Galactic Halo substructure in the Sloan Digital Sky Survey: the ancient tidal stream from the Sagittarius dwarf galaxy

Two studies have recently reported the discovery of pronounced Halo substructure in the Sloan Digital Sky Survey (SDSS) commissioning data. Here we show that this Halo substructure is almost in its entirety due to the expected tidal stream torn off the Sagittarius dwarf galaxy during the course of its many close encounters with the Milky Way. This interpretation makes strong predictions on the kinematics and distances of these stream stars. Comparison of the structure in old horizontal branch stars, detected by the SDSS team, with the carbon star structure discovered in our own survey, indicates that this halo stream is of comparable age to the Milky Way. It would appear that the Milky Way and the Sagittarius dwarf galaxy have been a strongly interacting system for most of their existence. Once complete, the SDSS will provide a unique dataset with which to constrain the dynamical evolution of the Sagittarius dwarf galaxy, it will also strongly constrain the mass distribution of the outer Milky Way.Comment: 7 pages, 3 figures (1 color figure chunky due to PS compression), minor revisions,accepted by ApJ

The detection of microplastics in beach sediments: extraction methods, biases, and results from samples along the German Baltic coast

The spatial and temporal variations of microplastic concentrations in beach sediments at the German Baltic coast are investigated. A total of 11 locations were sampled in the Rostock area, on Ruegen island, in the Oder / Peene estuary, and in the North Sea Jade Bay. Microplastic particle and fibre concentrations were in the range 0-11 coloured pieces/kg sediment, with typical numbers of 1-3 particles/kg. Industrial and urban river discharge, fishing activity, and tourism are identified as the most likely sources for the observed microplastic contaminations.In der Masterarbeit wurde die räumliche und zeitliche Verteilung von Mikroplastik in Strandsedimenten an der deutschen Ostseekueste untersucht. Sedimentproben wurden an 11 Stränden entlang der Rostocker und Ruegener Küsten, im Oder / Peene Ästuar und im Jadebusen an der Nordsee genommen. Die Konzentrationen von Mikroplastik-Partikeln und -Fasern lagen im Bereich 0-11 farbige Teilchen/kg Sediment, mit typischen Konzentrationen von 1-3 Partikeln/kg. Als wahrscheinlichste Eintrittspfade für Mikroplastik in die Ostsee wurden industrielle und städtische Abwässer (Rostock, Stettin), Fischerei (Oder / Peene) und Tourismus (Warnemuende) identifiziert

The orbital motion of the Arches cluster — clues on cluster formation near the galactic center

The Arches cluster is one of the most massive, young clusters in the Milky Way. Located inside the central molecular zone in the inner 200 pc of the Galactic center, it formed in one of the most extreme star-forming environments in the present-day Galaxy. Its young age of only 2.5 Myr allows us to observe the cluster despite the strong tidal shear forces in the inner Galaxy. The orbit of the cluster determines its dynamical evolution, tidal stripping, and hence its fate. We have measured the proper motion of the Arches cluster relative to the ambient field from Keck/NIRC2 LGS-AO and VLT/NAOS-CONICA NGS-AO observations taken 4.3 years earlier. When combined with the radial velocity, we derive a 3D space motion of 232 ± 30 km/s for the Arches. This motion is exceptionally large when compared to molecular cloud orbits in the GC, and places stringent constraints on the formation scenarios for starburst clusters in dense, nuclear environments

The Discovery of a Very Massive Star in W49

Very massive stars (M>100 M$_{\odot}$) are very rare objects, but have a strong influence on their environment. The formation of this kind of objects is of prime importance in star formation, but observationally still poorly constrained. We report on the identification of a very massive star in the central cluster of the star-forming region W49. We investigate near-infrared K-band spectroscopic observations of W49 from VLT/ISAAC together with JHK images obtained with NTT/SOFI and LBT/LUCI. We derive a spectral type of W49nr1, the brightest star in the dense core of the central cluster of W49. On the basis of its K-band spectrum, W49nr1 is classified as an O2-3.5If* star with a K-band absolute magnitude of -6.27$\pm$0.10 mag. The effective temperature and bolometric correction are estimated from stars of similar spectral type. After comparison to the Geneva evolutionary models, we find an initial mass between 100 M$_{\odot}$ and 180 M$_{\odot}$. Varying the extinction law results in a larger initial mass range of 90 - 250 M$_{\odot}$.Comment: 5 pages, 3 figures, 1 table, accepted for publication in A&A Letter

A Review and Taxonomy of Methods for Quantifying Dataset Similarity

In statistics and machine learning, measuring the similarity between two or more datasets is important for several purposes. The performance of a predictive model on novel datasets, referred to as generalizability, critically depends on how similar the dataset used for fitting the model is to the novel datasets. Exploiting or transferring insights between similar datasets is a key aspect of meta-learning and transfer-learning. In two-sample testing, it is checked, whether the underlying (multivariate) distributions of two datasets coincide or not. Extremely many approaches for quantifying dataset similarity have been proposed in the literature. A structured overview is a crucial first step for comparisons of approaches. We examine more than 100 methods and provide a taxonomy, classifying them into ten classes, including (i) comparisons of cumulative distribution functions, density functions, or characteristic functions, (ii) methods based on multivariate ranks, (iii) discrepancy measures for distributions, (iv) graph-based methods, (v) methods based on inter-point distances, (vi) kernel-based methods, (vii) methods based on binary classification, (viii) distance and similarity measures for datasets, (ix) comparisons based on summary statistics, and (x) different testing approaches. Here, we present an extensive review of these methods. We introduce the main underlying ideas, formal definitions, and important properties.Comment: 90 pages, submitted to Statistics Survey

Mass Functions and Mass Segregation in Young Starburst Clusters

The Milky Way starburst clusters Arches in the Galactic Center region and NGC 3603 in the Carina spiral arm are studied with the aim to gain deeper insight into the stellar mass distribution in starburst clusters. The dense stellar population in both clusters is resolved in unprecedented detail with high angular resolution, near-infrared instruments. In the case of the Arches cluster, diffraction-limited, adaptive optics observations are analysed, and the achievements and limitations of ground-based vs. space-based diffraction-limited imaging are revealed by comparison with HST/NICMOS data. In the case of NGC 3603, seeing-limited JHKL photometry is used to derive colour-excess fractions, and is complemented by space-based Halpha data, both serving as tracers for circumstellar disks. Disk survival in starburst clusters is discussed. The present-day mass function (MF) of both clusters is deduced from colour-magnitude diagrams. Radial variations in the MFs reveal a heavily mass-segregated core in both starburst clusters. Dynamical timescales are estimated and interpreted with respect to primordial and dynamical segregation. The implications for massive star and cluster formation scenarios are discussed. Evidence for a low-mass cut-off is observed in the Arches MF, but not in NGC 3603, indicating a reduced formation efficiency for M < 10 Msun stars in the Galactic Center. This environmental difference has strong implications for the formation of stellar populations in galactic nuclei and starburst galaxies

Optimizing green hydrogen production from wind and solar for hard-to-abate industrial sectors across multiple sites in Europe

This article analyzes a power-to-hydrogen system, designed to provide high-temperature heat to hard-to-abate industries. We leverage on a geospatial analysis for wind and solar availability and different industrial demand profiles with the aim to identify the ideal sizing of plant components and the resulting Levelized Cost of Hydrogen (LCOH). We assess the carbon intensity of the produced hydrogen, especially when grid electricity is utilized. A methodology is developed to size and optimize the PV and wind energy capacity, the electrolyzer unit, and hybrid storage, by combining compressed hydrogen storage with lithium-ion batteries. The hydrogen demand profile is generated synthetically, thus allowing different industrial consumption profiles to be investigated. The LCOH in a baseline scenario ranges from 3.5 to 8.9 €/kg, with the lowest values in wind-rich climates. Solar PV only plays a role in locations with high PV full-load hours. It was found that optimal hydrogen storage can cover the users’ demand for 2–3 days. Most of the considered scenarios comply with the emission intensity thresholds set by the EU. A sensitivity analysis reveals that a lower variability of the demand profile is associated with cost savings. An ideally constant demand profile results in a cost reduction of approximately 11 %

The orbital motion of the Quintuplet cluster - a common origin for the Arches and Quintuplet clusters?

We investigate the orbital motion of the Quintuplet cluster near the Galactic center with the aim of constraining formation scenarios of young, massive star clusters in nuclear environments. Three epochs of adaptive optics high-angular resolution imaging with Keck/NIRC2 and VLT/NACO were obtained over a time baseline of 5.8 years, delivering an astrometric accuracy of 0.5-1 mas/yr. Proper motions were derived in the cluster reference frame and were used to distinguish cluster members from the majority of field stars. Fitting the cluster and field proper motion distributions with 2D gaussian models, we derive the orbital motion of the cluster for the first time. The Quintuplet is moving with a 2D velocity of 132 +/- 15 km/s with respect to the field along the Galactic plane, which yields a 3D orbital velocity of 167 +/- 15 km/s when combined with the previously known radial velocity. From a sample of 119 stars measured in three epochs, we derive an upper limit to the velocity dispersion in the core of the Quintuplet cluster of sigma_1D < 10 km/s. Knowledge of the three velocity components of the Quintuplet allows us to model the cluster orbit in the potential of the inner Galaxy. Comparing the Quintuplet's orbit with the Arches orbit, we discuss the possibility that both clusters originated in the same area of the central molecular zone. [abridged]Comment: 40 pages, 12 figures, accepted for publication in Ap

Circumstellar discs in Galactic centre clusters: Disc-bearing B-type stars in the Quintuplet and Arches clusters

We investigate the circumstellar disc fraction as determined from L-band excess observations of the young, massive Arches and Quintuplet clusters residing in the central molecular zone of the Milky Way. The Quintuplet cluster was searched for L-band excess sources for the first time. We find a total of 26 excess sources in the Quintuplet cluster and 21 in the Arches cluster, of which 13 are new detections. With the aid of proper motion membership samples, the disc fraction of the Quintuplet cluster was derived for the first time to be 4.0 +/- 0.7%. There is no evidence for a radially varying disc fraction in this cluster. In the case of the Arches cluster, a disc fraction of 9.2 +/- 1.2% approximately out to the cluster's predicted tidal radius, r < 1.5 pc, is observed. This excess fraction is consistent with our previously found disc fraction in the cluster in the radial range 0.3 < r < 0.8 pc. In both clusters, the host star mass range covers late A- to early B-type stars, 2 < M < 15 Msun, as derived from J-band photospheric magnitudes. We discuss the unexpected finding of dusty circumstellar discs in these UV intense environments in the context of primordial disc survival and formation scenarios of secondary discs. We consider the possibility that the L-band excess sources in the Arches and Quintuplet clusters could be the high-mass counterparts to T Tauri pre-transitional discs. As such a scenario requires a long pre-transitional disc lifetime in a UV intense environment, we suggest that mass transfer discs in binary systems are a likely formation mechanism for the B-star discs observed in these starburst clusters.Comment: 47 pages, 22 figures, accepted by A&

Massive Star Formation

The enormous radiative and mechanical luminosities of massive stars impact a vast range of scales and processes, from the reionization of the universe, to the evolution of galaxies, to the regulation of the interstellar medium, to the formation of star clusters, and even to the formation of planets around stars in such clusters. Two main classes of massive star formation theory are under active study, Core Accretion and Competitive Accretion. In Core Accretion, the initial conditions are self-gravitating, centrally concentrated cores that condense with a range of masses from the surrounding, fragmenting clump environment. They then undergo relatively ordered collapse via a central disk to form a single star or a small-N multiple. In this case, the pre-stellar core mass function has a similar form to the stellar initial mass function. In Competitive Accretion, the material that forms a massive star is drawn more chaotically from a wider region of the clump without passing through a phase of being in a massive, coherent core. In this case, massive star formation must proceed hand in hand with star cluster formation. If stellar densities become very high near the cluster center, then collisions between stars may also help to form the most massive stars. We review recent theoretical and observational progress towards understanding massive star formation, considering physical and chemical processes, comparisons with low and intermediate-mass stars, and connections to star cluster formation.Comment: Accepted for publication as a chapter in Protostars and Planets VI, University of Arizona Press (2014), eds. H. Beuther, R. Klessen, C. Dullemond, Th. Hennin