bluuebunny/crossref_metadata_2025_split huggingface dataset:
Neuroprotective effects of hypothermia in inflammatory‐sensitized hypoxic‐ischemic encephalopathy
Authors: Chevin Mathilde , Guiraut Clémence , Maurice‐Gelinas Caroline , Deslauriers Jessica , Grignon Sylvain , Sébire Guillaume 
Published: September 2016

AbstractBackgroundDespite the recent introduction of hypothermia as a mandatory standard of care, the incidence of neonatal encephalopathy in full‐term newborns and its devastating neuro‐behavioral outcomes continues to be a major individual, familial and social issue. Neonatal encephalopathy is mainly due to the compounding and interacting effects of hypoxia‐ischemia and inflammation resulting from placental and other perinatal infections. It is unclear why hypothermia is effective in alleviating neonatal encephalopathy in some, but not all, full‐term newborns. However, newborns exposed to inflammatory‐sensitized hypoxia‐ischemia seem to have less therapeutic benefit from hypothermia than those exposed to hypoxia‐ischemia alone.ObjectivesTo clarify this uncertainty, we tested the efficacy of hypothermia in a double‐hit model of neonatal encephalopathy induced by inflammatory‐sensitized hypoxia‐ischemia.MethodsUsing a rat preclinical model of endotoxin plus hypoxia‐ischemia‐induced neonatal encephalopathy of term newborns, we assessed the following in pups exposed (or not) to hypothermia: the extent of brain injuries and the expressions of molecules implicated in neural cell death, namely: pro‐inflammatory cytokines, matrix metalloproteinase‐9, antioxidant enzymes, as well as receptor‐interacting protein‐3.ResultsHypothermia was neuroprotective on inflammatory‐sensitized hypoxia‐ischemia‐induced penumbra, but not core, brain injuries. This beneficial effect was associated with a hypothermia‐induced increase of antioxidant enzymes (superoxide dismutase‐1, glutathione peroxidase‐1), but was not associated with any variations of the other inflammatory mediators tested, namely: interleukin‐1β, interleukin‐1 receptor antagonist, tumor necrosis factor‐α and matrix metalloproteinase‐9.ConclusionHypothermia is neuroprotective against inflammatory‐sensitized hypoxia‐ischemia possibly through a hypothermia‐induced increase of antioxidant enzymes. This neuroprotective effect seems to be independent of the interleukin‐1 system.
Phosphorus fertilizing potential of bagasse ash and rice husk ash in wheat–rice system on alkaline loamy sand soil
Authors: THIND H. S. , YADVINDER-SINGH  , SHARMA SANDEEP , VARINDERPAL-SINGH  , SRAN H. S. , BIJAY-SINGH  
Published: September 2016

SUMMARYBagasse and rice husk are two important agro-industrial by-products that are used as fuel in the sugar and rice mill industries, thus producing large quantities of bagasse ash (BA; 0·05 of bagasse) and rice husk ash (0·20 of rice husk) as waste material. Applying BA and rice husk ash (RHA) to agricultural land improves yield, nutrient uptake and chemical fertility of soil, particularly with special reference to available phosphorus (P) and potassium (K). The present field experiment was conducted for 3 years to evaluate the P fertilizer value of these agro-industrial waste materials in a wheat–rice system (WRS). The experiment was laid out in a split-plot design with RHA and BA applied at 10 t/ha and including a no-amendment control as the main plot treatments and three levels of fertilizer P (0, 13 and 26 kg P/ha; designated P0, P13and P26, respectively) as sub-plot treatments to wheat in WRS. Application of fertilizer P increased the wheat grain yield up to P26in the un-amended control treatment. However, a significant response of wheat to fertilizer P was also observed up to P13in the presence of BA and RHA, thereby saving 50% of fertilizer P. Both RHA and BA increased wheat productivity by 12 and 16%, respectively, over the un-amended control. The subsequent rice crop also produced 14% higher paddy yield when the two ashes were applied along with P13to the previous wheat crop. The increases in grain yield were accompanied by significant increases in the uptake of P and K, and P content (Olsen P) in the soil. The application of recommended P (P26) in un-amended plots resulted in a negative P balance of 9·3 kg P/ha/year. On the other hand, the application of BA alone and RHA along with P13resulted in neutral/slightly positive P balance. A strong linear relationship (R2= 0·98) was observed between P balance and Olsen-P build up in the soil. It may be concluded that application of BA and RHA has the potential to increase system productivity and reduce the cost of inputs in terms of reduced application of fertilizer P to wheat and rice.
The ALMA view of the Antennae galaxy collision: How galaxy interaction triggers the formation of super star clusters
Authors: Herrera Cinthya N. , Boulanger François , Falgarone Edith G. , Pineau des Forêts Guillaume , García-Burillo Santiago , Iono Daisuke , Guillard Pierre 
Published: September 2016

AbstractThe Antennae galaxies are a spectacular example of a burst of star formation triggered by the encounter of two galaxies, being an ideal source to understand how the dynamics of galaxy mergers drives star formation. We present archive ALMA CO(3−2) and VLT near-IR H2spectro-imaging observations, and new ALMA13CO(2−1) and dust continuum observations, at ~50 pc resolution. Combining tracers of density and velocity structure of the gas and its energetics, we demonstrate that star formation involves a complex interplay of merger-driven gas dynamics and turbulence, and the dissipation of the gas kinetic energy. We focus on a compact, bright H2source, associated with cold molecular gas and dust continuum emission, located where the velocity gradient in the interaction region is observed to be the largest. The characteristics of this source suggest that we are witnessing the formation, initiated by turbulent dissipation, of a cloud massive enough (~4×106M⊙) to form a super star cluster within 1 Myr.
Molecular gas, stars, and dust in sub-L⋆ star-forming galaxies at z ~ 2: Evidence for universal star formation and non-universal dust-to-gas ratio
Authors: Dessauges-Zavadsky Miroslava , Zamojski Michel , Schaerer Daniel , Combes Françoise , Egami Eiichi , Sklias Panos , Swinbank Mark A. , Richard Johan , Rawle Tim 
Published: September 2016

AbstractCurrent star-forming galaxies (SFGs) with CO measurements at z ~ 2 suffer from a bias toward high star formation rates (SFR) and high stellar masses (M*). It is yet essential to extend the CO measurements to the more numerous z ~ 2 SFGs with LIR < L⋆ = 4× 1011 L⊙ and M* < 2.5× 1010 M⊙. We have achieved CO, stars, and dust measurements in 8 such sub-L⋆ SFGs with the help of gravitational lensing. Combined with CO-detected galaxies from the literature, we find that the LIR, L′CO(1−0) data are best-fitted with a single relation that favours a universal star formation. This picture emerges because of the enlarged star formation efficiency spread of the current z>1 SFGs sample. We show that this spread is mostly triggered by the combination of redshift, specific SFR, and M*. Finally, we find evidence for a non-universal dust-to-gas ratio (DGR) with a clear trend for a lower DGR mean in z>1 SFGs by a factor of 2 with respect to local galaxies and high-redshift sub-mm galaxies at fixed about solar metallicity.
Detecting H II Regions in “Pure” Starburst Galaxies with SDSS Data
Authors: Crider Anthony , Richardson Chris , Kaiser Ben 
Published: September 2016

AbstractThe relationship between active galactic nuclei (AGN) and starburst galaxies is poorly understood, partially due to galaxies exhibiting both AGN and starburst activity. To better understand the connection, we analyze a sample of “pure” AGN or starburst at redshift z = 0.1 selected using mean field independent component analysis (MFICA). Simulations of starburst galaxy emission suggests that the locally optimally-emitting cloud (LOC) model can fit observations and improve our ability to distinguish the impact of differences in metallicity, ionization parameter, and ionizing flux. To test for the existence of such clouds in our galaxy sample, we examine the Sloan Digital Sky Survey (SDSS) images of our pure galaxies. At this distance, even large star-forming H II regions (e.g. 30 Doradus) only fill part of an SDSS pixel. However, we compare the morphology of the distant galaxies to more nearby ones (i.e. NGC 4713, NGC 4038/4039) to estimate the number of larger H II regions. While the clumpiness parameter of a galaxy in theory might indicate the existence of these regions, a straightforward calculation of the clumpiness parameter is ineffective for galaxies at z = 0.1. Typically, one subtracts a smoothed version of a galaxy image from the same image. We instead test a different approach to establish a smooth image and thus better identify the clumps. We subtract the smoother infrared z-band from the sharper ultraviolet u-band. We test this procedure using NGC 4713, a nearby starburst galaxy, artificially degraded to match images of our “pure” starburst galaxies.
Herschel spectroscopic observations of Zw 049.057 and Arp 299a
Authors: Falstad Niklas , González-Alfonso Eduardo , Aalto Susanne 
Published: September 2016

AbstractThe presence of compact obscured nuclei in luminous infrared galaxies (LIRGs) is very well probed by the detection of highly excited absorption lines of OH and H2O in the far-infrared (far-IR), which require warm and optically thick dust to pump the high-lying rotational levels. We are using a spherically symmetric radiative transfer code to model the H2O lines, OH lines and continuum from these objects. We discuss the results and analysis of Herschel observations of the compact obscured nucleus in the extremely H2O luminous LIRG Zw 049.057. In this galaxy we have found very high H2O abundances in a Compton thick compact core. Abundant 18O bearing species also suggest the presence of a relatively young starburst. We compare this to our observations and modeling of the luminous merger component Arp 299a, which is another source with prominent H2O and OH lines. Our preliminary results, however, suggest that its nuclear activity is in a different evolutionary state compared to Zw 049.057.
HI Gas in Disk and Dwarf Galaxies in the Semi-analytic Models of Galaxy Formation
Authors: Fu Jian , Wang Jing , Luo Yu 
Published: September 2016

AbstractWe construct the radially-resolved semi-analytic models of galaxy formation based on the L-Galaxies model framework, which include both atomic and molecular gas phase in ISM. The models run on the halo outputs of ΛCDM cosmology N-body simulation. Our models can reproduce varies observations of HI gas in nearby galaxies, e.g. the HI mass function, the HI-to-star ratio vs stellar mass and stellar surface density, universal HI radial surface density profile in outer disks etc. We also give the physical origin of HI size-mass relation. Based on our model results for local dwarf galaxies, we show that the “missing satellite problem” also exists in the HI component, i.e., the models over-predict dwarf galaxies with low HI mass around the Milky Way. That is a shortcoming of current ΛCDM cosmology framework. Future survey for HI gas in local dwarf galaxies (e.g. MeerKAT, SKA & FAST) can help to verify the nature of dark matter (cold or warm).
Structure and Stability of Filamentary Clouds Supported by Lateral Magnetic Field
Authors: Hanawa Tomoyuki , Tomisakar Kohji 
Published: September 2016

AbstractWe have constructed two types of analytical models for an isothermal filamentary cloud supported mainly by magnetic tension. The first one describes an isolated cloud while the second considers filamentary clouds spaced periodically. The filamentary clouds are assumed to be highly flattened in both the models. The former is proved to be the asymptotic limit of the latter in which each filamentary cloud is much thinner than the distance to the neighboring filaments. These models show that the mass to flux ratio is crucial for the magnetohydrodynamical equilibrium. The upper bound for the line density, i.e., the mass per unit length, is proportional to the magnetic flux. The mass to flux ratio is slightly larger than the critical value, ($2 \pi \sqrt{G}$)−1, in the first model and lower in the second model. The first model is unstable against fragmentation and the wavelength of the fastest growing mode is several times longer than the cloud diameter. The second model is likely to be unstable only when the mass to flux ratio is supercritical.
All-sky catalogs and analysis of interstellar clouds
Authors: Hojaev A.S. 
Published: September 2016

AbstractAll available databases of molecular and gas-dust clouds in the Galaxy and other galaxies including their main properties such as position, angular and linear dimensions, distances, radial velocities, atomic and molecular hydrogen mass and column densities, temperatures, masses and others available are briefly described in the paper. An initial list of about 10 000 entries was condensed into a cross-identified all-sky catalogue containing molecular and gas-dust clouds. Some relationships were studied between main physical features of clouds. Finally, we prepared the complex observing program and address prospective work for gaining the gaps.
Bridging Galaxy Dynamics and Baryon Efficiency of 40 EDGE-CALIFA galaxies
Authors: Kalinova Veselina , Colombo Dario , Rosolowsky Erik 
Published: September 2016

AbstractWe apply the Jeans Axisymmetric Multi-Gaussian Expansion method to the stellar kinematic maps of 40 Sa–Sd EDGE-CALIFA galaxies and derive their circular velocity curves (CVCs). The CVCs are classified using the Dynamical Classification method developed in Kalinova et al. (2015). We also calculate the observational baryon efficiency, OBE, where M*/Mb=M*/(M*+MHI+MH2) of the galaxies using their stellar mass, total neutral hydrogen mass and total molecular gas from CO luminosities. Slow-rising, Flat and Round-peaked CVC types correspond to specific OBEs, stellar and dark matter (DM) halo mass values, while the Sharp-peaked CVCs span in the whole DM halo mass range of 1011-1014M⊙.
A Study of Magnetic Fields on Bright-Rimmed Clouds
Authors: Kusune Takayoshi , Sugitani Koji 
Published: September 2016

AbstractWe have made near-infrared (JHKs) imaging polarimetry toward 24 bright-rimmed clouds in the southern hemisphere in order to reveal their magnetic field structures. The obtained polarization vector maps show that the magnetic field directions inside the bright rim are different from its ambient magnetic field direction, implying that magnetic field structures just inside the ionized front of the clouds are due to the gas compression by UV radiation from nearby massive star. Our investigation into the relation between the magnetic field configuration and the shape of the cloud suggests that the magnetic field configuration affects the evolution of the cloud shape.
Warm dust and gas of massive young stellar objects revealed by Herschel PACS spectroscopy
Authors: Kwon Woojin , van der Tak Floris F. S. , Karska Agata , Herczeg Gregory J. , Chavarría Luis , Herpin Fabrice , Wyrowski Friedrich , Braine Jonathan , van Dishoeck Ewine F. 
Published: September 2016

AbstractWe present results of Herschel PACS imaging spectroscopy data toward ten massive young stellar objects taken as part of the WISH project. Our sample consists of four high mass protostellar objects (HMPOs), two hot molecular cores (HMCs), and four ultracompact HII regions (UCHIIs), and the spectra cover a broad range of wavelengths (55 to 210 μm) imaged over an ~50” field with 5×5 spaxels. By fitting the continua utilizing a modified black-body formula we estimate mass-weighted dust temperature and column density distributions of warm dust and find that UCHII regions are hottest and HMCs are most deeply embedded. We also estimate rotational temperature and column density distributions of warm CO gas using the rotational diagram analysis, which are comparable over targets in contrast to continuum results. By comparing high J CO line fluxes to the RATRAN estimates of centrally heated envelope models, we find that majority of warm CO originates from bipolar outflow shocks.
Dissipation of turbulence by magnetohydrodynamic shock waves
Authors: Lehmann Andrew , Wardle Mark 
Published: September 2016

AbstractWe characterise steady, one-dimensional fast and slow magnetohydrodynamic (MHD) shocks using a two-fluid model. Fast MHD shocks are magnetically driven, forcing ions to stream through the neutral gas ahead of the shock front. This magnetic precursor heats the gas sufficiently to create a large, warm transition zone where all fluid variables only weakly change in the shock front. In contrast, slow MHD shocks are driven by gas pressure where neutral species collide with ion species in a thin hot slab that closely resembles an ordinary gas dynamic shock.We computed observational diagnostics for fast and slow shocks at velocities vs=2–4 km/s and preshock Hydrogen nuclei densities nH = 102-4 cm−3. We followed the abundances of molecules relevant for a simple oxygen chemistry and include cooling by CO, H2 and H2O. Estimates of intensities of 12CO rotational lines show that high-J lines, above J = 6 → 5, are more strongly excited in slow MHD shocks.
Massive Star Formation in the Sparsest Environments
Authors: Oey Sally , Lamb Joel B. 
Published: September 2016

AbstractThere is growing evidence that massive stars sometimes form in extremely sparse environments. The RIOTS4 survey presents a variety of evidence supporting this scenario, including a sample of 14 OB stars in the Small Magellanic Cloud (SMC) that appear to have formed in situ as field stars. This is based on the presence of dense, symmetric HII regions hosting apparent non-runaway stars. We also present a spatially complete IMF of SMC field OB stars for masses > 7 M⊙, showing that the slope is much steeper than the Salpeter value. The binary fraction among field OB stars is also the same as in clusters, based on a RIOTS4 subsample. These results suggest a relative, but incomplete, suppression of massive star formation in the sparsest regimes.
Young Stellar Objects in the Magellanic Clouds: Herschel Spectroscopy First Results
Authors: Oliveira Joana M. , van Loon Jacco Th. , Sewiło Marta 
Published: September 2016

AbstractWe present preliminary results from spectroscopy obtained with PACS and SPIRE onboard the Herschel Space Observatory of a sample of massive Young Stellar Objects in the Magellanic Clouds. We analyse key gas-phase cooling species (Oi], [Cii], H2O, CO, OH), in order to characterise the physical conditions in these metal-poor environments.
Large-Scale Molecular Gas Survey in 12CO, 13CO and C18O (J = 2–1) with the Osaka 1.85m mm-submm Telescope
Authors: Onishi Toshikazu , Nishimura Atsushi , Tokuda Kazuki , Harada Ryohei , Dobashi Kazuhito , Shimoikura Tomomi , Kimura Kimihiro , Ogawa Hideo 
Published: September 2016

AbstractWe have developed a new mm-submm telescope with a diameter of 1.85 m (hereafter, Osaka 1.85-m telescope) installed at the Nobeyama Radio Observatory. The scientific goal is to precisely reveal physical properties of molecular clouds in the Galaxy by obtaining a large-scale distribution of molecular gas, which also can be compared with large-scale observations in various wavelengths. The target frequency is ~230 GHz; simultaneous observations in J = 2–1 lines of 12CO, 13CO and C18O are achieved with a beam size (HPBW) of 2.7 arcmin. Here we present the progress of observations and the scientific results obtained by Osaka 1.85-m telescope. We note that these J = 2–1 data of the Galactic molecular clouds will be precious for the comparison with those of extra-galactic ones that will be obtained with the ALMA with the comparable spatial resolutions.
Star formation in early-type galaxies: the role of stellar winds and kinematics
Authors: Pellegrini Silvia , Negri Andrea , Ciotti Luca 
Published: September 2016

AbstractEarly-type galaxies (ETGs) host a hot ISM produced mainly by stellar winds, and heated by Type Ia supernovae and the thermalization of stellar motions. High resolution 2D hydrodynamical simulations showed that ordered rotation in the stellar component results in the formation of a centrifugally supported cold equatorial disc. In a recent numerical investigation we found that subsequent generations of stars are formed in this cold disc; this process consumes most of the cold gas, leaving at the present epoch cold masses comparable to those observed. Most of the new stellar mass formed a few Gyrs ago, and resides in a disc.
From cloud crash to star birth: star formation in cloud collisions
Authors: Shima Kazuhiro , Tasker Elizabeth J. , Habe Asao 
Published: September 2016

AbstractWe performed three-dimensional hydrodynamical simulations of idealized giant molecular cloud collisions including star formation and radiative transfer. We found that the characteristics of the colliding systems are similar to the observations of the Spitzer bubbles, suggesting these objects could be created in such interactions. A high velocity collision creates a top-heavy core mass distribution but is not strongly affected by radiation. At lower collision speeds, the HII regions have time to expand within the shock and promote the formation of massive cores.
Characterising the Protostellar Population of the Magellanic Clouds with VLT/SINFONI
Authors: Ward Jacob , Oliveira Joana , van Loon Jacco , Sewilo Marta 
Published: September 2016

AbstractAt distances of ~50 kpc and ~60 kpc for the Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC) respectively the Magellanic Clouds present us with a unique opportunity to study star formation in environments outside our own galaxy. Through Spitzer and Herschel photometry and spectroscopy, samples of Young Stellar Objects (YSOs) have been selected and spectroscpically confirmed in the Magellanic Clouds. Here we present some of the key results of our SINFONI K-band observations towards massive YSOs in the Magellanic Clouds. We resolve a number of Spitzer sources into multiple, previously unresolved, components and our analysis of emission lines suggest higher accretion rates and different disc properties compared with massive YSOs in the Milky Way.
Diffuse Interstellar Bands in Emission
Authors: Williams T. B. , Sarre P. , Marshall C. C. M. , Spekkens K. , de Naray R. Kuzio 
Published: September 2016

AbstractRecent Fabry-Pérot observations towards the galaxy NGC 1325 with the Southern African Large Telescope (SALT) led to the serendipitous discovery of an emission feature centered at 661.3 nm arising from material in the interstellar medium (ISM) of our Galaxy; this emission feature lies at the wavelength of one of the sharper and stronger diffuse bands normally seen in absorption. The flux of the feature is 4.2 ± 0.5 × 10−18 es−1 cm−2 arcsec−2. It appears that this is the first observation of emission from a diffuse band carrier in the ISM, excited in this case by the interstellar radiation field. We present the discovery spectra and describe follow-up measurements proposed for SALT.