bluuebunny/crossref_metadata_2025_split huggingface dataset:
Detrital zircon provenance of the Lower Yangtze foreland basin deposits: constraints on the evolution of the early Palaeozoic Wuyi–Yunkai orogenic belt in South China
Authors: LI HAI-BIN , JIA DONG , WU LONG , ZHANG YONG , YIN HONG-WEI , WEI GUO-QI , LI BEN-LIANG 
Published: March 2013

AbstractThe Lower Yangtze foreland basin is situated to the northwest of the early Palaeozoic Wuyi–Yunkai orogen in South China. To demonstrate its provenance history and the denudation of the orogen, seven sandstone samples were collected from the upper Ordovician to Silurian strata for U–Pb dating. The zircons show a broad range of ages that can be linked with the ages of specific units in the Wuyi–Yunkai orogen. The zircon spectra in the late Ordovician samples are similar to those in the pre-orogenic strata, suggesting a recycled source. The dominant age population of 880–740 Ma in the early Llandovery samples indicates that the middle Neoproterozoic volcanic rocks were the primary source. A significant age population of 460–425 Ma in the late Llandovery to Wenlock samples reflects the fact that the synorogenic magmatic and metamorphic rocks were exposed to provide detritus. The youngest zircons from the uppermost Silurian strata yield an age of 425 Ma, which approximates the inferred depositional age. This age, together with available biostratigraphic data, indicates that the foreland basin was formed 448–425 Ma ago. We surmise a possible link between the Wuyi–Yunkai orogen and the Appalachian–Caledonian orogen based on the geological constraints and palaeomagnetic data.
NEGOTIATION FOR SAFER SEX AMONG MARRIED WOMEN IN CAMBODIA: THE ROLE OF WOMEN'S AUTONOMY
Authors: UNG MENGIENG , BOATENG GODFRED O. , ARMAH FREDERICK A. , AMOYAW JONATHAN A. , LUGINAAH ISAAC , KUUIRE VINCENT 
Published: March 2013

SummaryNegotiating safer sex among married women has been identified as an important determinant of vulnerability or resilience to new HIV infections. Using the Cambodia Demographic and Health Survey data of 2010, this paper examined negotiation for safer sex among 11,218 married women in the context of Cambodia's highly touted reduction in HIV/AIDS prevalence. The results from a complementary log-log regression model indicate that wealthier and highly educated married women were more likely to report that they can refuse sexual intercourse and ask their husbands to use a condom. Interestingly, while women who were fully involved in decision-making on their own health care were 19% more likely to refuse sex, they were 14% less likely to be able to ask their husbands to use a condom, compared with their counterparts who were not involved in this decision-making. Women who were partially involved in decision-making on family visits were 17% less likely to be able to ask their husbands to use a condom compared with those who were not involved. In this context, involvement in decision-making may have translated into trust and risk compensation. Those who believed in HIV transmission myths were less likely to negotiate safer sex relative to their counterparts who did not hold such myths to be true. Women's ability to negotiate for safer sex is, therefore, a function of their autonomy in terms of their full participation in decision-making in health care, household expenditure and mobility. Policy implications of the capacity of women to negotiate for safer sex are delineated.
The life history ofPleurogenoides malampuzhensissp. nov. (Digenea: Pleurogenidae) from amphibious and aquatic hosts in Kerala, India
Authors: Brinesh R. , Janardanan K.P. 
Published: March 2013

AbstractThe life-cycle stages ofPleurogenoides malampuzhensissp. nov. infecting the Indian bullfrogHoplobatrachus tigerinus(Daudin) and the skipper frogEuphlyctiscyanophlyctis(Schneider) occurring in irrigation canals and paddy fields in Malampuzha, which forms part of the district of Palakkad, Kerala, are described. The species is described, its systematic position discussed and compared with the related species,P. gastroporus(Luhe, 1901) andP. orientalis(Srivastava, 1934). The life-cycle stages, from cercaria to egg-producing adult, were successfully established in the laboratory. Virgulate xiphidiocercariae emerged from the snailDigoniostoma pulchella(Benson). Metacercariae are found in muscle tissues of dragonfly nymphs and become infective to the frogs within 22 days. The pre-patent period is 20 days. Growth and development of both metacercariae and adults are described.
Elevated alanine aminotransferase independently predicts new onset of depression in employees undergoing health screening examinations
Authors: Zelber-Sagi S. , Toker S. , Armon G. , Melamed S. , Berliner S. , Shapira I. , Halpern Z. , Santo E. , Shibolet O. 
Published: March 2013

BackgroundNon-alcoholic fatty liver disease (NAFLD) is the most common cause of elevated alanine aminotransferase (ALT). NAFLD is associated with insulin resistance and hepatic inflammation. Similarly, patients with depression exhibit insulin resistance and increased inflammatory markers. However, no study has shown a clear association between elevated ALT and the development of depression. The aim of the study was to test whether elevated ALT, a surrogate marker for NAFLD, predicts the development of depression.MethodThe present prospective cohort study investigated 12 180 employed adults referred for health examinations that included fasting blood tests and anthropometric measurements between 2003 and 2010. Exclusion criteria were: baseline minor/major depression, excessive alcohol consumption and other causes for ALT elevation. Depression was evaluated by the eight-item Patient Health Questionnaire (PHQ-8) score.ResultsThe final cohort included 5984 subjects [69.4% men, aged 45.0 (s.d. = 10.24) years]. The incidence rate of minor and major depression was 3.8% and 1.4%, respectively. Elevated ALT was a significant independent predictor for the occurrence of minor [odds ratio (OR) 2.02, 95% confidence interval (CI) 1.40–2.92] and major (OR 3.132, 95% CI 1.81–5.40) depression after adjusting for age, gender, body mass index, education level, serum levels of lipids, glucose, smoking and physical activity. Adding subjective health and affective state parameters (sleep disturbances, self-rated health, anxiety and burnout) as potential mediators only slightly ameliorated the association. Persistently elevated ALT was associated with the greatest risk for minor or major depression as compared with elevation only at baseline or follow-up (p for trend < 0.001).ConclusionsElevated ALT was associated with developing depressive symptoms, thus suggesting that NAFLD may represent an independent modifiable risk factor for depression.
Aortic isthmic atresia and aorta–right atrial communication: a case report
Authors: Deniz Ali , Kanadasi Mehmet , Ozbarlas Nazan 
Published: March 2013

AbstractThe development of an aorta–right atrial fistula is a very rare complication of aortic isthmic atresia. We described a case of aorta–right atrial communication associated with isthmic atresia.
Star Formation in the Long Filamentary Infrared Dark Cloud at l ∼ 53°.2
Authors: Kim Hyun-Jeong , Koo Bon-Chul , Davis Chris 
Published: March 2013

AbstractMassive stars govern the evolution of galaxies by providing ionizing photons and energy as well as enriching heavy elements into interstellar medium; however, their formation is still poorly understood. Infrared dark clouds (IRDCs) are cold (< 25 K) and very dense (> 105 cm−3) interstellar clouds which are seen silhouette against the bright Galactic background in mid-IR. With very high column densities (∼ 1023–1025cm−2), IRDCs are believed to be the precursors to massive stars and star clusters (Simon et al. 2006).We report a remarkable IRDC at (l, b) ∼ (53°.2, 0°.0) which shows a number of bright mid-IR stellar sources along the cloud that are likely young stellar objects (YSOs). There are also several H2 (at 2.122 μm) outflow features in the cloud revealed by UWISH2 (Ukirt Widefield Infrared Survey for H2, Froebrich et al. 2011), in particular where earlier evolutionary stage of YSOs are located. The IRDC was previously partly identified as three separate IRDCs in the MSXDC catalog (Simon et al. 2006), whereas we have found that a long, filamentary cloud extending ∼ 30 pc including these three IRDCs is very well coincident with a CO cloud at v ∼ 23.5 km/s (or at d ∼ 2 kpc) which is clearly distinct from the other velocity components. Therefore, in this study, we investigate the overall star formation activity in this IRDC (IRDC G53.2, hereafter).We perform the PRF photometry of Spitzer MIPSGAL 24 μm data using MOPEX and build a catalog of YSOs by matching the detected 24 μm sources with published catalogs. The limiting magnitude in 24 μm is ∼ 7.8 mag, and YSO candidates which have counterparts in GLIMPSE I catalog are 354. The YSO candidates are classified using spectral index derived between 2 and 24 μm, following Greene et al. (1994). We also remove the field-star contamination using reference fields where there is no CO cloud; the fraction of each class after reference field analysis is 18, 22, 45, 10, and 5% for Class I, Flat, Class II, Class III, and sources which cannot be classified due to the lack of data. The spatial distribution that earlier classes (i.e., Class I and Flat) are concentrated where far-IR or millimeter emission is strong and larger fraction of Flat objects compared to other low-mass star forming regions (e.g., Evans et al. 2009 and Billot et al. 2010) may imply that the IRDC G53.2 is indeed an active star-forming region in rather early evolutionary stage. Further investigation of each YSO such as SED modeling will reveal detailed information on star formation activity in this intriguing IRDC.
Filamentary structure formation in the Interstellar Radiation Field (ISRF)
Authors: Miao Jingqi , Lieu M. , Cox Philip , Kinnear Tim , Cornwall Paul 
Published: March 2013

AbstractA new mechanism is proposed for the formation of filament/core structure by ISRF and clumpy molecular cloud interaction. The derived characterizes of the filament/core network is consistent with that produced by the compressive forcing turbulence model.
Large column densities and [12CII] 158 μm self-absorption in Orion B
Authors: Stutzki J. , Graf U. U. , Simon R. , Colgan S. W. J. , Guan X. , Güsten R. , Honingh C. E. 
Published: March 2013

AbstractWe present a preliminary analysis of the self-absorbed [CII]-spectra observed with SOFIA/GREAT towards NGC 2024. Together with the detected [13CII] hyperfine satellites, the observed spectra require surprisingly high column densities of C+, both in the warm core and the foreground absorption component. Such high column densities are a challenge to explain with present state-of-the-art PDR models of the UV/molecular cloud interaction.
Formaldehyde observations at XAO
Authors: Wu Gang , Esimbek Jarken , Zhou Jian-Jun , Ji Wei-Guang 
Published: March 2013

AbstractIn recent years our team has performed H2CO(110 − 111) observations towards GMCs and HII regions with the Xinjiang Astronomical Observatory, CAS. Here, we provide a summary of these observations. More than 200 new formaldehyde sources are detected, 8 extended GMC have been mapped, kinetic distances, Galactic structure and a related discussion are provided.
The Methanol Multibeam Survey: a unique window on high-mass star formation in our Galaxy
Authors: Caswell J. L. 
Published: March 2013

AbstractThe Methanol Multibeam (MMB) survey has yielded over 1000 masers at the 6668-MHz methanol transition: a near-complete census throughout the Galactic disc, as evident from the discovery statistics, and corroborated by preliminary distance determinations. Each maser pinpoints a massive star in a brief early evolutionary phase. Follow-up comparisons reveal in most cases a matching IR source in the GLIMPSE survey. The methanol masers effectively distinguish the genuine high mass proto-stars from the many thousand IR mimics of similar color. Longer IR wavelength follow-ups by Herschel instruments, and in the radio mm-continuum, will refine the mass-range encompassed by the masers; and, complemented by radio measurements at short cm-wavelengths, will define the evolutionary stage of each site, distinguishing hyper-compact HII regions from an earlier phase. Follow-up studies of key molecular gas tracers, including closely associated masers (other methanol transitions, water and OH), reveal the extent of homogeneity in the population and environments of high mass stars.Distance estimates based on the maser velocities have already allowed useful exploration of Galactic structure. Future astrometric parallax measurements extended to the full maser sample will precisely define the geometry of Galactic spiral arms of our Galaxy and independently define the velocity field, allowing a model-free study of Galactic rotation and dynamics. Associated OH masers (present at about half of the methanol sites) are being exploited to provide the first Galaxy-wide grid of ‘in situ’ magnetic field estimates.Our detailed characterization of the Galactic methanol maser population provides a yardstick for extragalactic comparisons with M31 and the LMC. Notably, our survey of the LMC has shown its methanol maser population to be remarkably small relative to our Galaxy - a likely consequence of low LMC metallicity.
From Gas to Stars in Energetic Environments: Dense Gas Clumps in the 30 Doradus Region
Authors: Anderson C. N. , Meier D. S. , Ott J. , Hughes A. , Wong T. 
Published: March 2013

AbstractWe present parsec-scale interferometric maps of HCN(1-0) and HCO+(1-0) emission from dense gas in the star-forming region 30Dor10, obtained using the Australia Telescope Compact Array. This extreme star-forming region, located in the Large Magellanic Cloud, is characterized by a very intense ionizing radiation field and sub-solar metallicity, both of which are expected to affect molecular cloud structure. We detect 13 clumps of dense molecular gas, some of which are aligned in a filamentary structure. Our analysis of the clump properties shows that they have similar mass but slightly wider linewidths than clumps detected in other LMC star-forming regions.
Magnetohydrodynamic Simulations of the Interaction of Magnetic Tower Jets with Interstellar Clouds including Cooling
Authors: Asahina Y. , Ogawa T. , Matsumoto R. 
Published: March 2013

AbstractWe carried out magnetohydrodynamic (MHD) simulations to reveal the formation mechanism of molecular towers observed in the central region of our galaxy. These molecular clouds can be formed by the interaction of magnetic tower jet with the interstellar gas. When the jet collides with dense HI clouds, the HI gas is compressed by the bow shock ahead of the jet. Since the density enhancement triggers the cooling instability because it increases the cooling rate, the shocked gas cools down and forms cold, dense gas. We carried out MHD simulations including the cooling. The magnetized jet which triggers the formation of the molecular column appears in global magnetohydrodynamic simulations of accretion disks, in which the magnetic loops emerging from the disk are twisted by the differential rotation between the footpoints of magnetic loops anchored to the disk. Numerical results indicate that the magnetic loops expand, and form a magnetic tower. When the ambient density is small, the propagation speed of the tower can be as large as the rotation speed of the disk. When the ambient density is high, the collision of the jet and the HI cloud forms dense molecular tower.
Supernova Remnants in Starburst Regions
Authors: Asvarov A. I. 
Published: March 2013

AbstractWe study the evolution of SNRs in starburst regions taking into consideration the role of the high ambient pressure and the influence of gravitational forces from the stellar component within the shell of a SNR. On this basis, we discuss the connection between the radio, infrared, and gamma emissions from starburst regions.
The density model of the Milky Way from the tangent-point measurements of the rotation curve
Authors: Golubov Oleksiy , Just Andreas 
Published: March 2013

AbstractWe use measurements of the rotation curve of the Milky Way by the tangent point method to reconstruct the density model of the Milky Way. The observed inner rotation curve is fitted by a theoretical density model, consisting of a Dehnen bulge, an exponential disc with a hole, and a flattened dark matter halo with a cored isothermal or NFW density profile. The density model is also set to be consistent with the local density constraints in the solar neighborhood.
Infrared observation of Mira variables and their galactic distribution
Authors: Miyanoshita Ryo , Omodaka Toshihiro , Handa Toshihiro , Kamezaki Tatsuya , Nakai Chihiro , Fujiwara Hiroshi 
Published: March 2013

AbstractSince November 2003, we have monitored AGB candidates in infrared wavelengths with the Kagoshima 1m telescope. We present the latest results based on the data until June 2011. For each of 400 monitored AGB stars, we estimate the periods, amplitudes, and mean apparent magnitudes in K band. Based on the two color diagram we choose 259 objects as Miras. We use the period–luminosity relation to obtain distances to them. As results we show the 3 dimensional distribution of 259 Mira variables.
MAGMA-SMC: The Molecular Cloud Survey of the SMC
Authors: Muller Erik , Wong Tony , Hughes Annie , Ott Jürgen , Pineda Jorge L. ,   the MAGMA collaboration
Published: March 2013

AbstractWe present a brief summary and description of the upcoming 12CO(1-0) Magellanic Mopra Assesment (MAGMA) SMC survey data release. The MAGMA-SMC survey has sampled 100% of the known CO in the SMC (at ∼33″ resolution; 12 pc at D = 60 kpc). Having explored 522 × 103 square parsecs throughout the SMC with 69 5′ × 5′ fields, to a sensitivity of ∼150 mK, we apply the cloudprops (Rosolowsky & Leroy 2006) cloud-search algorithm optimized for low S/N data, to detect more than 30 CO clouds with virial masses between 103–104 M⊙, mean radii ∼5 pc and 0.3–0.9 km s−1 velocity width. Typical brightness temperatures are ∼1 K Tmb. All detected molecular regions are associated with at least one 24 μm compact emission source. Smoothing rarely increases the total detected CO flux, implying the CO emission is typically confined to small spatial scales. As recent dust maps of the SMC imply extended H2 mass, the apparent compact nature of the CO population indicates some departures from the canonical Galactic XCO-factor in the low-metallicity and relatively un-evolved ISM of the SMC.
Different Evolutionary Stages in the Massive Star-forming Complex W3 Main
Authors: Wang Yuan , Beuther Henrik , Zhang Qizhou , Bik Arjan , Rodón Javier A. , Jiang Zhibo , Fallscheer Cassandra 
Published: March 2013

AbstractWe observed with the Submillimeter Array and IRAM 30 m telescope three high-mass star-forming regions in different evolutionary stages in the W3 high-mass star formation complex. These regions, i.e. W3 SMS1 (W3 IRS5), SMS2 (W3 IRS4) and SMS3, are located within the same large-scale environment, which allows us to study rotation and outflows as well as chemical properties in an evolutionary sense. While we find multiple mm continuum sources toward all regions, these three subregions exhibit different dynamical and chemical properties, which indicates that they are in different evolutionary stages. Even within each sub-region, massive cores of different ages are found, e.g. in SMS2, sub-sources from the most evolved UCHii region to potential starless cores exist within 30 000 AU (left panel, Fig. 1). Outflows and rotational structures are found in SMS1 and SMS2. Evidence for interactions between the molecular cloud and the HII regions is found in the 13CO channel maps (right panel, Fig. 1), which may indicate triggered star formation.
An Updated View of Giant Molecular Clouds, Gas Flows and Star Formation in M51 with PAWS
Authors: Meidt S. E. , Schinnerer E. , Hughes A. , Colombo D. , Pety J. , Garcia-Burillo S. , Leroy A. , Dobbs C. L. , Schuster K. F. , Kramer C. , Dumas G. , Thompson T. 
Published: March 2013

AbstractWe present an overview of the latest results from the PdBI Arcsecond Whirlpool Survey (PAWS, PI: E. Schinnerer), which has mapped CO(1-0) emission in the nearby grand-design spiral galaxy M51 at 40pc resolution. Our data are sensitive to GMCs above 105 M⊙, allowing the construction of the largest GMC catalog to date – containing over 1500 objects – using the CPROPS algorithm (Rosolowsky & Leroy 2006). In the inner disk of M51, the properties of the CO emission show significant variation that can be linked to the dynamical environment in which the molecular gas is located. We find that dynamically distinct regions host clouds with different properties and exhibit different GMC mass spectra, as well as distinct patterns of star formation. To understand how this sensitivity to environment emerges, we consider the role of pressure on GMC stabilization (including shear and star formation feedback-driven turbulence). We suggest that, in the presence of significant external pressure, streaming motions driven by the spiral arm can act to reduce the surface pressure on clouds. The resulting stabilization impacts the global pattern of star formation and can account for the observed non-monotonic radial dependence of the gas depletion time. Our findings have implications for the observed scatter in the standard GMC relations and extragalactic star formation laws.
Environmental effects on the atomic gas content of galaxies in the local universe
Authors: Li Cheng 
Published: March 2013

AbstractEffects of galaxy environment on its cold gas content are studied in detail using different date sets and statistics. These include measuring the clustering of galaxies as a function of their Hi mass fraction, quantifying the depletion of Hi gas content of cluster galaxies as a function of cluster-centric radius, and comparing the dependence of environmental density on galaxy star formation rate with the dependence on Hi gas mass fraction. Results from these studies are all consistent with a picture in which ram-pressure stripping may play an important role in removing atomic gas from the outer disks of low mass satellite galaxies.
Probing the black hole - bulge relationship at high redshift with CO molecular lines
Authors: Wu Xue-Bing 
Published: March 2013

AbstractIt has been suggested that the CO line width (FWHM(CO)) is a surrogate for the bulge velocity dispersion (σ) of the host galaxies of high-redshift quasars, and the black hole – bulge (M−σ) relation obtained with this assumption departs significantly from the M−σ relation in the local universe. Based on an investigation of the correlation between the CO line width and the bulge velocity dispersion using a sample of 33 nearby Seyfert galaxies, we find that the formula adopted in previous studies, σ=FWHM(CO)/2.35, is generally not a good approximation. By involving the galactic inclination angle i as an additional parameter, we obtain a tight correlation between the inclination-corrected CO line width and the bulge velocity dispersion, namely, FWHM(CO)/sin i=−67.16±80.18+(3.62±0.68)σ. Using this new relation, we can better estimate the bulge velocity dispersion from the CO line width if the galactic inclination is known. We apply this new relation to nine high-redshift quasars with CO line detections and find that they are consistent with the local M−σ relation if their inclination angles are around 15°. The possible smaller inclinations of the high-redshift quasars are preferred because of their relatively greater likelihood of detection, and are also consistent with their relatively smaller CO line widths compared to the submillimeter galaxies (SMGs) at high redshift having a similar total amount of molecular gas.