TY - CHAP A1 - Bogin, Barry A1 - Hermanussen, Michael A1 - Scheffler, Christiane T1 - Fear, violence, inequality and stunting in Guatemala T2 - American journal of human biology : the official journal of the Human Biology Association Y1 - 2021 U6 - https://doi.org/10.1002/ajhb.23593 SN - 1520-6300 SN - 1042-0533 VL - 33 PB - Wiley Interscience CY - New York, NY [u.a.] ER - TY - JOUR A1 - Anders, Friedrich A1 - Khalatyan, Arman A1 - Queiroz, Anna B. A. A1 - Chiappini, Cristina A1 - Ardèvol, Judith A1 - Casamiquela, Laia A1 - Figueras, Francesca A1 - Jiménez-Arranz, Óscar A1 - Jordi, Carme A1 - Monguio, Maria A1 - Romero-Gómez, Merce A1 - Altamirano, Diego A1 - Antoja, Teresa A1 - Assaad, R. A1 - Cantat-Gaudin, Tristan A1 - Castro-Ginard, Alfred A1 - Enke, Harry A1 - Girardi, Léo A1 - Guiglion, Guillaume A1 - Khan, Saniya A1 - Luri, Xavier A1 - Miglio, Andrea A1 - Minchev, Ivan A1 - Ramos, Pau A1 - Santiago, Basillio Xavier A1 - Steinmetz, Matthias T1 - Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia EDR3 stars brighter than G=18.5 JF - Astronomy and astrophysics N2 - We present a catalogue of 362 million stellar parameters, distances, and extinctions derived from Gaia's Early Data Release (EDR3) cross-matched with the photometric catalogues of Pan-STARRS1, SkyMapper, 2MASS, and All WISE. The higher precision of the Gaia EDR3 data, combined with the broad wavelength coverage of the additional photometric surveys and the new stellar-density priors of the StarHorse code, allows us to substantially improve the accuracy and precision over previous photo-astrometric stellar-parameter estimates. At magnitude G = 14 (17), our typical precisions amount to 3% (15%) in distance, 0.13 mag (0.15 mag) in V-band extinction, and 140 K (180 K) in effective temperature. Our results are validated by comparisons with open clusters, as well as with asteroseismic and spectroscopic measurements, indicating systematic errors smaller than the nominal uncertainties for the vast majority of objects. We also provide distance- and extinction-corrected colour-magnitude diagrams, extinction maps, and extensive stellar density maps that reveal detailed substructures in the Milky Way and beyond. The new density maps now probe a much greater volume, extending to regions beyond the Galactic bar and to Local Group galaxies, with a larger total number density. We publish our results through an ADQL query interface (gaia . aip . de) as well as via tables containing approximations of the full posterior distributions. Our multi-wavelength approach and the deep magnitude limit render our results useful also beyond the next Gaia release, DR3. KW - stars: distances KW - stars: fundamental parameters KW - Galaxy: general KW - Galaxy: stellar content KW - Galaxy: structure Y1 - 2022 U6 - https://doi.org/10.1051/0004-6361/202142369 SN - 0004-6361 SN - 1432-0746 VL - 658 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Keles, Engin A1 - Mallonn, Matthias A1 - Kitzmann, Daniel A1 - Poppenhäger, Katja A1 - Hoeijmakers, H. Jens A1 - Ilyin, Ilya A1 - Alexoudi, Xanthippi A1 - Carroll, Thorsten A. A1 - Alvarado-Gomez, Julian A1 - Ketzer, Laura A1 - Bonomo, Aldo S. A1 - Borsa, Francesco A1 - Gaudi, B. Scott A1 - Henning, Thomas A1 - Malavolta, Luca A1 - Molaverdikhani, Karan A1 - Nascimbeni, Valerio A1 - Patience, Jennifer A1 - Pino, Lorenzo A1 - Scandariato, Gaetano A1 - Schlawin, Everett A1 - Shkolnik, Evgenya A1 - Sicilia, Daniela A1 - Sozzetti, Alessandro A1 - Foster, Mary G. A1 - Veillet, Christian A1 - Wang, Ji A1 - Yan, Fei A1 - Strassmeier, Klaus G. T1 - The PEPSI exoplanet transit survey (PETS) I: Investigating the presence of a silicate atmosphere on the super-earth 55 Cnc e JF - Monthly notices of the Royal Astronomical Society N2 - The study of exoplanets and especially their atmospheres can reveal key insights on their evolution by identifying specific atmospheric species. For such atmospheric investigations, high-resolution transmission spectroscopy has shown great success, especially for Jupiter-type planets. Towards the atmospheric characterization of smaller planets, the super-Earth exoplanet 55 Cnc e is one of the most promising terrestrial exoplanets studied to date. Here, we present a high-resolution spectroscopic transit observation of this planet, acquired with the PEPSI instrument at the Large Binocular Telescope. Assuming the presence of Earth-like crust species on the surface of 55 Cnc e, from which a possible silicate-vapor atmosphere could have originated, we search in its transmission spectrum for absorption of various atomic and ionized species such as Fe , Fe (+), Ca , Ca (+), Mg, and K , among others. Not finding absorption for any of the investigated species, we are able to set absorption limits with a median value of 1.9 x R-P. In conclusion, we do not find evidence of a widely extended silicate envelope on this super-Earth reaching several planetary radii. KW - planets and satellites: atmospheres KW - planets and satellites: composition Y1 - 2022 U6 - https://doi.org/10.1093/mnras/stac810 SN - 0035-8711 SN - 1365-2966 VL - 513 IS - 1 SP - 1544 EP - 1556 PB - Oxford University Press CY - Oxford ER - TY - GEN A1 - Wachs, Sebastian A1 - Wright, Michelle F. A1 - Gámez-Guadix, Manuel T1 - Call for special issue papers: predictors, consequences, and prevention of hate speech and fake news involvement across the lifespan T2 - Cyberpsychology, behavior and social networking Y1 - 2022 U6 - https://doi.org/10.1089/cyber.2022.29243.cfp SN - 2152-2715 SN - 2152-2723 VL - 25 IS - 3 SP - 159 EP - 160 PB - Mary Ann Liebert ER - TY - JOUR A1 - Philipowski, Katharina A1 - Eming, Jutta T1 - Nachhaltig und dauerhaft verändert BT - Akademische Lehre nach der Corona-Pandemie JF - Forschung und Lehre N2 - Im Zuge der Pandemiebekämpfung und der Digitalisierung entstehen an den Universitäten neue Strukturen, die die akademische Lehre nachhaltig verändern werden. Die Autorinnen schlagen Rahmenbedingungen für die Etablierung digitaler Lehre vor. Y1 - 2022 UR - https://www.forschung-und-lehre.de/lehre/wie-corona-die-akademische-lehre-dauerhaft-veraendert-4678 UR - https://www.wissenschaftsmanagement-online.de/system/files/downloads-wimoarticle/f%26l5-22_Akademische_Lehre_nach_Corona_Eming_Philipowski.pdf SN - 0945-5604 VL - 29 IS - 5 SP - 364 EP - 365 PB - Deutscher Hochschulverband; ESV CY - Bonn ER - TY - JOUR A1 - Schaerer, Daniel A1 - Izotov, Yuri I. A1 - Worseck, Gábor A1 - Berg, Danielle A1 - Chisholm, John A1 - Jaskot, Anne A1 - Nakajima, Kimihiko A1 - Ravindranath, Swara A1 - Thuan, Trinh X. A1 - Verhamme, Anne T1 - Strong Lyman continuum emitting galaxies show intense C IV λ 1550 emission JF - Astronomy and astrophysics N2 - Using the Space Telescope Imaging Spectrograph, we have obtained ultraviolet spectra from similar to 1200 to 2000 angstrom of known Lyman continuum (LyC) emitting galaxies at low redshift (z similar to 0.3-0.4) with varying absolute LyC escape fractions ( f(esc) similar to 0.01-0.72). Our observations include in particular the galaxy J1243+4646, which has the highest known LyC escape fraction at low redshift. While all galaxies are known Lyman alpha emitters, we consistently detect an inventory of additional emission lines, including C IV lambda 1550, He II lambda 1640, O III] lambda 1666, and C III] lambda 1909, whose origin is presumably essentially nebular. C IV lambda 1550 emission is detected above 4 sigma in six out of eight galaxies, with equivalent widths of EW(C IV) = 12-15 angstrom for two galaxies, which exceeds the previously reported maximum emission in low-z star-forming galaxies. We detect C IV lambda 1550 emission in all LyC emitters with escape fractions f(esc) > 0.1 and find a tentative increase in the flux ratio C IV lambda 1550 /C III] lambda 1909 with f(esc). Based on the data, we propose a new criterion to select and classify strong leakers (galaxies with f(esc) > 0.1): C IV lambda 1550 /C III] lambda 1909 greater than or similar to 0.75. Finally, we also find He II lambda 1640 emission in all the strong leakers with equivalent widths from 3 to 8 angstrom rest frame. These are among the highest values observed in star-forming galaxies and are primarily due to a high rate of ionizing photon production. The nebular He II lambda 1640 emission of the strong LyC emitters does not require harder ionizing spectra at >54 eV compared to those of typical star-forming galaxies at similarly low metallicity. KW - galaxies: starburst KW - galaxies: high-redshift KW - dark ages, reionization KW - first stars KW - ultraviolet: galaxies Y1 - 2022 U6 - https://doi.org/10.1051/0004-6361/202243149 SN - 0004-6361 SN - 1432-0746 VL - 658 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Izotov, Yuri I. A1 - Chisholm, John A1 - Worseck, Gábor A1 - Guseva, Natalia G. A1 - Schaerer, Daniel A1 - Prochaska, Jason Xavier T1 - Lyman alpha and Lyman continuum emission of Mg II-selected star-forming galaxies JF - Monthly notices of the Royal Astronomical Society N2 - We present observations with the Cosmic Origins Spectrograph onboard the Hubble Space Telescope of seven compact low-mass star-forming galaxies at redshifts, z, in the range 0.3161-0.4276, with various O3Mg2 = [O III] lambda 5007/Mg II lambda 2796+2803 and Mg-2 = Mg II lambda 2796/Mg II lambda 2803 emission-line ratios. We aim to study the dependence of leaking Lyman continuum (LyC) emission on the characteristics of Mg ii emission together with the dependencies on other indirect indicators of escaping ionizing radiation. LyC emission with escape fractions f(esc)(LyC) = 3.1-4.6 per cent is detected in four galaxies, whereas only 1 sigma upper limits of f(esc)(LyC) in the remaining three galaxies were derived. A strong narrow Ly alpha emission line with two peaks separated by V-sep similar to 298-592 km s(-1) was observed in four galaxies with detected LyC emission and very weak Ly alpha emission is observed in galaxies with LyC non-detections. Our new data confirm the tight anticorrelation between f(esc)(LyC) and V-sep found for previous low-redshift galaxy samples. V-sep remains the best indirect indicator of LyC leakage among all considered indicators. It is found that escaping LyC emission is detected predominantly in galaxies with Mg-2 greater than or similar to 1.3. A tendency of an increase of f(esc)(LyC) with increasing of both the O3Mg2 and Mg-2 is possibly present. However, there is substantial scatter in these relations not allowing their use for reliable prediction of f(esc)(LyC). KW - galaxies: abundances KW - galaxies: dwarf KW - galaxies: fundamental parameters KW - galaxies: ISM KW - galaxies: starburst KW - dark ages KW - reionization KW - first stars Y1 - 2022 U6 - https://doi.org/10.1093/mnras/stac1899 SN - 0035-8711 SN - 1365-2966 VL - 515 IS - 2 SP - 2864 EP - 2881 PB - Oxford University Press CY - Oxford ER - TY - JOUR A1 - Bobone, Sara A1 - Hilsch, Malte A1 - Storm, Julian A1 - Dunsing, Valentin A1 - Herrmann, Andreas A1 - Chiantia, Salvatore T1 - Phosphatidylserine Lateral Organization Influences the Interaction of Influenza Virus Matrix Protein 1 with Lipid Membranes JF - Journal of virology N2 - Influenza A virus matrix protein 1 (M1) is an essential component involved in the structural stability of the virus and in the budding of new virions from infected cells. A deeper understanding of the molecular basis of virion formation and the budding process is required in order to devise new therapeutic approaches. We performed a detailed investigation of the interaction between M1 and phosphatidylserine (PS) (i.e., its main binding target at the plasma membrane [PM]), as well as the distribution of PS itself, both in model membranes and in living cells. To this end, we used a combination of techniques, including Forster resonance energy transfer (FRET), confocal microscopy imaging, raster image correlation spectroscopy, and number and brightness (N&B) analysis. Our results show that PS can cluster in segregated regions in the plane of the lipid bilayer, both in model bilayers constituted of PS and phosphatidylcholine and in living cells. The viral protein M1 interacts specifically with PS-enriched domains, and such interaction in turn affects its oligomerization process. Furthermore, M1 can stabilize PS domains, as observed in model membranes. For living cells, the presence of PS clusters is suggested by N&B experiments monitoring the clustering of the PS sensor lactadherin. Also, colocalization between M1 and a fluorescent PS probe suggest that, in infected cells, the matrix protein can specifically bind to the regions of PM in which PS is clustered. Taken together, our observations provide novel evidence regarding the role of PS-rich domains in tuning M1-lipid and M1-M1 interactions at the PM of infected cells. IMPORTANCE Influenza virus particles assemble at the plasma membranes (PM) of infected cells. This process is orchestrated by the matrix protein M1, which interacts with membrane lipids while binding to the other proteins and genetic material of the virus. Despite its importance, the initial step in virus assembly (i.e., M1-lipid interaction) is still not well understood. In this work, we show that phosphatidylserine can form lipid domains in physical models of the inner leaflet of the PM. Furthermore, the spatial organization of PS in the plane of the bilayer modulates M1-M1 interactions. Finally, we show that PS domains appear to be present in the PM of living cells and that M1 seems to display a high affinity for them. KW - influenza KW - assembly KW - confocal microscopy KW - fluorescence image analysis KW - lipid rafts KW - matrix protein KW - model membranes KW - phosphatidylserine KW - plasma membrane Y1 - 2017 U6 - https://doi.org/10.1128/JVI.00267-17 SN - 0022-538X SN - 1098-5514 VL - 91 PB - American Society for Microbiology CY - Washington ER - TY - JOUR A1 - Günther, Kerstin A1 - Schmidt, Marcus A1 - Quitt, Heinz A1 - Heinken, Thilo T1 - Veränderungen der Waldvegetation im Elbe-Havelwinkel von 1960 bis 2015 JF - Tuexenia : Mitteilungen der Floristisch-Soziologischen Arbeitsgemeinschaft N2 - Forest ecosystems are subject to a variety of influences such as forest management, nitrogen deposition, changes in the groundwater level or the immigration of invasive species. The repetition of historical releves is an important means of documenting the resulting changes in plant communities and determining their main drivers. In 2015, we examined the vegetation change in 140 semi-permanent plots in managed forests in the Elbe valley in the NE German lowlands (Saxony-Anhalt, Brandenburg). The first survey took place from 1956 to 1963. The releves cover an almost uniquely broad spectrum of different site conditions, ranging from wet forests (alluvial, swamp and bog forests of Alnion incanae, Alnion glutinosae and Betulion pubescentis) to acidic mixed oak forests (Quercion roboris) up to acidic, mostly dry pine forests with different nutrient status (Dicrano-Pinion). We analyzed the changes in the vegetation with the help of forest stand data, winner and loser species, alpha- and beta-diversity as well as the Ellenberg indicator values for nitrogen, reaction, moisture and light. In contrast to previous resurvey studies, areas were also taken into account on which a complete change of forest stand had taken place before the second survey. Particularly in the wet forests and acidic forests with a moderately good nutrient supply, changes in the main tree species have been recorded, and many pine stands have been newly established in the meantime. The species richness has decreased overall and in almost all forest types, but the beta-diversity has remained unchanged or has increased. The Ellenberg values indicate a decrease in soil moisture in the wet forests, while the acidic pine forests in particular have become darker, richer in nutrients and more humid. The number of loser species is more than twice as high as that of the winner species, but with different developments in the individual forest types. In particular, the wet forests, the acidic mixed oak forests and the lichen-pine forests have lost most of their characteristic species. The resurvey after more than 50 years shows a different development of the individual forest types. Vegetation changes in the wet forests are mainly due to local groundwater level drawdown and the resulting increased availability of nutrients. The alluvial forests were also strongly influenced by forest interventions. The reasons for the trend towards more humid and more nutrient-rich conditions in formerly dry acidic pine and oak forests are nitrogen depositions and a succession after the abandonment of historical forms of forest use (litter raking, forest pasture). Although the individual forest types have developed differently, eutrophication, falling groundwater levels and silviculture are the most important causes for the changes in vegetation. Silvicultural interventions such as clear cutting and stand conversion with a change of tree species are at the same time the main reason why the vegetation has not been homogenized despite the leveling of the site gradient as measured by the beta-diversity. N2 - Waldökosysteme unterliegen vielfältigen Einflüssen wie forstlicher Bewirtschaftung, Stickstoffdeposition, Veränderung des Grundwasserspiegels oder der Einwanderung invasiver Arten. Die Wiederholung historischer Vegetationsaufnahmen ist ein wichtiges Mittel, um Veränderungen der Pflanzengesellschaften zu dokumentieren und mögliche Hauptursachen (Treiber) zu bestimmen. Wir haben 2015 den Vegetationswandel auf 140 semi-permanenten Plots in Wirtschaftswäldern der Elbtalniederung im Nordostdeutschen Tiefland (Sachsen-Anhalt, Brandenburg) untersucht. Die Erstaufnahme erfolgte von 1956 bis 1963. Die Vegetationsaufnahmen decken ein fast einzigartig breites Spektrum unterschiedlicher Waldstandorte ab, das von Feuchtwäldern (Au-, Bruch- und Moorwäldern des Alnion incanae, Alnion glutinosae und Betulion pubescentis) über bodensaure Eichen-Mischwälder (Quercion roboris) bis hin zu bodensauren, meist trockenen Kiefernwäldern mit unterschiedlicher Nährstoffausstattung (Dicrano-Pinion) reicht. Die Veränderungen der Vegetation haben wir mit Hilfe von Bestandesdaten, Gewinner- und Verliererarten, der α- und β -Diversität sowie der Ellenberg-Zeigerwerte für Stickstoff, Reaktion, Feuchte und Licht analysiert. Dabei wurden, anders als in den meisten bisherigen Wiederholungsuntersuchungen, auch Flächen berücksichtigt, auf denen bis zur Zweitaufnahme ein vollständiger Bestandeswechsel stattgefunden hatte. Insbesondere in den Feuchtwäldern und den bodensauren Wäldern mit mäßig guter Nährstoffversorgung sind Wechsel der Hauptbaumarten zu verzeichnen; außerdem wurden viele Kiefernbestände zwischenzeitlich neu begründet. Die Artenzahl hat insgesamt und in fast allen Waldtypen abgenommen, die β-Diversität ist jedoch unverändert geblieben bzw. hat sich erhöht. Die Zeigerwerte deuten auf eine Abnahme der Bodenfeuchte in den Au-, Bruch-, und Moorwäldern hin, während insbesondere die bodensauren Kiefernwälder dunkler, nährstoffreicher und feuchter geworden sind. Die Anzahl der Verlierer-Arten ist mehr als doppelt so hoch wie die der Gewinner-Arten, jedoch mit unterschiedlicher Entwicklung in den einzelnen Waldtypen. Insbesondere die nassen und feuchten Wälder, die bodensauren Eichen-Mischwälder und die Flechten-Kiefernwälder haben die meisten ihrer charakteristischen Arten verloren. Veränderungen der Vegetation in den Feuchtwäldern gehen v. a. auf lokal gesunkene Grundwasserspiegel und eine dadurch gestiegene Nährstoffverfügbarkeit zurück; die Artenzusammensetzung der Auwälder wurde zudem sehr stark durch forstliche Eingriffe beeinflusst. Ursachen für den Trend zu feuchteren und nährstoffreicheren Bedingungen in ehemals trockenen bodensauren Kiefern- und Eichenwäldern sind Stickstoffeinträge sowie eine Sukzession nach Aufgabe historischer Waldnutzungs-formen (Streunutzung, Waldweide). Obwohl sich die einzelnen Waldtypen unterschiedlich entwickelt haben, sind Eutrophierung, sinkende Grundwasserspiegel und Waldbaumaßnahmen insgesamt die wichtigsten Ursachen für die beobachteten Vegetationsveränderungen. Forstliche Eingriffe wie Kahlschlag und Bestandesumbau mit Baumartenwechsel sind zugleich die Hauptursache dafür, dass es trotz Nivellierung des Standortsgradienten, gemessen an der β-Diversität, nicht zu einer Homogenisierung der Vegetation gekommen ist. T2 - Vegetation change in the forests between the Elbe and Havel rivers (NE Germany) from 1960 to 2015 KW - environmental gradient KW - eutrophication KW - falling groundwater level KW - homogenisation KW - phytodiversity KW - silviculture KW - vegetation change Y1 - 2021 U6 - https://doi.org/10.14471/2021.41.005 SN - 0722-494X SN - 2748-3452 IS - 41 SP - 53 EP - 85 PB - Floristisch-Soziologische Arbeitsgemeinschaft CY - Göttingen ER - TY - JOUR A1 - Gerlach, Moritz Reinhardt A1 - Glück, Jochen T1 - On a convergence theorem for semigroups of positive integral operators JF - Comptes Rendus Mathematique N2 - We give a new and very short proof of a theorem of Greiner asserting that a positive and contractive -semigroup on an -space is strongly convergent in case it has a strictly positive fixed point and contains an integral operator. Our proof is a streamlined version of a much more general approach to the asymptotic theory of positive semigroups developed recently by the authors. Under the assumptions of Greiner's theorem, this approach becomes particularly elegant and simple. We also give an outlook on several generalisations of this result. Y1 - 2017 U6 - https://doi.org/10.1016/j.crma.2017.07.017 SN - 1631-073X SN - 1778-3569 VL - 355 SP - 973 EP - 976 PB - Elsevier CY - Paris ER - TY - JOUR A1 - Culpan, Richard A1 - Geier, Stephan A1 - Reindl, Nicole A1 - Pelisoli, Ingrid A1 - Gentile Fusillo, Nicola Pietro A1 - Vorontseva, Alina T1 - The population of hot subdwarf stars studied with Gaia BT - IV. catalogues of hot subluminous stars based on Gaia EDR3 JF - Astronomy and astrophysics : an international weekly journal N2 - In light of substantial new discoveries of hot subdwarfs by ongoing spectroscopic surveys and the availability of the Gaia mission Early Data Release 3 (EDR3), we compiled new releases of two catalogues of hot subluminous stars: the data release 3 (DR3) catalogue of the known hot subdwarf stars contains 6616 unique sources and provides multi-band photometry, and astrometry from Gaia EDR3 as well as classifications based on spectroscopy and colours. This is an increase of 742 objects over the DR2 catalogue. This new catalogue provides atmospheric parameters for 3087 stars and radial velocities for 2791 stars from the literature. In addition, we have updated the Gaia Data Release 2 (DR2) catalogue of hot subluminous stars using the improved accuracy of the Gaia EDR3 data set together with updated quality and selection criteria to produce the Gaia EDR3 catalogue of 61 585 hot subluminous stars, representing an increase of 21 785 objects. The improvements in Gaia EDR3 astrometry and photometry compared to Gaia DR2 have enabled us to define more sophisticated selection functions. In particular, we improved hot subluminous star detection in the crowded regions of the Galactic plane as well as in the direction of the Magellanic Clouds by including sources with close apparent neighbours but with flux levels that dominate the neighbourhood. KW - subdwarfs KW - Hertzsprung-Russell and C-M diagrams KW - binaries: general KW - stars: horizontal-branch KW - catalogs Y1 - 2022 U6 - https://doi.org/10.1051/0004-6361/202243337 SN - 1432-0746 VL - 662 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Schaffenroth, Veronika A1 - Casewell, Sarah L. A1 - Schneider, D. A1 - Kilkenny, David A1 - Geier, Stephan A1 - Heber, Ulrich A1 - Irrgang, Andreas A1 - Przybilla, Norbert A1 - Marsh, Thomas R. A1 - Littlefair, Stuart P. A1 - Dhillon, Vik S. T1 - A quantitative in-depth analysis of the prototype sdB plus BD system SDSS J08205+0008 revisited in the Gaia era JF - Monthly notices of the Royal Astronomical Society N2 - Subdwarf B stars are core-helium-burning stars located on the extreme horizontal branch (EHB). Extensive mass loss on the red giant branch is necessary to form them. It has been proposed that substellar companions could lead to the required mass loss when they are engulfed in the envelope of the red giant star. J08205+0008 was the first example of a hot subdwarf star with a close, substellar companion candidate to be found. Here, we perform an in-depth re-analysis of this important system with much higher quality data allowing additional analysis methods. From the higher resolution spectra obtained with ESO-VLT/XSHOOTER, we derive the chemical abundances of the hot subdwarf as well as its rotational velocity. Using the Gaia parallax and a fit to the spectral energy distribution in the secondary eclipse, tight constraints to the radius of the hot subdwarf are derived. From a long-term photometric campaign, we detected a significant period decrease of -3.2(8) x 10(-12) dd(-1). This can be explained by the non-synchronized hot subdwarf star being spun up by tidal interactions forcing it to become synchronized. From the rate of period decrease we could derive the synchronization time-scale to be 4 Myr, much smaller than the lifetime on EHB. By combining all different methods, we could constrain the hot subdwarf to a mass of 0.39-0.50 M-circle dot and a radius of R-sdB = 0.194 +/- 0.008 R-circle dot, and the companion to 0.061-0.071 M-circle dot with a radius of R-comp = 0.092 +/- 0.005 R-circle dot, below the hydrogen-burning limit. We therefore confirm that the companion is most likely a massive brown dwarf. KW - stars: abundances KW - stars: atmospheres KW - stars: fundamental parameters KW - stars: horizontal branch KW - stars: low-mass KW - subdwarfs Y1 - 2020 U6 - https://doi.org/10.1093/mnras/staa3661 SN - 0035-8711 SN - 1365-2966 VL - 501 IS - 3 SP - 3847 EP - 3870 PB - Oxford Univ. Press CY - Oxford ER - TY - JOUR A1 - Werner, Klaus A1 - Reindl, Nicole A1 - Dorsch, Matti A1 - Geier, Stephan A1 - Munari, Ulisse A1 - Raddi, Roberto T1 - Non-local thermodynamic equilibrium spectral analysis of five hot, hydrogen-deficient pre-white dwarfs JF - Astronomy and Astrophysics N2 - Hot, compact, hydrogen-deficient pre-white dwarfs (pre-WDs) with effective temperatures of Teff > 70 000 K and a surface gravity of 5.0 < logg < 7.0 are rather rare objects despite recent and ongoing surveys. It is believed that they are the outcome of either single star evolution (late helium-shell flash or late helium-core flash) or binary star evolution (double WD merger). Their study is interesting because the surface elemental abundances reflect the physics of thermonuclear flashes and merger events. Spectroscopically they are divided in three different classes, namely PG1159, O(He), or He-sdO. We present a spectroscopic analysis of five such stars that turned out to have atmospheric parameters in the range Teff = 70 000-80 000 K and logg = 5.2-6.3. The three investigated He-sdOs have a relatively high hydrogen mass fraction (10%) that is unexplained by both single (He core flash) and binary evolution (He-WD merger) scenarios. The O(He) star JL 9 is probably a binary helium-WD merger, but its hydrogen content (6%) is also at odds with merger models. We found that RL 104 is the 'coolest' (Teff = 80 000 K) member of the PG1159 class in a pre-WD stage. Its optical spectrum is remarkable because it exhibits C※ IV lines involving Rydberg states with principal quantum numbers up to n = 22. Its rather low mass (0.48-0.02+0.03 M·) is difficult to reconcile with the common evolutionary scenario for PG1159 stars due to it being the outcome of a (very) late He-shell flash. The same mass-problem faces a merger model of a close He-sdO plus CO WD binary that predicts PG1159-like abundances. Perhaps RL 104 originates from a very late He-shell flash in a CO/He WD formed by a merger of two low-mass He-WDs. KW - stars: atmospheres KW - stars: abundances KW - stars: evolution KW - subdwarfs KW - white dwarfs Y1 - 2022 U6 - https://doi.org/10.1051/0004-6361/202142397 SN - 0004-6361 SN - 1432-0746 VL - 658 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Geier, Stephan T1 - The population of hot subdwarf stars studied with Gaia BT - III. catalogue of known hot subdwarf stars : data release JF - Astronomy and astrophysics : an international weekly journal N2 - In light of substantial new discoveries of hot subdwarfs by ongoing spectroscopic surveys and the availability of new all-sky data from ground-based photometric surveys and the Gaia mission Data Release 2, we compiled an updated catalogue of the known hot subdwarf stars. The catalogue contains 5874 unique sources including 528 previously unknown hot subdwarfs and provides multi-band photometry, astrometry from Gaia, and classifications based on spectroscopy and colours. This new catalogue provides atmospheric parameters of 2187 stars and radial velocities of 2790 stars from the literature. Using colour, absolute magnitude, and reduced proper motion criteria, we identified 268 previously misclassified objects, most of which are less luminous white dwarfs or more luminous blue horizontal branch and main-sequence stars. KW - subdwarfs KW - stars: horizontal-branch KW - catalogs Y1 - 2020 U6 - https://doi.org/10.1051/0004-6361/202037526 SN - 0004-6361 SN - 1432-0746 VL - 635 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Irrgang, Andreas A1 - Geier, Stephan A1 - Kreuzer, Simon A1 - Pelisoli, Ingrid Domingos A1 - Heber, Ulrich T1 - A stripped helium star in the potential black hole binary LB-1 JF - Astronomy and astrophysics : an international weekly journal N2 - Context The recently claimed discovery of a massive (M-BH = 68(-13)(+11) M-circle dot) black hole in the Galactic solar neighborhood has led to controversial discussions because it severely challenges our current view of stellar evolution. Aims A crucial aspect for the determination of the mass of the unseen black hole is the precise nature of its visible companion, the B-type star LSV +22 25. Because stars of different mass can exhibit B-type spectra during the course of their evolution, it is essential to obtain a comprehensive picture of the star to unravel its nature and, thus, its mass. Methods To this end, we study the spectral energy distribution of LSV +22 25 and perform a quantitative spectroscopic analysis that includes the determination of chemical abundances for He, C, N, O, Ne, Mg, Al, Si, S, Ar, and Fe. Results Our analysis clearly shows that LSV +22 25 is not an ordinary main sequence B-type star. The derived abundance pattern exhibits heavy imprints of the CNO bi-cycle of hydrogen burning, that is, He and N are strongly enriched at the expense of C and O. Moreover, the elements Mg, Al, Si, S, Ar, and Fe are systematically underabundant when compared to normal main-sequence B-type stars. We suggest that LSV +22 25 is a stripped helium star and discuss two possible formation scenarios. Combining our photometric and spectroscopic results with the Gaia parallax, we infer a stellar mass of 1.1 +/- 0.5 M-circle dot. Based on the binary system's mass function, this yields a minimum mass of 2-3 M-circle dot for the compact companion, which implies that it may not necessarily be a black hole but a massive neutron- or main sequence star. Conclusions The star LSV +22 25 has become famous for possibly having a very massive black hole companion. However, a closer look reveals that the star itself is a very intriguing object. Further investigations are necessary for complete characterization of this object. KW - stars: abundances KW - stars: chemically peculiar KW - stars: early-type KW - pulsars: individual: LS V+22 25 Y1 - 2020 U6 - https://doi.org/10.1051/0004-6361/201937343 SN - 0004-6361 SN - 1432-0746 VL - 633 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Raddi, Roberto A1 - Hollands, M. A. A1 - Koester, D. A1 - Hermes, J. J. A1 - Gansicke, B. T. A1 - Heber, Ulrich A1 - Shen, Ken J. A1 - Townsley, D. M. A1 - Pala, Anna Francesca A1 - Reding, J. S. A1 - Toloza, O. F. A1 - Pelisoli, Ingrid Domingos A1 - Geier, Stephan A1 - Fusillo, Nicola Pietro Gentile A1 - Munari, Ullisse A1 - Strader, J. T1 - Partly burnt runaway stellar remnants from peculiar thermonuclear supernovae JF - Monthly notices of the Royal Astronomical Society N2 - We report the discovery of three stars that, along with the prototype LP 40-365, form a distinct class of chemically peculiar runaway stars that are the survivors of thermonuclear explosions. Spectroscopy of the four confirmed LP 40-365 stars finds ONe-dominated atmospheres enriched with remarkably similar amounts of nuclear ashes of partial O- and Si-burning. Kinematic evidence is consistent with ejection from a binary supernova progenitor; at least two stars have rest-frame velocities indicating they are unbound to the Galaxy. With masses and radii ranging between 0.20 and 0.28M(circle dot) and between 0.16 and 0.60 R-circle dot, respectively, we speculate these inflated white dwarfs are the partly burnt remnants of either peculiar Type Iax or electron-capture supernovae. Adopting supernova rates from the literature, we estimate that similar to 20 LP 40-365 stars brighter than 19 mag should be detectable within 2 kpc from the Sun at the end of the Gaia mission. We suggest that as they cool, these stars will evolve in their spectroscopic appearance, and eventually become peculiar O-rich white dwarfs. Finally, we stress that the discovery of new LP 40-365 stars will be useful to further constrain their evolution, supplying key boundary conditions to the modelling of explosion mechanisms, supernova rates, and nucleosynthetic yields of peculiar thermonuclear explosions. KW - stars: individual: LP 40-365 KW - subdwarfs KW - supernovae: general KW - white dwarfs KW - Galaxy: kinematics and dynamics Y1 - 2019 U6 - https://doi.org/10.1093/mnras/stz1618 SN - 0035-8711 SN - 1365-2966 VL - 489 IS - 2 SP - 1489 EP - 1508 PB - Oxford Univ. Press CY - Oxford ER - TY - JOUR A1 - Irrgang, Andreas A1 - Geier, Stephan A1 - Heber, Ulrich A1 - Kupfer, Thomas A1 - Fürst, F. T1 - PG 1610+062: a runaway B star challenging classical ejection mechanisms JF - Astronomy and astrophysics : an international weekly journal N2 - Hypervelocity stars are rare objects, mostly main-sequence (MS) B stars, traveling so fast that they will eventually escape from the Milky Way. Recently, it has been shown that the popular Hills mechanism, in which a binary system is disrupted via a close encounter with the supermassive black hole at the Galactic center, may not be their only ejection mechanism. The analyses of Gaia data ruled out a Galactic center origin for some of them, and instead indicated that they are extreme disk runaway stars ejected at velocities exceeding the predicted limits of classical scenarios (dynamical ejection from star clusters or binary supernova ejection). We present the discovery of a new extreme disk runaway star, PG 1610+062, which is a slowly pulsating B star bright enough to be studied in detail. A quantitative analysis of spectra taken with ESI at the Keck Observatory revealed that PG 1610+062 is a late B-type MS star of 4–5 M⊙ with low projected rotational velocity. Abundances (C, N, O, Ne, Mg, Al, Si, S, Ar, and Fe) were derived differentially with respect to the normal B star HD 137366 and indicate that PG 1610+062 is somewhat metal rich. A kinematic analysis, based on our spectrophotometric distance (17.3 kpc) and on proper motions from Gaia’s second data release, shows that PG 1610+062 was probably ejected from the Carina-Sagittarius spiral arm at a velocity of 550 ± 40 km s−1, which is beyond the classical limits. Accordingly, the star is in the top five of the most extreme MS disk runaway stars and is only the second among the five for which the chemical composition is known. KW - stars: abundances KW - stars: individual: HD 137366 KW - stars: kinematics and dynamics KW - stars: individual: PG 1610+062 KW - stars: early-type Y1 - 2019 U6 - https://doi.org/10.1051/0004-6361/201935429 SN - 1432-0746 VL - 628 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Schaffenroth, Veronika A1 - Barlow, Brad N. A1 - Geier, Stephan A1 - Vuckovic, Maja A1 - Kilkenny, D. A1 - Wolz, M. A1 - Kupfer, Thomas A1 - Heber, Ulrich A1 - Drechsel, H. A1 - Kimeswenger, S. A1 - Marsh, T. A1 - Wolf, M. A1 - Pelisoli, Ingrid Domingos A1 - Freudenthal, Joseph A1 - Dreizler, S. A1 - Kreuzer, S. A1 - Ziegerer, E. T1 - The EREBOS project: Investigating the effect of substellar and low-mass stellar companions on late stellar evolution Survey, target selection, and atmospheric parameters JF - Astronomy and astrophysics : an international weekly journal N2 - Eclipsing post-common-envelope binaries are highly important for resolving the poorly understood, very short-lived common-envelope phase of stellar evolution. Most hot subdwarfs (sdO/Bs) are the bare helium-burning cores of red giants that have lost almost all of their hydrogen envelope. This mass loss is often triggered by common-envelope interactions with close stellar or even substellar companions. Cool companions to hot subdwarf stars such as late-type stars and brown dwarfs are detectable from characteristic light-curve variations - reflection effects and often eclipses. In the recently published catalog of eclipsing binaries in the Galactic Bulge and in the Asteroid Terrestrial-impact Last Alert System (ATLAS) survey, we discovered 125 new eclipsing systems showing a reflection effect seen by visual inspection of the light curves and using a machine-learning algorithm, in addition to the 36 systems previously discovered by the Optical Gravitational Lesing Experiment (OGLE) team. The Eclipsing Reflection Effect Binaries from Optical Surveys (EREBOS) project aims at analyzing all newly discovered eclipsing binaries of the HW Vir type (hot subdwarf + close, cool companion) based on a spectroscopic and photometric follow up to derive the mass distribution of the companions, constrain the fraction of substellar companions, and determine the minimum mass needed to strip off the red-giant envelope. To constrain the nature of the primary we derived the absolute magnitude and the reduced proper motion of all our targets with the help of the parallaxes and proper motions measured by the Gaia mission and compared those to the Gaia white-dwarf candidate catalog. It was possible to derive the nature of a subset of our targets, for which observed spectra are available, by measuring the atmospheric parameter of the primary, confirming that less than 10% of our systems are not sdO/Bs with cool companions but are white dwarfs or central stars of planetary nebula. This large sample of eclipsing hot subdwarfs with cool companions allowed us to derive a significant period distribution for hot subdwarfs with cool companions for the first time showing that the period distribution is much broader than previously thought and is ideally suited to finding the lowest-mass companions to hot subdwarf stars. The comparison with related binary populations shows that the period distribution of HW Vir systems is very similar to WD+dM systems and central stars of planetary nebula with cool companions. In the future, several new photometric surveys will be carried out, which will further increase the sample of this project, providing the potential to test many aspects of common-envelope theory and binary evolution. KW - binaries: eclipsing KW - brown dwarfs KW - binaries: spectroscopic KW - binaries: close KW - subdwarfs KW - surveys Y1 - 2019 U6 - https://doi.org/10.1051/0004-6361/201936019 SN - 1432-0746 VL - 630 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Latour, Marilyn A1 - Randall, Suzanna K. A1 - Calamida, Annalisa A1 - Geier, Stephan A1 - Moehler, Sabine T1 - The ultimate spectroscopic census of extreme horizontal branch stars in omega Centauri JF - Astronomy and astrophysics : an international weekly journal N2 - The presence of extreme horizontal branch (EHB) and blue hook stars in some Galactic globular clusters (GGCs) constitutes one of the remaining mysteries of stellar evolution. While several evolutionary scenarios have been proposed to explain the characteristics of this peculiar population of evolved stars, their observational verification has been limited by the availability of spectroscopic data for a statistically significant sample of such objects in any single GGC. We recently launched the SHOTGLAS project with the aim of providing a comprehensive picture of this intriguing stellar population in terms of spectroscopic properties for all readily accessible GGCs hosting an EHB. In this first paper, we focus on omega Cen, a peculiar, massive GGC that hosts multiple stellar populations. We use non-LTE model atmospheres to derive atmospheric parameters (Te ff, log g and N(He) / N(H)) and spectroscopic masses for 152 EHB stars in the cluster. This constitutes the largest spectroscopic sample of EHB stars ever analyzed in a GGC and represents similar to 20% of the EHB population of omega Cen. We also search for close binaries among these stars based on radial velocity variations. Our results show that the EHB population of omega Cen is divided into three spectroscopic groups that are very distinct in the Te ff helium abundance plane. The coolest sdB-type stars (Te ff. 30 000 K) have a hydrogen-rich atmosphere, populate the theoretical EHB region in the Te ff log g plane, and form 26% of our sample. The hottest sdO-type stars (Te ff & 42 000 K) make up 10% of the sample, have a hydrogen-rich atmosphere and are thought to be in a post-EHB evolutionary phase. The majority of our sample is found at intermediate temperatures and consists of sdOB stars that have roughly solar or super-solar atmospheric helium abundances. It is these objects that constitute the blue hook at V > 18 : 5 mag in the omega Cen color-magnitude diagram. Interestingly, the helium-enriched sdOBs do not have a significant counterpart population in the Galactic field, indicating that their formation is dependent on the particular environment found in omega Cen and other select GGCs. Another major di ff erence between the EHB stars in omega Cen and the field is the fraction of close binaries. From our radial velocity survey we identify two binary candidates, however no orbital solutions could be determined. We estimate an EHB close binary fraction of similar to 5% in omega Cen. This low fraction is in line with findings for other GGCs, but in sharp contrast to the situation in the field, where around 50% of the sdB stars reside in close binaries. Finally, the mass distribution derived is very similar for all three spectroscopic groups, however the average mass (0.38 M fi) is lower than that expected from stellar evolution theory. While this mass conundrum has previously been noted for EHB stars in omega Cen, it so far appears to be unique to that cluster. KW - stars: atmospheres KW - stars: horizontal-branch KW - subdwarfs KW - stars: fundamental parameters KW - binaries: close KW - globular clusters: individual: NGC5139 Y1 - 2018 U6 - https://doi.org/10.1051/0004-6361/201833129 SN - 1432-0746 VL - 618 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Geier, Stephan A1 - Raddi, Roberto A1 - Fusillo, Nicola Pietro Gentile A1 - Marsh, T. R. T1 - The population of hot subdwarf stars studied with Gaia BT - II. The Gaia DR2 catalogue of hot subluminous stars JF - Astronomy and astrophysics : an international weekly journal N2 - Based on data from the ESA Gaia Data Release 2 (DR2) and several ground-based, multi-band photometry surveys we have compiled an all-sky catalogue of 39 800 hot subluminous star candidates selected in Gaia DR2 by means of colour, absolute magnitude, and reduced proper motion cuts. We expect the majority of the candidates to be hot subdwarf stars of spectral type B and O, followed by blue horizontal branch stars of late B-type (HBB), hot post-AGB stars, and central stars of planetary nebulae. The contamination by cooler stars should be about 10%. The catalogue is magnitude limited to Gaia G < 19 mag and covers the whole sky. Except within the Galactic plane and LMC/SMC regions, we expect the catalogue to be almost complete up to about 1.5 kpc. The main purpose of this catalogue is to serve as input target list for the large-scale photometric and spectroscopic surveys which are ongoing or scheduled to start in the coming years. In the long run, securing a statistically significant sample of spectroscopically confirmed hot subluminous stars is key to advance towards a more detailed understanding of the latest stages of stellar evolution for single and binary stars. KW - subdwarfs KW - stars: horizontal-branch KW - catalogs Y1 - 2019 U6 - https://doi.org/10.1051/0004-6361/201834236 SN - 0004-6361 SN - 1432-0746 VL - 621 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Reindl, Nicole A1 - Bainbridge, M. A1 - Przybilla, Norbert A1 - Geier, Stephan A1 - Prvak, M. A1 - Krticka, Jiri A1 - Ostensen, R. H. A1 - Telting, J. A1 - Werner, K. T1 - Unravelling the baffling mystery of the ultrahot wind phenomenon in white dwarfs JF - Monthly notices of the Royal Astronomical Society N2 - The presence of ultrahigh excitation (UHE) absorption lines (e.g. OVIII) in the optical spectra of several of the hottest white dwarfs poses a decades-long mystery and is something that has never been observed in any other astrophysical object. The occurrence of such features requires a dense environment with temperatures near 10(6) K, by far exceeding the stellar effective temperature. Here we report the discovery of a new hot wind white dwarf, GALEXJ014636.8+323615. Astonishingly, we found for the first time rapid changes of the equivalent widths of the UHE features, which are correlated to the rotational period of the star (P=0.242035 d). We explain this with the presence of a wind-fed circumstellar magnetosphere in which magnetically confined wind shocks heat up the material to the high temperatures required for the creation of the UHE lines. The photometric and spectroscopic variability of GALEXJ014636.8+323615 can then be understood as consequence of the obliquity of the magnetic axis with respect to the rotation axis of the white dwarf. This is the first time a wind-fed circumstellar magnetosphere around an apparently isolated white dwarf has been discovered and finally offers a plausible explanation of the ultrahot wind phenomenon. KW - stars: AGB and post-AGB KW - stars: evolution KW - stars: magnetic field Y1 - 2018 U6 - https://doi.org/10.1093/mnrasl/sly191 SN - 0035-8711 SN - 1365-2966 VL - 482 IS - 1 SP - L93 EP - L98 PB - Oxford Univ. Press CY - Oxford ER - TY - JOUR A1 - Wittig, Alice A1 - Miranda, Fabio Malcher A1 - Hölzer, Martin A1 - Altenburg, Tom A1 - Bartoszewicz, Jakub Maciej A1 - Beyvers, Sebastian A1 - Dieckmann, Marius Alfred A1 - Genske, Ulrich A1 - Giese, Sven Hans-Joachim A1 - Nowicka, Melania A1 - Richard, Hugues A1 - Schiebenhoefer, Henning A1 - Schmachtenberg, Anna-Juliane A1 - Sieben, Paul A1 - Tang, Ming A1 - Tembrockhaus, Julius A1 - Renard, Bernhard Y. A1 - Fuchs, Stephan T1 - CovRadar BT - continuously tracking and filtering SARS-CoV-2 mutations for genomic surveillance JF - Bioinformatics N2 - The ongoing pandemic caused by SARS-CoV-2 emphasizes the importance of genomic surveillance to understand the evolution of the virus, to monitor the viral population, and plan epidemiological responses. Detailed analysis, easy visualization and intuitive filtering of the latest viral sequences are powerful for this purpose. We present CovRadar, a tool for genomic surveillance of the SARS-CoV-2 Spike protein. CovRadar consists of an analytical pipeline and a web application that enable the analysis and visualization of hundreds of thousand sequences. First, CovRadar extracts the regions of interest using local alignment, then builds a multiple sequence alignment, infers variants and consensus and finally presents the results in an interactive app, making accessing and reporting simple, flexible and fast. Y1 - 2022 U6 - https://doi.org/10.1093/bioinformatics/btac411 SN - 1367-4803 SN - 1367-4811 VL - 38 IS - 17 SP - 4223 EP - 4225 PB - Oxford Univ. Press CY - Oxford ER - TY - JOUR A1 - Abdirashid, Hashim A1 - Lenhard, Michael T1 - Say it with double flowers JF - Journal of experimental botany N2 - Every year, lovers world-wide rely on mutants to show their feelings on Valentine's Day. This is because many of the most popular ornamental flowering plants have been selected to form extra petals at the expense of reproductive organs to enhance their attractiveness and aesthetic value to humans. This so-called 'double flower' (DF) phenotype, first described more than 2000 years ago (Meyerowitz et al., 1989) is present, for example, in many modern roses, carnations, peonies, and camellias. Gattolin et al. (2020) now identify a unifying explanation for the molecular basis of many of these DF cultivars. KW - ABCE model KW - APETALA2 KW - double flowers KW - flower development KW - homoeotic KW - mutants KW - microRNA172 Y1 - 2020 U6 - https://doi.org/10.1093/jxb/eraa109 SN - 0022-0957 SN - 1460-2431 VL - 71 IS - 9 SP - 2469 EP - 2471 PB - Oxford Univ. Press CY - Oxford ER - TY - GEN A1 - Sicard, Adrien A1 - Lenhard, Michael T1 - Capsella T2 - Current biology Y1 - 2018 U6 - https://doi.org/10.1016/j.cub.2018.06.033 SN - 0960-9822 SN - 1879-0445 VL - 28 IS - 17 SP - R920 EP - R921 PB - Cell Press CY - Cambridge ER - TY - JOUR A1 - Schneider, Hans Julius T1 - Buddhist Meditation as a Mystical Practice JF - Philosophia : philosophical quarterly of Israel N2 - On the basis of many years of personal experience the paper describes Buddhist meditation (Zazen, Vipassanā) as a mystical practice. After a short discussion of the role of some central concepts (longing, suffering, and love) in Buddhism, William James’ concept of religious experience is used to explain the goal of meditators as the achievement of a special kind of an experience of this kind. Systematically, its main point is to explain the difference between (on the one hand) a craving for pleasant ‘mental events’ in the sense of short-term moods, and (on the other) the long-term project of achieving a deep change in one’s attitude to life as a whole, a change that allows the acceptance of suffering and death. The last part argues that there is no reason to call the discussed practice irrational in a negative sense. Changes of attitude of the discussed kind cannot be brought about by argument alone. Therefore, a considered use of age-old practices like meditation should be seen as an addition, not as an undermining of reason. KW - Experience KW - Mood KW - Meditation KW - Mysticism KW - William James KW - Rationality Y1 - 2017 U6 - https://doi.org/10.1007/s11406-017-9925-x SN - 0048-3893 SN - 1574-9274 VL - 45 SP - 1621 EP - 1622 PB - Springer CY - Dordrecht ER - TY - JOUR A1 - Chan, Lili A1 - Chaudhary, Kumardeep A1 - Saha, Aparna A1 - Chauhan, Kinsuk A1 - Vaid, Akhil A1 - Zhao, Shan A1 - Paranjpe, Ishan A1 - Somani, Sulaiman A1 - Richter, Felix A1 - Miotto, Riccardo A1 - Lala, Anuradha A1 - Kia, Arash A1 - Timsina, Prem A1 - Li, Li A1 - Freeman, Robert A1 - Chen, Rong A1 - Narula, Jagat A1 - Just, Allan C. A1 - Horowitz, Carol A1 - Fayad, Zahi A1 - Cordon-Cardo, Carlos A1 - Schadt, Eric A1 - Levin, Matthew A. A1 - Reich, David L. A1 - Fuster, Valentin A1 - Murphy, Barbara A1 - He, John C. A1 - Charney, Alexander W. A1 - Böttinger, Erwin A1 - Glicksberg, Benjamin A1 - Coca, Steven G. A1 - Nadkarni, Girish N. T1 - AKI in hospitalized patients with COVID-19 JF - Journal of the American Society of Nephrology : JASN N2 - Background: Early reports indicate that AKI is common among patients with coronavirus disease 2019 (COVID-19) and associatedwith worse outcomes. However, AKI among hospitalized patients with COVID19 in the United States is not well described. Methods: This retrospective, observational study involved a review of data from electronic health records of patients aged >= 18 years with laboratory-confirmed COVID-19 admitted to the Mount Sinai Health System from February 27 to May 30, 2020. We describe the frequency of AKI and dialysis requirement, AKI recovery, and adjusted odds ratios (aORs) with mortality. Results: Of 3993 hospitalized patients with COVID-19, AKI occurred in 1835 (46%) patients; 347 (19%) of the patientswith AKI required dialysis. The proportionswith stages 1, 2, or 3 AKIwere 39%, 19%, and 42%, respectively. A total of 976 (24%) patients were admitted to intensive care, and 745 (76%) experienced AKI. Of the 435 patients with AKI and urine studies, 84% had proteinuria, 81% had hematuria, and 60% had leukocyturia. Independent predictors of severe AKI were CKD, men, and higher serum potassium at admission. In-hospital mortality was 50% among patients with AKI versus 8% among those without AKI (aOR, 9.2; 95% confidence interval, 7.5 to 11.3). Of survivors with AKI who were discharged, 35% had not recovered to baseline kidney function by the time of discharge. An additional 28 of 77 (36%) patients who had not recovered kidney function at discharge did so on posthospital follow-up. Conclusions: AKI is common among patients hospitalized with COVID-19 and is associated with high mortality. Of all patients with AKI, only 30% survived with recovery of kidney function by the time of discharge. KW - acute renal failure KW - clinical nephrology KW - dialysis KW - COVID-19 Y1 - 2021 U6 - https://doi.org/10.1681/ASN.2020050615 SN - 1046-6673 SN - 1533-3450 VL - 32 IS - 1 SP - 151 EP - 160 PB - American Society of Nephrology CY - Washington ER - TY - JOUR A1 - Vaid, Akhil A1 - Chan, Lili A1 - Chaudhary, Kumardeep A1 - Jaladanki, Suraj K. A1 - Paranjpe, Ishan A1 - Russak, Adam J. A1 - Kia, Arash A1 - Timsina, Prem A1 - Levin, Matthew A. A1 - He, John Cijiang A1 - Böttinger, Erwin A1 - Charney, Alexander W. A1 - Fayad, Zahi A. A1 - Coca, Steven G. A1 - Glicksberg, Benjamin S. A1 - Nadkarni, Girish N. T1 - Predictive approaches for acute dialysis requirement and death in COVID-19 JF - Clinical journal of the American Society of Nephrology : CJASN N2 - Background and objectives AKI treated with dialysis initiation is a common complication of coronavirus disease 2019 (COVID-19) among hospitalized patients. However, dialysis supplies and personnel are often limited. Design, setting, participants, & measurements Using data from adult patients hospitalized with COVID-19 from five hospitals from theMount Sinai Health System who were admitted between March 10 and December 26, 2020, we developed and validated several models (logistic regression, Least Absolute Shrinkage and Selection Operator (LASSO), random forest, and eXtreme GradientBoosting [XGBoost; with and without imputation]) for predicting treatment with dialysis or death at various time horizons (1, 3, 5, and 7 days) after hospital admission. Patients admitted to theMount Sinai Hospital were used for internal validation, whereas the other hospitals formed part of the external validation cohort. Features included demographics, comorbidities, and laboratory and vital signs within 12 hours of hospital admission. Results A total of 6093 patients (2442 in training and 3651 in external validation) were included in the final cohort. Of the different modeling approaches used, XGBoost without imputation had the highest area under the receiver operating characteristic (AUROC) curve on internal validation (range of 0.93-0.98) and area under the precisionrecall curve (AUPRC; range of 0.78-0.82) for all time points. XGBoost without imputation also had the highest test parameters on external validation (AUROC range of 0.85-0.87, and AUPRC range of 0.27-0.54) across all time windows. XGBoost without imputation outperformed all models with higher precision and recall (mean difference in AUROC of 0.04; mean difference in AUPRC of 0.15). Features of creatinine, BUN, and red cell distribution width were major drivers of the model's prediction. Conclusions An XGBoost model without imputation for prediction of a composite outcome of either death or dialysis in patients positive for COVID-19 had the best performance, as compared with standard and other machine learning models. KW - COVID-19 KW - dialysis KW - machine learning KW - prediction KW - AKI Y1 - 2021 U6 - https://doi.org/10.2215/CJN.17311120 SN - 1555-9041 SN - 1555-905X VL - 16 IS - 8 SP - 1158 EP - 1168 PB - American Society of Nephrology CY - Washington ER - TY - JOUR A1 - Sigel, Keith Magnus A1 - Swartz, Talia H. A1 - Golden, Eddye A1 - Paranjpe, Ishan A1 - Somani, Sulaiman A1 - Richter, Felix A1 - De Freitas, Jessica K. A1 - Miotto, Riccardo A1 - Zhao, Shan A1 - Polak, Paz A1 - Mutetwa, Tinaye A1 - Factor, Stephanie A1 - Mehandru, Saurabh A1 - Mullen, Michael A1 - Cossarini, Francesca A1 - Böttinger, Erwin A1 - Fayad, Zahi A1 - Merad, Miriam A1 - Gnjatic, Sacha A1 - Aberg, Judith A1 - Charney, Alexander A1 - Nadkarni, Girish A1 - Glicksberg, Benjamin S. T1 - Coronavirus 2019 and people living with human immunodeficiency virus BT - outcomes for hospitalized patients in New York City JF - Clinical infectious diseases : electronic edition N2 - Background: There are limited data regarding the clinical impact of coronavirus disease 2019 (COVID-19) on people living with human immunodeficiency virus (PLWH). In this study, we compared outcomes for PLWH with COVID-19 to a matched comparison group. Methods: We identified 88 PLWH hospitalized with laboratory-confirmed COVID-19 in our hospital system in New York City between 12 March and 23 April 2020. We collected data on baseline clinical characteristics, laboratory values, HIV status, treatment, and outcomes from this group and matched comparators (1 PLWH to up to 5 patients by age, sex, race/ethnicity, and calendar week of infection). We compared clinical characteristics and outcomes (death, mechanical ventilation, hospital discharge) for these groups, as well as cumulative incidence of death by HIV status. Results: Patients did not differ significantly by HIV status by age, sex, or race/ethnicity due to the matching algorithm. PLWH hospitalized with COVID-19 had high proportions of HIV virologic control on antiretroviral therapy. PLWH had greater proportions of smoking (P < .001) and comorbid illness than uninfected comparators. There was no difference in COVID-19 severity on admission by HIV status (P = .15). Poor outcomes for hospitalized PLWH were frequent but similar to proportions in comparators; 18% required mechanical ventilation and 21% died during follow-up (compared with 23% and 20%, respectively). There was similar cumulative incidence of death over time by HIV status (P = .94). Conclusions: We found no differences in adverse outcomes associated with HIV infection for hospitalized COVID-19 patients compared with a demographically similar patient group. KW - human immunodeficiency virus KW - coronavirus 2019 KW - severe acute respiratory KW - syndrome coronavirus 2 Y1 - 2020 U6 - https://doi.org/10.1093/cid/ciaa880 SN - 1058-4838 SN - 1537-6591 VL - 71 IS - 11 SP - 2933 EP - 2938 PB - Oxford Univ. Press CY - Cary, NC ER - TY - JOUR A1 - Abdalla, Hassan E. A1 - Abramowski, A. A1 - Aharonian, Felix A. A1 - Benkhali, F. Ait A1 - Akhperjanian, A. G. A1 - Andersson, T. A1 - Anguener, E. O. A1 - Arrieta, M. A1 - Aubert, P. A1 - Backes, M. A1 - Balzer, A. A1 - Barnard, M. A1 - Becherini, Y. A1 - Tjus, J. Becker A1 - Berge, D. A1 - Bernhard, S. A1 - Bernloehr, K. A1 - Blackwell, R. A1 - Boettcher, M. A1 - Boisson, C. A1 - Bolmont, J. A1 - Bordas, Pol A1 - Bregeon, J. A1 - Brun, F. A1 - Brun, P. A1 - Bryan, M. A1 - Bulik, T. A1 - Capasso, M. A1 - Carr, J. A1 - Carrigan, S. A1 - Casanova, Sabrina A1 - Cerruti, M. A1 - Chakraborty, N. A1 - Chalme-Calvet, R. A1 - Chaves, R. C. G. A1 - Chen, A. A1 - Chevalier, J. A1 - Chretien, M. A1 - Colafrancesco, S. A1 - Cologna, G. A1 - Condon, B. A1 - Conrad, J. A1 - Couturier, C. A1 - Cui, Y. A1 - Davids, I. D. A1 - Degrange, B. A1 - Deil, C. A1 - Devin, J. A1 - dewilt, P. A1 - Dirson, L. A1 - Djannati-Atai, A. A1 - Domainko, W. A1 - Donath, A. A1 - Dubus, G. A1 - Dutson, K. A1 - Dyks, J. A1 - Edwards, T. A1 - Egberts, Kathrin A1 - Eger, P. A1 - Ernenwein, J. -P. A1 - Eschbach, S. A1 - Farnier, C. A1 - Fegan, S. A1 - Fernandes, M. V. A1 - Fiasson, A. A1 - Fontaine, G. A1 - Foerster, A. A1 - Funk, S. A1 - Fuessling, M. A1 - Gabici, S. A1 - Gajdus, M. A1 - Gallant, Y. A. A1 - Garrigoux, T. A1 - Giavitto, G. A1 - Giebels, B. A1 - Glicenstein, J. F. A1 - Gottschall, D. A1 - Goyal, A. A1 - Grondin, M. -H. A1 - Hadasch, D. A1 - Hahn, J. A1 - Haupt, M. A1 - Hawkes, J. A1 - Heinzelmann, G. A1 - Henri, G. A1 - Hermann, G. A1 - Hervet, O. A1 - Hillert, A. A1 - Hinton, J. A. A1 - Hofmann, W. A1 - Hoischen, Clemens A1 - Holler, M. A1 - Horns, D. A1 - Ivascenko, A. A1 - Jacholkowska, A. A1 - Jamrozy, M. A1 - Janiak, M. A1 - Jankowsky, D. A1 - Jankowsky, F. A1 - Jingo, M. A1 - Jogler, T. A1 - Jouvin, L. A1 - Jung-Richardt, I. A1 - Kastendieck, M. A. A1 - Katarzynski, K. A1 - Katz, U. A1 - Kerszberg, D. A1 - Khelifi, B. A1 - Kieffer, M. A1 - King, J. A1 - Klepser, S. A1 - Klochkov, D. A1 - Kluzniak, W. A1 - Kolitzus, D. A1 - Komin, Nu. A1 - Kosack, K. A1 - Krakau, S. A1 - Kraus, M. A1 - Krayzel, F. A1 - Krueger, P. P. A1 - Laffon, H. A1 - Lamanna, G. A1 - Lau, J. A1 - Lees, J. -P. A1 - Lefaucheur, J. A1 - Lefranc, V. A1 - Lemiere, A. A1 - Lemoine-Goumard, M. A1 - Lenain, J. -P. A1 - Leser, Eva A1 - Lohse, T. A1 - Lorentz, M. A1 - Liu, R. A1 - Lopez-Coto, R. A1 - Lypova, I. A1 - Marandon, V. A1 - Marcowith, Alexandre A1 - Mariaud, C. A1 - Marx, R. A1 - Maurin, G. A1 - Maxted, N. A1 - Mayer, M. A1 - Meintjes, P. J. A1 - Meyer, M. A1 - Mitchell, A. M. W. A1 - Moderski, R. A1 - Mohamed, M. A1 - Mohrmann, L. A1 - Mora, K. A1 - Moulin, Emmanuel A1 - Murach, T. A1 - de Naurois, M. A1 - Niederwanger, F. A1 - Niemiec, J. A1 - Oakes, L. A1 - Odaka, H. A1 - Oettl, S. A1 - Ohm, S. A1 - Wilhelmi, E. de Ona A1 - Ostrowski, M. A1 - Oya, I. A1 - Padovani, M. A1 - Panter, M. A1 - Parsons, R. D. A1 - Arribas, M. Paz A1 - Pekeur, N. W. A1 - Pelletier, G. A1 - Perennes, C. A1 - Petrucci, P. -O. A1 - Peyaud, B. A1 - Pita, S. A1 - Poon, H. A1 - Prokhorov, D. A1 - Prokoph, H. A1 - Puehlhofer, G. A1 - Punch, M. A1 - Quirrenbach, A. A1 - Raab, S. A1 - Reimer, A. A1 - Reimer, O. A1 - Renaud, M. A1 - de los Reyes, R. A1 - Rieger, F. A1 - Romoli, C. A1 - Rosier-Lees, S. A1 - Rowell, G. A1 - Rudak, B. A1 - Rulten, C. B. A1 - Sahakian, V. A1 - Salek, D. A1 - Sanchez, D. A. A1 - Santangelo, Andrea A1 - Sasaki, M. A1 - Schlickeiser, R. A1 - Schuessler, F. A1 - Schulz, A. A1 - Schwanke, U. A1 - Schwemmer, S. A1 - Settimo, M. A1 - Seyffert, A. S. A1 - Shafi, N. A1 - Shilon, I. A1 - Simoni, R. A1 - Sol, H. A1 - Spanier, F. A1 - Spengler, G. A1 - Spies, F. A1 - Stawarz, L. A1 - Steenkamp, R. A1 - Stegmann, Christian A1 - Stinzing, F. A1 - Stycz, K. A1 - Sushch, I. A1 - Tavernet, J. -P. A1 - Tavernier, T. A1 - Taylor, A. M. A1 - Terrier, R. A1 - Tibaldo, L. A1 - Tiziani, D. A1 - Tluczykont, M. A1 - Trichard, C. A1 - Tuffs, R. A1 - Uchiyama, Y. A1 - Valerius, K. A1 - van der Walt, D. J. A1 - van Eldik, C. A1 - van Soelen, B. A1 - Vasileiadis, G. A1 - Veh, J. A1 - Venter, C. A1 - Viana, A. A1 - Vincent, P. A1 - Vink, J. A1 - Voisin, F. A1 - Voelk, H. J. A1 - Vuillaume, T. A1 - Wadiasingh, Z. A1 - Wagner, S. J. A1 - Wagner, P. A1 - Wagner, R. M. A1 - White, R. A1 - Wierzcholska, A. A1 - Willmann, P. A1 - Woernlein, A. A1 - Wouters, D. A1 - Yang, R. A1 - Zabalza, V. A1 - Zaborov, D. A1 - Zacharias, M. A1 - Zdziarski, A. A. A1 - Zech, Alraune A1 - Zefi, F. A1 - Ziegler, A. A1 - Zywucka, N. T1 - The population of TeV pulsar wind nebulae in the HESS Galactic Plane Survey JF - Astronomy and astrophysics : an international weekly journal N2 - The nine-year H.E.S.S. Galactic Plane Survey (HGPS) has yielded the most uniform observation scan of the inner Milky Way in the TeV gamma-ray band to date. The sky maps and source catalogue of the HGPS allow for a systematic study of the population of TeV pulsar wind nebulae found throughout the last decade. To investigate the nature and evolution of pulsar wind nebulae, for the first time we also present several upper limits for regions around pulsars without a detected TeV wind nebula. Our data exhibit a correlation of TeV surface brightness with pulsar spindown power (E) over dot. This seems to be caused both by an increase of extension with decreasing (E) over dot, and hence with time, compatible with a power law R-PWN((E) over dot) similar to(E) over dot(0.65 +/- 0.20), and by a mild decrease of TeV gamma-ray luminosity with decreasing (E) over dot, compatible with L-1 (10 TeV) similar to (E) over dot(0.59 +/- 0.21). We also find that the off sets of pulsars with respect to the wind nebula centre with ages around 10 kyr are frequently larger than can be plausibly explained by pulsar proper motion and could be due to an asymmetric environment. In the present data, it seems that a large pulsar off set is correlated with a high apparent TeV efficiency L1- 10 TeV / (E) over dot. In addition to 14 HGPS sources considered firmly identified pulsar wind nebulae and 5 additional pulsar wind nebulae taken from literature, we find 10 HGPS sources that are likely TeV pulsar wind nebula candidates. Using a model that subsumes the present common understanding of the very high-energy radiative evolution of pulsar wind nebulae, we find that the trends and variations of the TeV observables and limits can be reproduced to a good level, drawing a consistent picture of present-day TeV data and theory. KW - gamma rays: general KW - catalogs KW - surveys KW - ISM: supernova remnants KW - pulsars: general Y1 - 2018 U6 - https://doi.org/10.1051/0004-6361/201629377 SN - 1432-0746 VL - 612 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Abdalla, Hassan E. A1 - Aharonian, Felix A. A1 - Benkhali, F. Ait A1 - Angüner, Ekrem Oǧuzhan A1 - Arakawa, M. A1 - Arcaro, C. A1 - Armand, C. A1 - Arrieta, M. A1 - Backes, M. A1 - Barnard, M. A1 - Becherini, Y. A1 - Tjus, J. Becker A1 - Berge, D. A1 - Bernloehr, K. A1 - Blackwell, R. A1 - Bottcher, M. A1 - Boisson, C. A1 - Bolmont, J. A1 - Bonnefoy, S. A1 - Bordas, Pol A1 - Bregeon, J. A1 - Brun, F. A1 - Brun, P. A1 - Bryan, M. A1 - Buechele, M. A1 - Bulik, T. A1 - Bylund, T. A1 - Capasso, M. A1 - Caroff, S. A1 - Carosi, A. A1 - Casanova, Sabrina A1 - Cerruti, M. A1 - Chakraborty, N. A1 - Chand, T. A1 - Chandra, S. A1 - Chaves, R. C. G. A1 - Chen, A. A1 - Colafrancesco, S. A1 - Condon, B. A1 - Davids, I. D. A1 - Deil, C. A1 - Devin, J. A1 - deWilt, P. A1 - Dirson, L. A1 - Djannati-Atai, A. A1 - Dmytriiev, A. A1 - Donath, A. A1 - Doroshenko, V A1 - Dyks, J. A1 - Egberts, Kathrin A1 - Emery, G. A1 - Ernenwein, J-P A1 - Eschbach, S. A1 - Fegan, S. A1 - Fiasson, A. A1 - Fontaine, G. A1 - Funk, S. A1 - Fuessling, M. A1 - Gabici, S. A1 - Gallant, Y. A. A1 - Gate, F. A1 - Giavitto, G. A1 - Glawion, D. A1 - Glicenstein, J. F. A1 - Gottschall, D. A1 - Grondin, M-H A1 - Hahn, J. A1 - Haupt, M. A1 - Heinzelmann, G. A1 - Henri, G. A1 - Hermann, G. A1 - Hinton, James Anthony A1 - Hofmann, W. A1 - Hoischen, Clemens A1 - Holch, Tim Lukas A1 - Holler, M. A1 - Horns, D. A1 - Huber, D. A1 - Iwasaki, H. A1 - Jacholkowska, A. A1 - Jamrozy, M. A1 - Jankowsky, D. A1 - Jankowsky, F. A1 - Jouvin, L. A1 - Jung-Richardt, I A1 - Kastendieck, M. A. A1 - Katarzynski, K. A1 - Katsuragawa, M. A1 - Katz, U. A1 - Kerszberg, D. A1 - Khangulyan, D. A1 - Khelifi, B. A1 - King, J. A1 - Klepser, S. A1 - Kluzniak, W. A1 - Komin, Nu A1 - Kosack, K. A1 - Kraus, M. A1 - Lamanna, G. A1 - Lau, J. A1 - Lefaucheur, J. A1 - Lemiere, A. A1 - Lemoine-Goumard, M. A1 - Lenain, J-P A1 - Leser, Eva A1 - Lohse, T. A1 - Lopez-Coto, R. A1 - Lypova, I A1 - Malyshev, D. A1 - Marandon, V A1 - Marcowith, Alexandre A1 - Mariaud, C. A1 - Marti-Devesa, G. A1 - Marx, R. A1 - Maurin, G. A1 - Meintjes, P. J. A1 - Mitchell, A. M. W. A1 - Moderski, R. A1 - Mohamed, M. A1 - Mohrmann, L. A1 - Moore, C. A1 - Moulin, Emmanuel A1 - Murach, T. A1 - Nakashima, S. A1 - de Naurois, M. A1 - Ndiyavala, H. A1 - Niederwanger, F. A1 - Niemiec, J. A1 - Oakes, L. A1 - Odaka, H. A1 - Ohm, S. A1 - Ostrowski, M. A1 - Oya, I A1 - Panter, M. A1 - Parsons, R. D. A1 - Perennes, C. A1 - Petrucci, P-O A1 - Peyaud, B. A1 - Piel, Q. A1 - Pita, S. A1 - Poireau, V A1 - Noel, A. Priyana A1 - Prokhorov, D. A. A1 - Prokoph, H. A1 - Puehlhofer, G. A1 - Punch, M. A1 - Quirrenbach, A. A1 - Raab, S. A1 - Rauth, R. A1 - Reimer, A. A1 - Reimer, O. A1 - Renaud, M. A1 - Rieger, F. A1 - Rinchiuso, L. A1 - Romoli, C. A1 - Rowell, G. A1 - Rudak, B. A1 - Ruiz-Velasco, E. A1 - Sahakian, V A1 - Saito, S. A1 - Sanchez, David M. A1 - Santangelo, Andrea A1 - Sasaki, M. A1 - Schlickeiser, R. A1 - Schussler, F. A1 - Schulz, A. A1 - Schutte, H. A1 - Schwanke, U. A1 - Schwemmer, S. A1 - Seglar-Arroyo, M. A1 - Senniappan, M. A1 - Seyffert, A. S. A1 - Shafi, N. A1 - Shilon, I A1 - Shiningayamwe, K. A1 - Simoni, R. A1 - Sinha, A. A1 - Sol, H. A1 - Specovius, A. A1 - Spir-Jacob, M. A1 - Stawarz, L. A1 - Steenkamp, R. A1 - Stegmann, Christian A1 - Steppa, Constantin Beverly A1 - Takahashi, T. A1 - Tavernet, J-P A1 - Tavernier, T. A1 - Taylor, A. M. A1 - Terrier, R. A1 - Tibaldo, L. A1 - Tiziani, D. A1 - Tluczykont, M. A1 - Trichard, C. A1 - Tsirou, M. A1 - Tsuji, N. A1 - Tuffs, R. A1 - Uchiyama, Y. A1 - van der Walt, D. J. A1 - van Eldik, C. A1 - van Rensburg, C. A1 - van Soelen, B. A1 - Vasileiadis, G. A1 - Veh, J. A1 - Venter, C. A1 - Vincent, P. A1 - Vink, J. A1 - Voisin, F. A1 - Voelk, H. J. A1 - Vuillaume, T. A1 - Wadiasingh, Z. A1 - Wagner, S. J. A1 - Wagner, R. M. A1 - White, R. A1 - Wierzcholska, A. A1 - Yang, R. A1 - Yoneda, H. A1 - Zaborov, D. A1 - Zacharias, M. A1 - Zanin, R. A1 - Zdziarski, A. A. A1 - Zech, Alraune A1 - Zefi, F. A1 - Ziegler, A. A1 - Zorn, J. A1 - Zywucka, N. T1 - Particle transport within the pulsar wind nebula HESS J1825-137 JF - Astronomy and astrophysics : an international weekly journal N2 - Context. We present a detailed view of the pulsar wind nebula (PWN) HESS J1825-137. We aim to constrain the mechanisms dominating the particle transport within the nebula, accounting for its anomalously large size and spectral characteristics. Aims. The nebula was studied using a deep exposure from over 12 years of H.E.S.S. I operation, together with data from H.E.S.S. II that improve the low-energy sensitivity. Enhanced energy-dependent morphological and spatially resolved spectral analyses probe the very high energy (VHE, E > 0.1 TeV) gamma-ray properties of the nebula. Methods. The nebula emission is revealed to extend out to 1.5 degrees from the pulsar, similar to 1.5 times farther than previously seen, making HESS J1825-137, with an intrinsic diameter of similar to 100 pc, potentially the largest gamma-ray PWN currently known. Characterising the strongly energy-dependent morphology of the nebula enables us to constrain the particle transport mechanisms. A dependence of the nebula extent with energy of R proportional to E alpha with alpha = -0.29 +/- 0.04(stat) +/- 0.05(sys) disfavours a pure diffusion scenario for particle transport within the nebula. The total gamma-ray flux of the nebula above 1 TeV is found to be (1.12 +/- 0.03(stat) +/- 0.25(sys)) +/- 10(-11) cm(-2) s(-1), corresponding to similar to 64% of the flux of the Crab nebula. Results. HESS J1825-137 is a PWN with clearly energy-dependent morphology at VHE gamma-ray energies. This source is used as a laboratory to investigate particle transport within intermediate-age PWNe. Based on deep observations of this highly spatially extended PWN, we produce a spectral map of the region that provides insights into the spectral variation within the nebula. KW - gamma rays: general KW - acceleration of particles KW - convection KW - diffusion KW - pulsars: general Y1 - 2019 U6 - https://doi.org/10.1051/0004-6361/201834335 SN - 1432-0746 VL - 621 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Abramowski, A. A1 - Aharonian, Felix A. A1 - Benkhali, F. Ait A1 - Akhperjanian, A. G. A1 - Anguener, E. O. A1 - Backes, M. A1 - Balzer, A. A1 - Becherini, Y. A1 - Tjus, J. Becker A1 - Berge, D. A1 - Bernhard, S. A1 - Bernloehr, K. A1 - Birsin, E. A1 - Blackwell, R. A1 - Boettcher, M. A1 - Boisson, C. A1 - Bolmont, J. A1 - Bordas, Pol A1 - Bregeon, J. A1 - Brun, F. A1 - Brun, P. A1 - Bryan, M. A1 - Bulik, T. A1 - Carr, J. A1 - Casanova, Sabrina A1 - Chakraborty, N. A1 - Chalme-Calvet, R. A1 - Chaves, R. C. G. A1 - Chen, A. A1 - Chevalier, J. A1 - Chretien, M. A1 - Colafrancesco, S. A1 - Cologna, G. A1 - Condon, B. A1 - Conrad, J. A1 - Couturier, C. A1 - Cui, Y. A1 - Davids, I. D. A1 - Degrange, B. A1 - Deil, C. A1 - deWilt, P. A1 - Djannati-Atai, A. A1 - Domainko, W. A1 - Donath, A. A1 - Dubus, G. A1 - Dutson, K. A1 - Dyks, J. A1 - Dyrda, M. A1 - Edwards, T. A1 - Egberts, Kathrin A1 - Eger, P. A1 - Ernenwein, J. -P. A1 - Espigat, P. A1 - Farnier, C. A1 - Fegan, S. A1 - Feinstein, F. A1 - Fernandes, M. V. A1 - Fernandez, D. A1 - Fiasson, A. A1 - Fontaine, G. A1 - Foerster, A. A1 - Fuessling, M. A1 - Gabici, S. A1 - Gajdus, M. A1 - Gallant, Y. A. A1 - Garrigoux, T. A1 - Giavitto, G. A1 - Giebels, B. A1 - Glicenstein, J. F. A1 - Gottschall, D. A1 - Goyal, A. A1 - Grondin, M. -H. A1 - Grudzinska, M. A1 - Hadasch, D. A1 - Haeffner, S. A1 - Hahn, J. A1 - Hawkes, J. A1 - Heinzelmann, G. A1 - Henri, G. A1 - Hermann, G. A1 - Hervet, O. A1 - Hillert, A. A1 - Hinton, J. A. A1 - Hofmann, W. A1 - Hofverberg, P. A1 - Hoischen, Clemens A1 - Holler, M. A1 - Horns, D. A1 - Ivascenko, A. A1 - Jacholkowska, A. A1 - Jamrozy, M. A1 - Janiak, M. A1 - Jankowsky, F. A1 - Jung-Richardt, I. A1 - Kastendieck, M. A. A1 - Katarzynski, K. A1 - Katz, U. A1 - Kerszberg, D. A1 - Khelifi, B. A1 - Kieffer, M. A1 - Klepser, S. A1 - Klochkov, D. A1 - Kluzniak, W. A1 - Kolitzus, D. A1 - Komin, Nu. A1 - Kosack, K. A1 - Krakau, S. A1 - Krayzel, F. A1 - Krueger, P. P. A1 - Laffon, H. A1 - Lamanna, G. A1 - Lau, J. A1 - Lefaucheur, J. A1 - Lefranc, V. A1 - Lemiere, A. A1 - Lemoine-Goumard, M. A1 - Lenain, J. -P. A1 - Lohse, T. A1 - Lopatin, A. A1 - Lorentz, M. A1 - Lu, C. -C. A1 - Lui, R. A1 - Marandon, V. A1 - Marcowith, Alexandre A1 - Mariaud, C. A1 - Marx, R. A1 - Maurin, G. A1 - Maxted, N. A1 - Mayer, M. A1 - Meintjes, P. J. A1 - Menzler, U. A1 - Meyer, M. A1 - Mitchell, A. M. W. A1 - Moderski, R. A1 - Mohamed, M. A1 - Mora, K. A1 - Moulin, Emmanuel A1 - Murach, T. A1 - de Naurois, M. A1 - Niemiec, J. A1 - Oakes, L. A1 - Odaka, H. A1 - Oettl, S. A1 - Ohm, S. A1 - Opitz, B. A1 - Ostrowski, M. A1 - Oya, I. A1 - Panter, M. A1 - Parsons, R. D. A1 - Arribas, M. Paz A1 - Pekeur, N. W. A1 - Pelletier, G. A1 - Petrucci, P. -O. A1 - Peyaud, B. A1 - Pita, S. A1 - Poon, H. A1 - Prokhorov, D. A1 - Prokoph, H. A1 - Puehlhofer, G. A1 - Punch, M. A1 - Quirrenbach, A. A1 - Raab, S. A1 - Reichardt, I. A1 - Reimer, A. A1 - Reimer, O. A1 - Renaud, M. A1 - de los Reyes, R. A1 - Rieger, F. A1 - Romoli, C. A1 - Rosier-Lees, S. A1 - Rowell, G. A1 - Rudak, B. A1 - Rulten, C. B. A1 - Sahakian, V. A1 - Salek, D. A1 - Sanchez, D. A. A1 - Santangelo, Andrea A1 - Sasaki, M. A1 - Schlickeiser, R. A1 - Schuessler, F. A1 - Schulz, A. A1 - Schwanke, U. A1 - Schwemmer, S. A1 - Seyffert, A. S. A1 - Simoni, R. A1 - Sol, H. A1 - Spanier, F. A1 - Spengler, G. A1 - Spies, F. A1 - Stawarz, L. A1 - Steenkamp, R. A1 - Stegmann, Christian A1 - Stinzing, F. A1 - Stycz, K. A1 - Sushch, I. A1 - Tavernet, J. -P. A1 - Tavernier, T. A1 - Taylor, A. M. A1 - Terrier, R. A1 - Tluczykont, M. A1 - Trichard, C. A1 - Tuffs, R. A1 - Valerius, K. A1 - van der Walt, J. A1 - van Eldik, C. A1 - van Soelen, B. A1 - Vasileiadis, G. A1 - Veh, J. A1 - Venter, C. A1 - Viana, A. A1 - Vincent, P. A1 - Vink, J. A1 - Voisin, F. A1 - Voelk, H. J. A1 - Vuillaume, T. A1 - Wagner, S. J. A1 - Wagner, P. A1 - Wagner, R. M. A1 - Weidinger, M. A1 - White, R. A1 - Wierzcholska, A. A1 - Willmann, P. A1 - Woernlein, A. A1 - Wouters, D. A1 - Yang, R. A1 - Zabalza, V. A1 - Zaborov, D. A1 - Zacharias, M. A1 - Zdziarski, A. A. A1 - Zech, Alraune A1 - Zefi, F. A1 - Zywucka, N. T1 - Detailed spectral and morphological analysis of the shell type supernova remnant RCW 86 JF - Astronomy and astrophysics : an international weekly journal N2 - Aims. We aim for an understanding of the morphological and spectral properties of the supernova remnant RCW 86 and for insights into the production mechanism leading to the RCW 86 very high-energy gamma-ray emission. Methods. We analyzed High Energy Spectroscopic System (H.E.S.S.) data that had increased sensitivity compared to the observations presented in the RCW 86 H.E.S.S. discovery publication. Studies of the morphological correlation between the 0.5-1 keV X-ray band, the 2-5 keV X-ray band, radio, and gamma-ray emissions have been performed as well as broadband modeling of the spectral energy distribution with two different emission models. Results. We present the first conclusive evidence that the TeV gamma-ray emission region is shell-like based on our morphological studies. The comparison with 2-5 keV X-ray data reveals a correlation with the 0.4-50 TeV gamma-ray emission. The spectrum of RCW 86 is best described by a power law with an exponential cutoff at E-cut = (3.5 +/- 1.2(stat)) TeV and a spectral index of Gamma approximate to 1.6 +/- 0.2. A static leptonic one-zone model adequately describes the measured spectral energy distribution of RCW 86, with the resultant total kinetic energy of the electrons above 1 GeV being equivalent to similar to 0.1% of the initial kinetic energy of a Type Ia supernova explosion (10(51) erg). When using a hadronic model, a magnetic field of B approximate to 100 mu G is needed to represent the measured data. Although this is comparable to formerly published estimates, a standard E-2 spectrum for the proton distribution cannot describe the gamma-ray data. Instead, a spectral index of Gamma(p) approximate to 1.7 would be required, which implies that similar to 7 x 10(49)/n(cm-3) erg has been transferred into high-energy protons with the effective density n(cm-3) = n/1 cm(-3). This is about 10% of the kinetic energy of a typical Type Ia supernova under the assumption of a density of 1 cm(-3). KW - astroparticle physics KW - gamma rays: general KW - ISM: supernova remnants KW - cosmic rays Y1 - 2018 U6 - https://doi.org/10.1051/0004-6361/201526545 SN - 1432-0746 VL - 612 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Abdalla, Hassan E. A1 - Abramowski, A. A1 - Aharonian, Felix A. A1 - Benkhali, F. Ait A1 - Akhperjanian, A. G. A1 - Andersson, T. A1 - Anguener, E. O. A1 - Arakawa, M. A1 - Arrieta, M. A1 - Aubert, P. A1 - Backes, M. A1 - Balzer, A. A1 - Barnard, M. A1 - Becherini, Y. A1 - Tjus, J. Becker A1 - Berge, D. A1 - Bernhard, S. A1 - Bernloehr, K. A1 - Blackwell, R. A1 - Boettcher, M. A1 - Boisson, C. A1 - Bolmont, J. A1 - Bordas, Pol A1 - Bregeon, J. A1 - Brun, F. A1 - Brun, P. A1 - Bryan, M. A1 - Bilchele, M. A1 - Bulik, T. A1 - Capasso, M. A1 - Carr, J. A1 - Casanova, Sabrina A1 - Cerruti, M. A1 - Chakraborty, N. A1 - Chalme-Calvet, R. A1 - Chaves, R. C. G. A1 - Chen, A. A1 - Chevalier, J. A1 - Chretien, M. A1 - Coffaro, M. A1 - Colafrancesco, S. A1 - Cologna, G. A1 - Condon, B. A1 - Conrad, J. A1 - Cui, Y. A1 - Davids, I. D. A1 - Decock, J. A1 - Degrange, B. A1 - Deil, C. A1 - Devin, J. A1 - deWilt, P. A1 - Dirson, L. A1 - Djannati-Atai, A. A1 - Domainko, W. A1 - Donath, A. A1 - Dutson, K. A1 - Dyks, J. A1 - Edwards, T. A1 - Egberts, Kathrin A1 - Eger, P. A1 - Ernenwein, J. -P. A1 - Eschbach, S. A1 - Farnier, C. A1 - Fegan, S. A1 - Fernandes, M. V. A1 - Fiasson, A. A1 - Fontaine, G. A1 - Foerster, A. A1 - Funk, S. A1 - Fuessling, M. A1 - Gabici, S. A1 - Gajdus, M. A1 - Gallant, Y. A. A1 - Garrigoux, T. A1 - Giavitto, G. A1 - Giebels, B. A1 - Glicenstein, J. F. A1 - Gottschall, D. A1 - Goya, A. A1 - Grondin, M. -H. A1 - Hahn, J. A1 - Haupt, M. A1 - Hawkes, J. A1 - Heinzelmann, G. A1 - Henri, G. A1 - Hermann, G. A1 - Hervet, O. A1 - Hinton, J. A. A1 - Hofmann, W. A1 - Hoischen, Clemens A1 - Holler, M. A1 - Horns, D. A1 - Ivascenko, A. A1 - Iwasaki, H. A1 - Jacholkowska, A. A1 - Jamrozy, M. A1 - Janiak, M. A1 - Jankowsky, D. A1 - Jankowsky, F. A1 - Jingo, M. A1 - Jogler, T. A1 - Jouvin, L. A1 - Jung-Richardt, I. A1 - Kastendieck, M. A. A1 - Katarzynski, K. A1 - Katsuragawa, M. A1 - Katz, U. A1 - Kerszberg, D. A1 - Khangulyan, D. A1 - Khelifi, B. A1 - Kieffer, M. A1 - King, J. A1 - Klepser, S. A1 - Klochkov, D. A1 - Kluzniak, W. A1 - Kolitzus, D. A1 - Komin, Nu. A1 - Kosack, K. A1 - Krakau, S. A1 - Kraus, M. A1 - Krueger, P. P. A1 - Laffon, H. A1 - Lamanna, G. A1 - Lau, J. A1 - Lees, J. -P. A1 - Lefaucheur, J. A1 - Lefranc, V. A1 - Lemiere, A. A1 - Lemoine-Goumard, M. A1 - Lenain, J. -P. A1 - Leser, Eva A1 - Lohse, T. A1 - Lorentz, M. A1 - Liu, R. A1 - Lopez-Coto, R. A1 - Lypova, I. A1 - Marandon, V. A1 - Marcowith, Alexandre A1 - Mariaud, C. A1 - Marx, R. A1 - Maurin, G. A1 - Maxted, N. A1 - Mayer, M. A1 - Meintjes, P. J. A1 - Meyer, M. A1 - Mitche, A. M. W. A1 - Moderski, R. A1 - Mohamed, M. A1 - Mohrmann, L. A1 - Mora, K. A1 - Moulin, Emmanuel A1 - Murach, T. A1 - Nakashima, S. A1 - de Naurois, M. A1 - Niederwanger, F. A1 - Niemiec, J. A1 - Oakes, L. A1 - Odaka, H. A1 - Oettl, S. A1 - Ohm, S. A1 - Ostrowski, M. A1 - Oya, I. A1 - Padovani, M. A1 - Panter, M. A1 - Parsons, R. D. A1 - Arribas, M. Paz A1 - Pekeur, N. W. A1 - Pelletier, G. A1 - Perennes, C. A1 - Petrucci, P. -O. A1 - Peyaud, B. A1 - Piel, Q. A1 - Pita, S. A1 - Poon, H. A1 - Prokhorov, D. A1 - Prokoph, H. A1 - Puehlhofer, G. A1 - Punch, M. A1 - Quirrenbach, A. A1 - Raab, S. A1 - Reimer, A. A1 - Reimer, O. A1 - Renaud, M. A1 - de los Reyes, R. A1 - Richter, S. A1 - Rieger, F. A1 - Romoli, C. A1 - Rowell, G. A1 - Rudak, B. A1 - Rulten, C. B. A1 - Sahakian, V. A1 - Saito, S. A1 - Salek, D. A1 - Sanchez, D. A. A1 - Santangelo, Andrea A1 - Sasaki, M. A1 - Schlickeiser, R. A1 - Schuessler, F. A1 - Schulz, A. A1 - Schwanke, U. A1 - Schwemmer, S. A1 - Seglar-Arroyo, M. A1 - Settimo, M. A1 - Seyffert, A. S. A1 - Shafi, N. A1 - Shilon, I. A1 - Simoni, R. A1 - Sol, H. A1 - Spanier, F. A1 - Spengler, G. A1 - Spies, F. A1 - Stawarz, L. A1 - Steenkamp, R. A1 - Stegmann, Christian A1 - Stycz, K. A1 - Sushch, I. A1 - Takahashi, T. A1 - Tavernet, J. -P. A1 - Tavernier, T. A1 - Taylor, A. M. A1 - Terrier, R. A1 - Tibaldo, L. A1 - Tiziani, D. A1 - Tluczykont, M. A1 - Trichard, C. A1 - Tsuji, N. A1 - Tuffs, R. A1 - Uchiyama, Y. A1 - van der Walt, D. J. A1 - van Eldik, C. A1 - van Rensburg, C. A1 - van Soelen, B. A1 - Vasileiadis, G. A1 - Veh, J. A1 - Venter, C. A1 - Viana, A. A1 - Vincent, P. A1 - Vink, J. A1 - Voisin, F. A1 - Voelk, H. J. A1 - Vuillaume, T. A1 - Wadiasingh, Z. A1 - Wagner, S. J. A1 - Wagner, P. A1 - Wagner, R. M. A1 - White, R. A1 - Wierzcholska, A. A1 - Willmann, P. A1 - Woernlein, A. A1 - Wouters, D. A1 - Yang, R. A1 - Zabalza, V. A1 - Zaborov, D. A1 - Zacharias, M. A1 - Zanin, R. A1 - Zdziarski, A. A. A1 - Zech, Alraune A1 - Zefi, F. A1 - Ziegler, A. A1 - Zywucka, N. T1 - Deeper HESS observations of Vela Junior (RX J0852.0-4622) BT - Morphology studies and resolved spectroscopy JF - Astronomy and astrophysics : an international weekly journal N2 - Aims. We study gamma-ray emission from the shell-type supernova remnant (SNR) RXJ0852.0-4622 to better characterize its spectral properties and its distribution over the SNR. Methods. The analysis of an extended High Energy Spectroscopic System (H.E.S.S.) data set at very high energies (E > 100 GeV) permits detailed studies, as well as spatially resolved spectroscopy, of the morphology and spectrum of the whole RXJ0852.0-4622 region. The H.E.S.S. data are combined with archival data from other wavebands and interpreted in the framework of leptonic and hadronic models. The joint Fermi-LAT-H.E.S.S. spectrum allows the direct determination of the spectral characteristics of the parent particle population in leptonic and hadronic scenarios using only GeV-TeV data. Results. An updated analysis of the H.E.S.S. data shows that the spectrum of the entire SNR connects smoothly to the high-energy spectrum measured by Fermi-LAT. The increased data set makes it possible to demonstrate that the H.E.S.S. spectrum deviates significantly from a power law and is well described by both a curved power law and a power law with an exponential cutoff at an energy of E-cut = (6.7 +/- 1.2(stat) +/- 1.2(syst)) TeV. The joint Fermi-LAT-H.E.S.S. spectrum allows the unambiguous identification of the spectral shape as a power law with an exponential cutoff. No significant evidence is found for a variation of the spectral parameters across the SNR, suggesting similar conditions of particle acceleration across the remnant. A simple modeling using one particle population to model the SNR emission demonstrates that both leptonic and hadronic emission scenarios remain plausible. It is also shown that at least a part of the shell emission is likely due to the presence of a pulsar wind nebula around PSR J0855-4644. KW - astroparticle physics KW - gamma rays: general KW - acceleration of particles KW - cosmic rays KW - ISM: supernova remnants Y1 - 2018 U6 - https://doi.org/10.1051/0004-6361/201630002 SN - 1432-0746 VL - 612 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Abdalla, Hassan E. A1 - Abramowski, A. A1 - Aharonian, Felix A. A1 - Benkhali, F. Ait A1 - Akhperjanian, A. G. A1 - Andersson, T. A1 - Anguener, E. O. A1 - Arakawa, M. A1 - Arrieta, M. A1 - Aubert, P. A1 - Backes, M. A1 - Balzer, A. A1 - Barnard, M. A1 - Becherini, Y. A1 - Tjus, J. Becker A1 - Berge, D. A1 - Bernhard, S. A1 - Bernloehr, K. A1 - Blackwell, R. A1 - Boettcher, M. A1 - Boisson, C. A1 - Bolmont, J. A1 - Bonnefoy, S. A1 - Bordas, Pol A1 - Bregeon, J. A1 - Brun, F. A1 - Brun, P. A1 - Bryan, M. A1 - Buechele, M. A1 - Bulik, T. A1 - Capasso, M. A1 - Carr, J. A1 - Casanova, Sabrina A1 - Cerruti, M. A1 - Chakraborty, N. A1 - Chaves, R. C. G. A1 - Chen, A. A1 - Chevalier, J. A1 - Coffaro, M. A1 - Colafrancesco, S. A1 - Cologna, G. A1 - Condon, B. A1 - Conrad, J. A1 - Cui, Y. A1 - Davids, I. D. A1 - Decock, J. A1 - Degrange, B. A1 - Deil, C. A1 - Devin, J. A1 - deWilt, P. A1 - Dirson, L. A1 - Djannati-Atai, A. A1 - Domainko, W. A1 - Donath, A. A1 - Dutson, K. A1 - Dyks, J. A1 - Edwards, T. A1 - Egberts, Kathrin A1 - Eger, P. A1 - Ernenwein, J. -P. A1 - Eschbach, S. A1 - Farnier, C. A1 - Fegan, S. A1 - Fernandes, M. V. A1 - Fiasson, A. A1 - Fontaine, G. A1 - Foerster, A. A1 - Funk, S. A1 - Fuessling, M. A1 - Gabici, S. A1 - Gajdus, M. A1 - Gallant, Y. A. A1 - Garrigoux, T. A1 - Giavitto, G. A1 - Giebels, B. A1 - Glicenstein, J. F. A1 - Gottschall, D. A1 - Goyal, A. A1 - Grondin, M. -H. A1 - Hahn, J. A1 - Haupt, M. A1 - Hawkes, J. A1 - Heinzelmann, G. A1 - Henri, G. A1 - Hermann, G. A1 - Hervet, O. A1 - Hinton, J. A. A1 - Hofmann, W. A1 - Hoischen, Clemens A1 - Holch, T. L. A1 - Holler, M. A1 - Horns, D. A1 - Ivascenko, A. A1 - Iwasaki, H. A1 - Jacholkowska, A. A1 - Jamrozy, M. A1 - Janiak, M. A1 - Jankowsky, D. A1 - Jankowsky, F. A1 - Jingo, M. A1 - Jogler, T. A1 - Jouvin, L. A1 - Jung-Richardt, I. A1 - Kastendieck, M. A. A1 - Katarzynski, K. A1 - Katsuragawa, M. A1 - Katz, U. A1 - Kerszberg, D. A1 - Khangulyan, D. A1 - Khelifi, B. A1 - King, J. A1 - Klepser, S. A1 - Klochkov, D. A1 - Kluzniak, W. A1 - Kolitzus, D. A1 - Komin, Nu. A1 - Kosack, K. A1 - Krakau, S. A1 - Kraus, M. A1 - Krueger, P. P. A1 - Laffon, H. A1 - Lamanna, G. A1 - Lau, J. A1 - Lees, J. -P. A1 - Lefaucheur, J. A1 - Lefranc, V. A1 - Lemiere, A. A1 - Lemoine-Goumard, M. A1 - Lenain, J. -P. A1 - Leser, Eva A1 - Lohse, T. A1 - Lorentz, M. A1 - Liu, R. A1 - Lopez-Coto, R. A1 - Lypova, I. A1 - Marandon, V. A1 - Marcowith, Alexandre A1 - Mariaud, C. A1 - Marx, R. A1 - Maurin, G. A1 - Maxted, N. A1 - Mayer, M. A1 - Meintjes, P. J. A1 - Meyer, M. A1 - Mitche, A. M. W. A1 - Moderski, R. A1 - Mohamed, M. A1 - Mohrmann, L. A1 - Mora, K. A1 - Moulin, Emmanuel A1 - Murach, T. A1 - Nakashima, S. A1 - de Naurois, M. A1 - Niederwanger, F. A1 - Niemiec, J. A1 - Oakes, L. A1 - Odaka, H. A1 - Oettl, S. A1 - Ohm, S. A1 - Ostrowski, M. A1 - Oya, I. A1 - Padovani, M. A1 - Panter, M. A1 - Parsons, R. D. A1 - Pekeur, N. W. A1 - Pelletier, G. A1 - Perennes, C. A1 - Petrucci, P. -O. A1 - Peyaud, B. A1 - Piel, Q. A1 - Pita, S. A1 - Poon, H. A1 - Prokhorov, D. A1 - Prokoph, H. A1 - Puehlhofer, G. A1 - Punch, M. A1 - Quirrenbach, A. A1 - Raab, S. A1 - Reimer, A. A1 - Reimer, O. A1 - Renaud, M. A1 - de los Reyes, R. A1 - Richter, S. A1 - Rieger, F. A1 - Romoli, C. A1 - Rowell, G. A1 - Rudak, B. A1 - Rulten, C. B. A1 - Sahakian, V. A1 - Saito, S. A1 - Salek, D. A1 - Sanchez, D. A. A1 - Santangelo, Andrea A1 - Sasaki, M. A1 - Schlickeiser, R. A1 - Schuessler, F. A1 - Schulz, A. A1 - Schwanke, U. A1 - Schwemmer, S. A1 - Seglar-Arroyo, M. A1 - Settimo, M. A1 - Seyffert, A. S. A1 - Shafi, N. A1 - Shilon, I. A1 - Simoni, R. A1 - Sol, H. A1 - Spanier, F. A1 - Spengler, G. A1 - Spies, F. A1 - Stawarz, L. A1 - Steenkamp, R. A1 - Stegmann, Christian A1 - Stycz, K. A1 - Sushch, I. A1 - Takahashi, T. A1 - Tavernet, J. -P. A1 - Tavernier, T. A1 - Taylor, A. M. A1 - Terrier, R. A1 - Tibaldo, L. A1 - Tiziani, D. A1 - Tluczykont, M. A1 - Trichard, C. A1 - Tsuji, N. A1 - Tuffs, R. A1 - Uchiyama, Y. A1 - van der Wale, D. J. A1 - van Eldik, C. A1 - van Rensburg, C. A1 - van Soelen, B. A1 - Vasileiadis, G. A1 - Veh, J. A1 - Venter, C. A1 - Viana, A. A1 - Vincent, P. A1 - Vink, J. A1 - Voisin, F. A1 - Voelk, H. J. A1 - Vuillaume, T. A1 - Wadiasingh, Z. A1 - Wagner, S. J. A1 - Wagner, P. A1 - Wagner, R. M. A1 - White, R. A1 - Wierzcholska, A. A1 - Willmann, P. A1 - Woernlein, A. A1 - Wouters, D. A1 - Yang, R. A1 - Zabalza, V. A1 - Zaborov, D. A1 - Zacharias, M. A1 - Zanin, R. A1 - Zdziarski, A. A. A1 - Zech, Alraune A1 - Zefi, F. A1 - Ziegler, A. A1 - Zywucka, N. A1 - Bamba, A. A1 - Fukui, Y. A1 - Sano, H. A1 - Yoshiike, S. T1 - A search for new supernova remnant shells in the Galactic plane with HESS JF - Astronomy and astrophysics : an international weekly journal N2 - A search for new supernova remnants (SNRs) has been conducted using TeV gamma-ray data from the H.E.S.S. Galactic plane survey. As an identification criterion, shell morphologies that are characteristic for known resolved TeV SNRs have been used. Three new SNR candidates were identified in the H.E.S.S. data set with this method. Extensive multiwavelength searches for counterparts were conducted. A radio SNR candidate has been identified to be a counterpart to HESS J1534-571. The TeV source is therefore classified as a SNR. For the other two sources, HESS J1614-518 and HESS J1912 + 101, no identifying counterparts have been found, thus they remain SNR candidates for the time being. TeV-emitting SNRs are key objects in the context of identifying the accelerators of Galactic cosmic rays. The TeV emission of the relativistic particles in the new sources is examined in view of possible leptonic and hadronic emission scenarios, taking the current multiwavelength knowledge into account. KW - astroparticle physics KW - ISM: supernova remnants KW - cosmic rays Y1 - 2018 U6 - https://doi.org/10.1051/0004-6361/201730737 SN - 1432-0746 VL - 612 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Abdalla, Hassan E. A1 - Abramowski, A. A1 - Aharonian, Felix A. A1 - Benkhali, F. Ait A1 - Akhperjanian, A. G. A1 - Andersson, T. A1 - Anguener, E. O. A1 - Arrieta, M. A1 - Aubert, P. A1 - Backes, M. A1 - Balzer, A. A1 - Barnard, M. A1 - Becherini, Y. A1 - Tjus, J. Becker A1 - Berge, D. A1 - Bernhard, S. A1 - Bernloehr, K. A1 - Blackwell, R. A1 - Boettcher, M. A1 - Boisson, C. A1 - Bolmont, J. A1 - Bordas, Pol A1 - Bregeon, J. A1 - Brun, F. A1 - Brun, P. A1 - Bryan, M. A1 - Bulik, T. A1 - Capasso, M. A1 - Carr, J. A1 - Casanova, Sabrina A1 - Cerruti, M. A1 - Chakraborty, N. A1 - Chalme-Calvet, R. A1 - Chaves, R. C. G. A1 - Chen, A. A1 - Chevalier, J. A1 - Chretien, M. A1 - Colafrancesco, S. A1 - Cologna, G. A1 - Condon, B. A1 - Conrad, J. A1 - Cui, Y. A1 - Davids, I. D. A1 - Decock, J. A1 - Degrange, B. A1 - Dei, C. A1 - Devin, J. A1 - deWilt, P. A1 - Dirson, L. A1 - Djannati-Atai, A. A1 - Domainko, W. A1 - Donath, A. A1 - Dubus, G. A1 - Dutson, K. A1 - Dyks, J. A1 - Edwards, T. A1 - Egberts, Kathrin A1 - Eger, P. A1 - Ernenwein, J. -P. A1 - Eschbach, S. A1 - Farnier, C. A1 - Fegan, S. A1 - Fernandes, M. V. A1 - Fiasson, A. A1 - Fontaine, G. A1 - Foerster, A. A1 - Fukuyama, T. A1 - Funk, S. A1 - Fuessling, M. A1 - Gabici, S. A1 - Gajdus, M. A1 - Gallant, Y. A. A1 - Garrigoux, T. A1 - Giavitto, G. A1 - Giebels, B. A1 - Glicenstein, J. F. A1 - Gottschall, D. A1 - Goyal, A. A1 - Grondin, M. -H. A1 - Hadasch, D. A1 - Hahn, J. A1 - Haupt, M. A1 - Hawkes, J. A1 - Heinzelmann, G. A1 - Henri, G. A1 - Hermann, G. A1 - Hervet, O. A1 - Hinton, J. A. A1 - Hofmann, W. A1 - Hoischen, Clemens A1 - Holler, M. A1 - Horns, D. A1 - Ivascenko, A. A1 - Jacholkowska, A. A1 - Jamrozy, M. A1 - Janiak, M. A1 - Jankowsky, D. A1 - Jankowsky, F. A1 - Jingo, M. A1 - Jogler, T. A1 - Jouvin, L. A1 - Jung-Richardt, I. A1 - Kastendieck, M. A. A1 - Katarzynski, K. A1 - Katz, U. A1 - Kerszberg, D. A1 - Khelifi, B. A1 - Kieffer, M. A1 - King, J. A1 - Klepser, S. A1 - Klochkov, D. A1 - Kluzniak, W. A1 - Kolitzus, D. A1 - Komin, Nu. A1 - Kosack, K. A1 - Krakau, S. A1 - Kraus, M. A1 - Krayzel, F. A1 - Krueger, P. P. A1 - Laffon, H. A1 - Lamanna, G. A1 - Lau, J. A1 - Lees, J. -P. A1 - Lefaucheur, J. A1 - Lefranc, V. A1 - Lemiere, A. A1 - Lemoine-Goumard, M. A1 - Lenain, J. -P. A1 - Leser, Eva A1 - Lohse, T. A1 - Lorentz, M. A1 - Liu, R. A1 - Lopez-Coto, R. A1 - Lypova, I. A1 - Marandon, V. A1 - Marcowith, Alexandre A1 - Mariaud, C. A1 - Marx, R. A1 - Maurin, G. A1 - Maxted, N. A1 - Mayer, M. A1 - Meintjes, P. J. A1 - Meyer, M. A1 - Mitchell, A. M. W. A1 - Moderski, R. A1 - Mohamed, M. A1 - Mohrmann, L. A1 - Mora, K. A1 - Moulin, Emmanuel A1 - Murach, T. A1 - de Naurois, M. A1 - Niederwanger, F. A1 - Niemiec, J. A1 - Oakes, L. A1 - Odaka, H. A1 - Oettl, S. A1 - Ohm, S. A1 - Ostrowski, M. A1 - Oya, I. A1 - Padovani, M. A1 - Panter, M. A1 - Parsons, R. D. A1 - Pekeur, N. W. A1 - Pelletier, G. A1 - Perennes, C. A1 - Petrucci, P. -O. A1 - Peyaud, B. A1 - Piel, Q. A1 - Pita, S. A1 - Poon, H. A1 - Prokhorov, D. A1 - Prokoph, H. A1 - Puehlhofer, G. A1 - Punch, M. A1 - Quirrenbach, A. A1 - Raab, S. A1 - Reimer, A. A1 - Reimer, O. A1 - Renaud, M. A1 - de los Reyes, R. A1 - Rieger, F. A1 - Romoli, C. A1 - Rosier-Lees, S. A1 - Rowell, G. A1 - Rudak, B. A1 - Rulten, C. B. A1 - Sahakian, V. A1 - Salek, D. A1 - Sanchez, D. A. A1 - Santangelo, Andrea A1 - Sasaki, M. A1 - Schlickeiser, R. A1 - Schuessler, F. A1 - Schulz, A. A1 - Schwanke, U. A1 - Schwemmer, S. A1 - Settimo, M. A1 - Seyffert, A. S. A1 - Shafi, N. A1 - Shilon, I. A1 - Simoni, R. A1 - Sol, H. A1 - Spanie, F. A1 - Spengler, G. A1 - Spies, F. A1 - Stawarz, L. A1 - Steenkamp, R. A1 - Stegmann, Christian A1 - Stinzing, F. A1 - Stycz, K. A1 - Sushch, I. A1 - Takahashi, T. A1 - Tavernet, J. -P. A1 - Tavernier, T. A1 - Taylor, A. M. A1 - Terrier, R. A1 - Tibaldo, L. A1 - Tiziani, D. A1 - Tluczykont, M. A1 - Trichard, C. A1 - Tuffs, R. A1 - Uchiyama, Y. A1 - van der Walt, D. J. A1 - van Edik, C. A1 - van Rensburg, C. A1 - van Soelen, B. A1 - Vasileiadis, G. A1 - Veh, J. A1 - Venter, C. A1 - Viana, A. A1 - Vincent, P. A1 - Vink, J. A1 - Voisin, F. A1 - Voelk, H. J. A1 - Volpe, F. A1 - Vuillaume, T. A1 - Wadiasingh, Z. A1 - Wagner, S. J. A1 - Wagner, P. A1 - Wagner, R. M. A1 - White, R. A1 - Wierzcholska, A. A1 - Willmann, P. A1 - Woernlein, A. A1 - Wouters, D. A1 - Yang, R. A1 - Zabalza, V. A1 - Zaborov, D. A1 - Zacharias, M. A1 - Zdziarski, A. A. A1 - Zech, Alraune A1 - Zefi, F. A1 - Ziegler, A. A1 - Zywucka, N. T1 - HESS observations of RX J1713.7-3946 with improved angular and spectral resolution BT - Evidence for gamma-ray emission extending beyond the X-ray emitting shell JF - Astronomy and astrophysics : an international weekly journal KW - acceleration of particles KW - cosmic rays KW - ISM: supernova remnants KW - gamma rays: general KW - astroparticle physic Y1 - 2018 U6 - https://doi.org/10.1051/0004-6361/201629790 SN - 1432-0746 VL - 612 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - De Angelis, A. A1 - Tatischeff, V. A1 - Grenier, I. A. A1 - McEnery, J. A1 - Mallamaci, Manuela A1 - Tavani, M. A1 - Oberlack, U. A1 - Hanlon, L. A1 - Walter, R. A1 - Argan, A. A1 - Von Ballmoos, P. A1 - Bulgarelli, A. A1 - Bykov, A. A1 - Hernanz, M. A1 - Kanbach, G. A1 - Kuvvetli, I. A1 - Pearce, M. A1 - Zdziarski, A. A1 - Conrad, J. A1 - Ghisellini, G. A1 - Harding, A. A1 - Isern, J. A1 - Leising, M. A1 - Longo, F. A1 - Madejski, G. A1 - Martinez, M. A1 - Mazziotta, Mario Nicola A1 - Paredes, J. M. A1 - Pohl, Martin A1 - Rando, R. A1 - Razzano, M. A1 - Aboudan, A. A1 - Ackermann, M. A1 - Addazi, A. A1 - Ajello, M. A1 - Albertus, C. A1 - Alvarez, J. M. A1 - Ambrosi, G. A1 - Anton, S. A1 - Antonelli, L. A. A1 - Babic, A. A1 - Baibussinov, B. A1 - Balbom, M. A1 - Baldini, L. A1 - Balman, S. A1 - Bambi, C. A1 - Barres de Almeida, U. A1 - Barrio, J. A. A1 - Bartels, R. A1 - Bastieri, D. A1 - Bednarek, W. A1 - Bernard, D. A1 - Bernardini, E. A1 - Bernasconi, T. A1 - Bertucci, B. A1 - Biland, A. A1 - Bissaldi, E. A1 - Boettcher, M. A1 - Bonvicini, V. A1 - Bosch-Ramon, V. A1 - Bottacini, E. A1 - Bozhilov, V. A1 - Bretz, T. A1 - Branchesi, M. A1 - Brdar, V. A1 - Bringmann, T. A1 - Brogna, A. A1 - Jorgensen, C. Budtz A1 - Busetto, G. A1 - Buson, S. A1 - Busso, M. A1 - Caccianiga, A. A1 - Camera, S. A1 - Campana, R. A1 - Caraveo, P. A1 - Cardillo, M. A1 - Carlson, P. A1 - Celestin, S. A1 - Cermeno, M. A1 - Chen, A. A1 - Cheung, C. C. A1 - Churazov, E. A1 - Ciprini, S. A1 - Coc, A. A1 - Colafrancesco, S. A1 - Coleiro, A. A1 - Collmar, W. A1 - Coppi, P. A1 - Curado da Silva, R. A1 - Cutini, S. A1 - De Lotto, B. A1 - de Martino, D. A1 - De Rosa, A. A1 - Del Santo, M. A1 - Delgado, L. A1 - Diehl, R. A1 - Dietrich, S. A1 - Dolgov, A. D. A1 - Dominguez, A. A1 - Prester, D. Dominis A1 - Donnarumma, I. A1 - Dorner, D. A1 - Doro, M. A1 - Dutra, M. A1 - Elsaesser, D. A1 - Fabrizio, M. A1 - Fernandez-Barral, A. A1 - Fioretti, V. A1 - Foffano, L. A1 - Formato, V. A1 - Fornengo, N. A1 - Foschini, L. A1 - Franceschini, A. A1 - Franckowiak, A. A1 - Funk, S. A1 - Fuschino, F. A1 - Gaggero, D. A1 - Galanti, G. A1 - Gargano, F. A1 - Gasparrini, D. A1 - Gehrz, R. A1 - Giammaria, P. A1 - Giglietto, N. A1 - Giommi, P. A1 - Giordano, F. A1 - Giroletti, M. A1 - Ghirlanda, G. A1 - Godinovic, N. A1 - Gouiffes, C. A1 - Grove, J. E. A1 - Hamadache, C. A1 - Hartmann, D. H. A1 - Hayashida, M. A1 - Hryczuk, A. A1 - Jean, P. A1 - Johnson, T. A1 - Jose, J. A1 - Kaufmann, S. A1 - Khelifi, B. A1 - Kiener, J. A1 - Knodlseder, J. A1 - Kolem, M. A1 - Kopp, J. A1 - Kozhuharov, V. A1 - Labanti, C. A1 - Lalkovski, S. A1 - Laurent, P. A1 - Limousin, O. A1 - Linares, M. A1 - Lindfors, E. A1 - Lindner, M. A1 - Liu, J. A1 - Lombardi, S. A1 - Loparco, F. A1 - Lopez-Coto, R. A1 - Lopez Moya, M. A1 - Lott, B. A1 - Lubrano, P. A1 - Malyshev, D. A1 - Mankuzhiyil, N. A1 - Mannheim, K. A1 - Marcha, M. J. A1 - Marciano, A. A1 - Marcote, B. A1 - Mariotti, M. A1 - Marisaldi, M. A1 - McBreen, S. A1 - Mereghetti, S. A1 - Merle, A. A1 - Mignani, R. A1 - Minervini, G. A1 - Moiseev, A. A1 - Morselli, A. A1 - Moura, F. A1 - Nakazawa, K. A1 - Nava, L. A1 - Nieto, D. A1 - Orienti, M. A1 - Orio, M. A1 - Orlando, E. A1 - Orleanski, P. A1 - Paiano, S. A1 - Paoletti, R. A1 - Papitto, A. A1 - Pasquato, M. A1 - Patricelli, B. A1 - Perez-Garcia, M. A. A1 - Persic, M. A1 - Piano, G. A1 - Pichel, A. A1 - Pimenta, M. A1 - Pittori, C. A1 - Porter, T. A1 - Poutanen, J. A1 - Prandini, E. A1 - Prantzos, N. A1 - Produit, N. A1 - Profumo, S. A1 - Queiroz, F. S. A1 - Raino, S. A1 - Raklev, A. A1 - Regis, M. A1 - Reichardt, I. A1 - Rephaeli, Y. A1 - Rico, J. A1 - Rodejohann, W. A1 - Fernandez, G. Rodriguez A1 - Roncadelli, M. A1 - Roso, L. A1 - Rovero, A. A1 - Ruffini, R. A1 - Sala, G. A1 - Sanchez-Conde, M. A. A1 - Santangelo, Andrea A1 - Parkinson, P. Saz A1 - Sbarrato, T. A1 - Shearer, A. A1 - Shellard, R. A1 - Short, K. A1 - Siegert, T. A1 - Siqueira, C. A1 - Spinelli, P. A1 - Stamerra, A. A1 - Starrfield, S. A1 - Strong, A. A1 - Strumke, I. A1 - Tavecchio, F. A1 - Taverna, R. A1 - Terzic, T. A1 - Thompson, D. J. A1 - Tibolla, O. A1 - Torres, D. F. A1 - Turolla, R. A1 - Ulyanov, A. A1 - Ursi, A. A1 - Vacchi, A. A1 - Van den Abeele, J. A1 - Vankova-Kirilovai, G. A1 - Venter, C. A1 - Verrecchia, F. A1 - Vincent, P. A1 - Wang, X. A1 - Weniger, C. A1 - Wu, X. A1 - Zaharijas, G. A1 - Zampieri, L. A1 - Zane, S. A1 - Zimmer, S. A1 - Zoglauer, A. T1 - Science with e-ASTROGAM A space mission for MeV-GeV gamma-ray astrophysics JF - Journal of High Energy Astrophysics Y1 - 2018 U6 - https://doi.org/10.1016/j.jheap.2018.07.001 SN - 2214-4048 SN - 2214-4056 VL - 19 SP - 1 EP - 106 PB - Elsevier CY - Amsterdam ER - TY - JOUR A1 - Gorski, Mathias A1 - Jung, Bettina A1 - Li, Yong A1 - Matias-Garcia, Pamela R. A1 - Wuttke, Matthias A1 - Coassin, Stefan A1 - Thio, Chris H. L. A1 - Kleber, Marcus E. A1 - Winkler, Thomas W. A1 - Wanner, Veronika A1 - Chai, Jin-Fang A1 - Chu, Audrey Y. A1 - Cocca, Massimiliano A1 - Feitosa, Mary F. A1 - Ghasemi, Sahar A1 - Hoppmann, Anselm A1 - Horn, Katrin A1 - Li, Man A1 - Nutile, Teresa A1 - Scholz, Markus A1 - Sieber, Karsten B. A1 - Teumer, Alexander A1 - Tin, Adrienne A1 - Wang, Judy A1 - Tayo, Bamidele O. A1 - Ahluwalia, Tarunveer S. A1 - Almgren, Peter A1 - Bakker, Stephan J. L. A1 - Banas, Bernhard A1 - Bansal, Nisha A1 - Biggs, Mary L. A1 - Boerwinkle, Eric A1 - Böttinger, Erwin A1 - Brenner, Hermann A1 - Carroll, Robert J. A1 - Chalmers, John A1 - Chee, Miao-Li A1 - Chee, Miao-Ling A1 - Cheng, Ching-Yu A1 - Coresh, Josef A1 - de Borst, Martin H. A1 - Degenhardt, Frauke A1 - Eckardt, Kai-Uwe A1 - Endlich, Karlhans A1 - Franke, Andre A1 - Freitag-Wolf, Sandra A1 - Gampawar, Piyush A1 - Gansevoort, Ron T. A1 - Ghanbari, Mohsen A1 - Gieger, Christian A1 - Hamet, Pavel A1 - Ho, Kevin A1 - Hofer, Edith A1 - Holleczek, Bernd A1 - Foo, Valencia Hui Xian A1 - Hutri-Kahonen, Nina A1 - Hwang, Shih-Jen A1 - Ikram, M. Arfan A1 - Josyula, Navya Shilpa A1 - Kahonen, Mika A1 - Khor, Chiea-Chuen A1 - Koenig, Wolfgang A1 - Kramer, Holly A1 - Kraemer, Bernhard K. A1 - Kuehnel, Brigitte A1 - Lange, Leslie A. A1 - Lehtimaki, Terho A1 - Lieb, Wolfgang A1 - Loos, Ruth J. F. A1 - Lukas, Mary Ann A1 - Lyytikainen, Leo-Pekka A1 - Meisinger, Christa A1 - Meitinger, Thomas A1 - Melander, Olle A1 - Milaneschi, Yuri A1 - Mishra, Pashupati P. A1 - Mononen, Nina A1 - Mychaleckyj, Josyf C. A1 - Nadkarni, Girish N. A1 - Nauck, Matthias A1 - Nikus, Kjell A1 - Ning, Boting A1 - Nolte, Ilja M. A1 - O'Donoghue, Michelle L. A1 - Orho-Melander, Marju A1 - Pendergrass, Sarah A. A1 - Penninx, Brenda W. J. H. A1 - Preuss, Michael H. A1 - Psaty, Bruce M. A1 - Raffield, Laura M. A1 - Raitakari, Olli T. A1 - Rettig, Rainer A1 - Rheinberger, Myriam A1 - Rice, Kenneth M. A1 - Rosenkranz, Alexander R. A1 - Rossing, Peter A1 - Rotter, Jerome A1 - Sabanayagam, Charumathi A1 - Schmidt, Helena A1 - Schmidt, Reinhold A1 - Schoettker, Ben A1 - Schulz, Christina-Alexandra A1 - Sedaghat, Sanaz A1 - Shaffer, Christian M. A1 - Strauch, Konstantin A1 - Szymczak, Silke A1 - Taylor, Kent D. A1 - Tremblay, Johanne A1 - Chaker, Layal A1 - van der Harst, Pim A1 - van der Most, Peter J. A1 - Verweij, Niek A1 - Voelker, Uwe A1 - Waldenberger, Melanie A1 - Wallentin, Lars A1 - Waterworth, Dawn M. A1 - White, Harvey D. A1 - Wilson, James G. A1 - Wong, Tien-Yin A1 - Woodward, Mark A1 - Yang, Qiong A1 - Yasuda, Masayuki A1 - Yerges-Armstrong, Laura M. A1 - Zhang, Yan A1 - Snieder, Harold A1 - Wanner, Christoph A1 - Boger, Carsten A. A1 - Kottgen, Anna A1 - Kronenberg, Florian A1 - Pattaro, Cristian A1 - Heid, Iris M. T1 - Meta-analysis uncovers genome-wide significant variants for rapid kidney function decline JF - Kidney international : official journal of the International Society of Nephrology N2 - Rapid decline of glomerular filtration rate estimated from creatinine (eGFRcrea) is associated with severe clinical endpoints. In contrast to cross-sectionally assessed eGFRcrea, the genetic basis for rapid eGFRcrea decline is largely unknown. To help define this, we meta-analyzed 42 genome-wide association studies from the Chronic Kidney Diseases Genetics Consortium and United Kingdom Biobank to identify genetic loci for rapid eGFRcrea decline. Two definitions of eGFRcrea decline were used: 3 mL/min/1.73m(2)/year or more ("Rapid3"; encompassing 34,874 cases, 107,090 controls) and eGFRcrea decline 25% or more and eGFRcrea under 60 mL/min/1.73m(2) at follow-up among those with eGFRcrea 60 mL/min/1.73m(2) or more at baseline ("CKDi25"; encompassing 19,901 cases, 175,244 controls). Seven independent variants were identified across six loci for Rapid3 and/or CKDi25: consisting of five variants at four loci with genome-wide significance (near UMOD-PDILT (2), PRKAG2, WDR72, OR2S2) and two variants among 265 known eGFRcrea variants (near GATM, LARP4B). All these loci were novel for Rapid3 and/or CKDi25 and our bioinformatic follow-up prioritized variants and genes underneath these loci. The OR2S2 locus is novel for any eGFRcrea trait including interesting candidates. For the five genome-wide significant lead variants, we found supporting effects for annual change in blood urea nitrogen or cystatin-based eGFR, but not for GATM or (LARP4B). Individuals at high compared to those at low genetic risk (8-14 vs. 0-5 adverse alleles) had a 1.20-fold increased risk of acute kidney injury (95% confidence interval 1.08-1.33). Thus, our identified loci for rapid kidney function decline may help prioritize therapeutic targets and identify mechanisms and individuals at risk for sustained deterioration of kidney function. KW - acute kidney injury KW - end-stage kidney disease KW - genome-wide association KW - study KW - rapid eGFRcrea decline Y1 - 2020 U6 - https://doi.org/10.1016/j.kint.2020.09.030 SN - 0085-2538 SN - 1523-1755 VL - 99 IS - 4 SP - 926 EP - 939 PB - Elsevier CY - New York ER - TY - JOUR A1 - Vladova, Gergana A1 - Gronau, Norbert T1 - KI-basierte Assistenzsysteme in betrieblichen Lernprozessen JF - Industrie 4.0 Management : Gegenwart und Zukunft industrieller Geschäftsprozesse N2 - Assistenzsysteme finden im Kontext der digitalen Transformation immer mehr Einsatz. Sie können Beschäftigte in industriellen Produktionsprozessen sowohl in der Anlern- als auch in der aktiven Arbeitsphase unterstützen. Kompetenzen können so arbeitsplatz- und prozessnah sowie bedarfsorientiert aufgebaut werden. In diesem Beitrag wird der aktuelle Forschungsstand zu den Einsatzmöglichkeiten dieser Assistenzsysteme diskutiert und mit Beispielen illustriert. Es werden unter anderem auch Herausforderungen für den Einsatz aufgezeigt. Am Ende des Beitrags werden Potenziale für die zukünftige Nutzung von AS in industriellen Lernprozessen und für die Forschung identifiziert. KW - KI KW - kognitive Assistenzsysteme KW - betriebliche Lernprozesse KW - Weiterbildung Y1 - 2022 U6 - https://doi.org/10.30844/I40M_22-2_11-14 SN - 2364-9216 SN - 2364-9208 VL - 38 IS - 2 SP - 11 EP - 14 PB - GITO mbH Verlag für Industrielle Informationstechnik und Organisation CY - Berlin ER - TY - JOUR A1 - Ahnen, M. L. A1 - Ansoldi, S. A1 - Antonelli, L. A. A1 - Arcaro, C. A1 - Babie, A. A1 - Banerjee, B. A1 - Bangale, P. A1 - de Almeida, U. Barres A1 - Barrio, J. A. A1 - Gonzalez, J. Becerra A1 - Bednarek, W. A1 - Bernardini, E. A1 - Berti, A. A1 - Biasuzzi, B. A1 - Biland, A. A1 - Blanch, O. A1 - Bonnefoy, S. A1 - Bonnoli, G. A1 - Borracci, F. A1 - Carosi, R. A1 - Carosi, A. A1 - Chatterjee, A. A1 - Colin, P. A1 - Colombo, E. A1 - Contreras, J. L. A1 - Cortina, J. A1 - Covino, S. A1 - Cumani, P. A1 - Da Vela, P. A1 - Dazzi, F. A1 - De Angelis, A. A1 - De Lotto, B. A1 - Wilhelmi, E. de Ona A1 - Di Pierro, F. A1 - Doert, M. A1 - Dominguez, A. A1 - Prester, D. Dominis A1 - Dorner, D. A1 - Doro, M. A1 - Einecke, S. A1 - Glawion, D. Eisenacher A1 - Elsaesser, D. A1 - Engelkemeier, M. A1 - Ramazani, V. Fallah A1 - Fernandez-Barra, A. A1 - Fidalgo, D. A1 - Fonseca, M. V. A1 - Font, L. A1 - Fruck, C. A1 - Galindo, D. A1 - Lopez, R. J. Garcia A1 - Garczarczyk, M. A1 - Gaug, M. A1 - Giammaria, P. A1 - Godinovie, N. A1 - Gora, D. A1 - Griffiths, S. A1 - Guberman, D. A1 - Hadasch, D. A1 - Hahn, A. A1 - Hassan, T. A1 - Hayashida, M. A1 - Herrera, J. A1 - Hose, J. A1 - Hrupec, D. A1 - Hughes, G. A1 - Ishio, K. A1 - Konno, Y. A1 - Kubo, H. A1 - Kushida, J. A1 - Kuvezdie, D. A1 - Lelas, D. A1 - Lindfors, E. A1 - Lombardi, S. A1 - Longo, F. A1 - Lopez, M. A1 - Lopez-Oramas, A. A1 - Majumdar, P. A1 - Makariev, M. A1 - Maneva, G. A1 - Manganaro, M. A1 - Mannheim, K. A1 - Maraschi, L. A1 - Mariotti, M. A1 - Martinez, M. A1 - Mazin, D. A1 - Menzel, U. A1 - Minev, M. A1 - Mirzoyan, R. A1 - Moralejo, A. A1 - Moreno, V. A1 - Moretti, E. A1 - Munar-Adrover, P. A1 - Neustroev, V. A1 - Niedzwiecki, A. A1 - Rosillo, M. Nievas A1 - Nilsson, K. A1 - Nishijima, K. A1 - Noda, K. A1 - Nogues, L. A1 - Paiano, S. A1 - Palacio, J. A1 - Paneque, D. A1 - Paoletti, R. A1 - Paredes, J. M. A1 - Paredes-Fortuny, X. A1 - Pedaletti, G. A1 - Peresano, M. A1 - Perri, L. A1 - Persic, M. A1 - Moroni, P. G. Prada A1 - Prandini, E. A1 - Puljak, I. A1 - Garcia, J. R. A1 - Reichardt, I. A1 - Rhode, W. A1 - Riti, M. A1 - Rico, J. A1 - Saito, T. A1 - Satalecka, K. A1 - Schroeder, S. A1 - Schweizer, T. A1 - Shore, S. N. A1 - Sillanpaa, A. A1 - Sitarek, J. A1 - Sobczynskall, D. A1 - Stamerra, A. A1 - Strzys, M. A1 - Surie, T. A1 - Takalo, L. A1 - Tavecchio, F. A1 - Temnikov, P. A1 - Terzie, T. A1 - Tescaro, D. A1 - Teshima, M. A1 - Torres, D. F. A1 - Torres-Alla, N. A1 - Treves, A. A1 - Vanzo, G. A1 - Acosta, M. Vazquez A1 - Vovk, I. A1 - Ward, J. E. A1 - Will, M. A1 - Wu, M. H. A1 - Zarie, D. A1 - Abdalla, Hassan E. A1 - Abramowski, A. A1 - Aharonian, Felix A. A1 - Benkhali, F. Ait A1 - Akhperjanian, A. G. A1 - Andersson, T. A1 - Angüner, Ekrem Oǧuzhan A1 - Arakawa, M. A1 - Arrieta, M. A1 - Aubert, P. A1 - Backes, M. A1 - Balzer, A. A1 - Barnard, M. A1 - Becherini, Y. A1 - Tjus, J. Becker A1 - Berge, D. A1 - Bernhard, S. A1 - Bernlohr, K. A1 - Blackwell, R. A1 - Bottcher, M. A1 - Boisson, C. A1 - Bolmont, J. A1 - Bordas, Pol A1 - Bregeon, J. A1 - Brun, F. A1 - Brun, P. A1 - Bryan, M. A1 - Btichele, M. A1 - Bulik, T. A1 - Capasso, M. A1 - Carr, J. A1 - Casanova, Sabrina A1 - Cerruti, M. A1 - Chakraborty, N. A1 - Chalme-Calvet, R. A1 - Chaves, R. C. G. A1 - Chen, A. A1 - Chevalier, J. A1 - Chretien, M. A1 - Coffaro, M. A1 - Colafrancesco, S. A1 - Cologna, G. A1 - Condon, B. A1 - Conrad, J. A1 - Cui, Y. A1 - Davids, I. D. A1 - Decock, J. A1 - Degrange, B. A1 - Dei, C. A1 - Devin, J. A1 - Dewilt, P. A1 - Dirson, L. A1 - Djannati-Atai, A. A1 - Domainko, W. A1 - Donath, A. A1 - Dutson, K. A1 - Dyks, J. A1 - Edwards, T. A1 - Egberts, Kathrin A1 - Eger, P. A1 - Ernenwein, J. -P. A1 - Eschbach, S. A1 - Farnier, C. A1 - Fegan, S. A1 - Fernandes, M. V. A1 - Fiasson, A. A1 - Fontaine, G. A1 - Forster, A. A1 - Funk, S. A1 - Ftifiling, M. A1 - Gabici, S. A1 - Gajdus, M. A1 - Gallant, Y. A. A1 - Garrigoux, T. A1 - Giavitto, G. A1 - Giebels, B. A1 - Glicenstein, J. F. A1 - Gottschal, D. A1 - Goya, A. A1 - Grondin, M. -H. A1 - Hahn, J. A1 - Haupt, M. A1 - Hawkes, J. A1 - Heinzelmann, G. A1 - Henri, G. A1 - Hermann, G. A1 - Hervet, O. A1 - Hinton, J. A. A1 - Hofmann, W. A1 - Hoischen, Clemens A1 - Holler, M. A1 - Horns, D. A1 - Ivascenko, A. A1 - Iwasaki, H. A1 - Jacholkowska, A. A1 - Jamrozy, M. A1 - Janiak, M. A1 - Jankowsky, D. A1 - Jankowsky, F. A1 - Jingo, M. A1 - Jogler, T. A1 - Jouvin, L. A1 - Jung-Richardt, I. A1 - Kastendieck, M. A. A1 - Katarzyfiski, K. A1 - Katsuragawa, M. A1 - Katz, U. A1 - Kerszberg, D. A1 - Khangulyan, D. A1 - Khelifi, B. A1 - Kieffer, M. A1 - King, J. A1 - Klepser, S. A1 - Klochkov, D. A1 - Kluiniak, W. A1 - Kolitzus, D. A1 - Komin, Nu. A1 - Kosack, K. A1 - Krakau, S. A1 - Kraus, M. A1 - Krtiger, P. P. A1 - Laffon, H. A1 - Lamanna, G. A1 - Lau, J. A1 - Lees, J. -P. A1 - Lefaucheur, J. A1 - Lefranc, V. A1 - Lemiere, A. A1 - Lemoine-Goumard, M. A1 - Lenain, J. -P. A1 - Leser, Eva A1 - Lohse, T. A1 - Lorentz, M. A1 - Liu, R. A1 - Lopez-Coto, R. A1 - Lypova, I. A1 - Marandon, V. A1 - Marcowith, Alexandre A1 - Mariaud, C. A1 - Marx, R. A1 - Maurin, G. A1 - Maxted, N. A1 - Mayer, M. A1 - Meintjes, P. J. A1 - Meyer, M. A1 - Mitche, A. M. W. A1 - Moderski, R. A1 - Mohamed, M. A1 - Mohrmann, L. A1 - Mora, K. A1 - Moulin, Emmanuel A1 - Murach, T. A1 - Nakashima, S. A1 - De Naurois, M. A1 - Niederwanger, F. A1 - Niemiec, J. A1 - Oakes, L. A1 - Odaka, H. A1 - Ott, S. A1 - Ohm, S. A1 - Ostrowski, M. A1 - Oya, I. A1 - Padovani, M. A1 - Panter, M. A1 - Parsons, R. D. A1 - Pekeur, N. W. A1 - Pelletier, G. A1 - Perennes, C. A1 - Petrucci, P. -O. A1 - Peyaud, B. A1 - Pie, Q. A1 - Pita, S. A1 - Poon, H. A1 - Prokhorov, D. A1 - Prokoph, H. A1 - Ptffilhofer, G. A1 - Punch, M. A1 - Quirrenbach, A. A1 - Raab, S. A1 - Reimer, A. A1 - Reimer, O. A1 - Renaud, M. A1 - De Los Reyes, R. A1 - Richter, S. A1 - Rieger, F. A1 - Romoli, C. A1 - Rowell, G. A1 - Rudak, B. A1 - Rulten, C. B. A1 - Safi-Harb, S. A1 - Sahakian, V. A1 - Saito, S. A1 - Salek, D. A1 - Sanchez, D. A. A1 - Santangelo, Andrea A1 - Sasaki, M. A1 - Schlickeiser, R. A1 - Schtissler, F. A1 - Schulz, A. A1 - Schwanke, U. A1 - Schwemmer, S. A1 - Seglar-Arroyo, M. A1 - Settimo, M. A1 - Seyffert, A. S. A1 - Shafi, N. A1 - Shilon, I. A1 - Simoni, R. A1 - So, H. A1 - Spanier, F. A1 - Spengler, G. A1 - Spies, F. A1 - Stawarz, L. A1 - Steenkamp, R. A1 - Stegmann, Christian A1 - Stycz, K. A1 - Sushch, I. A1 - Takahashi, T. A1 - Tavernet, J. -P. A1 - Tavernier, T. A1 - Taylor, A. M. A1 - Terrier, R. A1 - Tibaldo, L. A1 - Tiziani, D. A1 - Tluczykont, M. A1 - Trichard, C. A1 - Tsuji, N. A1 - Tuffs, R. A1 - Uchiyama, Y. A1 - Van der Walt, D. J. A1 - Van Eldik, C. A1 - Van Rensburg, C. A1 - Van Soelen, B. A1 - Vasileiadis, G. A1 - Veh, J. A1 - Venter, C. A1 - Viana, A. A1 - Vincent, P. A1 - Vink, J. A1 - Voisin, F. A1 - Vok, H. J. A1 - Vuillaume, T. A1 - Wadiasingh, Z. A1 - Wagner, S. J. A1 - Wagner, P. A1 - Wagner, R. M. A1 - White, R. A1 - Wierzcholska, A. A1 - Willmann, P. A1 - Wornlein, A. A1 - Wouters, D. A1 - Yang, R. A1 - Zabalza, V. A1 - Zaborov, D. A1 - Zacharias, M. A1 - Zanin, R. A1 - Zdziarski, A. A. A1 - Zech, Alraune A1 - Zefi, F. A1 - Ziegler, A. A1 - Zywuckan, N. T1 - Constraints on particle acceleration in SS433/W50 from MAGIC and HESS observations JF - Astronomy and astrophysics : an international weekly journal N2 - Context. The large jet kinetic power and non-thermal processes occurring in the microquasar SS 433 make this source a good candidate for a very high-energy (VHE) gamma-ray emitter. Gamma-ray fluxes above the sensitivity limits of current Cherenkov telescopes have been predicted for both the central X-ray binary system and the interaction regions of SS 433 jets with the surrounding W50 nebula. Non-thermal emission at lower energies has been previously reported, indicating that efficient particle acceleration is taking place in the system. Aims. We explore the capability of SS 433 to emit VHE gamma rays during periods in which the expected flux attenuation due to periodic eclipses (P-orb similar to 13.1 days) and precession of the circumstellar disk (P-pre similar to 162 days) periodically covering the central binary system is expected to be at its minimum. The eastern and western SS 433/W50 interaction regions are also examined using the whole data set available. We aim to constrain some theoretical models previously developed for this system with our observations. Methods. We made use of dedicated observations from the Major Atmospheric Gamma Imaging Cherenkov telescopes (MAGIC) and High Energy Spectroscopic System (H.E.S.S.) of SS 433 taken from 2006 to 2011. These observation were combined for the first time and accounted for a total effective observation time of 16.5 h, which were scheduled considering the expected phases of minimum absorption of the putative VHE emission. Gamma-ray attenuation does not affect the jet/medium interaction regions. In this case, the analysis of a larger data set amounting to similar to 40-80 h, depending on the region, was employed. Results. No evidence of VHE gamma-ray emission either from the central binary system or from the eastern/western interaction regions was found. Upper limits were computed for the combined data set. Differential fluxes from the central system are found to be less than or similar to 10(-12)-10(-13) TeV-1 cm(-2) s(-1) in an energy interval ranging from similar to few x 100 GeV to similar to few TeV. Integral flux limits down to similar to 10(-12)-10(-13) ph cm(-2) s(-1) and similar to 10(-13)-10(-14) ph cm(-2) s(-1) are obtained at 300 and 800 GeV, respectively. Our results are used to place constraints on the particle acceleration fraction at the inner jet regions and on the physics of the jet/medium interactions. Conclusions. Our findings suggest that the fraction of the jet kinetic power that is transferred to relativistic protons must be relatively small in SS 433, q(p) <= 2.5 x 10(-5), to explain the lack of TeV and neutrino emission from the central system. At the SS 433/W50 interface, the presence of magnetic fields greater than or similar to 10 mu G is derived assuming a synchrotron origin for the observed X-ray emission. This also implies the presence of high-energy electrons with E-e up to 50 TeV, preventing an efficient production of gamma-ray fluxes in these interaction regions. KW - gamma rays: general KW - stars: black holes KW - X-rays: binaries KW - ISM: jets and outflows Y1 - 2018 U6 - https://doi.org/10.1051/0004-6361/201731169 SN - 1432-0746 VL - 612 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Abdalla, Hassan E. A1 - Collaboration, H. E. S. S. A1 - Abramowski, A. A1 - Aharonian, Felix A. A1 - Benkhali, F. Ait A1 - Angüner, Ekrem Oǧuzhan A1 - Arakawa, M. A1 - Armand, C. A1 - Arrieta, M. A1 - Backes, M. A1 - Balzer, A. A1 - Barnard, M. A1 - Becherini, Y. A1 - Tjus, J. Becker A1 - Berge, D. A1 - Bernhard, S. A1 - Bernloehr, K. A1 - Blackwell, R. A1 - Bottcher, M. A1 - Boisson, C. A1 - Bolmont, J. A1 - Bonnefoy, S. A1 - Bordas, Pol A1 - Bregeon, J. A1 - Brun, F. A1 - Brun, P. A1 - Bryan, M. A1 - Buechele, M. A1 - Bulik, T. A1 - Capasso, M. A1 - Caroff, S. A1 - Carosi, A. A1 - Casanova, Sabrina A1 - Cerruti, M. A1 - Chakraborty, N. A1 - Chaves, R. C. G. A1 - Chen, A. A1 - Chevalier, J. A1 - Colafrancesco, S. A1 - Condon, B. A1 - Conrad, J. A1 - Davids, I. D. A1 - Decock, J. A1 - Deil, C. A1 - Devin, J. A1 - deWilt, P. A1 - Dirson, L. A1 - Djannati-Atai, A. A1 - Donath, A. A1 - Dyks, J. A1 - Edwards, T. A1 - Egberts, Kathrin A1 - Emery, G. A1 - Ernenwein, J. -P. A1 - Eschbach, S. A1 - Farnier, C. A1 - Fegan, S. A1 - Fernandes, M. V. A1 - Fiasson, A. A1 - Fontaine, G. A1 - Funk, S. A1 - Fuessling, M. A1 - Gabici, S. A1 - Gallant, Y. A. A1 - Garrigoux, T. A1 - Gate, F. A1 - Giavitto, G. A1 - Glawion, D. A1 - Glicenstein, J. F. A1 - Gottschall, D. A1 - Grondin, M. -H. A1 - Hahn, J. A1 - Haupt, M. A1 - Hawkes, J. A1 - Heinzelmann, G. A1 - Henri, G. A1 - Hermann, G. A1 - Hinton, J. A. A1 - Hofmann, W. A1 - Hoischen, Clemens A1 - Holch, T. L. A1 - Holler, M. A1 - Horns, D. A1 - Ivascenko, A. A1 - Iwasaki, H. A1 - Jacholkowska, A. A1 - Jamrozy, M. A1 - Jankowsky, D. A1 - Jankowsky, F. A1 - Jingo, M. A1 - Jouvin, L. A1 - Jung-Richardt, I. A1 - Kastendieck, M. A. A1 - Katarzynski, K. A1 - Katsuragawa, M. A1 - Katz, U. A1 - Kerszberg, D. A1 - Khangulyan, D. A1 - Khelifi, B. A1 - King, J. A1 - Klepser, S. A1 - Klochkov, D. A1 - Kluzniak, W. A1 - Komin, Nu. A1 - Kosack, K. A1 - Krakau, S. A1 - Kraus, M. A1 - Kruger, P. P. A1 - Laffon, H. A1 - Lamanna, G. A1 - Lau, J. A1 - Lefaucheur, J. A1 - Lemiere, A. A1 - Lemoine-Goumard, M. A1 - Lenain, J. -P. A1 - Leser, Eva A1 - Lohse, T. A1 - Lorentz, M. A1 - Liu, R. A1 - Lopez-Coto, R. A1 - Lypova, I. A1 - Malyshev, D. A1 - Marandon, V. A1 - Marcowith, Alexandre A1 - Mariaud, C. A1 - Marx, R. A1 - Maurin, G. A1 - Maxted, N. A1 - Mayer, M. A1 - Meintjes, P. J. A1 - Meyer, M. A1 - Mitchell, A. M. W. A1 - Moderski, R. A1 - Mohamed, M. A1 - Mohrmann, L. A1 - Mora, K. A1 - Moulin, Emmanuel A1 - Murach, T. A1 - Nakashima, S. A1 - de Naurois, M. A1 - Ndiyavala, H. A1 - Niederwanger, F. A1 - Niemiec, J. A1 - Oakes, L. A1 - Odaka, H. A1 - Ohm, S. A1 - Ostrowski, M. A1 - Oya, I. A1 - Padovani, M. A1 - Panter, M. A1 - Parsons, R. D. A1 - Pekeur, N. W. A1 - Pelletier, G. A1 - Perennes, C. A1 - Petrucci, P. -O. A1 - Peyaud, B. A1 - Piel, Q. A1 - Pita, S. A1 - Poireau, V. A1 - Prokhorov, D. A. A1 - Prokoph, H. A1 - Puehlhofer, G. A1 - Punch, M. A1 - Quirrenbach, A. A1 - Raab, S. A1 - Rauth, R. A1 - Reimer, A. A1 - Reimer, O. A1 - Renaud, M. A1 - de los Reyes, R. A1 - Rieger, F. A1 - Rinchiuso, L. A1 - Romoli, C. A1 - Rowell, G. A1 - Rudak, B. A1 - Rulten, C. B. A1 - Sahakian, V. A1 - Saito, S. A1 - Sanchez, D. A. A1 - Santangelo, Andrea A1 - Sasaki, M. A1 - Schlickeiser, R. A1 - Schussler, F. A1 - Schulz, A. A1 - Schwanke, U. A1 - Schwemmer, S. A1 - Seglar-Arroyo, M. A1 - Seyffert, A. S. A1 - Shafi, N. A1 - Shilon, I. A1 - Shiningayamwe, K. A1 - Simoni, R. A1 - Sol, H. A1 - Spanier, F. A1 - Spir-Jacob, M. A1 - Stawarz, L. A1 - Steenkamp, R. A1 - Stegmann, Christian A1 - Steppa, Constantin Beverly A1 - Sushch, I. A1 - Takahashi, T. A1 - Tavernet, J. -P. A1 - Tavernier, T. A1 - Taylor, A. M. A1 - Terrier, R. A1 - Tibaldo, L. A1 - Tiziani, D. A1 - Tluczykont, M. A1 - Trichard, C. A1 - Tsirou, M. A1 - Tsuji, N. A1 - Tuffs, R. A1 - Uchiyama, Y. A1 - van der Walt, D. J. A1 - van Eldik, C. A1 - van Rensburg, C. A1 - van Soelen, B. A1 - Vasileiadis, G. A1 - Veh, J. A1 - Venter, C. A1 - Viana, A. A1 - Vincent, P. A1 - Vink, J. A1 - Voisin, F. A1 - Voelk, H. J. A1 - Vuillaume, T. A1 - Wadiasingh, Z. A1 - Wagner, S. J. A1 - Wagner, P. A1 - Wagner, R. M. A1 - White, R. A1 - Wierzcholska, A. A1 - Willmann, P. A1 - Woernlein, A. A1 - Wouters, D. A1 - Yang, R. A1 - Zaborov, D. A1 - Zacharias, M. A1 - Zanin, R. A1 - Zdziarski, A. A. A1 - Zech, Alraune A1 - Zefi, F. A1 - Ziegler, A. A1 - Zorn, J. A1 - Zywucka, N. T1 - Detection of variable VHE gamma-ray emission from the extra-galactic gamma-ray binary LMC P3 JF - Astronomy and astrophysics : an international weekly journal N2 - Context. Recently, the high-energy (HE, 0.1-100 GeV) gamma-ray emission from the object LMC P3 in the Large Magellanic Cloud (LMC) has been discovered to be modulated with a 10.3-day period, making it the first extra-galactic gamma-ray binary. Aims. This work aims at the detection of very-high-energy (VHE, >100 GeV) gamma-ray emission and the search for modulation of the VHE signal with the orbital period of the binary system. Methods. LMC P3 has been observed with the High Energy Stereoscopic System (H.E.S.S.); the acceptance-corrected exposure time is 100 h. The data set has been folded with the known orbital period of the system in order to test for variability of the emission. Results. VHE gamma-ray emission is detected with a statistical significance of 6.4 sigma. The data clearly show variability which is phase-locked to the orbital period of the system. Periodicity cannot be deduced from the H.E.S.S. data set alone. The orbit-averaged luminosity in the 1-10 TeV energy range is (1.4 +/- 0.2) x 10(35) erg s(-1). A luminosity of (5 +/- 1) x 10(35) erg s(-1) is reached during 20% of the orbit. HE and VHE gamma-ray emissions are anti-correlated. LMC P3 is the most luminous gamma-ray binary known so far. KW - gamma rays: stars KW - binaries: general KW - stars: massive Y1 - 2018 U6 - https://doi.org/10.1051/0004-6361/201732426 SN - 1432-0746 VL - 610 PB - EDP Sciences CY - Les Ulis ER - TY - GEN A1 - Braun, David R. A1 - Aldeias, Vera A1 - Archer, Will A1 - Arrowsmith, J. Ramon A1 - Baraki, Niguss A1 - Campisano, Christopher J. A1 - Deino, Alan L. A1 - DiMaggio, Erin N. A1 - Dupont-Nivet, Guillaume A1 - Engda, Blade A1 - Feary, David A. A1 - Garello, Dominique I. A1 - Kerfelew, Zenash A1 - McPherron, Shannon P. A1 - Patterson, David B. A1 - Reeves, Jonathan S. A1 - Thompson, Jessica C. A1 - Reed, Kaye E. T1 - Reply to Sahle and Gossa: Technology and geochronology at the earliest known Oldowan site at Ledi-Geraru, Ethiopia T2 - Proceedings of the National Academy of Sciences of the United States of America Y1 - 2019 U6 - https://doi.org/10.1073/pnas.1911952116 SN - 0027-8424 N1 - Letter VL - 116 IS - 41 SP - 20261 EP - 20262 PB - National Acad. of Sciences CY - Washington ER - TY - JOUR A1 - Bender, Benedict A1 - Lewandowski, Stefanie T1 - Potenziale plattformbasierter Geschäftsmodelle im Kunststoffspritzguss T1 - Potential of platform-based business models in the plastics industry JF - Industrie 4.0 Management : Gegenwart und Zukunft industrieller Geschäftsprozesse N2 - Die Potenziale plattformbasierter Geschäftsmodelle im Kontext von Industrie 4.0 sind bisher nicht vollständig erschlossen. Ansatzpunkte für Plattformen und ökosystembasierte Wertschöpfung variieren zwischen Industrien. Die Kunststoffindustrie ist dahingehend bisher weitestgehend unberücksichtigt. Aufgrund der Industriestruktur, insb. der einheitlichen Wertschöpfungsstrukturen eignet sich die Kunststoffindustrie für den Einsatz digitaler Plattformen. Neben Ansätzen für Plattformen in der Spritzgussindustrie bietet der Beitrag ein Vorgehensmodell für die Erweiterung etablierte Geschäftsmodelle. Somit kann der Einstieg in plattformbasierte Geschäftsmodelle für KMUs erleichtert werden. N2 - The potential of platform-based business models in the context of Industry 4.0 has not yet been fully realized. Approaches for platforms and ecosystem-based value creation vary between industries. The plastics industry has so far been widely ignored in this respect. Due to its industrial structure, in particular the uniform value creation structures, the plastics industry is suitable for digital platforms. In addition to approaches for platforms in the injection molding industry, the article offers a procedure model for the expansion of established business models. This can facilitate the entry into the field of platform-based business models for SMEs. KW - Digitale Plattformen KW - plattformbasierte Geschäftsmodelle KW - Kunststoffindustrie KW - Plattform Ökosystem KW - Potenziale KW - Industrie 4.0 KW - digital platforms KW - platform-based business models KW - plastics industry KW - platform ecosystem KW - potentials KW - Industry 4.0 Y1 - 2022 U6 - https://doi.org/10.30844/IM_22-6_14-18 SN - 2364-9208 SN - 2364-9216 VL - 38 IS - 6 SP - 14 EP - 18 PB - GITO mbH Verlag CY - Berlin ER - TY - JOUR A1 - Ganghof, Steffen A1 - Eppner, Sebastian A1 - Pörschke, Alexander T1 - Australian bicameralism as semi-parliamentarism BT - patterns of majority formation in 29 democracies JF - Australian Journal of Political Science N2 - The article analyses the type of bicameralism we find in Australia as a distinct executive-legislative system – a hybrid between parliamentary and presidential government – which we call ‘semi-parliamentary government’. We argue that this hybrid presents an important and underappreciated alternative to pure parliamentary government as well as presidential forms of the power-separation, and that it can achieve a certain balance between competing models or visions of democracy. We specify theoretically how the semi-parliamentary separation of powers contributes to the balancing of democratic visions and propose a conceptual framework for comparing democratic visions. We use this framework to locate the Australian Commonwealth, all Australian states and 22 advanced democratic nation-states on a two-dimensional empirical map of democratic patterns for the period from 1995 to 2015. KW - Executive-legislative relations KW - bicameralism KW - parliamentary government KW - presidential government KW - visions of democracy Y1 - 2018 U6 - https://doi.org/10.1080/10361146.2018.1451487 SN - 1036-1146 SN - 1363-030X VL - 53 IS - 2 SP - 211 EP - 233 PB - Routledge, Taylor & Francis Group CY - Abingdon ER - TY - JOUR A1 - Deino, Alan L. A1 - Sier, Mark Jan A1 - Garello, Dominique A1 - Keller, B. A1 - Kingston, John A1 - Scott, Jennifer J. A1 - Dupont-Nivet, Guillaume A1 - Cohen, Andrew T1 - Chronostratigraphy of the Baringo-Tugen-Barsemoi (HSPDP-BTB13-1A) core-Ar-40/Ar-39 dating, magnetostratigraphy, tephrostratigraphy, sequence stratigraphy and Bayesian age modeling JF - Palaeogeography, palaeoclimatology, palaeoecology : an international journal for the geo-sciences N2 - The Baringo-Tugen-Barsemoi 2013 drillcore (BTB13), acquired as part of the Hominin Sites and Paleolakes Drilling Project, recovered 228 m of fluviolacustrine sedimentary rocks and tuffs spanning a similar to 3.29-2.56 Ma interval of the highly fossiliferous and hominin-bearing Chemeron Formation, Tugen Hills, Kenya. Here we present a Bayesian stratigraphic age model for the core employing chronostratigraphic control points derived from Ar-40/Ar-39 dating of tuffs from core and outcrop, Ar-40/Ar-39 age calibration of related outcrop diatomaceous units, and core magnetostratigraphy. The age model reveals three main intervals with distinct sediment accumulation rates: an early rapid phase from 3.2 to 2.9 Ma; a relatively slow phase from 2.9 to 2.7 Ma; and the highest rate of accumulation from 2.7 to 2.6 Ma. The intervals of rapid accumulation correspond to periods of high Earth orbital eccentricity, whereas the slow accumulation interval corresponds to low eccentricity at 2.9-2.7 Ma, suggesting that astronomically mediated climate processes may be responsible for the observed changes in sediment accumulation rate. Lacustrine transgression-regression events, as delineated using sequence stratigraphy, dominantly operate on precession scale, particularly within the high eccentricity periods. A set of erosively based fluvial conglomerates correspond to the 2.9-2.7 Ma interval, which could be related to either the depositional response to low eccentricity or to the development of unconformities due to local tectonic activity. Age calibration of core magnetic susceptibility and gamma density logs indicates a close temporal correspondence between a shift from high- to low-frequency signal variability at similar to 3 Ma, approximately coincident the end of the mid-Piacenzian Warm Period, and the beginning of the cooling of world climate leading to the initiation of Northern Hemispheric glaciation c. 2.7 Ma. BTB13 and the Baringo Basin records may thus provide evidence of a connection between high-latitude glaciation and equatorial terrestrial climate toward the end of the Pliocene. KW - Chemeron Formation KW - Pliocene KW - Eccentricity KW - Precession KW - Paleoclimate KW - Paleolimnology Y1 - 2019 U6 - https://doi.org/10.1016/j.palaeo.2019.109258 SN - 0031-0182 SN - 1872-616X VL - 532 PB - Elsevier CY - Amsterdam ER - TY - JOUR A1 - Mühlenbruch, Marco A1 - Grossart, Hans-Peter A1 - Eigemann, Falk A1 - Voss, Maren T1 - Mini-review: Phytoplankton-derived polysaccharides in the marine environment and their interactions with heterotrophic bacteria JF - Environmental microbiology N2 - Within the wealth of molecules constituting marine dissolved organic matter, carbohydrates make up the largest coherent and quantifiable fraction. Their main sources are from primary producers, which release large amounts of photosynthetic products – mainly polysaccharides – directly into the surrounding water via passive and active exudation. The organic carbon and other nutrients derived from these photosynthates enrich the ‘phycosphere’ and attract heterotrophic bacteria. The rapid uptake and remineralization of dissolved free monosaccharides by heterotrophic bacteria account for the barely detectable levels of these compounds. By contrast, dissolved combined polysaccharides can reach high concentrations, especially during phytoplankton blooms. Polysaccharides are too large to be taken up directly by heterotrophic bacteria, instead requiring hydrolytic cleavage to smaller oligo- or monomers by bacteria with a suitable set of exoenzymes. The release of diverse polysaccharides by various phytoplankton taxa is generally interpreted as the deposition of excess organic material. However, these molecules likely also fulfil distinct, yet not fully understood functions, as inferred from their active modulation in terms of quality and quantity when phytoplankton becomes nutrient limited or is exposed to heterotrophic bacteria. This minireview summarizes current knowledge regarding the exudation and composition of phytoplankton-derived exopolysaccharides and acquisition of these compounds by heterotrophic bacteria. Y1 - 2018 U6 - https://doi.org/10.1111/1462-2920.14302 SN - 1462-2912 SN - 1462-2920 VL - 20 IS - 8 SP - 2671 EP - 2685 PB - Wiley CY - Hoboken ER - TY - JOUR A1 - Rojas-Jimenez, Keilor A1 - Fonvielle, Jeremy Andre A1 - Ma, Hua A1 - Grossart, Hans-Peter T1 - Transformation of humic substances by the freshwater Ascomycete Cladosporium sp. JF - Waterbird N2 - The ecological relevance of fungi in freshwater ecosystems is becoming increasingly evident, particularly in processing the extensive amounts of polymeric organic carbon such as cellulose, chitin, and humic substances (HS). We isolated several fungal strains from oligo-mesotrophic Lake Stechlin, Brandenburg, Germany, and analyzed their ability to degrade polymeric-like substrates. Using liquid chromatography-organic carbon detection, we determined the byproducts of HS transformation by the freshwater fungus Cladosporium sp. KR14. We demonstrate the ability of this fungus to degrade and simultaneously synthesize HS, and that transformation processes were intensified when iron, as indicator of the occurrence of Fenton reactions, was present in the medium. Furthermore, we showed that structural complexity of the HS produced changed with the availability of other polymeric substances in the medium. Our study highlights the contribution of freshwater Ascomycetes to the transformation of complex organic compounds. As such, it has important implications for understanding the ecological contribution of fungi to aquatic food webs and related biogeochemical cycles. Y1 - 2017 U6 - https://doi.org/10.1002/lno.10545 SN - 1524-4695 SN - 1938-5390 VL - 40 SP - 282 EP - 288 PB - Waterbird SOC CY - Washington ER - TY - JOUR A1 - Perscheid, Michael A1 - Plattner, Hasso A1 - Ritter, Daniel A1 - Schlosser, Rainer A1 - Teusner, Ralf T1 - Enterprise platform and integration concepts research at HPI JF - SIGMOD record N2 - The Hasso Plattner Institute (HPI), academically structured as the independent Faculty of Digital Engineering at the University of Potsdam, unites computer science research and teaching with the advantages of a privately financed institute and a tuition-free study program. Founder and namesake of the institute is the SAP co-founder Hasso Plattner, who also heads the Enterprise Platform and Integration Concepts (EPIC) research center which focuses on the technical aspects of business software with a vision to provide the fastest way to get insights out of enterprise data. Founded in 2006, the EPIC combines three research groups comprising autonomous data management, enterprise software engineering, and data-driven decision support. Y1 - 2023 U6 - https://doi.org/10.1145/3582302.3582322 SN - 0163-5808 SN - 1943-5835 VL - 51 IS - 4 SP - 68 EP - 73 PB - Association for Computing Machinery CY - New York ER - TY - JOUR A1 - Schmalzgruber, Hedwig T1 - Niklas Holzberg, Avian/Romulus. Fabelsammlungen der Spätantike, lateinisch – deutsch, Sammlung Tusculum, Berlin-Boston: De Gruyter, 2022, 237 pp., 39.95 €, ISBN 978-3-11-075705-7, https://doi.org/10.1515/9783110757064 JF - Exemplaria classica Y1 - 2022 SN - 1699-3225 SN - 2173-6839 VL - 26 SP - 390 EP - 397 PB - Universidad de Huelva CY - Huelva ER - TY - GEN A1 - Brand, Ralf A1 - Timme, Sinika T1 - Physical inactivity or exercise? A simple decision test predicts exercise behavior over the next 14 days T2 - Journal of sport & exercise psychology Y1 - 2022 U6 - https://doi.org/10.1123/jsep.2022-0071 SN - 0895-2779 SN - 1543-2904 VL - 44 IS - S1 SP - S68 EP - S68 PB - Human Kinetics Publishing CY - Champaign ER - TY - RPRT A1 - Angenendt, Steffen A1 - Koch, Anne A1 - Tjaden, Jasper T1 - Predicting irregular migration BT - SWP research paper T2 - high hopes, meagre results N2 - German and European migration policy operates in permanent crisis mode. Sudden increases in irregular immigration create a sense of loss of control, which is instrumentalised by populist forces. This has generated great interest in quantitative migration predictions. High expectations are placed in the AI-based tools currently under devel­op­ment for forecasting irregular migration. The potential applications of these tools are manifold. They range from managing and strengthening the EU's reception capacity and border protections to configuring humanitarian aid provision and longer-term planning of development programmes. There is a significant gap between the expectations placed in the new instruments and their practical utility. Technical limits exist, medium-term forecasts are methodologically implausible, and channels for feeding the results into political decision-making processes are lacking. The great demand for predictions is driven by the political functions of migration prediction, which include its uses in political communication, funding acquisition and legitimisation of political decisions. Investment in the quality of the underlying data will be more productive than developing a succession of new prediction tools. Funding for applications in emergency relief and development cooperation should be prioritised. Crisis early warning and risk analysis should also be strengthened and their networking improved. KW - Migration KW - Migrationspolitik KW - Wanderungsprognosen KW - Vorhersage KW - Vorausschau KW - displacement forecasting KW - Krisenfrüherkennung KW - Risikoanalyse KW - Künstliche Intelligenz KW - maschinelles Lernen KW - Agentenbasierte Modellierung KW - predicting irregular migration KW - forecast KW - quantitative migration prediction KW - UNHCR KW - IOM KW - Frontex Risk Analysis Network (FRAN) KW - Common Integrated Risk Analysis Model (CIRAM) KW - Emergency Response Coordination Centre (ERCC) KW - Frontex KW - Pact on Migration and Asylum Y1 - 2023 U6 - https://doi.org/10.18449/2023RP11 SN - 2747-5115 SN - 1611-6372 VL - 11 PB - Stiftung Wissenschaft und Politik (SWP) CY - Berlin ER - TY - RPRT A1 - Angenendt, Steffen A1 - Koch, Anne A1 - Tjaden, Jasper T1 - Die Prognose ungeregelter Wanderungen BT - große Erwartungen, begrenzter Nutzen T2 - SWP-Studie N2 - Die deutsche und europäische Migrationspolitik befindet sich im permanenten Krisenmodus. Plötzliche Anstiege ungeregelter Zuwanderung nähren ein Gefühl von Kontrollverlust, das wiederum von populistischen Kräften instrumentalisiert wird. Daher hat die Politik großes Interesse an quantitativen Migrationsprognosen. Besondere Erwartungen wecken KI-gestützte Instrumente zur Vorhersage ungeregelter Wanderungsbewegungen, wie sie zurzeit entwickelt werden. Die Anwendungsfelder dieser Instrumente sind vielfältig. Sie reichen von einer Stärkung der Aufnahmekapazitäten in der EU über die präventive Verschärfung von Grenzschutzmaßnahmen und eine bedarfsgerechte Bereitstellung von Ressourcen in humanitären Krisen bis zur längerfristigen entwicklungspolitischen Programmplanung. Allerdings besteht eine deutliche Kluft zwischen den Erwartungen an die neuen Instrumente und ihrem praktischen Mehrwert. Zum einen sind die technischen Möglichkeiten begrenzt, und mittelfristige Vorhersagen zu ungeregelten Wanderungen sind methodisch kaum möglich. Zum anderen mangelt es an Verfahren, um die Ergebnisse in politische Entscheidungsprozesse einfließen zu lassen. Die hohe Nachfrage nach Prognosen erklärt sich aus den politischen Funktionen quantitativer Migrationsvorhersage - beispielsweise ihrem Potential für die politische Kommunikation, die Mitteleinwerbung und die Legitimierung politischer Entscheidungen. Investitionen in die Qualität der den Prognosen zugrunde liegenden Daten sind sinnvoller als die Entwicklung immer neuer Instrumente. Bei der Mittelvergabe für Prognosen sollten Anwendungen in der Nothilfe und der Entwicklungszusammenarbeit priorisiert werden. Zudem sollten die Krisenfrüherkennung und die Risikoanalyse gestärkt werden, und die beteiligten Akteure sollten sich besser vernetzen. KW - Migration KW - Migrationspolitik KW - Wanderungsprognosen KW - Vorhersage KW - Vorausschau KW - Displacement Forecasting KW - Krisenfrüherkennung KW - Risikoanalyse KW - Künstliche Intelligenz KW - maschinelles Lernen KW - Agentenbasierte Modellierung Y1 - 2023 U6 - https://doi.org/10.18449/2023S10 SN - 2747-5115 SN - 1611-6372 VL - 10 PB - Stiftung Wissenschaft und Politik (SWP) CY - Berlin ER - TY - JOUR A1 - Zhu, Hui A1 - Chen, Lunjin A1 - Liu, Xu A1 - Shprits, Yuri T1 - Modulation of locally generated equatorial noise by ULF wave JF - Journal of geophysical research : Space physics N2 - In this paper we report a rare and fortunate event of fast magnetosonic (MS, also called equatorial noise) waves modulated by compressional ultralow frequency (ULF) waves measured by Van Allen Probes. The characteristics of MS waves, ULF waves, proton distribution, and their potential correlations are analyzed. The results show that ULF waves can modulate the energetic ring proton distribution and in turn modulate the MS generation. Furthermore, the variation of MS intensities is attributed to not only ULF wave activities but also the variation of background parameters, for example, number density. The results confirm the opinion that MS waves are generated by proton ring distribution and propose a new modulation phenomenon. Y1 - 2019 U6 - https://doi.org/10.1029/2018JA026199 SN - 2169-9380 SN - 2169-9402 VL - 124 IS - 4 SP - 2779 EP - 2787 PB - American Geophysical Union CY - Washington ER - TY - JOUR A1 - Cabalar, Pedro A1 - Kaminski, Roland A1 - Schaub, Torsten A1 - Schuhmann, Anna T1 - Temporal answer set programming on finite traces JF - Theory and practice of logic programming N2 - In this paper, we introduce an alternative approach to Temporal Answer Set Programming that relies on a variation of Temporal Equilibrium Logic (TEL) for finite traces. This approach allows us to even out the expressiveness of TEL over infinite traces with the computational capacity of (incremental) Answer Set Programming (ASP). Also, we argue that finite traces are more natural when reasoning about action and change. As a result, our approach is readily implementable via multi-shot ASP systems and benefits from an extension of ASP's full-fledged input language with temporal operators. This includes future as well as past operators whose combination offers a rich temporal modeling language. For computation, we identify the class of temporal logic programs and prove that it constitutes a normal form for our approach. Finally, we outline two implementations, a generic one and an extension of the ASP system clingo. Under consideration for publication in Theory and Practice of Logic Programming (TPLP) Y1 - 2018 U6 - https://doi.org/10.1017/S1471068418000297 SN - 1471-0684 SN - 1475-3081 VL - 18 IS - 3-4 SP - 406 EP - 420 PB - Cambridge Univ. Press CY - New York ER - TY - GEN A1 - Shprits, Yuri A1 - Zhelavskaya, Irina A1 - Green, Janet C. A1 - Pulkkinen, Antti A. A1 - Horne, Richard B. A1 - Pitchford, David A1 - Glover, Alexi T1 - Discussions on Stakeholder Requirements for Space Weather-Related Models T2 - Space Weather: The International Journal of Research and Applications N2 - Participants of the 2017 European Space Weather Week in Ostend, Belgium, discussed the stakeholder requirements for space weather-related models. It was emphasized that stakeholders show an increased interest in space weather-related models. Participants of the meeting discussed particular prediction indicators that can provide first-order estimates of the impact of space weather on engineering systems. KW - 7924 KW - 7934 KW - 7959 Y1 - 2018 U6 - https://doi.org/10.1002/2018SW001864 SN - 1542-7390 VL - 16 IS - 4 SP - 341 EP - 342 PB - American Geophysical Union CY - Washington ER - TY - GEN A1 - Schaub, Torsten A1 - Woltran, Stefan T1 - Special issue on answer set programming T2 - Künstliche Intelligenz Y1 - 2018 U6 - https://doi.org/10.1007/s13218-018-0554-8 SN - 0933-1875 SN - 1610-1987 VL - 32 IS - 2-3 SP - 101 EP - 103 PB - Springer CY - Heidelberg ER - TY - JOUR A1 - Zhelayskaya, Irina S. A1 - Vasile, Ruggero A1 - Shprits, Yuri A1 - Stolle, Claudia A1 - Matzka, Jürgen T1 - Systematic Analysis of Machine Learning and Feature Selection Techniques for Prediction of the Kp Index JF - Space Weather: The International Journal of Research and Applications N2 - The Kp index is a measure of the midlatitude global geomagnetic activity and represents short-term magnetic variations driven by solar wind plasma and interplanetary magnetic field. The Kp index is one of the most widely used indicators for space weather alerts and serves as input to various models, such as for the thermosphere and the radiation belts. It is therefore crucial to predict the Kp index accurately. Previous work in this area has mostly employed artificial neural networks to nowcast Kp, based their inferences on the recent history of Kp and on solar wind measurements at L1. In this study, we systematically test how different machine learning techniques perform on the task of nowcasting and forecasting Kp for prediction horizons of up to 12 hr. Additionally, we investigate different methods of machine learning and information theory for selecting the optimal inputs to a predictive model. We illustrate how these methods can be applied to select the most important inputs to a predictive model of Kp and to significantly reduce input dimensionality. We compare our best performing models based on a reduced set of optimal inputs with the existing models of Kp, using different test intervals, and show how this selection can affect model performance. KW - Kp index KW - Predictive models KW - Feature selection KW - Machine learning KW - Validation Y1 - 2019 U6 - https://doi.org/10.1029/2019SW002271 SN - 1542-7390 VL - 17 IS - 10 SP - 1461 EP - 1486 PB - American Geophysical Union CY - Washington ER - TY - JOUR A1 - Rabl, Tilmann T1 - Reminiscences on influential papers JF - SIGMOD record N2 - When I started my PhD, I wanted to do something related to systems but I wasn't sure exactly what. I didn't consider data management systems initially, because I was unaware of the richness of the systems work that data management systems were build on. I thought the field was mainly about SQL. Luckily, that view changed quickly. Y1 - 2023 U6 - https://doi.org/10.1145/3582302.3582310 SN - 0163-5808 SN - 1943-5835 VL - 51 IS - 4 SP - 42 EP - 44 PB - Association for Computing Machinery CY - New York ER - TY - JOUR A1 - Shenar, Tomer A1 - Sablowski, D. P. A1 - Hainich, Rainer A1 - Todt, Helge Tobias A1 - Moffat, Anthony F. J. A1 - Oskinova, Lidia M. A1 - Ramachandran, Varsha A1 - Sana, Hugues A1 - Sander, Andreas Alexander Christoph A1 - Schnurr, O. A1 - St-Louis, N. A1 - Vanbeveren, D. A1 - Gotberg, Y. A1 - Hamann, Wolf-Rainer T1 - The Wolf-Rayet binaries of the nitrogen sequence in the Large Magellanic Cloud Spectroscopy, orbital analysis, formation, and evolution JF - Astronomy and astrophysics : an international weekly journal N2 - Context. Massive Wolf-Rayet (WR) stars dominate the radiative and mechanical energy budget of galaxies and probe a critical phase in the evolution of massive stars prior to core collapse. It is not known whether core He-burning WR stars (classical WR; cWR) form predominantly through wind stripping (w-WR) or binary stripping (b-WR). Whereas spectroscopy of WR binaries has so-far largely been avoided because of its complexity, our study focuses on the 44 WR binaries and binary candidates of the Large Magellanic Cloud (LMC; metallicity Z approximate to 0.5 Z(circle dot)), which were identified on the basis of radial velocity variations, composite spectra, or high X-ray luminosities. Aims. Relying on a diverse spectroscopic database, we aim to derive the physical and orbital parameters of our targets, confronting evolution models of evolved massive stars at subsolar metallicity and constraining the impact of binary interaction in forming these stars. Methods. Spectroscopy was performed using the Potsdam Wolf-Rayet (PoWR) code and cross-correlation techniques. Disentanglement was performed using the code Spectangular or the shift-and-add algorithm. Evolutionary status was interpreted using the Binary Population and Spectral Synthesis (BPASS) code, exploring binary interaction and chemically homogeneous evolution. Results. Among our sample, 28/44 objects show composite spectra and are analyzed as such. An additional five targets show periodically moving WR primaries but no detected companions (SB1); two (BAT99 99 and 112) are potential WR + compact-object candidates owing to their high X-ray luminosities. We cannot confirm the binary nature of the remaining 11 candidates. About two-thirds of the WN components in binaries are identified as cWR, and one-third as hydrogen-burning WR stars. We establish metallicity-dependent mass-loss recipes, which broadly agree with those recently derived for single WN stars, and in which so-called WN3/O3 stars are clear outliers. We estimate that 45 +/- 30% of the cWR stars in our sample have interacted with a companion via mass transfer. However, only approximate to 12 +/- 7% of the cWR stars in our sample naively appear to have formed purely owing to stripping via a companion (12% b-WR). Assuming that apparently single WR stars truly formed as single stars, this comprises approximate to 4% of the whole LMC WN population, which is about ten times less than expected. No obvious differences in the properties of single and binary WN stars, whose luminosities extend down to log L approximate to 5.2 [L-circle dot], are apparent. With the exception of a few systems (BAT99 19, 49, and 103), the equatorial rotational velocities of the OB-type companions are moderate (v(eq) less than or similar to 250 km s(-1)) and challenge standard formalisms of angular-momentum accretion. For most objects, chemically homogeneous evolution can be rejected for the secondary, but not for the WR progenitor. Conclusions. No obvious dichotomy in the locations of apparently single and binary WN stars on the Hertzsprung-Russell diagram is apparent. According to commonly used stellar evolution models (BPASS, Geneva), most apparently single WN stars could not have formed as single stars, implying that they were stripped by an undetected companion. Otherwise, it must follow that pre-WR mass-loss/mixing (e.g., during the red supergiant phase) are strongly underestimated in standard stellar evolution models. KW - stars: massive KW - stars: Wolf-Rayet KW - Magellanic Clouds KW - binaries: close KW - binaries: spectroscopic KW - stars: evolution Y1 - 2019 U6 - https://doi.org/10.1051/0004-6361/201935684 SN - 0004-6361 SN - 1432-0746 VL - 627 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Shenar, Tomer A1 - Hainich, Rainer A1 - Todt, Helge Tobias A1 - Moffat, Anthony F. J. A1 - Sander, Andreas Alexander Christoph A1 - Oskinova, Lidia M. A1 - Ramachandran, Varsha A1 - Munoz, M. A1 - Pablo, H. A1 - Sana, Hugues A1 - Hamann, Wolf-Rainer T1 - The shortest-period Wolf-Rayet binary in the small magellanic cloud BT - Part of a high-order multiple system Spectral and orbital analysis of SMC AB 6 JF - Astronomy and astrophysics : an international weekly journal N2 - Context. SMC AB6 is the shortest-period (P = 6.5 d) Wolf-Rayet (WR) binary in the Small Magellanic Cloud. This binary is therefore a key system in the study of binary interaction and formation of WR stars at low metallicity. The WR component in AB6 was previously found to be very luminous (log L = 6.3 [L-circle dot]) compared to its reported orbital mass (approximate to 8 M-circle dot), placing it significantly above the Eddington limit. Aims. Through spectroscopy and orbital analysis of newly acquired optical data taken with the Ultraviolet and Visual Echelle Spectrograph (UVES), we aim to understand the peculiar results reported for this system and explore its evolutionary history. Methods. We measured radial velocities via cross-correlation and performed a spectral analysis using the Potsdam Wolf-Rayet model atmosphere code. The evolution of the system was analyzed using the Binary Population and Spectral Synthesis evolution code. Results. AB6 contains at least four stars. The 6.5 d period WR binary comprises the WR primary (WN3:h, star A) and a rather rapidly rotating (v(eq) = 265 km s(-1)) early O-type companion (O5.5 V, star B). Static N III and N IV emission lines and absorption signatures in He lines suggest the presence of an early-type emission line star (O5.5 I(f), star C). Finally, narrow absorption lines portraying a long-term radial velocity variation show the existence of a fourth star (O7.5 V, star D). Star D appears to form a second 140 d period binary together with a fifth stellar member, which is a B-type dwarf or a black hole. It is not clear that these additional components are bound to the WR binary. We derive a mass ratio of M-O/M-WR = 2.2 +/- 0.1. The WR star is found to be less luminous than previously thought (log L = 5.9 [L-circle dot]) and, adopting M-O = 41 M-circle dot for star B, more massive (M-WR = 18 M-circle dot). Correspondingly, the WR star does not exceed the Eddington limit. We derive the initial masses of M-i,M-WR = 60 M-circle dot and M-i,M-O = 40 M-circle dot and an age of 3.9 Myr for the system. The WR binary likely experienced nonconservative mass transfer in the past supported by the relatively rapid rotation of star B. Conclusions. Our study shows that AB6 is a multiple - probably quintuple - system. This finding resolves the previously reported puzzle of the WR primary exceeding the Eddington limit and suggests that the WR star exchanged mass with its companion in the past. KW - stars: massive KW - binaries: spectroscopic KW - stars: Wolf-Rayet KW - Magellanic Clouds KW - stars: individual: SMC AB 6 KW - stars: atmospheres Y1 - 2018 U6 - https://doi.org/10.1051/0004-6361/201833006 SN - 1432-0746 SN - 0004-6361 VL - 616 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Ramachandran, Varsha A1 - Hamann, Wolf-Rainer A1 - Hainich, Rainer A1 - Oskinova, Lidia M. A1 - Shenar, Tomer A1 - Sander, Andreas Alexander Christoph A1 - Todt, Helge Tobias A1 - Gallagher, John S. T1 - Stellar population of the superbubble N206 in the LMC II. Parameters of the OB and WR stars, and the total massive star feedback JF - Astronomy and astrophysics : an international weekly journal N2 - Context. Clusters or associations of early-type stars are often associated with a "superbubble" of hot gas. The formation of such superbubbles is caused by the feedback from massive stars. The complex N206 in the Large Magellanic Cloud (LMC) exhibits a superbubble and a rich massive star population. Aims. Our goal is to perform quantitative spectral analyses of all massive stars associated with the N206 superbubble in order to determine their stellar and wind parameters. We compare the superbubble energy budget to the stellar energy input and discuss the star formation history of the region. Results. We present the stellar and wind parameters of the OB stars and the two Wolf-Rayet (WR) binaries in the N206 complex. Twelve percent of the sample show Oe/Be type emission lines, although most of them appear to rotate far below critical. We found eight runaway stars based on their radial velocity. The wind-momentum luminosity relation of our OB sample is consistent with the expectations. The Hertzsprung-Russell diagram (HRD) of the OB stars reveals a large age spread (1-30 Myr), suggesting different episodes of star formation in the complex. The youngest stars are concentrated in the inner part of the complex, while the older OB stars are scattered over outer regions. We derived the present day mass function for the entire N206 complex as well as for the cluster NGC2018. The total ionizing photon flux produced by all massive stars in the N206 complex is Q(0) approximate to 5 x 10(50) s(-1), and the mechanical luminosity of their stellar winds amounts to L-mec = 1.7 x 10(38) erg s(-1). Three very massive Of stars are found to dominate the feedback among 164 OB stars in the sample. The two WR winds alone release about as much mechanical luminosity as the whole OB star sample. The cumulative mechanical feedback from all massive stellar winds is comparable to the combined mechanical energy of the supernova explosions that likely occurred in the complex. Accounting also for the WR wind and supernovae, the mechanical input over the last five Myr is approximate to 2.3 x 10(52) erg. Conclusions. The N206 complex in the LMC has undergone star formation episodes since more than 30 Myr ago. From the spectral analyses of its massive star population, we derive a current star formation rate of 2.2 x 10(-3) M-circle dot yr(-1). From the combined input of mechanical energy from all stellar winds, only a minor fraction is emitted in the form of X-rays. The corresponding input accumulated over a long time also exceeds the current energy content of the complex by more than a factor of five. The morphology of the complex suggests a leakage of hot gas from the superbubble. KW - stars: massive KW - Magellanic Clouds KW - stars: winds, outflows KW - Hertzsprung-Russell and C-M diagrams KW - techniques: spectroscopic KW - ISM: bubbles Y1 - 2018 U6 - https://doi.org/10.1051/0004-6361/201832816 SN - 1432-0746 VL - 615 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Ramachandran, Varsha A1 - Hainich, Rainer A1 - Hamann, Wolf-Rainer A1 - Oskinova, Lidia M. A1 - Shenar, T. A1 - Sander, Andreas Alexander Christoph A1 - Todt, Helge Tobias A1 - Gallagher, John S. T1 - Stellar population of the superbubble N206 in the LMC I. Analysis of the Of-type stars JF - Astronomy and astrophysics : an international weekly journal N2 - Context. Massive stars severely influence their environment by their strong ionizing radiation and by the momentum and kinetic energy input provided by their stellar winds and supernovae. Quantitative analyses of massive stars are required to understand how their feedback creates and shapes large scale structures of the interstellar medium. The giant H II region N206 in the Large Magellanic Cloud contains an OB association that powers a superbubble filled with hot X-ray emitting gas, serving as an ideal laboratory in this context. Aims. We aim to estimate stellar and wind parameters of all OB stars in N206 by means of quantitative spectroscopic analyses. In this first paper, we focus on the nine Of-type stars located in this region. We determine their ionizing flux and wind mechanical energy. The analysis of nitrogen abundances in our sample probes rotational mixing. Methods. We obtained optical spectra with the multi-object spectrograph FLAMES at the ESO-VLT. When possible, the optical spectroscopy was complemented by UV spectra from the HST, IUE, and FUSE archives. Detailed spectral classifications are presented for our sample Of-type stars. For the quantitative spectroscopic analysis we used the Potsdam Wolf-Rayet model atmosphere code. We determined the physical parameters and nitrogen abundances of our sample stars by fitting synthetic spectra to the observations. Results. The stellar and wind parameters of nine Of-type stars, which are largely derived from spectral analysis are used to construct wind momentum luminosity relationship. We find that our sample follows a relation close to the theoretical prediction, assuming clumped winds. The most massive star in the N206 association is an Of supergiant that has a very high mass-loss rate. Two objects in our sample reveal composite spectra, showing that the Of primaries have companions of late O subtype. All stars in our sample have an evolutionary age of less than 4 million yr, with the O2-type star being the youngest. All these stars show a systematic discrepancy between evolutionary and spectroscopic masses. All stars in our sample are nitrogen enriched. Nitrogen enrichment shows a clear correlation with increasing projected rotational velocities. Conclusions. The mechanical energy input from the Of stars alone is comparable to the energy stored in the N206 superbubble as measured from the observed X-ray and H alpha emission. KW - stars: early-type KW - Magellanic Clouds KW - stars: atmospheres KW - stars: winds, outflows KW - stars: mass-loss KW - stars: massive Y1 - 2017 U6 - https://doi.org/10.1051/0004-6361/201731093 SN - 1432-0746 SN - 0004-6361 VL - 609 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Sander, Andreas Alexander Christoph A1 - Fürst, F. A1 - Kretschmar, P. A1 - Oskinova, Lidia M. A1 - Todt, Helge Tobias A1 - Hainich, Rainer A1 - Shenar, Tomer A1 - Hamann, Wolf-Rainer T1 - Coupling hydrodynamics with comoving frame radiative transfer BT - Stellar wind stratification in the high-mass X-ray binary Vela X-1 JF - Astronomy and astrophysics : an international weekly journal N2 - Aims. To gain a realistic picture of the donor star in Vela X-1, we constructed a hydrodynamically consistent atmosphere model describing the wind stratification while properly reproducing the observed donor spectrum. To investigate how X-ray illumination affects the stellar wind, we calculated additional models for different X-ray luminosity regimes. Methods. We used the recently updated version of the Potsdam Wolf-Rayet code to consistently solve the hydrodynamic equation together with the statistical equations and the radiative transfer. Results. The wind flow in Vela X-1 is driven by ions from various elements, with Fe III and S III leading in the outer wind. The model-predicted mass-loss rate is in line with earlier empirical studies. The mass-loss rate is almost unaffected by the presence of the accreting NS in the wind. The terminal wind velocity is confirmed at u(infinity) approximate to 600 km s(-1). On the other hand, the wind velocity in the inner region where the NS is located is only approximate to 100 km s(-1), which is not expected on the basis of a standard beta-velocity law. In models with an enhanced level of X-rays, the velocity field in the outer wind can be altered. If the X-ray flux is too high, the acceleration breaks down because the ionization increases. Conclusions. Accounting for radiation hydrodynamics, our Vela X-1 donor atmosphere model reveals a low wind speed at the NS location, and it provides quantitative information on wind driving in this important HMXB. KW - stars: mass-loss KW - stars: winds, outflows KW - stars: early-type KW - stars: atmospheres KW - stars: massive KW - X-rays: binaries Y1 - 2018 U6 - https://doi.org/10.1051/0004-6361/201731575 SN - 1432-0746 VL - 610 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Sander, Andreas Alexander Christoph A1 - Hamann, Wolf-Rainer A1 - Todt, Helge Tobias A1 - Hainich, Rainer A1 - Shenar, Tomer A1 - Ramachandran, Varsha A1 - Oskinova, Lidia M. T1 - The Galactic WC and WO stars BT - The impact of revised distances from Gaia DR2 and their role as massive black hole progenitors JF - Astronomy and astrophysics : an international weekly journal N2 - Wolf-Rayet stars of the carbon sequence (WC stars) are an important cornerstone in the late evolution of massive stars before their core collapse. As core-helium burning, hydrogen-free objects with huge mass-loss, they are likely the last observable stage before collapse and thus promising progenitor candidates for type Ib/c supernovae. Their strong mass-loss furthermore provides challenges and constraints to the theory of radiatively driven winds. Thus, the determination of the WC star parameters is of major importance for several astrophysical fields. With Gaia DR2, for the first time parallaxes for a large sample of Galactic WC stars are available, removing major uncertainties inherent to earlier studies. In this work, we re-examine a previously studied sample of WC stars to derive key properties of the Galactic WC population. All quantities depending on the distance are updated, while the underlying spectral analyzes remain untouched. Contrasting earlier assumptions, our study yields that WC stars of the same subtype can significantly vary in absolute magnitude. With Gaia DR2, the picture of the Galactic WC population becomes more complex: We obtain luminosities ranging from log L/L-circle dot = 4.9-6.0 with one outlier (WR 119) having log L/L-circle dot = 4.7. This indicates that the WC stars are likely formed from a broader initial mass range than previously assumed. We obtain mass-loss rates ranging between log(M) over dot = -5.1 and -4.1, with (M) over dot proportional to L-0.68 and a linear scaling of the modified wind momentum with luminosity. We discuss the implications for stellar evolution, including unsolved issues regarding the need of envelope inflation to address the WR radius problem, and the open questions in regard to the connection of WR stars with Gamma-ray bursts. WC and WO stars are progenitors of massive black holes, collapsing either silently or in a supernova that most-likely has to be preceded by a WO stage. KW - stars: evolution KW - stars: mass-loss KW - stars: Wolf-Rayet KW - stars: massive KW - stars: distances KW - Galaxy: stellar content Y1 - 2019 U6 - https://doi.org/10.1051/0004-6361/201833712 SN - 1432-0746 VL - 621 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Hainich, Rainer A1 - Ramachandran, Varsha A1 - Shenar, Tomer A1 - Sander, Andreas Alexander Christoph A1 - Todt, Helge Tobias A1 - Gruner, David A1 - Oskinova, Lidia M. A1 - Hamann, Wolf-Rainer T1 - PoWR grids of non-LTE model atmospheres for OB-type stars of various metallicities JF - Astronomy and astrophysics : an international weekly journal N2 - The study of massive stars in different metallicity environments is a central topic of current stellar research. The spectral analysis of massive stars requires adequate model atmospheres. The computation of such models is difficult and time-consuming. Therefore, spectral analyses are greatly facilitated if they can refer to existing grids of models. Here we provide grids of model atmospheres for OB-type stars at metallicities corresponding to the Small and Large Magellanic Clouds, as well as to solar metallicity. In total, the grids comprise 785 individual models. The models were calculated using the state-of-the-art Potsdam Wolf-Rayet (PoWR) model atmosphere code. The parameter domain of the grids was set up using stellar evolution tracks. For all these models, we provide normalized and flux-calibrated spectra, spectral energy distributions, feedback parameters such as ionizing photons, Zanstra temperatures, and photometric magnitudes. The atmospheric structures (the density and temperature stratification) are available as well. All these data are publicly accessible through the PoWR website. KW - stars: massive KW - stars: early-type KW - stars: atmospheres KW - stars: winds KW - outflows KW - stars: mass-loss KW - radiative transfer Y1 - 2019 U6 - https://doi.org/10.1051/0004-6361/201833787 SN - 1432-0746 VL - 621 PB - EDP Sciences CY - Les Ulis ER - TY - RPRT A1 - Siedler, Thomas A1 - Anger, Silke A1 - Christoph, Bernhard A1 - Galkiewicz, Agata Danuta A1 - Margaryan, Shushanik A1 - Peter, Frauke A1 - Sandner, Malte T1 - War, international spillovers, and adolescents BT - evidence from Russia’s invasion of Ukraine in 2022 T2 - Discussion paper series N2 - Using novel longitudinal data, this paper studies the short- and medium-term effects of Russia's invasion of Ukraine on February 24, 2022 on social trust of adolescents in Germany. Comparing adolescents who responded to our survey shortly before the start of the war with those who responded shortly after the conflict began and applying difference-in-differences (DiD) models over time, we find a significant decline in the outcome after the war started. These findings provide new evidence on how armed conflicts influence social trust and well-being among young people in a country not directly involved in the war. KW - war KW - trust KW - social capital KW - Russia’s invasion of Ukraine Y1 - 2024 UR - https://www.iza.org/publications/dp/16921/war-international-spillovers-and-adolescents-evidence-from-russias-invasion-of-ukraine-in-2022 SN - 2365-9793 N1 - published in: Journal of Economic Behavior & Organization, 2024, 224, 181-193 VL - No. 16921 PB - IZA CY - Bonn ER - TY - RPRT A1 - Brodeur, Abel A1 - Mikola, Derek A1 - Cook, Nikolai A1 - Brailey, Thomas A1 - Briggs, Ryan A1 - Gendre, Alexandra de A1 - Dupraz, Yannick A1 - Fiala, Lenka A1 - Gabani, Jacopo A1 - Gauriot, Romain A1 - Haddad, Joanne A1 - Lima, Goncalo A1 - Ankel-Peters, Jörg A1 - Dreber, Anna A1 - Campbell, Douglas A1 - Kattan, Lamis A1 - Fages, Diego Marino A1 - Mierisch, Fabian A1 - Sun, Pu A1 - Wright, Taylor A1 - Connolly, Marie A1 - Hoces de la Guardia, Fernando A1 - Johannesson, Magnus A1 - Miguel, Edward A1 - Vilhuber, Lars A1 - Abarca, Alejandro A1 - Acharya, Mahesh A1 - Adjisse, Sossou Simplice A1 - Akhtar, Ahwaz A1 - Lizardi, Eduardo Alberto Ramirez A1 - Albrecht, Sabina A1 - Andersen, Synve Nygaard A1 - Andlib, Zubaria A1 - Arrora, Falak A1 - Ash, Thomas A1 - Bacher, Etienne A1 - Bachler, Sebastian A1 - Bacon, Félix A1 - Bagues, Manuel A1 - Balogh, Timea A1 - Batmanov, Alisher A1 - Barschkett, Mara A1 - Basdil, B. Kaan A1 - Dower, Jaromneda A1 - Castek, Ondrej A1 - Caviglia-Harris, Jill A1 - Strand, Gabriella Chauca A1 - Chen, Shi A1 - Chzhen, Asya A1 - Chung, Jong A1 - Collins, Jason A1 - Coppock, Alexander A1 - Cordeau, Hugo A1 - Couillard, Ben A1 - Crechet, Jonathan A1 - Crippa, Lorenzo A1 - Cui, Jeanne A1 - Czymara, Christian A1 - Daarstad, Haley A1 - Dao, Danh Chi A1 - Dao, Dong A1 - Schmandt, Marco David A1 - Linde, Astrid de A1 - Melo, Lucas De A1 - Deer, Lachlan A1 - Vera, Micole De A1 - Dimitrova, Velichka A1 - Dollbaum, Jan Fabian A1 - Dollbaum, Jan Matti A1 - Donnelly, Michael A1 - Huynh, Luu Duc Toan A1 - Dumbalska, Tsvetomira A1 - Duncan, Jamie A1 - Duong, Kiet Tuan A1 - Duprey, Thibaut A1 - Dworschak, Christoph A1 - Ellingsrud, Sigmund A1 - Elminejad, Ali A1 - Eissa, Yasmine A1 - Erhart, Andrea A1 - Etingin-Frati, Giulian A1 - Fatemi-Pour, Elaheh A1 - Federice, Alexa A1 - Feld, Jan A1 - Fenig, Guidon A1 - Firouzjaeiangalougah, Mojtaba A1 - Fleisje, Erlend A1 - Fortier-Chouinard, Alexandre A1 - Engel, Julia Francesca A1 - Fries, Tilman A1 - Fortier, Reid A1 - Fréchet, Nadjim A1 - Galipeau, Thomas A1 - Gallegos, Sebastián A1 - Gangji, Areez A1 - Gao, Xiaoying A1 - Garnache, Cloé A1 - Gáspár, Attila A1 - Gavrilova, Evelina A1 - Ghosh, Arijit A1 - Gibney, Garreth A1 - Gibson, Grant A1 - Godager, Geir A1 - Goff, Leonard A1 - Gong, Da A1 - González, Javier A1 - Gretton, Jeremy A1 - Griffa, Cristina A1 - Grigoryeva, Idaliya A1 - Grtting, Maja A1 - Guntermann, Eric A1 - Guo, Jiaqi A1 - Gugushvili, Alexi A1 - Habibnia, Hooman A1 - Häffner, Sonja A1 - Hall, Jonathan D. A1 - Hammar, Olle A1 - Kordt, Amund Hanson A1 - Hashimoto, Barry A1 - Hartley, Jonathan S. A1 - Hausladen, Carina I. A1 - Havránek, Tomáš A1 - Hazen, Jacob A1 - He, Harry A1 - Hepplewhite, Matthew A1 - Herrera-Rodriguez, Mario A1 - Heuer, Felix A1 - Heyes, Anthony A1 - Ho, Anson T. Y. A1 - Holmes, Jonathan A1 - Holzknecht, Armando A1 - Hsu, Yu-Hsiang Dexter A1 - Hu, Shiang-Hung A1 - Huang, Yu-Shiuan A1 - Huebener, Mathias A1 - Huber, Christoph A1 - Huynh, Kim P. A1 - Irsova, Zuzana A1 - Isler, Ozan A1 - Jakobsson, Niklas A1 - Frith, Michael James A1 - Jananji, Raphaël A1 - Jayalath, Tharaka A. A1 - Jetter, Michael A1 - John, Jenny A1 - Forshaw, Rachel Joy A1 - Juan, Felipe A1 - Kadriu, Valon A1 - Karim, Sunny A1 - Kelly, Edmund A1 - Dang, Duy Khanh Hoang A1 - Khushboo, Tazia A1 - Kim, Jin A1 - Kjellsson, Gustav A1 - Kjelsrud, Anders A1 - Kotsadam, Andreas A1 - Korpershoek, Jori A1 - Krashinsky, Lewis A1 - Kundu, Suranjana A1 - Kustov, Alexander A1 - Lalayev, Nurlan A1 - Langlois, Audrée A1 - Laufer, Jill A1 - Lee-Whiting, Blake A1 - Leibing, Andreas A1 - Lenz, Gabriel A1 - Levin, Joel A1 - Li, Peng A1 - Li, Tongzhe A1 - Lin, Yuchen A1 - Listo, Ariel A1 - Liu, Dan A1 - Lu, Xuewen A1 - Lukmanova, Elvina A1 - Luscombe, Alex A1 - Lusher, Lester R. A1 - Lyu, Ke A1 - Ma, Hai A1 - Mäder, Nicolas A1 - Makate, Clifton A1 - Malmberg, Alice A1 - Maitra, Adit A1 - Mandas, Marco A1 - Marcus, Jan A1 - Margaryan, Shushanik A1 - Márk, Lili A1 - Martignano, Andres A1 - Marsh, Abigail A1 - Masetto, Isabella A1 - McCanny, Anthony A1 - McManus, Emma A1 - McWay, Ryan A1 - Metson, Lennard A1 - Kinge, Jonas Minet A1 - Mishra, Sumit A1 - Mohnen, Myra A1 - Möller, Jakob A1 - Montambeault, Rosalie A1 - Montpetit, Sébastien A1 - Morin, Louis-Philippe A1 - Morris, Todd A1 - Moser, Scott A1 - Motoki, Fabio A1 - Muehlenbachs, Lucija A1 - Musulan, Andreea A1 - Musumeci, Marco A1 - Nabin, Munirul A1 - Nchare, Karim A1 - Neubauer, Florian A1 - Nguyen, Quan M. P. A1 - Nguyen, Tuan A1 - Nguyen-Tien, Viet A1 - Niazi, Ali A1 - Nikolaishvili, Giorgi A1 - Nordstrom, Ardyn A1 - Nü, Patrick A1 - Odermatt, Angela A1 - Olson, Matt A1 - ien, Henning A1 - Ölkers, Tim A1 - Vert, Miquel Oliver i. A1 - Oral, Emre A1 - Oswald, Christian A1 - Ousman, Ali A1 - Özak, Ömer A1 - Pandey, Shubham A1 - Pavlov, Alexandre A1 - Pelli, Martino A1 - Penheiro, Romeo A1 - Park, RyuGyung A1 - Martel, Eva Pérez A1 - Petrovičová, Tereza A1 - Phan, Linh A1 - Prettyman, Alexa A1 - Procházka, Jakub A1 - Putri, Aqila A1 - Quandt, Julian A1 - Qiu, Kangyu A1 - Nguyen, Loan Quynh Thi A1 - Rahman, Andaleeb A1 - Rea, Carson H. A1 - Reiremo, Adam A1 - Renée, Laëtitia A1 - Richardson, Joseph A1 - Rivers, Nicholas A1 - Rodrigues, Bruno A1 - Roelofs, William A1 - Roemer, Tobias A1 - Rogeberg, Ole A1 - Rose, Julian A1 - Roskos-Ewoldsen, Andrew A1 - Rosmer, Paul A1 - Sabada, Barbara A1 - Saberian, Soodeh A1 - Salamanca, Nicolas A1 - Sator, Georg A1 - Sawyer, Antoine A1 - Scates, Daniel A1 - Schlüter, Elmar A1 - Sells, Cameron A1 - Sen, Sharmi A1 - Sethi, Ritika A1 - Shcherbiak, Anna A1 - Sogaolu, Moyosore A1 - Soosalu, Matt A1 - Srensen, Erik A1 - Sovani, Manali A1 - Spencer, Noah A1 - Staubli, Stefan A1 - Stans, Renske A1 - Stewart, Anya A1 - Stips, Felix A1 - Stockley, Kieran A1 - Strobel, Stephenson A1 - Struby, Ethan A1 - Tang, John A1 - Tanrisever, Idil A1 - Yang, Thomas Tao A1 - Tastan, Ipek A1 - Tatić, Dejan A1 - Tatlow, Benjamin A1 - Seuyong, Féraud Tchuisseu A1 - Thériault, Rémi A1 - Thivierge, Vincent A1 - Tian, Wenjie A1 - Toma, Filip-Mihai A1 - Totarelli, Maddalena A1 - Tran, Van-Anh A1 - Truong, Hung A1 - Tsoy, Nikita A1 - Tuzcuoglu, Kerem A1 - Ubfal, Diego A1 - Villalobos, Laura A1 - Walterskirchen, Julian A1 - Wang, Joseph Taoyi A1 - Wattal, Vasudha A1 - Webb, Matthew D. A1 - Weber, Bryan A1 - Weisser, Reinhard A1 - Weng, Wei-Chien A1 - Westheide, Christian A1 - White, Kimberly A1 - Winter, Jacob A1 - Wochner, Timo A1 - Woerman, Matt A1 - Wong, Jared A1 - Woodard, Ritchie A1 - Wroński, Marcin A1 - Yazbeck, Myra A1 - Yang, Gustav Chung A1 - Yap, Luther A1 - Yassin, Kareman A1 - Ye, Hao A1 - Yoon, Jin Young A1 - Yurris, Chris A1 - Zahra, Tahreen A1 - Zaneva, Mirela A1 - Zayat, Aline A1 - Zhang, Jonathan A1 - Zhao, Ziwei A1 - Yaolang, Zhong T1 - Mass reproducibility and replicability BT - a new hope T2 - I4R discussion paper series N2 - This study pushes our understanding of research reliability by reproducing and replicating claims from 110 papers in leading economic and political science journals. The analysis involves computational reproducibility checks and robustness assessments. It reveals several patterns. First, we uncover a high rate of fully computationally reproducible results (over 85%). Second, excluding minor issues like missing packages or broken pathways, we uncover coding errors for about 25% of studies, with some studies containing multiple errors. Third, we test the robustness of the results to 5,511 re-analyses. We find a robustness reproducibility of about 70%. Robustness reproducibility rates are relatively higher for re-analyses that introduce new data and lower for re-analyses that change the sample or the definition of the dependent variable. Fourth, 52% of re-analysis effect size estimates are smaller than the original published estimates and the average statistical significance of a re-analysis is 77% of the original. Lastly, we rely on six teams of researchers working independently to answer eight additional research questions on the determinants of robustness reproducibility. Most teams find a negative relationship between replicators' experience and reproducibility, while finding no relationship between reproducibility and the provision of intermediate or even raw data combined with the necessary cleaning codes. KW - conomics KW - open science KW - political science KW - replication KW - reproduction KW - research transparency Y1 - 2024 SN - 2752-1931 IS - 107 PB - Institute for Replication CY - Essen ER - TY - JOUR A1 - Kolmakova, Olesya V. A1 - Gladyshev, Michail I. A1 - Fonvielle, Jeremy Andre A1 - Ganzert, Lars A1 - Hornick, Thomas A1 - Grossart, Hans-Peter T1 - Effects of zooplankton carcasses degradation on freshwater bacterial community composition and implications for carbon cycling JF - Environmental microbiology N2 - Non-predatory mortality of zooplankton provides an abundant, yet, little studied source of high quality labile organic matter (LOM) in aquatic ecosystems. Using laboratory microcosms, we followed the decomposition of organic carbon of fresh C-13-labelled Daphnia carcasses by natural bacterioplankton. The experimental setup comprised blank microcosms, that is, artificial lake water without any organic matter additions (B), and microcosms either amended with natural humic matter (H), fresh Daphnia carcasses (D) or both, that is, humic matter and Daphnia carcasses (HD). Most of the carcass carbon was consumed and respired by the bacterial community within 15 days of incubation. A shift in the bacterial community composition shaped by labile carcass carbon and by humic matter was observed. Nevertheless, we did not observe a quantitative change in humic matter degradation by heterotrophic bacteria in the presence of LOM derived from carcasses. However, carcasses were the main factor driving the bacterial community composition suggesting that the presence of large quantities of dead zooplankton might affect the carbon cycling in aquatic ecosystems. Our results imply that organic matter derived from zooplankton carcasses is efficiently remineralized by a highly specific bacterial community, but does not interfere with the bacterial turnover of more refractory humic matter. Y1 - 2018 U6 - https://doi.org/10.1111/1462-2920.14418 SN - 1462-2912 SN - 1462-2920 VL - 21 IS - 1 SP - 34 EP - 49 PB - Wiley CY - Hoboken ER - TY - JOUR A1 - Block, Benjamin D. A1 - Denfeld, Blaize A. A1 - Stockwell, Jason D. A1 - Flaim, Giovanna A1 - Grossart, Hans-Peter A1 - Knoll, Lesley B. A1 - Maier, Dominique B. A1 - North, Rebecca L. A1 - Rautio, Milla A1 - Rusak, James A. A1 - Sadro, Steve A1 - Weyhenmeyer, Gesa A. A1 - Bramburger, Andrew J. A1 - Branstrator, Donn K. A1 - Salonen, Kalevi A1 - Hampton, Stephanie E. T1 - The unique methodological challenges of winter limnology JF - Limnology and Oceanography: Methods N2 - Winter is an important season for many limnological processes, which can range from biogeochemical transformations to ecological interactions. Interest in the structure and function of lake ecosystems under ice is on the rise. Although limnologists working at polar latitudes have a long history of winter work, the required knowledge to successfully sample under winter conditions is not widely available and relatively few limnologists receive formal training. In particular, the deployment and operation of equipment in below 0 degrees C temperatures pose considerable logistical and methodological challenges, as do the safety risks of sampling during the ice-covered period. Here, we consolidate information on winter lake sampling and describe effective methods to measure physical, chemical, and biological variables in and under ice. We describe variation in snow and ice conditions and discuss implications for sampling logistics and safety. We outline commonly encountered methodological challenges and make recommendations for best practices to maximize safety and efficiency when sampling through ice or deploying instruments in ice-covered lakes. Application of such practices over a broad range of ice-covered lakes will contribute to a better understanding of the factors that regulate lakes during winter and how winter conditions affect the subsequent ice-free period. Y1 - 2018 U6 - https://doi.org/10.1002/lom3.10295 SN - 1541-5856 VL - 17 IS - 1 SP - 42 EP - 57 PB - Wiley CY - Hoboken ER - TY - JOUR A1 - Beisner, Beatrix E. A1 - Grossart, Hans-Peter A1 - Gasol, Josep M. T1 - A guide to methods for estimating phago-mixotrophy in nanophytoplankton JF - Journal of plankton research N2 - Growing attention to phytoplankton mixotrophy as a trophic strategy has led to significant revisions of traditional pelagic food web models and ecosystem functioning. Although some empirical estimates of mixotrophy do exist, a much broader set of in situ measurements are required to (i) identify which organisms are acting as mixotrophs in real time and to (ii) assess the contribution of their heterotrophy to biogeochemical cycling. Estimates are needed through time and across space to evaluate which environmental conditions or habitats favour mixotrophy: conditions still largely unknown. We review methodologies currently available to plankton ecologists to undertake estimates of plankton mixotrophy, in particular nanophytoplankton phago-mixotrophy. Methods are based largely on fluorescent or isotopic tracers, but also take advantage of genomics to identify phylotypes and function. We also suggest novel methods on the cusp of use for phago-mixotrophy assessment, including single-cell measurements improving our capacity to estimate mixotrophic activity and rates in wild plankton communities down to the single-cell level. Future methods will benefit from advances in nanotechnology, micromanipulation and microscopy combined with stable isotope and genomic methodologies. Improved estimates of mixotrophy will enable more reliable models to predict changes in food web structure and biogeochemical flows in a rapidly changing world. KW - flow cytometry KW - phagotrophy KW - phytoplankton KW - methods KW - fluorescence KW - microscopy KW - FISH KW - isotopic methods KW - phylotypes KW - carbon flows KW - gene sequencing Y1 - 2019 U6 - https://doi.org/10.1093/plankt/fbz008 SN - 0142-7873 SN - 1464-3774 VL - 41 IS - 2 SP - 77 EP - 89 PB - Oxford Univ. Press CY - Oxford ER - TY - JOUR A1 - Arias-Andres, Maria A1 - Rojas-Jimenez, Keilor A1 - Grossart, Hans-Peter T1 - Collateral effects of microplastic pollution on aquatic microorganisms BT - An ecological perspective JF - Trends in Analytical Chemistry N2 - Microplastics (MP) provide a unique and extensive surface for microbial colonization in aquatic ecosystems. The formation of microorganism-microplastic complexes, such as biofilms, maximizes the degradation of organic matter and horizontal gene transfer. In this context, MP affect the structure and function of microbial communities, which in turn render the physical and chemical fate of MP. This new paradigm generates challenges for microbiology, ecology, and ecotoxicology. Dispersal of MP is concomitant with that of their associated microorganisms and their mobile genetic elements, including antibiotic resistance genes, islands of pathogenicity, and diverse metabolic pathways. Functional changes in aquatic microbiomes can alter carbon metabolism and food webs, with unknown consequences on higher organisms or human microbiomes and hence health. Here, we examine a variety of effects of MP pollution from the microbial ecology perspective, whose repercussions on aquatic ecosystems begin to be unraveled. (C) 2018 Elsevier B.V. All rights reserved. KW - Microplastics (MP) KW - Biofilms KW - HGT KW - Microbial ecology KW - Carbon cycling KW - Aquatic ecosystems KW - Health risk assessment Y1 - 2018 U6 - https://doi.org/10.1016/j.trac.2018.11.041 SN - 0165-9936 SN - 1879-3142 VL - 112 SP - 234 EP - 240 PB - Elsevier CY - Oxford ER - TY - JOUR A1 - Gebser, Martin A1 - Obermeier, Philipp A1 - Otto, Thomas A1 - Schaub, Torsten A1 - Sabuncu, Orkunt A1 - Van Nguyen, A1 - Tran Cao Son, T1 - Experimenting with robotic intra-logistics domains JF - Theory and practice of logic programming N2 - We introduce the asprilo1 framework to facilitate experimental studies of approaches addressing complex dynamic applications. For this purpose, we have chosen the domain of robotic intra-logistics. This domain is not only highly relevant in the context of today's fourth industrial revolution but it moreover combines a multitude of challenging issues within a single uniform framework. This includes multi-agent planning, reasoning about action, change, resources, strategies, etc. In return, asprilo allows users to study alternative solutions as regards effectiveness and scalability. Although asprilo relies on Answer Set Programming and Python, it is readily usable by any system complying with its fact-oriented interface format. This makes it attractive for benchmarking and teaching well beyond logic programming. More precisely, asprilo consists of a versatile benchmark generator, solution checker and visualizer as well as a bunch of reference encodings featuring various ASP techniques. Importantly, the visualizer's animation capabilities are indispensable for complex scenarios like intra-logistics in order to inspect valid as well as invalid solution candidates. Also, it allows for graphically editing benchmark layouts that can be used as a basis for generating benchmark suites. Y1 - 2018 U6 - https://doi.org/10.1017/S1471068418000200 SN - 1471-0684 SN - 1475-3081 VL - 18 IS - 3-4 SP - 502 EP - 519 PB - Cambridge Univ. Press CY - New York ER - TY - JOUR A1 - Liemohn, Michael W. A1 - McCollough, James P. A1 - Jordanova, Vania K. A1 - Ngwira, Chigomezyo M. A1 - Morley, Steven K. A1 - Cid, Consuelo A1 - Tobiska, W. Kent A1 - Wintoft, Peter A1 - Ganushkina, Natalia Yu A1 - Welling, Daniel T. A1 - Bingham, Suzy A1 - Balikhin, Michael A. A1 - Opgenoorth, Hermann J. A1 - Engel, Miles A. A1 - Weigel, Robert S. A1 - Singer, Howard J. A1 - Buresova, Dalia A1 - Bruinsma, Sean A1 - Zhelavskaya, Irina A1 - Shprits, Yuri A1 - Vasile, Ruggero T1 - Model Evaluation Guidelines for Geomagnetic Index Predictions JF - Space Weather: The International Journal of Research and Applications N2 - Geomagnetic indices are convenient quantities that distill the complicated physics of some region or aspect of near-Earth space into a single parameter. Most of the best-known indices are calculated from ground-based magnetometer data sets, such as Dst, SYM-H, Kp, AE, AL, and PC. Many models have been created that predict the values of these indices, often using solar wind measurements upstream from Earth as the input variables to the calculation. This document reviews the current state of models that predict geomagnetic indices and the methods used to assess their ability to reproduce the target index time series. These existing methods are synthesized into a baseline collection of metrics for benchmarking a new or updated geomagnetic index prediction model. These methods fall into two categories: (1) fit performance metrics such as root-mean-square error and mean absolute error that are applied to a time series comparison of model output and observations and (2) event detection performance metrics such as Heidke Skill Score and probability of detection that are derived from a contingency table that compares model and observation values exceeding (or not) a threshold value. A few examples of codes being used with this set of metrics are presented, and other aspects of metrics assessment best practices, limitations, and uncertainties are discussed, including several caveats to consider when using geomagnetic indices. Plain Language Summary One aspect of space weather is a magnetic signature across the surface of the Earth. The creation of this signal involves nonlinear interactions of electromagnetic forces on charged particles and can therefore be difficult to predict. The perturbations that space storms and other activity causes in some observation sets, however, are fairly regular in their pattern. Some of these measurements have been compiled together into a single value, a geomagnetic index. Several such indices exist, providing a global estimate of the activity in different parts of geospace. Models have been developed to predict the time series of these indices, and various statistical methods are used to assess their performance at reproducing the original index. Existing studies of geomagnetic indices, however, use different approaches to quantify the performance of the model. This document defines a standardized set of statistical analyses as a baseline set of comparison tools that are recommended to assess geomagnetic index prediction models. It also discusses best practices, limitations, uncertainties, and caveats to consider when conducting a model assessment. Y1 - 2018 U6 - https://doi.org/10.1029/2018SW002067 SN - 1542-7390 VL - 16 IS - 12 SP - 2079 EP - 2102 PB - American Geophysical Union CY - Washington ER - TY - JOUR A1 - Zhu, Hui A1 - Shprits, Yuri A1 - Chen, Lunjin A1 - Liu, Xu A1 - Kellerman, Adam C. T1 - An event on simultaneous amplification of exohiss and chorus waves associated with electron density enhancements JF - Journal of geophysical research : Space physics N2 - Whistler mode exohiss are the structureless hiss waves observed outside the plasma pause with featured equatorward Poynting flux. An event of the amplification of exohiss as well as chorus waves was recorded by Van Allen Probes during the recovery phase of a weak geomagnetic storm. Amplitudes of both types of the waves showed a significant increase at the regions of electron density enhancements. It is found that the electrons resonant with exohiss and chorus showed moderate pitch angle anisotropies. The ratio of the number of electrons resonating with exohiss to total electron number presented in-phase correlation with density variations, which suggests that exohiss can be amplified due to electron density enhancement in terms of cyclotron instability. The calculation of linear growth rates further supports above conclusion. We suggest that exohiss waves have potential to become more significant due to the background plasma fluctuation. Y1 - 2018 U6 - https://doi.org/10.1029/2017JA025023 SN - 2169-9380 SN - 2169-9402 VL - 123 IS - 11 SP - 8958 EP - 8968 PB - American Geophysical Union CY - Washington ER - TY - JOUR A1 - Oskinova, Lidia M. A1 - Feldmeier, Achim A1 - Hamann, Wolf-Rainer T1 - High-resolution X-ray spectroscopy of bright O-type stars JF - Monthly notices of the Royal Astronomical Society N2 - Archival X-ray spectra of the four prominent single, non-magnetic O stars zeta Pup, zeta Ori, xi Per and zeta Oph, obtained in high resolution with Chandra HETGS/MEG have been studied. The resolved X-ray emission line profiles provide information about the shocked, hot gas which emits the X-radiation, and about the bulk of comparably cool stellar wind material which partly absorbs this radiation. In this paper, we synthesize X-ray line profiles with a model of a clumpy stellar wind. We find that the geometrical shape of the wind inhomogeneities is important: better agreement with the observations can be achieved with radially compressed clumps than with spherical clumps. The parameters of the model, i.e. chemical abundances, stellar radius, mass-loss rate and terminal wind velocity, are taken from existing analyses of UV and optical spectra of the programme stars. On this basis, we also calculate the continuum-absorption coefficient of the cool-wind material, using the Potsdam Wolf-Rayet (POWR) model atmosphere code. The radial location of X-ray emitting gas is restricted from analysing the FIR line ratios of helium-like ions. The only remaining free parameter of our model is the typical distance between the clumps; here, we assume that at any point in the wind there is one clump passing by per one dynamical time-scale of the wind. The total emission in a model line is scaled to the observation. There is a good agreement between synthetic and observed line profiles. We conclude that the X-ray emission line profiles in O stars can be explained by hot plasma embedded in a cool wind which is highly clumped in the form of radially compressed shell fragments. KW - stars : individual : zeta Pup KW - stars : individual : zeta Ori KW - stars : individual : xi Per KW - stars : individual : zeta Oph KW - X-rays : stars Y1 - 2006 U6 - https://doi.org/10.1111/j.1365-2966.2006.10858.x SN - 0035-8711 VL - 372 SP - 313 EP - 326 PB - Oxford University Press CY - Oxford ER - TY - JOUR A1 - Robrade, Jan A1 - Oskinova, Lidia M. A1 - Schmitt, J. H. M. M. A1 - Leto, Paolo A1 - Trigilio, C. T1 - Outstanding X-ray emission from the stellar radio pulsar CU Virginis JF - Astronomy and astrophysics : an international weekly journal N2 - Context. Among the intermediate-mass magnetic chemically peculiar (MCP) stars, CU Vir is one of the most intriguing objects. Its 100% circularly polarized beams of radio emission sweep the Earth as the star rotates, thereby making this strongly magnetic star the prototype of a class of nondegenerate stellar radio pulsars. While CU Vir is well studied in radio, its high-energy properties are not known. Yet, X-ray emission is expected from stellar magnetospheres and confined stellar winds. Aims. Using X-ray data we aim to test CU Vir for intrinsic X-ray emission and investigate mechanisms responsible for its generation. Methods. We present X-ray observations performed with XMM-Newton and Chandra and study obtained X-ray images, light curves, and spectra. Basic X-ray properties are derived from spectral modelling and are compared with model predictions. In this context we investigate potential thermal and nonthermal X-ray emission scenarios. Results. We detect an X-ray source at the position of CU Vir. With LX approximate to 3 x 10(28) erg s(-1) it is moderately X-ray bright, but the spectrum is extremely hard compared to other Ap stars. Spectral modelling requires multi-component models with predominant hot plasma at temperatures of about T-X = 25MK or, alternatively, a nonthermal spectral component. Both types of model provide a virtually equivalent description of the X-ray spectra. The Chandra observation was performed six years later than those by XMM-Newton, yet the source has similar X-ray flux and spectrum, suggesting a steady and persistent X-ray emission. This is further confirmed by the X-ray light curves that show only mild X-ray variability. Conclusions. CU Vir is also an exceptional star at X-ray energies. To explain its full X-ray properties, a generating mechanism beyond standard explanations, like the presence of a low-mass companion or magnetically confined wind-shocks, is required. Magnetospheric activity might be present or, as proposed for fast-rotating strongly magnetic Bp stars, the X-ray emission of CU Vir is predominantly auroral in nature. KW - individual: CU Vir KW - stars: activity KW - stars: chemically peculiar KW - stars: magnetic field KW - X-rays: stars Y1 - 2018 U6 - https://doi.org/10.1051/0004-6361/201833492 SN - 1432-0746 VL - 619 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Oskinova, Lidia M. A1 - Bulik, Tomasz A1 - Gomez-Moran, Ada Nebot T1 - Infrared outbursts as potential tracers of common-envelope events in high-mass X-ray binary formation JF - Astronomy and astrophysics : an international weekly journal N2 - Context. Classic massive binary evolutionary scenarios predict that a transitional common-envelope (CE) phase could be preceded as well as succeeded by the evolutionary stage when a binary consists of a compact object and a massive star, that is, a high-mass X-ray binary (HMXB). The observational manifestations of common envelope are poorly constrained. We speculate that its ejection might be observed in some cases as a transient event at mid-infrared (IR) wavelengths. Aims. We estimate the expected numbers of CE ejection events and HMXBs per star formation unit rate, and compare these theoretical estimates with observations. Methods. We compiled a list of 85 mid-IR transients of uncertain nature detected by the Spitzer Infrared Intensive Transients Survey and searched for their associations with X-ray, optical, and UV sources. Results. Confirming our theoretical estimates, we find that only one potential HMXB may be plausibly associated with an IR-transient and tentatively propose that X-ray source NGC4490-X40 could be a precursor to the SPIRITS 16az event. Among other interesting sources, we suggest that the supernova remnant candidate [BWL2012] 063 might be associated with SPIRITS 16ajc. We also find that two SPIRITS events are likely associated with novae, and seven have potential optical counterparts. Conclusions. The massive binary evolutionary scenarios that involve CE events do not contradict currently available observations of IR transients and HMXBs in star-forming galaxies. KW - X-rays: binaries KW - stars: massive KW - infrared: general KW - infrared: galaxies Y1 - 2018 U6 - https://doi.org/10.1051/0004-6361/201832925 SN - 0004-6361 SN - 1432-0746 VL - 613 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Pillitteri, Ignazio A1 - Fossati, Luca A1 - Rodriguez, N. Castro A1 - Oskinova, Lidia M. A1 - Wolk, Scott J. T1 - Detection of magnetic field in the B2 star rho Ophiuchi A with ESO FORS2 JF - Astronomy and astrophysics : an international weekly journal N2 - Circumstantial evidence suggests that magnetism and enhanced X-ray emission are likely correlated in early B-type stars: similar fractions of them (similar to 10%) are strong and hard X-ray sources and possess strong magnetic fields. It is also known that some B-type stars have spots on their surface. Yet up to now no X-ray activity associated with spots on early-type stars was detected. In this Letter we report the detection of a magnetic field on the B2V star rho Oph A. Previously, we assessed that the X-ray activity of this star is associated with a surface spot, herewith we establish its magnetic origin. We analyze spectra of rho Oph A obtained with the FORS2 spectrograph at ESO Very Large Telescope (VLT) at two epochs, and detect a longitudinal component of the magnetic field of the order of similar to 500 G in one of the datasets. The detection of the magnetic field only at one epoch can be explained by stellar rotation which is also invoked to explain observed periodic X-ray activity. From archival HARPS ESO VLT high resolution spectra we derived the fundamental stellar parameters of rho Oph A and further constrained its age. We conclude that rho Oph A provides strong evidence for the presence of active X-ray emitting regions on young magnetized early type stars. KW - stars: activity KW - stars: early-type KW - stars: magnetic field KW - pulsars: individual: rho Ophiuchi A Y1 - 2017 U6 - https://doi.org/10.1051/0004-6361/201732078 SN - 1432-0746 VL - 610 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Gruner, David A1 - Hainich, Rainer A1 - Sander, Andreas Alexander Christoph A1 - Shenar, Tomer A1 - Todt, Helge Tobias A1 - Oskinova, Lidia M. A1 - Ramachandran, Varsha A1 - Ayres, T. A1 - Hamann, Wolf-Rainer T1 - The extreme O-type spectroscopic binary HD 93129A A quantitative, multiwavelength analysis JF - Astronomy and astrophysics : an international weekly journal N2 - Context. HD 93129A was classified as the earliest O-type star in the Galaxy (O2 If*) and is considered as the prototype of its spectral class. However, interferometry shows that this object is a binary system, while recent observations even suggest a triple configuration. None of the previous spectral analyses of this object accounted for its multiplicity. With new high-resolution UV and optical spectra, we have the possibility to reanalyze this key object, taking its binary nature into account for the first time. Aims. We aim to derive the fundamental parameters and the evolutionary status of HD 93129A, identifying the contributions of both components to the composite spectrum Results. Despite the similar spectral types of the two components, we are able to find signatures from each of the components in the combined spectrum, which allows us to estimate the parameters of both stars. We derive log(L/L-circle dot) = 6.15, T-eff = 52 kK, and log (M)over dot = -4.7[M-circle dot yr(-1)] for the primary Aa, and log(L/L-circle dot) = 5.58, T-eff = 45 kK, and log (M)over dot = -5.8 [M(circle dot)yr(-1)] for the secondary Ab. Conclusions. Even when accounting for the binary nature, the primary of HD 93129A is found to be one of the hottest and most luminous O stars in our Galaxy. Based on the theoretical decomposition of the spectra, we assign spectral types O2 If* and O3 III(f*) to components Aa and Ab, respectively. While we achieve a good fit for a wide spectral range, specific spectral features are not fully reproduced. The data are not sufficient to identify contributions from a hypothetical third component in the system. KW - stars: individual: HD 93129A KW - stars: atmospheres KW - stars: fundamental parameters KW - stars: early-typeP Y1 - 2018 U6 - https://doi.org/10.1051/0004-6361/201833178 SN - 1432-0746 VL - 621 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Hainich, Rainer A1 - Oskinova, Lidia M. A1 - Shenar, Tomer A1 - Marchant Campos, Pablo A1 - Eldridge, J. J. A1 - Sander, Andreas Alexander Christoph A1 - Hamann, Wolf-Rainer A1 - Langer, Norbert A1 - Todt, Helge Tobias T1 - Observational properties of massive black hole binary progenitors JF - Astronomy and astrophysics : an international weekly journal N2 - Context: The first directly detected gravitational waves (GW 150914) were emitted by two coalescing black holes (BHs) with masses of ≈ 36 M⊙ and ≈ 29 M⊙. Several scenarios have been proposed to put this detection into an astrophysical context. The evolution of an isolated massive binary system is among commonly considered models. Aims: Various groups have performed detailed binary-evolution calculations that lead to BH merger events. However, the question remains open as to whether binary systems with the predicted properties really exist. The aim of this paper is to help observers to close this gap by providing spectral characteristics of massive binary BH progenitors during a phase where at least one of the companions is still non-degenerate. Methods: Stellar evolution models predict fundamental stellar parameters. Using these as input for our stellar atmosphere code (Potsdam Wolf-Rayet), we compute a set of models for selected evolutionary stages of massive merging BH progenitors at different metallicities. Results: The synthetic spectra obtained from our atmosphere calculations reveal that progenitors of massive BH merger events start their lives as O2-3V stars that evolve to early-type blue supergiants before they undergo core-collapse during the Wolf-Rayet phase. When the primary has collapsed, the remaining system will appear as a wind-fed high-mass X-ray binary. Based on our atmosphere models, we provide feedback parameters, broad band magnitudes, and spectral templates that should help to identify such binaries in the future. Conclusions: While the predicted parameter space for massive BH binary progenitors is partly realized in nature, none of the known massive binaries match our synthetic spectra of massive BH binary progenitors exactly. Comparisons of empirically determined mass-loss rates with those assumed by evolution calculations reveal significant differences. The consideration of the empirical mass-loss rates in evolution calculations will possibly entail a shift of the maximum in the predicted binary-BH merger rate to higher metallicities, that is, more candidates should be expected in our cosmic neighborhood than previously assumed. KW - gravitational waves KW - binaries: close KW - stars: early-type KW - stars: atmospheres KW - stars: winds KW - outflows KW - stars: mass-loss Y1 - 2018 U6 - https://doi.org/10.1051/0004-6361/201731449 SN - 1432-0746 VL - 609 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Fulmer, Leah M. A1 - Gallagher, John S. A1 - Hamann, Wolf-Rainer A1 - Oskinova, Lidia M. A1 - Ramachandran, Varsha T1 - Testing massive star evolution, star-formation history, and feedback at low metallicity BT - photometric analysis of OB stars in the SMC Wing JF - Astronomy and astrophysics : an international weekly journal N2 - Context. The supergiant ionized shell SMC-SGS 1 (DEM 167), which is located in the outer Wing of the Small Magellanic Cloud (SMC), resembles structures that originate from an energetic star-formation event and later stimulate star formation as they expand into the ambient medium. However, stellar populations within and surrounding SMC-SGS 1 tell a different story. Aims. We present a photometric study of the stellar population encompassed by SMC-SGS 1 in order to trace the history of such a large structure and its potential influence on star formation within the low-density, low-metallicity environment of the SMC. Methods. For a stellar population that is physically associated with SMC-SGS 1, we combined near-ultraviolet (NUV) photometry from the Galaxy Evolution Explorer with archival optical (V-band) photometry from the ESO Danish 1.54 m Telescope. Given their colors and luminosities, we estimated stellar ages and masses by matching observed photometry to theoretical stellar isochrone models. Results. We find that the investigated region supports an active, extended star-formation event spanning similar to 25-40 Myr ago, as well as continued star formation into the present. Using a standard initial mass function, we infer a lower bound on the stellar mass from this period of similar to 3 x 10(4) M-circle dot, corresponding to a star-formation intensity of similar to 6 x 10(-3) M-circle dot kpc(-2) yr(-1). Conclusions. The spatial and temporal distributions of young stars encompassed by SMC-SGS 1 imply a slow, consistent progression of star formation over millions of years. Ongoing star formation, both along the edge and interior to SMC-SGS 1, suggests a combined stimulated and stochastic mode of star formation within the SMC Wing. We note that a slow expansion of the shell within this low-density environment may preserve molecular clouds within the volume of the shell, leaving them to form stars even after nearby stellar feedback expels local gas and dust. KW - galaxies KW - stellar content KW - stars KW - formation KW - individual KW - Small KW - Magellanic Cloud Y1 - 2020 U6 - https://doi.org/10.1051/0004-6361/201834314 SN - 0004-6361 SN - 1432-0746 VL - 633 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Geist, Emily A1 - Gallagher, John S. A1 - Kotulla, Ralf A1 - Oskinova, Lidia M. A1 - Hamann, Wolf-Rainer A1 - Ramachandran, Varsha A1 - Sabbi, Elena A1 - Smith, Linda J. A1 - Kniazev, Alexey A1 - Nota, Antonella A1 - Rickard, Matthew J. T1 - Ionization and star formation in the giant H ii region SMC-N66 JF - Publications of the Astronomical Society of the Pacific N2 - The NGC 346 young stellar system and associated N66 giant H ii region in the Small Magellanic Cloud are the nearest example of a massive star-forming event in a low metallicity (Z approximate to 0.2Z (circle dot)) galaxy. With an age of less than or similar to 3 Myr this system provides a unique opportunity to study relationships between massive stars and their associated H ii region. Using archival data, we derive a total H alpha luminosity of L(H alpha) = 4.1 x 10(38) erg s(-1) corresponding to an H-photoionization rate of 3 x 10(50) s(-1). A comparison with a predicted stellar ionization rate derived from the more than 50 known O-stars in NGC 346, including massive stars recently classified from Hubble Space Telescope far-ultraviolet (FUV) spectra, indicates an approximate ionization balance. Spectra obtained with SALT suggest the ionization structure of N66 could be consistent with some leakage of ionizing photons. Due to the low metallicity, the FUV luminosity from NGC 346 is not confined to the interstellar cloud associated with N66. Ionization extends through much of the spatial extent of the N66 cloud complex, and most of the cloud mass is not ionized. The stellar mass estimated from nebular L(H alpha) appears to be lower than masses derived from the census of resolved stars which may indicate a disconnect between the formation of high and low mass stars in this region. We briefly discuss implications of the properties of N66 for studies of star formation and stellar feedback in low metallicity environments. Y1 - 2022 U6 - https://doi.org/10.1088/1538-3873/ac697b SN - 0004-6280 SN - 1538-3873 VL - 134 IS - 1036 PB - IOP Publishing CY - Bristol ER -