assessment of new health technology in Korea.Methods: We analyzed the decision-making results of the Committee for New Health Technology Assessment (CnHTA) on fifty-three new nondrug health technologies in Korea from July 2007 to December 2010. The scope of the committee was mainly limited to safety and efficacy/effectiveness, and every decision was based on a systematic review of the literature. The committee was composed of healthcare professionals, policy makers, lawyers, and representatives from nongovernmental organizations. Decisions made on therapeutic interventions were included, while those on diagnostic procedures were excluded.Results: Factors that positively influenced decisions were lower complication rate than existing technology, similar or greater effectiveness compared with existing technology, ability to save critical organs, absence of alternative intervention, decreased invasiveness, expansion of patient's set of choices, and similarity to the mechanism of existing technology. Factors that negatively influenced decisions were higher complication rates than existing technology, lower effectiveness than comparable technology, low levels of evidence, unknown mechanisms of intervention, inconsistency, lack of long-term outcomes, lack of comparative data, nonstandardized technology, heterogeneity between control and treatment, excessively diverse indications, and nongeneralizability.Conclusions: This qualitative analysis of past decision-making results provided us with clues on the values that decision makers on the Korean CnHTA considered in terms of safety and effectiveness. These findings will help us develop appraisal guidelines and enhance the objectivity of decision-making processes in Korea.
HYPERBARIC OXYGEN THERAPY FOR DIABETIC ULCERS: SYSTEMATIC REVIEW AND META-ANALYSIS
Authors: O'Reilly Daria , Pasricha Anjori , Campbell Kaitryn , Burke Natasha , Assasi Nazila , Bowen James M. , Tarride Jean-Eric , Goeree Ron 
Published: July 2013

Objectives: Approximately 10–15 percent of individuals with diabetes mellitus develop foot ulcers, which precede 85 percent of amputations. Increased oxygen, through the use of hyperbaric oxygen therapy (HBOT), has been suggested to encourage ulcer healing thus reducing the risk of amputation. The objective of this systematic review is to evaluate the efficacy of systemic HBOT for nonhealing ulcers of the lower limb in diabetes patients.Methods: A systematic search, using controlled and keyword terms focusing on “HBOT” and “lower limb diabetic ulcers,” was conducted. Databases searched included Medline, EMBASE, CINAHL, PubMed, Wiley's Cochrane Library, and Biosis. Randomized controlled trials (RCTs) and observational studies were included. Pooled estimates of outcomes were determined when appropriate.Results: Of the 654 citations identified, 157 articles underwent full-text review. Data were abstracted from twelve publications (six RCTs and six comparative observational studies). Pooled analysis of the RCT and observational data showed that treatment with HBOT reduced the risk of major amputation by 60 percent (p = .29) and 61 percent (p = .003) compared with standard wound care, respectively. The RCT data revealed that the relative risk of having an unhealed wound following HBOT was 0.54 (p = .10) and 0.24 (p < .0001) based on observational data.Conclusions: Due to the limited RCT evidence, it is not possible to conclusively establish the benefits and harms of treating diabetic lower limb ulcers with HBOT. No significant effects on amputation rates were found in the RCT evidence and in the high quality studies, no difference was found.
Norm resolvent convergence of singularly scaled Schrödinger operators and δ′-potentials
Authors: Golovaty Yu. D. , Hryniv R. O. 
Published: July 2013

For a real-valued function V of the Faddeev–Marchenko class, we prove the norm-resolvent convergence, as ε → 0, of a family Sε of one-dimensional Schrödinger operators on the line of the form
Under certain conditions, the functions ε−2V (x/ε) converge in the sense of distributions as ε → 0 to δ′ (x), and then the limit S0 of Sε may be considered as a ‘physically motivated’ interpretation of the one-dimensional Schrödinger operator with potential δ′.
Net returns and risk for cover crop use in Alabama tomato production
Authors: Duzy Leah M. , Kornecki Ted S. , Balkcom Kipling S. , Arriaga Francisco J. 
Published: July 2013

AbstractTomato (Solanum lycopersicumL.) producers are faced with uncertain yields and prices, and utilizing a production system that will reduce risk while maintaining yield may keep tomato producers economically sustainable into the future. A conservation tillage production system with high biomass cover crops may be an economically viable alternative for tomato producers in Alabama. The objective of this study was to compare the economics of alternative production systems using different cover crops, such as cereal rye (Secale cerealeL.) and crimson clover (Trifolium incarnatumL.), and different subsoiler shanks for fresh-market tomato production relative to a commonly used plastic mulch system to determine the preferred treatment. Gross revenues and net returns from tomato production using a rye cover crop were higher than tomato production using plastic mulch in 2 of the 4 years. For the clover cover crop, gross revenues and net returns were higher in 1 out of the 4 years. Under tomato prices and weather conditions observed during 2005–2008, the preferred treatment for a risk neutral producer was planting tomatoes into a rye cover crop with a wide shank. For a strongly risk averse producer, all cover crop treatments were preferred to plastic mulch. The use of a cover crop in tomato production has the potential to be an equally profitable, less risky alternative to plastic mulch in Alabama.
The size and mass evolution of the massive galaxies over cosmic time
Authors: Trujillo Ignacio 
Published: July 2013

AbstractOnce understood as the paradigm of passively evolving objects, the discovery that massive galaxies experienced an enormous structural evolution in the last ten billion years has opened an active line of research. The most significant pending question in this field is the following: which mechanism has made galaxies to grow largely in size without altering their stellar populations properties dramatically? The most viable explanation is that massive galaxies have undergone a significant number of minor mergers which have deposited most of their material in the outer regions of the massive galaxies. This scenario, although appealing, is still far from be observationally proved since the number of satellite galaxies surrounding the massive objects appears insufficient at all redshifts. The presence also of a population of nearby massive compact galaxies with mixture stellar properties is another piece of the puzzle that still does not nicely fit within a comprehensive scheme. I will review these and other intriguing properties of the massive galaxies in this contribution.
The Morphologies of Massive Galaxies at 1<z<3 in the CANDELS-UDS Field: Compact Bulges, and the Rise and Fall of Massive Disks
Authors: Bruce V. A. , Dunlop J. S. , Cirasuolo M. , McLure R. J. , Targett T. A. , Bell E. F. , Croton D. J. , Dekel A. , Faber S. M. , Ferguson H. C. , Grogin N. A. , Kocevski D. D. , Koekemoer A. M. , Koo D. C. , Lai K. , Lotz J. M. , McGrath E. J. , Newman J. A. , van der Wel A. 
Published: July 2013

AbstractWe have used high-resolution, HST WFC3/IR, near-infrared imaging to conduct a detailed bulge-disk decomposition of the morphologies of ≃ 200 of the most massive (M* > 1011 M⊙) galaxies at 1 < z < 3 in the CANDELS-UDS field. We find that, while such massive galaxies at low redshift are generally bulge-dominated, at redshifts 1<z<2 they are predominantly mixed bulge+disk systems, and by z > 2 they are mostly disk-dominated. Interestingly, we find that while most of the quiescent galaxies are bulge-dominated, a significant fraction (25–40%) of the most quiescent galaxies, have disk-dominated morphologies. Thus, our results suggest that the physical mechanisms which quench star-formation activity are not simply connected to those responsible for the morphological transformation of massive galaxies.
The extended gas halo of QSO host galaxies
Authors: Falomo R. , Farina E. P. , Decarli R. , Treves A. , Kotilainen J. 
Published: July 2013

AbstractWe investigate the MgII 2800 and CIV 1540 absorption features of the gas in the halo of a foreground QSO through the absorption imprinting on the spectra of a background QSO that is closely aligned with the nearest quasar. We present the results for 13 QSO pairs (0.7 < z < 2.2) that allow us to probe the gas at distances between 60 kpc and 120 kpc from the QSO nucleus. We identify absorption features associated with the foreground QSO in 7 out of 10 systems for MgII, and one out of 3 for CIV (see example in Fig. 1). At variance with the case of inactive and less massive galaxies we find that relatively strong (EW ~ 1 Ang) absorption features are present out to a radius of 100 kpc. This suggests that a large extended halo is associated with massive galaxies.The comparison of these results with those for inactive (not hosting active black holes) galaxies (see e.g. Chen et al. 2010a) shows that the halo of QSOs is similar to that of inactive galaxies. In the observed sample we do not detect a significant enhancement of the absorption strengths, as it could be expected if the QSO nuclear activity were driven by intense gas accretion onto the black hole. Moreover along the line of sight of the QSO we do not detect any Mg II absorbers of the same strength of the transverse one. These results are in agreement with models that consider a non-isotropic emission of the QSO, which are hosted by massive gaseous halos.
Star Formation & Molecular Gas over Cosmic Time
Authors: Daddi E. , Sargent M. T. , Béthermin M. , Magdis G. 
Published: July 2013

AbstractRecent observations have revealed the existence of a ‘main sequence’ of star-forming galaxies out to high redshift. While the majority of star-forming galaxies are observed to be close to this relation between star formation rate (SFR) and stellar mass, a smaller subset of the population – so-called ‘starbursts’ – displays specific star-formation rates and star-formation efficiencies that exceed those of normal (main-sequence) galaxies by up to an order of magnitude. A large degree of homogeneity and similarity has been observed for the properties of the population of normal galaxies across a broad redshift range, including a narrow correlation between their CO luminosity (hence gas content) and IR luminosity and an almost invariable IR SED getting warmer with redshift, while starburst galaxies display systematically different properties. This can be used to devise a simple description of the evolution of the star-forming galaxy population since z ~ 2 and, with a higher degree of uncertainty, even further back in time, in a scheme that we dub two star formation mode framework (2-SFM). We show how this can successfully reproduce the shape of the IR luminosity function of galaxies as a function of redshifts, and the IR number counts. Furthermore, we can link the cosmic evolution of the sSFR of main-sequence galaxies to the evolution of the molecular fuel reservoir and to derive estimates of the molecular gas mass functions of star-forming galaxies that are based on their empirically measured gas properties rather than simulations or semi-analytical modelling. We also infer the evolution of the cosmic abundance of molecular gas and briefly discuss its expected observational signature by molecular line emission, the CO luminosity function.
Connection between the Star Formation Rate and the Gamma-Ray Bursts
Authors: Mészáros Attila , Bagoly Zsolt , Balázs Lajos G. , Horváth István 
Published: July 2013

AbstractIt is remarkable that the long gamma-ray bursts, as objects connected with the supernovae - i.e. with the end-stages of massive stars, trace the star formation rate. This connection is discussed in this contribution. The presentation is in essence a recapitulation of the article by Mészáros et al. (2006).
Stacking of Interferometric Data
Authors: Lindroos Lukas , Knudsen Kirsten K. 
Published: July 2013

AbstractRadio and mm observations play an important role in determining the star formation properties of high redshift galaxies. However, most galaxies at high redshift are too faint to be detected individually at these wavelengths. A way to study this population of galaxies is to use stacking. By averaging the emission of a large number of galaxies detected in optical or near infrared surveys, we can achieve statistical detection.We investigate methods for stacking data from interferometric surveys. Interferometry poses unique challenges in stacking due to the nature of imaging of this data. We have compared directly stacking the uv data with stacking of the imaged data, the latter being the typically used approach. Using simulated data, we find that uv-stacking may provide around 50% less noise and that image based stacking systematically loses around 10% of the flux.
The emergence of the red sequence at z~2 seen through galaxy clustering in the UKIDSS UDS
Authors: Hartley William G. , Almaini Omar , Mortlock Alice , Conselice Chris ,   the UDS team
Published: July 2013

AbstractWe use the UKIDSS Ultra-Deep Survey, the deepest degree-scale near-infrared survey to date, to investigate the clustering of star-forming and passive galaxies to z ~ 3.5. Our new measurements include the first determination of the clustering for passive galaxies at z > 2, which we achieve using a cross-correlation technique. We find that passive galaxies are the most strongly clustered, typically hosted by massive dark matter halos with Mhalo > 1013 M⊙ irrespective of redshift or stellar mass. Our findings are consistent with models in which a critical halo mass determines the transition from star-forming to passive galaxies.
The Co-Evolution of Supermassive Black Holes and Galaxies: Observational Constraints
Authors: Zheng Xian Zhong 
Published: July 2013

AbstractThe connection between the growth of supermassive black holes (SMBHs) and the assembly of their host galaxies is termed ‘co-evolution’. Understanding co-evolution is one of the most fundamental issues in modern astrophysics. In this contribution, we review recent progress in addressing how the growth of SMBHs is linked to the properties of their host galaxies in the context of galaxy evolution, from the observational point of view. Although a coherent picture has not yet emerged, multiple pathways of co-evolution appear to be favored with a probable dependence on AGN luminosity and redshift.
The stellar populations in low excitation and high excitation radio galaxies
Authors: Pracy Michael B. , Ching John , Croom Scott , Sadler Elaine M. 
Published: July 2013

AbstractWe have conducted deep optical spectroscopic follow up of a sample of radio galaxies with redshifts z < 0.7. The spectra were used to construct robust sub-samples of low excitation and high excitation AGN and perform stellar population analysis via line indices and spectral fitting. While the high excitation objects have lower luminosity-weighted ages and lower metallicities than the low excitation galaxies, this can be explained by the different stellar mass distributions of the samples. When stellar mass is taken into account the age and metallicity distribution of both populations are consistent with the galaxy population as a whole.
Understanding the growth of massive galaxies via stellar populations
Authors: Ferreras Ignacio 
Published: July 2013

AbstractThe formation and evolution of massive galaxies represent one of the most intriguing open problems in astrophysics. Their underlying stellar populations encode valuable information about their past history. Detailed spectroscopic observations allow us to constrain the star formation histories, revealing a complicated mixture of a strong, early formation process, followed by passive evolution in the cores, along with an extended assembly of the outer regions via minor mergers. In this contributed talk, some recent results are presented from the analysis of samples of massive galaxies both at z ~ 0 and moderate redshift.
Stellar velocity dispersions and emission line properties of SDSS-III/BOSS galaxies
Authors: Thomas D. , Steele O. , Maraston C. , Johansson J. , Beifiori A. , Pforr J. , Strömbäck G. , Tremonti C. A. , Wake D. ,   the BOSS collaboration
Published: July 2013

AbstractWe perform a spectroscopic analysis of 492,450 galaxy spectra from the first two years of observations of the Sloan Digital Sky Survey-III/Baryonic Oscillation Spectroscopic Survey (BOSS) collaboration. This data set has been released in the ninth SDSS data release, the first public data release of BOSS spectra. We show that the typical signal-to-noise ratio of BOSS spectra is sufficient to measure stellar velocity dispersion and emission line fluxes for individual objects. The typical velocity dispersion of a BOSS galaxy is 240 km/s, with an accuracy of better than 30 per cent for 93 per cent of BOSS galaxies. The distribution in velocity dispersion is redshift independent between redshifts 0.15 and 0.7, which reflects the survey design targeting massive galaxies with an approximately uniform mass distribution in this redshift interval. The majority of BOSS galaxies lack detectable emission lines. We analyse the emission line properties and present diagnostic diagrams using the emission lines [OII], Hβ, [OIII], Halpha, and [NII] (detected in about 4 per cent of the galaxies). We show that the emission line properties are strongly redshift dependent and that there is a clear correlation between observed frame colours and emission line properties. Within in the low-z sample around 0.15 < z < 0.3, half of the emission-line galaxies have LINER-like emission line ratios, followed by Seyfert-AGN dominated spectra, and only a small fraction of a few per cent are purely star forming galaxies. AGN and LINER-like objects, instead, are less prevalent in the high-z sample around 0.4 < z < 0.7, where more than half of the emission line objects are star forming. This is a pure selection effect caused by the non-detection of weak Hβ emission lines in the BOSS spectra. Finally, we show that star forming, AGN and emission line free galaxies are well separated in the g - r vs r - i target selection diagram.
Evolution of the most massive galaxies to z ~ 0.6
Authors: Chen Yanmei 
Published: July 2013

AbstractWe develop a new method to estimate galaxy physical parameters, such as stellar masses, or star formation histories. This method is based on principal component analysis (PCA), using the information in rest-frame 3700-5500Å spectral region. The derived physical parameters are then applied to study the evolution of the most massive galaxies from z ~ 0.6 to the local Universe, especially on how radio AGN influence the recent star formation histories of host galaxies.
A phenomenological approach to the evolution of galaxies
Authors: Lilly Simon J. , Peng Yingjie , Carollo Marcella , Renzini Alvio 
Published: July 2013

AbstractIncreasingly good statistical data on the galaxy population at high and low redshift enable the development of new phenomenological approaches to galaxy evolution based on application of the simplest continuity equations. This has given new insights into the different ways in which star-formation in galaxies is quenched, the role of merging in the population, and in to the control of star-formation in star-forming galaxies and the links with chemical evolution. The continuity approach provides a self-consistent view of the evolving population and exposes linkages between different aspects of galaxy evolution.
Evolution in cluster cores since z ~ 1
Authors: Burke Claire , Collins Chris , Stott John , Hilton Matt 
Published: July 2013

AbstractA large fraction of the stellar mass in galaxy clusters is thought to be contained in the diffuse low surface brightness intracluster light (ICL). Being bound to the gravitational potential of the cluster rather than any individual galaxy, the ICL contains much information about the evolution of its host cluster and the interactions between the galaxies within. However due its low surface brightness it is notoriously difficult to study. We present the first detection and measurement of the flux contained in the ICL at z ~ 1. We find that the fraction of the total cluster light contained in the ICL may have increased by factors of 2–4 since z ~ 1, in contrast to recent findings for the lack of mass and scale size evolution found for brightest cluster galaxies. Our results suggest that late time build-up in cluster cores may occur more through stripping than merging and we discuss the implications of our results for hierarchical simulations.
Evolution of the Fundamental Plane for early–type galaxies up to z = 1.2
Authors: Lorenzo M. Fernández , Cepa J. , Bongiovanni A. , García A. M. Pérez , Ederoclite A. , Lara-López M. A. , Pović M. , Sánchez-Portal M. 
Published: July 2013

AbstractWe studied the evolution of the Fundamental Plane in B– and g–bands, for two samples of early–type galaxies at 0.2 < z < 0.35 and 0.35 < z < 1.2. We found a difference in the intercept that can be interpreted as galaxies at < z > ~0.7 being 0.68 and 0.52 mag brighter in the B– and g–band respectively, than their local counterparts. From the study of the Kormendy relation, we found the existence of a population of very bright (−21.5 > Mg > −22.5) and compact (Re < 2 kpc) galaxies of which only a small fraction of 0.4% exists at z = 0, and that would be responsible for the apparent evolution in the Kormendy relation (Fernández Lorenzo et al. 2011). These compact objects would have evolved mainly in size by the action of “dry” minor mergers.We checked the effect of these bright and compact objects in the FP by comparing the galaxies with −21.5 > Mg > −22.5 of our high–redshift sample and the SDSS early–type galaxies of Bernardi et al. (2003) in Fig. 1. The previous evolution found in the FP seems to be caused mainly by these galaxies, which have virtually disappeared at z = 0.