CRIME - cosmic ray interactions in molecular environments

Molecular clouds act as targets for cosmic rays (CR), revealing their presence through either gamma-ray emission due to proton-proton interactions, and/or through the ionization level in the cloud, produced by the CR flux. The ionization rate is a unique tool, to some extent complementary to the gamma-ray emission, in that it allows to constrain the CR spectrum especially for energies below the pion production rate ($\approx 280$ MeV). Here we study the effect of ionization on $H_2$ clouds due to both CR protons and electrons, using the fully relativistic ionization cross sections, which is important to correctly account for the contribution due to relativistic CRs. The contribution to ionization due to secondary electrons is also included self-consistently. The whole calculation has been implemented into a numerical code which is publicly accessible through a web-interface. The code also include the calculation of gamma-ray emission once the CR spectrumComment: 8 pages 2 figures, The 34th International Cosmic Ray Conferenc

Resolved gamma ray emission of the supernova remnant W51C and HESS J1857+026 obtained with the MAGIC telescopes

Diese Dissertation untersucht den Urspung der kosmischen Strahlung mit Beobachtungen der MAGIC Teleskope im Bereich der hoch energeticher Gammastrahlenastronomie. Gammastrahlung wird bei der Wechselwirkung relativistischer Teilchen erzeugt. Im Gegensatz zur geladenen kosmichen Strahlung, werden Gammastrahlen nicht von interstellaren Magnetfeldern beinflusst. Daher erlaubt die Ankunftsrichtung von Gammastrahlen die Bestimmung ihres Ursprungs. Ein Teil dieser Arbeit widmet sich der Verbesserung der Analyse von MAGIC-daten. Im besonderen wurde ein neuer Algorithmus zur Hintergrundbestimmung entwickelt, wodurch die systematischen Unsicherheiten deutlich verbessert werden konnten. Zudem wurde die Reflekivitaet und Fokusierung beider MAGIC Teleskope anhand des Vergleichs zwischen echten und simulierten Muonereignissen bestimmt. Die heutige Meinung ist, dass die Ueberreste von Supernovae, die expandierende Schockwellen der Sternimplosionen, der Ursprung der galaktischen kosmischen Strahlung sind. Obwohl hoch energetische Gammastrahlung von vielen dieser Objekte beobachtet wurde, erlaubt die schwierige Unterscheidung von leptonisch und hadronsich produzierter Gammastrahlung in den meisten Faellen keine klaren Schlussfolgerungen ueber die Anwesenheit relativistischer Hadronen und damit kosmischer Strahlung. Da Gammastrahlung aus hadronischen Wechselwirkungen, nahezu ausschliesslich in inelastischen Proton-Proton Kollisionen erzeugt wird, ist ihre Produktion umso effektiver, desto hoeher die Dichte des mediums ist. Die Region W51 beherbergt den 30000 Jahre alten Supernovaueberrest W51C, welcher teilweise mit der grossen Molekuelwolke W51B kollidiert. MAGIC hat ausgedehnte Gammastrahlung von dieser Region mit hoher statistischer Signifikanz (11 sigma) gemessen. Es konnte gezeigt werden, dass das Zentrum der Emission in dem Bereich hoher Dichte liegt, wo der Supernovaueberrest mit der Molekuelwolke kollidiert. Das Energiespektrum wurde im Bereich von 75 GeV bis 5.5 TeV gemessen und folgt einem Potenzgesetz. Die moegliche Kontamination dieser Emission durch einen nahegelegenen potentiellen Pulsarwindnebel zeigt keine Energieabhaengigkeit und wurde als ~20\% der Gesamtemission bestimmt. Die Modellierung der nicht thermischen Mutliwellenlaengenemission deutet stark auf einen hadronischen Ursprung der Gammastrahlung hin. Diese Beschreibung impliziert, dass in etwa 16% der kinetsiche Energie der Schockwelle von W51C zur Produktion kosmischer Strahlung genutzt wurden. Damit is W51C eine der wenigen bekannten Supernovaueberreste wo eine Beschleunigung von Protonen der komsischer Strahlung, zumindestens bis 50 TeV, direkt beobachtet wird. HESS J1857+026 ist eine nicht identifizierte TeV-Quelle, die moeglicherweise den Pulsarwindnebel des, von der Gammastrahlung umschlossenen, hochenergetischen Pulsares PSR J1856+0245 darstellt. Eine augedehnte Emission wurde von MAGIC mit einer statistischen Signifikanz von mehr als 12 sigma gemessen. Das berechnete Spektrum verbindet die vorherigen Daten von Fermi/LAT und HESS, wobei es mit beiden Messungen ueberlappt. Anhand der MAGIC und Fermi/LAT Daten wurde ein Abweichung von einem einfachen Potenzgesetz bei ca. 100~GeV festgestellt. Bei hoeheren Energien werden zwei Emissionsregionen aufgeloest. Ueberhalb von einem TeV koennen zwei voneinander getrennte, einzeln signifikante Regionen festgestellt werden. Diese Dissertation zeigt die ersten morphologischen Untersuchungen, die mit den MAGIC Teleskopen durchgefuehrt wurden. Es wurde gezeigt, dass die Faehigkeit Strukturen in galaktischen Quellen aufloesen zu koennen, wichtige Informationen ueber die Physik der Teilchenbeschleunigung in astrophysikalischen Objekten liefert.This work addresses the long standing question of the origin of galactic cosmic rays by the use of very high energy gamma ray emission observed with the MAGIC telescopes. Gamma rays are produced in the interaction of relativistic particles. In contrast to the charged cosmic rays, gamma rays are not deflected by interstellar magnetic fields and therefore point back to their origin. A part of this work was dedicated to the improvement of the the MAGIC data analysis. In particular a new method to determine the background has been developed resulting in a reduction of the systematic uncertainties. Moreover, the optical point spread function and the light collection efficiency of both MAGIC telescopes have been determined by the comparison of real and simulated muon events. The common believe is that supernova remnants are the sources of galactic cosmic rays. While several supernova remnants are known to emit very high energy gamma rays, the difficulty to distinguish between leptonic and hadronic production mechanisms prevents in most cases clear evidence for the presence of relativistic hadrons and therefore cosmic rays. Gamma rays originating from relativistic hadrons are almost exclusively produced in inelastic proton-proton interactions and therefore more efficiently produced in regions of high matter density. The region W51 host the middle-age supernova remnant W51C which partially collides with the large molecular cloud W51B. MAGIC detected extended gamma ray emission in the W51 region with >11 sigma. It could be shown that the centroid of the emission is spatially consistent with the high density region of the interaction zone between the remnant and the molecular cloud. The differential energy spectrum extends from 75 GeV up to 5.5 TeV and follows simple power-law. A possible contribution of a nearby pulsar wind nebula candidate is constrained to be ~20% of the overall emission and shows no dependence on energy. A modeling of the non-thermal multiwavelength emission strongly suggests a hadronic origin of the observed emission. This models implies that about 16% of kinetic energy of the supernova remnant W51C has been converted into cosmic rays. W51C is therefore one of the few known supernova remnants where most likely the acceleration of cosmic rays, at least up to energies of 50 TeV per proton, is directly observed. HESS J1857+026 is an unidentified TeV source which could be explained as a pulsar wind nebula of the energetic pulsar PSR J1856+0245 enclosed in the gamma ray emission. MAGIC detected extended gamma ray emission with >12 sigma from the object. The derived spectrum connects previous measurements of Fermi/LAT and HESS and overlaps with both of them. The MAGIC and Fermi/LAT data reveal a spectral break at around 100 GeV. At high energies, the emission resolves in two regions. Two spatially distinct and statistically significant emission regions are established above 1 TeV. This thesis shows the first morphological studies in very high energy gamma rays performed with the MAGIC telescopes. The ability to resolve structures in galactic gamma ray sources has been proven to give important insights into the underlying physics of particle acceleration in astrophysical environments

Economic incentives for biodiversity conservation: what is the evidence for motivation crowding?

As economic incentives for biodiversity and ecosystem service protection (e.g., payments for ecosystem services) have become widespread in environmental science and policy, a major concern among conservationists and environmental scientists is that economic incentives may undermine people’s intrinsic motivations to conserve biodiversity. In this paper we review the theoretical insights and empirical findings on motivation crowding effects with economic instruments for biodiversity protection. First, we synthesize the psychological mechanisms behind motivation crowding effects relevant for environmental behavior as identified in the specialized literature. We then conduct a systematic review of the empirical evidence. Our results show that, although several empirical studies suggest the existence of crowding-out and crowding-in effects, evidence remains inconclusive due to i) methodological limitations for empirical studies to demonstrate crowding effects, ii) lack of adequate baseline information about pre-existing intrinsic motivations, iii) weak comparability of results across case studies resulting from inconsistent terminology and methods, and iv) the complexity stemming from cultural and contextual heterogeneity. We conclude that, as economic instruments for conservation are increasingly implemented, it becomes paramount to develop robust methodologies for assessing pre-existing intrinsic motivations and changes in people’s motivational structures. To address possible detrimental long term effects for conservation outcomes we call for caution in situations where high uncertainties remain

High energy astroparticle physics for high school students

The questions about the origin and type of cosmic particles are not only fascinating for scientists in astrophysics, but also for young enthusiastic high school students. To familiarize them with research in astroparticle physics, the Pierre Auger Collaboration agreed to make 1% of its data publicly available. The Pierre Auger Observatory investigates cosmic rays at the highest energies and consists of more than 1600 water Cherenkov detectors, located near Malarg\"{u}e, Argentina. With publicly available data from the experiment, students can perform their own hands-on analysis. In the framework of a so-called Astroparticle Masterclass organized alongside the context of the German outreach network Netzwerk Teilchenwelt, students get a valuable insight into cosmic ray physics and scientific research concepts. We present the project and experiences with students.Comment: 8 pages, 5 figures, Proceedings of the 34th International Cosmic Ray Conference (ICRC2015), The Hague, The Netherlands, PoS(ICRC2015)30

Community Seismic Network

The article describes the design of the Community Seismic Network, which is a dense open seismic network based on low cost sensors. The inputs are from sensors hosted by volunteers from the community by direct connection to their personal computers, or through sensors built into mobile devices. The server is cloud-based for robustness and to dynamically handle the load of impulsive earthquake events. The main product of the network is a map of peak acceleration, delivered within seconds of the ground shaking. The lateral variations in the level of shaking will be valuable to first responders, and the waveform information from a dense network will allow detailed mapping of the rupture process. Sensors in buildings may be useful for monitoring the state-of-health of the structure after major shaking

Subthalamic beta band suppression reflects effective neuromodulation in chronic recordings

Background and purpose: Biomarkers for future adaptive deep brain stimulation still need evaluation in clinical routine. Here, we aimed to assess stimulation-induced modulation of beta-band activity and clinical symptoms in a Parkinson's disease patient during chronic neuronal sensing using a novel implantable pulse generator. Methods: Subthalamic activity was recorded OFF and ON medication during a stepwise increase of stimulation amplitude. Off-line fast fourier transfom -based analysis of beta-band activity was correlated with motor performance rated from blinded videos. Results: The stepwise increase of stimulation amplitude resulted in decreased beta oscillatory activity and improvement of bradykinesia. Mean low beta-band (13-20 Hz) activity correlated significantly with bradykinesia (ρ = 0.662, p < 0.01). Conclusions: Motor improvement is reflected in reduced subthalamic beta-band activity in Parkinson's disease, supporting beta activity as a reliable biomarker. The novel PERCEPT neurostimulator enables chronic neuronal sensing in clinical routine. Our findings pave the way for a personalized precision-medicine approach to neurostimulation

Updates on ion and water transport by the Malpighian tubule

The Malpighian (renal) tubule is capable of transporting fluid at remarkable rates. This review will focus on recent insights into the mechanisms by which these high rates are achieved and controlled, with particular reference to the tubules of Drosophila melanogaster, in which the combination of physiology and genetics has led to particularly rapid progress. Like many vertebrate epithelia, the Drosophila tubule has specialized cell types, with active cation transport confined to a large, metabolically active principal cell; whereas the smaller intercalated stellate cell controls chloride and water shunts to achieve net fluid secretion. Recently, the genes underlying many of these processes have been identified, functionally validated and localized within the tubule. The imminent arrival of new types of post-genomic data (notably single cell sequencing) will herald an exciting era of new discovery

Developing composite indicators for ecological water quality assessment based on network interactions and expert judgment

Increasingly, composite indicators and multi-criteria approaches are applied in environmental assessment and decision-making, including the EU Water Framework Directive. For example, integrated evaluation of aquatic ecosystem conditions and functioning usually involves a group of criteria, such as biological organisms and communities, physicochemical and hydromorphological variables, which are measured individually and combined by a weighted linear function into an overall 'score’. We argue that the network interactions of evaluation components are useful information for expert judgments, which have not been sufficiently considered in existing multi-criteria combination strategies in environmental assessment and management. Built upon the Analytic Network Process and demonstrated with the Chishui River Basin in China, this paper introduces a network-based expert judgment approach to construct ecological water quality indicators, and to determine and adjust their variable weight settings with information of interaction networks. This approach has potential to construct composite indicators for a broad environmental context.</p

Yersinia pestis strains from Latvia show depletion of the pla virulence gene at the end of the second plague pandemic

Ancient genomic studies have identified Yersinia pestis (Y. pestis) as the causative agent of the second plague pandemic (fourteenth-eighteenth century) that started with the Black Death (1,347-1,353). Most of the Y. pestis strains investigated from this pandemic have been isolated from western Europe, and not much is known about the diversity and microevolution of this bacterium in eastern European countries. In this study, we investigated human remains excavated from two cemeteries in Riga (Latvia). Historical evidence suggests that the burials were a consequence of plague outbreaks during the seventeenth century. DNA was extracted from teeth of 16 individuals and subjected to shotgun sequencing. Analysis of the metagenomic data revealed the presence of Y. pestis sequences in four remains, confirming that the buried individuals were victims of plague. In two samples, Y. pestis DNA coverage was sufficient for genome reconstruction. Subsequent phylogenetic analysis showed that the Riga strains fell within the diversity of the already known post-Black Death genomes. Interestingly, the two Latvian isolates did not cluster together. Moreover, we detected a drop in coverage of the pPCP1 plasmid region containing the pla gene. Further analysis indicated the presence of two pPCP1 plasmids, one with and one without the pla gene region, and only one bacterial chromosome, indicating that the same bacterium carried two distinct pPCP1 plasmids. In addition, we found the same pattern in the majority of previously published post-Black Death strains, but not in the Black Death strains. The pla gene is an important virulence factor for the infection of and transmission in humans. Thus, the spread of pla-depleted strains may, among other causes, have contributed to the disappearance of the second plague pandemic in eighteenth century Europe

Phylogeography in an "oyster" shell provides first insights into the genetic structure of an extinct Ostrea edulis population

The historical phylogeography of Ostrea edulis was successfully depicted in its native range for the first time using ancient DNA methods on dry shells from museum collections. This research reconstructed the historical population structure of the European flat oyster across Europe in the 1870s-including the now extinct population in the Wadden Sea. In total, four haplogroups were identified with one haplogroup having a patchy distribution from the North Sea to the Atlantic coast of France. This irregular distribution could be the result of translocations. The other three haplogroups are restricted to narrow geographic ranges, which may indicate adaptation to local environmental conditions or geographical barriers to gene flow. The phylogenetic reconstruction of the four haplogroups suggests the signatures of glacial refugia and postglacial expansion. The comparison with present-day O. edulis populations revealed a temporally stable population genetic pattern over the past 150 years despite large-scale translocations. This historical phylogeographic reconstruction was able to discover an autochthonous population in the German and Danish Wadden Sea in the late nineteenth century, where O. edulis is extinct today. The genetic distinctiveness of a now-extinct population hints at a connection between the genetic background of O. edulis in the Wadden Sea and for its absence until today