bluuebunny/crossref_metadata_2025_split huggingface dataset:
The Impact of AuSSI-WA at a Primary School
Authors: Lewis Elaine , Baudains Catherine , Mansfield Caroline 
Published: February 2017

AbstractThis paper presents the findings of the first stage of research on the impact of the Australian Sustainable Schools Initiative (AuSSI) at an independent primary school in Western Australia. A longitudinal (20 year) case study is being conducted, utilising data related to Education for Sustainability (EfS) at the school from 1990-2009. 2005 was a critical year for the school because it marked the beginning of participation in the Sustainable Schools Initiative pilot in Western Australia (AuSSI-WA). The research investigates elements of EfS in operation at the school pre- and post- AuSSI-WA, as well as student and teacher outcomes after involvement in the Initiative. An analysis of the initial data suggests that participation in AuSSI-WA enabled the school to engage with a growing commitment to EfS in the context of a whole - school approach.
Microzooplankton composition in the winter sea ice of the Weddell Sea
Authors: Monti-Birkenmeier Marina , Diociaiuti Tommaso , Umani Serena Fonda , Meyer Bettina 
Published: February 2017

AbstractSympagic microzooplankton were studied during late winter in the northern Weddell Sea for diversity, abundance and carbon biomass. Ice cores were collected on an ice floe along three dive transects and seawater was taken from under the ice through the central dive hole from which all transects were connected. The areal and vertical microzooplankton distributions in the ice and water were compared. Abundance (max. 1300 ind. l-1) and biomass (max. 28.2 µg C l-1) were high in the ice cores and low in the water below the sea ice (max. 19 ind. l-1, 0.15 µg C l-1, respectively). The highest abundances were observed in the bottom 10 cm of the ice cores. The microzooplankton community within the sea ice comprised mainly aloricate ciliates, foraminifers and micrometazoans. In winter, microzooplankton represent an important fraction of the sympagic community in the Antarctic sea ice. They can potentially control microalgal production and contribute to particulate organic carbon concentrations when released into the water column during the ice melt in spring. Continued reduction of the sea ice may undermine the roles of microzooplankton, leading to a reduction or complete loss of diversity, abundance and biomass of these sympagic protists.
SWAG: Survey of Water and Ammonia in the Galactic Center
Authors: Ott Jürgen , Meier David S. , Krieger Nico , Rickert Matthew ,   the SWAG team
Published: February 2017

AbstractSWAG (“Survey of Water and Ammonia in the Galactic Center”) is a multi-line interferometric survey toward the Center of the Milky Way conducted with the Australia Telescope Compact Array. The survey region spans the entire ~400 pc Central Molecular Zone and comprises ~42 spectral lines at pc spatial and sub-km/s spectral resolution. In addition, we deeply map continuum intensity, spectral index, and polarization at the frequencies where synchrotron, free-free, and thermal dust sources emit. The observed spectral lines include many transitions of ammonia, which we use to construct maps of molecular gas temperature, opacity and gas formation temperature (see poster by Nico Krieger et al., this volume). Water masers pinpoint the sites of active star formation and other lines are good tracers for density, radiation field, shocks, and ionization. This extremely rich survey forms a perfect basis to construct maps of the physical parameters of the gas in this extreme environment.
Dark Matter and the Galactic Center
Authors: Bergstrom Lars 
Published: February 2017

AbstractThe question of the identity of dark matter is one of the most outstanding enigmas of contemporary cosmology and particle astrophysics. An overview is given of the subject, a brief history, some proposed particle candidates, and the several methods now available for finally solving this difficult problem. The galactic center is one of the most interesting places for the dark matter search using γ-rays, but also one that has challenging, maybe confusing, other sources of GeV-scale radiation.
Temperature Evolution of Molecular Clouds in the Central Molecular Zone
Authors: Krieger Nico , Ott Jürgen , Walter Fabian , Kruijssen J. M. Diederik , Beuther Henrik ,   the SWAG team
Published: February 2017

AbstractWe infer the absolute time dependence of kinematic gas temperature along a proposed orbit of molecular clouds in the Central Molecular Zone (CMZ) of the Galactic Center (GC). Ammonia gas temperature maps are one of the results of the “Survey of Water and Ammonia in the Galactic Center” (SWAG, PI: J. Ott); the dynamical model of molecular clouds in the CMZ was taken from Kruijssen et al. (2015). We find that gas temperatures increase as a function of time in both regimes before and after the cloud passes pericenter on its orbit in the GC potential. This is consistent with the recent proposal that pericenter passage triggers gravitational collapse. Other investigated quantities (line width, column density, opacity) show no strong sign of time dependence but are likely dominated by cloud-to-cloud variations.
Millisecond Pulsars in the Galactic Bulge? An Extended Discussion on the Wavelet Analysis of the Fermi-LAT data
Authors: Bartels Richard , Weniger Christoph 
Published: February 2017

AbstractA clear excess in the Fermi-LAT data is present at energies around a few GeV. The spectrum of this so-called ’GeV excess’ is remarkably similar to the expected annihilation signal of WIMP dark matter. However, a large bulge population of millisecond pulsars living below the Fermi–LAT detection threshold could also explain the excess spectrum. In a recent work we optimized the search for sub-threshold sources, by applying a wavelet transform to the Fermi–LAT gamma-ray data. In the Inner-Galaxy the wavelet signal is significantly enhanced, providing supportive evidence for the point source interpretation of the excess. In these proceedings we will extent our previous work with a spectral analysis and elaborate on the potential contamination from substructures in the gas.
Clump formation through colliding stellar winds in the Galactic Centre
Authors: Calderón D. , Cuadra J. , Ballone A. , Schartmann M. , Burkert A. , Prieto J. , Gillessen S. 
Published: February 2017

AbstractWe study the process of clump formation from hydrodynamic instabilities in stellar wind collisions, using analytical and numerical techniques. We show that the cloud G2 in the Galactic Centre could have been formed in this way, with the most promising sources being compact massive binaries, such as IRS 16SW.
Hitomi X-ray Astronomy Satellite: Power of High-Resolution Spectroscopy
Authors: Odaka Hirokazu ,   the Hitomi Collaboration
Published: February 2017

AbstractHitomi (ASTRO-H) is an X-ray observatory developed by an international collaboration led by JAXA. An X-ray microcalorimeter onboard this satellite has opened a new window of high-resolution spectroscopy with an unprecedented energy resolution of 5 eV (FWHM) at 6 keV. The spacecraft was launched on February 17, 2016 from Tanegashima Island, Japan, and we completed initial operations including deployment of the hard X-ray imagers on the extensible optical bench. All scientific instruments had successfully worked until the sudden loss of the mission on March 26. We have obtained a spectrum showing fully resolved emission lines through the first-light observation of the Perseus Cluster. The line-of-sight velocity dispersion of 164 ± 10 km s−1 reveals the quiescent environment of intracluster medium at the cluster core, implying that measured cluster mass requires little correction for the turbulent pressure. We also discuss observations to the Galactic Center which could be performed with Hitomi.
Deeply Embedded Protostellar Population in the Central Molecular Zone Suggested by H2O Masers and Dense Cores
Authors: Lu Xing , Zhang Qizhou , Kauffmann Jens , Pillai Thushara , Longmore Steven N. , Kruijssen J. M. Diederik , Battersby Cara 
Published: February 2017

AbstractThe Central Molecular Zone (CMZ), usually referring to the inner 500 pc of the Galaxy, contains a dozen of massive (~105M⊙) molecular clouds. Are these clouds going to actively form stars like Sgr B2? How are they affected by the extreme physical conditions in the CMZ, such as strong turbulence? Here we present a first step towards answering these questions. Using high-sensitivity, high angular resolution radio and (sub)millimeter observations, we studied deeply embedded star formation in six massive clouds in the CMZ, including the 20 and 50 km s−1 clouds, Sgr B1 off (as known as dust ridge clouds e/f), Sgr C, Sgr D, and G0.253 – 0.016. The VLA water maser observations suggest a population of deeply embedded protostellar candidates, many of which are new detections. The SMA 1.3 mm continuum observations reveal peaks in dust emission associated with the masers, suggesting the existence of dense cores. While our findings confirm that clouds such as G0.253 – 0.016 lack internal compact substructures and are quiescent in terms of star formation, two clouds (the 20 km s−1 cloud and Sgr C) stand out with clusters of water masers with associated dense cores which may suggest a population of deeply embedded protostars at early evolutionary phases. Follow-up observations with VLA and ALMA are necessary to confirm their protostellar nature.
Statistical Challenges in fitting stellar orbits around the super-massive black hole at the Galactic center
Authors: Martinez Gregory D. , Kosmo Kelly , Hees Aurelien , Ahn Joseph , Ghez Andrea 
Published: February 2017

AbstractOver two decades of astrometric and radial velocity data of short period stars at the Galactic center has the potential to provide unprecedented tests of General Relativity and insight into the astrophysics of the super-massive black hole. Fundamental to this is understanding the underlying statistical issues of fitting stellar orbits. Unintended prior effects can obscure actual physical effects from General Relativity and underlying extended mass distribution. At the heart of this is dealing with large parameter spaces inherent to multi-star fitting and ensuring acceptable coverage properties of the resulting confidence intervals in the Bayesian framework. This proceeding will detail some of the UCLA group's analysis and work in addressing these statistical issues.
Advances from Recent Multi-wavelength Campaigns on Sgr A*
Authors: Haggard Daryl 
Published: February 2017

AbstractSagittarius A* is the closest example of a supermassive black hole and our proximity allows us to detect emission from its accretion flow in the radio, submillimeter, near IR, and X-ray regimes. Ambitious monitoring campaigns have yielded rich multi-wavelength, time-resolved data that have the power to probe the physical processes underlying Sgr A*’s quiescent and flare emission. Here, I review the status of Sgr A* X-ray monitoring campaigns from the Chandra X-ray Observatory (also XMM Newton, and Swift), and efforts to coordinate these with observations across the electromagnetic spectrum. I also discuss how these observations constrain models for Sgr A*’s variability, which range from tidal disruption of asteroids to gravitational lensing to collimated outflows to magnetic reconnection.
Molecular and ionized gas kinematics in the GC Radio Arc
Authors: Butterfield N. , Lang C.C. , Mills E. A. C. , Ludovici D. , Ott J. , Morris M. R. 
Published: February 2017

AbstractWe present NH3 and H64α+H63α VLA observations of the Radio Arc region, including the M0.20 – 0.033 and G0.10 – 0.08 molecular clouds. These observations suggest the two velocity components of M0.20 – 0.033 are physically connected in the south. Additional ATCA observations suggest this connection is due to an expanding shell in the molecular gas, with the centroid located near the Quintuplet cluster. The G0.10 – 0.08 molecular cloud has little radio continuum, strong molecular emission, and abundant CH3OH masers, similar to a nearby molecular cloud with no star formation: M0.25+0.01. These features detected in G0.10 – 0.08 suggest dense molecular gas with no signs of current star formation.
A Brief Update on the CMZoom Survey
Authors: Battersby C. , Keto E. , Zhang Q. , Longmore S.N. , Kruijssen J. M. D. , Pillai T. , Kauffmann J. , Walker D. , Lu X. , Ginsburg A. , Bally J. , Mills E.A.C. , Henshaw J. , Immer K. , Patel N. , Tolls V. , Walsh A. , Johnston K. , Ho L. C. 
Published: February 2017

AbstractThe inner few hundred parsecs of the Milky Way, the Central Molecular Zone (CMZ), is our closest laboratory for understanding star formation in the extreme environments (hot, dense, turbulent gas) that once dominated the universe. We present an update on the first large-area survey to expose the sites of star formation across the CMZ at high-resolution in submillimeter wavelengths: the CMZoom survey with the Submillimeter Array (SMA). We identify the locations of dense cores and search for signatures of embedded star formation. CMZoom is a three-year survey in its final year and is mapping out the highest column density regions of the CMZ in dust continuum and a variety of spectral lines around 1.3 mm. CMZoom combines SMA compact and subcompact configurations with single-dish data from BGPS and the APEX telescope, achieving an angular resolution of about 4″ (0.2 pc) and good image fidelity up to large spatial scales.
The link between solenoidal turbulence and slow star formation in G0.253+0.016
Authors: Federrath C. , Rathborne J. M. , Longmore S. N. , Kruijssen J. M. D. , Bally J. , Contreras Y. , Crocker R. M. , Garay G. , Jackson J. M. , Testi L. , Walsh A. J. 
Published: February 2017

AbstractStar formation in the Galactic disc is primarily controlled by gravity, turbulence, and magnetic fields. It is not clear that this also applies to star formation near the Galactic Centre. Here we determine the turbulence and star formation in the CMZ cloud G0.253+0.016. Using maps of 3 mm dust emission and HNCO intensity-weighted velocity obtained with ALMA, we measure the volume-density variance σρ /ρ 0=1.3±0.5 and turbulent Mach number $\mathcal{M}$ = 11±3. Combining these with turbulence simulations to constrain the plasma β = 0.34±0.35, we reconstruct the turbulence driving parameter b=0.22±0.12 in G0.253+0.016. This low value of b indicates solenoidal (divergence-free) driving of the turbulence in G0.253+0.016. By contrast, typical clouds in the Milky Way disc and spiral arms have a significant compressive (curl-free) driving component (b > 0.4). We speculate that shear causes the solenoidal driving in G0.253+0.016 and show that this may reduce the star formation rate by a factor of 7 compared to nearby clouds.
Possible Detection of Quasi-Periodic Oscillations from Sgr A* at 43 GHz
Authors: Iwata Yuhei , Oka Tomoharu , Miyoshi Makoto 
Published: February 2017

AbstractQuasi-periodic oscillations (QPOs) are believed to be indirect evidence for black holes. Several authors have reported detections of QPOs from Sgr A*, the nucleus of our Galaxy, in infrared and X-ray wavelength during flare-ups. Miyoshi et al. (2011) reported a tentative detection of QPOs in the 43 GHz light curve of Sgr A* obtained with the Very Long Baseline Array (VLBA). To confirm their detection, we reanalysed their VLBA data very conservatively. The 43 GHz flux was calculated for every 15 seconds by assuming a two-dimensional Gaussian-shape spatial structure. The Lomb-Scargle periodogram of the 43 GHz flux just after a millimeter wave flare of Sgr A*, shows three apparent peaks at 10.2, 14.6 and 32.1 min. Two of them are barely consistent with the previously reported QPOs. Using the resonant oscillation model, we estimated the spin parameter of the Sgr A* black hole to be 0.56 assuming the mass of 4.3 × 106M⊙.
Thousands of Stellar SiO masers in the Galactic center: The Bulge Asymmetries and Dynamic Evolution (BAaDE) survey
Authors: Sjouwerman Loránt O. , Pihlström Ylva M. , Rich R. Michael , Morris Mark R. , Claussen Mark J 
Published: February 2017

AbstractA radio survey of red giant SiO sources in the inner Galaxy and bulge is not hindered by extinction. Accurate stellar velocities (<1 km/s) are obtained with minimal observing time (<1 min) per source. Detecting over 20,000 SiO maser sources yields data comparable to optical surveys with the additional strength of a much more thorough coverage of the highly obscured inner Galaxy. Modeling of such a large sample would reveal dynamical structures and minority populations; the velocity structure can be compared to kinematic structures seen in molecular gas, complex orbit structure in the bar, or stellar streams resulting from recently infallen systems. Our Bulge Asymmetries and Dynamic Evolution (BAaDE) survey yields bright SiO masers suitable for follow-up Galactic orbit and parallax determination using VLBI.Here we outline our early VLA observations at 43 GHz in the northern bulge and Galactic plane (0<l°<250), and ALMA observations at 86 GHz in the southern bulge (250<l°<360). We report a preliminary overall 70% detection rate in our color-selected MSX sources.
Time Evolution of the Giant Molecular Cloud Mass Functions across Galactic Disks
Authors: Kobayashi Masato I. N. , Inutsuka Shu-ichiro , Kobayashi Hiroshi , Hasegawa Kenji 
Published: February 2017

AbstractWe formulate and conduct the time-integration of time evolution equation for the giant molecular cloud mass function (GMCMF) including the cloud-cloud collision (CCC) effect. Our results show that the CCC effect is only limited in the massive-end of the GMCMF and indicate that future high resolution and sensitivity radio observations may constrain giant molecular cloud (GMC) timescales by observing the GMCMF slope in the lower mass regime.
Investigating Magnetic Activity in the Galactic Centre by Global MHD Simulation
Authors: Suzuki Takeru K. , Fukui Yasuo , Torii Kazufumi , Machida Mami , Matsumoto Ryoji , Kakiuchi Kensuke 
Published: February 2017

AbstractBy performing a global magnetohydrodynamical (MHD) simulation for the Milky Way with an axisymmetric gravitational potential, we propose that spatially dependent amplification of magnetic fields possibly explains the observed noncircular motion of the gas in the Galactic centre (GC) region. The radial distribution of the rotation frequency in the bulge region is not monotonic in general. The amplification of the magnetic field is enhanced in regions with stronger differential rotation, because magnetorotational instability and field-line stretching are more effective. The strength of the amplified magnetic field reaches ≳ 0.5 mG, and radial flows of the gas are excited by the inhomogeneous transport of angular momentum through turbulent magnetic field that is amplified in a spatially dependent manner. As a result, the simulated position-velocity diagram exhibits a time-dependent asymmetric parallelogram-shape owing to the intermittency of the magnetic turbulence; the present model provides a viable alternative to the bar-potential-driven model for the parallelogram shape of the central molecular zone. In addition, Parker instability (magnetic buoyancy) creates vertical magnetic structure, which would correspond to observed molecular loops, and frequently excited vertical flows. Furthermore, the time-averaged net gas flow is directed outward, whereas the flows are highly time dependent, which would contribute to the outflow from the bulge.
Millimeter VLBI observations of Sgr A* with KaVA and KVN
Authors: Zhao G.-Y. , Kino M. , Cho I.-J. , Akiyama K. , Sohn B. W. , Jung T. , Algaba J. C. , Hada K. , Hagiwara Y. , Hodgson J. , Honma M. , Kawaguchi N. , Koyama S. , Lee J. A. , Lee T. , Niinuma K. , Oh J. , Park J.-H. , Ro H. , Sawada-Satoh S. , Tazaki F. , Trippe S. , Wajima K. , Yoo H. 
Published: February 2017

AbstractWe present recent observation results of Sgr A* at millimeter obtained with VLBI arrays in Korea and Japan.7 mm monitoring of Sgr A* is part of our AGN large project. The results at 7 epochs during 2013-2014, including high resolution maps, flux density and two-dimensional size measurements are presented. The source shows no significant variation in flux and structure related to the G2 encounter in 2014. According to recent MHD simulations by kawashimaet al., flux and magnetic field energy can be expected to increase several years after the encounter; We will keep our monitoring in order to test this prediction.Astrometric observations of Sgr A* were performed in 2015 at 7 and 3.5 millimeter simultaneously. Source-frequency phase referencing was applied and a combined ”core-shift” of Sgr A* and a nearby calibrator was measured. Future observations and analysis are necessary to determine the core-shift in each source.
Can we infer the past activity of M31⋆ as we do for Sgr A⋆?
Authors: Clavel Maïca , Terrier Régis , Goldwurm Andrea , Morris Mark R. , Ponti Gabriele 
Published: February 2017

AbstractThe history of supermassive black holes’ activity can be partly constrained by monitoring the diffuse X-ray emission possibly created by the echoes of past events propagating through the molecular clouds of their respective environments. In particular, using this method we have demonstrated that our Galaxy’s supermassive black hole, Sgr A⋆, has experienced multiple periods of higher activity in the last centuries, likely due to several short but very energetic events, and we now investigate the possibility of studying the past activity of other supermassive black holes by applying the same method to M31⋆. We set strong constraints on putative phase transitions of this more distant galactic nucleus but the existence of short events such as the ones observed in the Galactic center cannot be assessed with the upper limits we derived.
Imperial Thirst: Water and Colonial Administration in Algeria, 1840–1880
Authors: Cutler Brock 
Published: February 2017

“Water,” wrote the mayor’s council late in the nineteenth century, “is the only thing holding Algiers back from expanding its glory as the queen of African cities.” Paris uses 240 liters of water per person per day, it reported; New York, Philadelphia and Chicago 400 liters. Algiers could only muster a meager 60 liters per day per person, far below the levels necessary to feed a population, fill wells, and scrub a city of its toxins. For over half a century, the council reported, Algiers had thirsted after the clean water necessary to make it a great city. If the French were to make Algiers truly modern, they would need to solve this vexing problem of water.Thus the council summed up one of the ongoing challenges in continuing settler colonialism in Algeria. Environmental projects—battling epidemic disease, drought, locust invasions, and providing/establishing hydraulic control—became important factors in the rise and expansion of the colonial state. In the midst of a crippling environmental disaster, water—access to fresh water for drinking, controlling agricultural infrastructure, and ensuring cities were “hygienic”—became a site of contention in the creation of the modern state. In this paper I will briefly examine how the physical control of water resources, along with discourses about modernity and modern governance, contributed to the expansion of the colonial state by the end of the 1860s.