Statistical properties of Radio Halos and the re-acceleration model

Galaxy clusters occupy a special position in the cosmic hierarchy as they are the largest bound structures in the Universe. There is now general agreement on a hierarchical picture for the formation of cosmic structures, in which galaxy clusters are supposed to form by accretion of matter and merging between smaller units. During merger events, shocks are driven by the gravity of the dark matter in the diffuse barionic component, which is heated up to the observed temperature. Radio and hard-X ray observations have discovered non-thermal components mixed with the thermal Intra Cluster Medium (ICM) and this is of great importance as it calls for a “revision” of the physics of the ICM. The bulk of present information comes from the radio observations which discovered an increasing number of Mpcsized emissions from the ICM, Radio Halos (at the cluster center) and Radio Relics (at the cluster periphery). These sources are due to synchrotron emission from ultra relativistic electrons diffusing through µG turbulent magnetic fields. Radio Halos are the most spectacular evidence of non-thermal components in the ICM and understanding the origin and evolution of these sources represents one of the most challenging goal of the theory of the ICM. Cluster mergers are the most energetic events in the Universe and a fraction of the energy dissipated during these mergers could be channelled into the amplification of the magnetic fields and into the acceleration of high energy particles via shocks and turbulence driven by these mergers. Present observations of Radio Halos (and possibly of hard X-rays) can be best interpreted in terms of the reacceleration scenario in which MHD turbulence injected during these cluster mergers re-accelerates high energy particles in the ICM. The physics involved in this scenario is very complex and model details are difficult to test, however this model clearly predicts some simple properties of Radio Halos (and resulting IC emission in the hard X-ray band) which are almost independent of the details of the adopted physics. In particular in the re-acceleration scenario MHD turbulence is injected and dissipated during cluster mergers and thus Radio Halos (and also the resulting hard X-ray IC emission) should be transient phenomena (with a typical lifetime <» 1 Gyr) associated with dynamically disturbed clusters. The physics of the re-acceleration scenario should produce an unavoidable cut-off in the spectrum of the re-accelerated electrons, which is due to the balance between turbulent acceleration and radiative losses. The energy at which this cut-off occurs, and thus the maximum frequency at which synchrotron radiation is produced, depends essentially on the efficiency of the acceleration mechanism so that observations at high frequencies are expected to catch only the most efficient phenomena while, in principle, low frequency radio surveys may found these phenomena much common in the Universe. These basic properties should leave an important imprint in the statistical properties of Radio Halos (and of non-thermal phenomena in general) which, however, have not been addressed yet by present modellings. The main focus of this PhD thesis is to calculate, for the first time, the expected statistics of Radio Halos in the context of the re-acceleration scenario. In particular, we shall address the following main questions: • Is it possible to model “self-consistently” the evolution of these sources together with that of the parent clusters? • How the occurrence of Radio Halos is expected to change with cluster mass and to evolve with redshift? How the efficiency to catch Radio Halos in galaxy clusters changes with the observing radio frequency? • How many Radio Halos are expected to form in the Universe? At which redshift is expected the bulk of these sources? • Is it possible to reproduce in the re-acceleration scenario the observed occurrence and number of Radio Halos in the Universe and the observed correlations between thermal and non-thermal properties of galaxy clusters? • Is it possible to constrain the magnetic field intensity and profile in galaxy clusters and the energetic of turbulence in the ICM from the comparison between model expectations and observations? Several astrophysical ingredients are necessary to model the evolution and statistical properties of Radio Halos in the context of re-acceleration model and to address the points given above. For these reason we deserve some space in this PhD thesis to review the important aspects of the physics of the ICM which are of interest to catch our goals. In Chapt. 1 we discuss the physics of galaxy clusters, and in particular, the clusters formation process; in Chapt. 2 we review the main observational properties of non-thermal components in the ICM; and in Chapt. 3 we focus on the physics of magnetic field and of particle acceleration in galaxy clusters. As a relevant application, the theory of Alfv´enic particle acceleration is applied in Chapt. 4 where we report the most important results from calculations we have done in the framework of the re-acceleration scenario. In this Chapter we show that a fraction of the energy of fluid turbulence driven in the ICM by the cluster mergers can be channelled into the injection of Alfv´en waves at small scales and that these waves can efficiently re-accelerate particles and trigger Radio Halos and hard X-ray emission. The main part of this PhD work, the calculation of the statistical properties of Radio Halos and non-thermal phenomena as expected in the context of the re-acceleration model and their comparison with observations, is presented in Chapts.5, 6, 7 and 8. In Chapt.5 we present a first approach to semi-analytical calculations of statistical properties of giant Radio Halos. The main goal of this Chapter is to model cluster formation, the injection of turbulence in the ICM and the resulting particle acceleration process. We adopt the semi–analytic extended Press & Schechter (PS) theory to follow the formation of a large synthetic population of galaxy clusters and assume that during a merger a fraction of the PdV work done by the infalling subclusters in passing through the most massive one is injected in the form of magnetosonic waves. Then the processes of stochastic acceleration of the relativistic electrons by these waves and the properties of the ensuing synchrotron (Radio Halos) and inverse Compton (IC, hard X-ray) emission of merging clusters are computed under the assumption of a constant rms average magnetic field strength in emitting volume. The main finding of these calculations is that giant Radio Halos are naturally expected only in the more massive clusters, and that the expected fraction of clusters with Radio Halos is consistent with the observed one. In Chapt. 6 we extend the previous calculations by including a scaling of the magnetic field strength with cluster mass. The inclusion of this scaling allows us to derive the expected correlations between the synchrotron radio power of Radio Halos and the X-ray properties (T, LX) and mass of the hosting clusters. For the first time, we show that these correlations, calculated in the context of the re-acceleration model, are consistent with the observed ones for typical µG strengths of the average B intensity in massive clusters. The calculations presented in this Chapter allow us to derive the evolution of the probability to form Radio Halos as a function of the cluster mass and redshift. The most relevant finding presented in this Chapter is that the luminosity functions of giant Radio Halos at 1.4 GHz are expected to peak around a radio power » 1024 W/Hz and to flatten (or cut-off) at lower radio powers because of the decrease of the electron re-acceleration efficiency in smaller galaxy clusters. In Chapt. 6 we also derive the expected number counts of Radio Halos and compare them with available observations: we claim that » 100 Radio Halos in the Universe can be observed at 1.4 GHz with deep surveys, while more than 1000 Radio Halos are expected to be discovered in the next future by LOFAR at 150 MHz. This is the first (and so far unique) model expectation for the number counts of Radio Halos at lower frequency and allows to design future radio surveys. Based on the results of Chapt. 6, in Chapt.7 we present a work in progress on a “revision” of the occurrence of Radio Halos. We combine past results from the NVSS radio survey (z » 0.05 − 0.2) with our ongoing GMRT Radio Halos Pointed Observations of 50 X-ray luminous galaxy clusters (at z » 0.2−0.4) and discuss the possibility to test our model expectations with the number counts of Radio Halos at z » 0.05 − 0.4. The most relevant limitation in the calculations presented in Chapt. 5 and 6 is the assumption of an “averaged” size of Radio Halos independently of their radio luminosity and of the mass of the parent clusters. This assumption cannot be released in the context of the PS formalism used to describe the formation process of clusters, while a more detailed analysis of the physics of cluster mergers and of the injection process of turbulence in the ICM would require an approach based on numerical (possible MHD) simulations of a very large volume of the Universe which is however well beyond the aim of this PhD thesis. On the other hand, in Chapt.8 we report our discovery of novel correlations between the size (RH) of Radio Halos and their radio power and between RH and the cluster mass within the Radio Halo region, MH. In particular this last “geometrical” MH − RH correlation allows us to “observationally” overcome the limitation of the “average” size of Radio Halos. Thus in this Chapter, by making use of this “geometrical” correlation and of a simplified form of the re-acceleration model based on the results of Chapt. 5 and 6 we are able to discuss expected correlations between the synchrotron power and the thermal cluster quantities relative to the radio emitting region. This is a new powerful tool of investigation and we show that all the observed correlations (PR − RH, PR − MH, PR − T, PR − LX, . . . ) now become well understood in the context of the re-acceleration model. In addition, we find that observationally the size of Radio Halos scales non-linearly with the virial radius of the parent cluster, and this immediately means that the fraction of the cluster volume which is radio emitting increases with cluster mass and thus that the non-thermal component in clusters is not self-similar.

Synthesis and evaluation of 18-F-radiopharmaceuticals within the serotonergic receptor system for molecular imaging

Molecular imaging technologies as Positron Emission Tomography (PET) are playing a key role in drug discovery, development and delivery due to the possibility to quantify e.g. the binding potential in vivo, non-invasively and repetitively. In this context, it provides a significant advance in the understanding of many CNS disorders and conditions. The serotonergic receptor system is involved in a number of important physiological processes and diseases such as depression, schizophrenia, Alzheimer’s disease, sleep or sexual behaviour. Especially, the 5-HT2A and the 5-HT1A receptor subtypes are in the focus of fundamental and clinical research due to the fact that many psychotic drugs interact with these neuronal transmembrane receptors. This work describes the successful development, as well as in vitro and in vivo evaluation of 5-HT2A and 5-HT1A selective antagonistic PET-radiotracers. The major achievements obtained in this thesis are: 1. the development and in vitro evaluation of several 5-HT2A antagonistic compounds, namely MH.MZ (Ki = 9.0 nM), (R)-MH.MZ (Ki = 0.72 nM) and MA-1 (Ki = 3.0 nM). 2. the 18F-labeling procedure of these compounds and their optimization, whereby radiochemical yields > 35 % in high specific activities (> 15 GBq/µmol) could be observed. Synthesis time inclusive secondary synthon synthesis, the radioactive labeling procedure, separation and final formulation took no longer than 120 min and provided the tracer in high radiochemical purity. 3. the in vivo µPET evaluation of [18F]MH.MZ and (R)-[18F]MH.MZ resulting in promising imaging agents of the 5-HT2A receptor status; from which (R)-[18F]MH.MZ seems to be the most promising ligand. 4. the determination of the influence of P-gp on the brain biodistribution of [18F]MH.MZ showing a strong P-gp dependency but no regional alteration. 5. the four-step radiosynthesis and evaluation of [18F]MDL 100907 resulting in another high affine tracer, which is, however, limited due to its low radiochemical yield. 6. the development and evaluation of 3 novel possible 5-HT2A imaging agents combining structural elements of altanserin, MDL 100907 and SR 46349B demonstrating different binding modes of these compounds. 7. the development, the labeling and in vitro evaluation of the novel 5-HT1A antagonistic tracer [18F]AH1.MZ (Ki = 4.2 nM).

Synthese und Evaluierung von [18 F]-Fluormethyltosylat als prosthetische Gruppe für die 18 F-Fluormethylierung von ZNS-Liganden für die PET

Die 11C-Methylierung von Radioliganden ist eine weit verbreitete Markierungsstrategie für PET-Liganden. Aber die kurze Halbwertszeit des Kohlenstoff-11 von 20,3 Minuten limitiert seinen Nutzen. Daher ist die 18F-Fluoralkylierung eine Möglichkeit, Fluor-18, das eine Halbwertszeit von 109,8 Minuten hat, in Target-Moleküle einzuführen. Während die 18F-Fluorethylierung eine weitverbreitete Markierungsstrategie ist, wird die 18F-Fluormethylierung bisher nur selten angewendet. Eine Ursache dafür ist die geringe Stabilität der 18F-Fluormethylgruppe in vivo. Durch Substitution des Wasserstoffs in der 18F-Fluormethylgruppe durch Deuterium kann deren Stabilität jedoch deutlich erhöht werden. Dadurch kann die 18F-Fluormethylierung eine wichtige Synthesestrategie für ZNS-Liganden sein, bei denen große strukturelle Varianz zum Einführen des Fluor-18 nicht möglich ist. rnAls prosthetische Gruppen zur 18F-Fluormethylierung wurden [18F]Fluormethyltosylat und [18F]Fluor-[d2]methyltosylat mit radiochemischen Ausbeuten bis zu 50% synthetisiert. Die Reaktionsbedingungen der 18F-Fluormethylierung mit d2-[18F]FMT und die Abtrennung der Radioliganden wurden an einer Modellverbindungen und den drei Zielstrukturen [18F]Fluor-[d2]methylharmol, [18F]Fluor-[d2]methyl-MH.MZ und [18F]Fluor-[d2]methylflumazenil optimiert. Es konnten radiochemischen Ausbeuten zwischen 25 und 60% erzielt werden. rnMit allen drei ZNS-Liganden wurden Kleintier-PET-Studien durchgeführt. Das d2-[18F]FMH zeigte eine schnelle und 1,5fach höhere Anreicherung im Hirn innerhalb der ersten fünf Minuten als die Vergleichssubstanz [18F]FEH. Für d2-[18F]FM-MH.MZ wurde in vivo eine höhere spezifische Anreicherung des Radiotracers im frontalen Cortex beobachtet als bei der 18F-fluorethylierten Vergleichssubstanz. Für das [18F]Fluor-[d2]methylflumazenil konnte keine Aufnahme ins Hirn festgestellt werden, sondern es kam zur vollständigen Zersetzung des Radioliganden durch Defluorierung. d2-[18F]FMH und d2-[18F]FM-MH.MZ waren bei physiologischen Bedingungen zu mehr als 90% stabil.rn

Entwicklung und Anwendung von mobilen Messstrategien und Analysemethoden zur Untersuchung urbanen Aerosols

Seit Anbeginn der Menschheitsgeschichte beeinflussen die Menschen ihre Umwelt. Durch anthropogene Emissionen ändert sich die Zusammensetzung der Atmosphäre, was einen zunehmenden Einfluss unter anderem auf die Atmosphärenchemie, die Gesundheit von Mensch, Flora und Fauna und das Klima hat. Die steigende Anzahl riesiger, wachsender Metropolen geht einher mit einer räumlichen Konzentration der Emission von Luftschadstoffen, was vor allem einen Einfluss auf die Luftqualität der windabwärts gelegenen ruralen Regionen hat. In dieser Doktorarbeit wurde im Rahmen des MEGAPOLI-Projektes die Abluftfahne der Megastadt Paris unter Anwendung des mobilen Aerosolforschungslabors MoLa untersucht. Dieses ist mit modernen, zeitlich hochauflösenden Instrumenten zur Messung der chemischen Zusammensetzung und Größenverteilung der Aerosolpartikel sowie einiger Spurengase ausgestattet. Es wurden mobile Messstrategien entwickelt und angewendet, die besonders geeignet zur Charakterisierung urbaner Emissionen sind. Querschnittsmessfahrten durch die Abluftfahne und atmosphärische Hintergrundluftmassen erlaubten sowohl die Bestimmung der Struktur und Homogenität der Abluftfahne als auch die Berechnung des Beitrags der urbanen Emissionen zur Gesamtbelastung der Atmosphäre. Quasi-Lagrange’sche Radialmessfahrten dienten der Erkundung der räumlichen Erstreckung der Abluftfahne sowie auftretender Transformationsprozesse der advehierten Luftschadstoffe. In Kombination mit Modellierungen konnte die Struktur der Abluftfahne vertieft untersucht werden. Flexible stationäre Messungen ergänzten den Datensatz und ließen zudem Vergleichsmessungen mit anderen Messstationen zu. Die Daten einer ortsfesten Messstation wurden zusätzlich verwendet, um die Alterung des organischen Partikelanteils zu beschreiben. Die Analyse der mobilen Messdaten erforderte die Entwicklung einer neuen Methode zur Bereinigung des Datensatzes von lokalen Störeinflüssen. Des Weiteren wurden die Möglichkeiten, Grenzen und Fehler bei der Anwendung komplexer Analyseprogramme zur Berechnung des O/C-Verhältnisses der Partikel sowie der Klassifizierung der Aerosolorganik untersucht. Eine Validierung verschiedener Methoden zur Bestimmung der Luftmassenherkunft war für die Auswertung ebenfalls notwendig. Die detaillierte Untersuchung der Abluftfahne von Paris ergab, dass diese sich anhand der Erhöhung der Konzentrationen von Indikatoren für unprozessierte Luftverschmutzung im Vergleich zu Hintergrundwerten identifizieren lässt. Ihre eher homogene Struktur kann zumeist durch eine Gauß-Form im Querschnitt mit einem exponentiellen Abfall der unprozessierten Schadstoffkonzentrationen mit zunehmender Distanz zur Stadt beschrieben werden. Hierfür ist hauptsächlich die turbulente Vermischung mit Umgebungsluftmassen verantwortlich. Es konnte nachgewiesen werden, dass in der advehierten Abluftfahne eine deutliche Oxidation der Aerosolorganik im Sommer stattfindet; im Winter hingegen ließ sich dieser Prozess während der durchgeführten Messungen nicht beobachten. In beiden Jahreszeiten setzt sich die Abluftfahne hauptsächlich aus Ruß und organischen Partikelkomponenten im PM1-Größenbereich zusammen, wobei die Quellen Verkehr und Kochen sowie zusätzlich Heizen in der kalten Jahreszeit dominieren. Die PM1-Partikelmasse erhöhte sich durch die urbanen Emissionen im Vergleich zum Hintergrundwert im Sommer in der Abluftfahne im Mittel um 30% und im Winter um 10%. Besonders starke Erhöhungen ließen sich für Polyaromaten beobachten, wo im Sommer eine mittlere Zunahme von 194% und im Winter von 131% vorlag. Jahreszeitliche Unterschiede waren ebenso in der Größenverteilung der Partikel der Abluftfahne zu finden, wo im Winter im Gegensatz zum Sommer keine zusätzlichen nukleierten kleinen Partikel, sondern nur durch Kondensation und Koagulation angewachsene Partikel zwischen etwa 10nm und 200nm auftraten. Die Spurengaskonzentrationen unterschieden sich ebenfalls, da chemische Reaktionen temperatur- und mitunter strahlungsabhängig sind. Weitere Anwendungsmöglichkeiten des MoLa wurden bei einer Überführungsfahrt von Deutschland an die spanische Atlantikküste demonstriert, woraus eine Kartierung der Luftqualität entlang der Fahrtroute resultierte. Es zeigte sich, dass hauptsächlich urbane Ballungszentren von unprozessierten Luftschadstoffen betroffen sind, advehierte gealterte Substanzen jedoch jede Region beeinflussen können. Die Untersuchung der Luftqualität an Standorten mit unterschiedlicher Exposition bezüglich anthropogener Quellen erweiterte diese Aussage um einen Einblick in die Variation der Luftqualität, abhängig unter anderem von der Wetterlage und der Nähe zu Emissionsquellen. Damit konnte gezeigt werden, dass sich die entwickelten Messstrategien und Analysemethoden nicht nur zur Untersuchung der Abluftfahne einer Großstadt, sondern auch auf verschiedene andere wissenschaftliche und umweltmesstechnische Fragestellungen anwenden lassen.

Stationary in-situ measurements of aerosols, gaseous pollutants and meteorology : chemical and physical characterization of natural and anthropogenic sources

Natural and anthropogenic emissions of gaseous and particulate matter affect the chemical composition of the atmosphere, impact visibility, air quality, clouds and climate. Concerning climate, a comprehensive characterization of the emergence, composition and transformation of aerosol particles is relevant as their influence on the radiation budget is still rarely understood. Regarding air quality and therefore human health, the formation of atmospheric aerosol particles is of particular importance as freshly formed, small particles penetrate into the human alveolar region and can deposit. Additionally, due to the long residence times of aerosol particles in the atmosphere it is crucial to examine their chemical and physical characteristics.This cumulative dissertation deals with stationary measurements of particles, trace gases and meteorological parameters during the DOMINO (Diel Oxidant Mechanism In relation to Nitrogen Oxide) campaign at the southwest coast of Spain in November/December 2008 and the ship emission campaign on the banks of the Elbe in Freiburg/Elbe in April 2011. Measurements were performed using the Mobile research Laboratory “MoLa” which is equipped with state-of-the-art aerosol particle and trace gas instruments as well as a meteorological station.

Connection between x-ray and radio properties of cool-core galaxy clusters hosting radio mini-halos

Gli ammassi di galassie sono gli oggetti gravitazionalmente legati più grandi dell’Universo. Questi emettono principalmente in banda X tramite bremsstrahlung. Una frazione mostra anche emissione radio diffusa da parte di elettroni relativistici che spiraleggiano nel campo magnetico. Si possono classificare tre tipi di emissione: alon, relitti e mini-aloni radio (MH). I MH sono sorgenti radio su scale di ≥ 200 – 500 kpc, osservate al centro di ammassi caratterizzati dalla presenze di cool-core (CC). L’origine dei MH non è ancora chiara. Gli elettroni relativistici che emettono in banda radio hanno tempi di vita radiativi di molto inferiori a quelli necessari per diffondere sulle scale dell’emissione diffusa. Quindi non sono semplicemente iniettati dalle galassie presenti negli ammassi ed è necessario un meccanismo di accelerazione “in-situ” nell’ICM. I MH testimoniano la presenza di meccanismi che canalizzano parte del budget energetico disponibile nei CC nell’ICM.Quindi lo studio è importante per comprendere la fisica dell’ICM e l’interazione fra le componenti non termiche e termiche. I MH si formano attraverso la riaccelerazione delle particelle relativistiche ad opera della turbolenza del gas. L’origine di questa turbolenza tuttavia non è ancora ben compresa. Gli ammassi CC sono caratterizzati da un picco della brillanza X nelle regioni centrali e da un drop della temperatura verso il centro accompagnata da aumento della densità del gas. Si ritiene che questo sia dovuto al raffreddamento del gas che quindi fluisce nelle zone centrali. Recenti osservazioni in X risultan inconsistenti con il modello classico di CF, suggerendo la presenza di una sorgente di riscaldamento del gas su scale del core degli ammassi. Recentemente Zhuravleva (2014) hanno mostrato che il riscaldamento dovuto alla turbolenza prodotta dall'AGN centrale è in grado di bilanciare il processo di raffreddamento. Abbiamo assunto che la turbolenza responsabile del riscaldamento del gas è anche responsabile dell’accelerazione delle particelle nei MH. Nell’ambito di questo scenario ci si aspetta una correlazione tra la potenza del cooling flow, PCF, che è una misura del tasso di energia emessa dal gas che raffredda nei CC, e la luminosità radio, che è una frazione dell’energia della turbolenza che è canalizzata nell’accelerazione delle particelle. In questo lavoro di tesi abbiamo utilizzato il più grande campione disponibile di MH, allo scopo di studiare la connessione fra le proprietà dei MH e quelle del gas termico nei core degli ammassi che li ospitano. Abbiamo analizzato i dati di 21 ammassi e ricavato i parametri fisici all’interno del raggio di cooling e del MH. Abbiamo ricavato la correlazione fra luminosità radio, e PCF. Abbiamo trovato che le due quantità correlano in modo quasi-lineare confermando i risultati precedenti. Tale correlazione suggerisce uno stretto legame fra le proprietà del gas nei CC e l’origine dei MH.

Development, characterization, and application of flowing atmospheric-pressure afterglow ionization for mass spectrometric analysis of ambient organic aerosols

Addressing current limitations of state-of-the-art instrumentation in aerosol research, the aim of this work was to explore and assess the applicability of a novel soft ionization technique, namely flowing atmospheric-pressure afterglow (FAPA), for the mass spectrometric analysis of airborne particulate organic matter. Among other soft ionization methods, the FAPA ionization technique was developed in the last decade during the advent of ambient desorption/ionization mass spectrometry (ADI–MS). Based on a helium glow discharge plasma at atmospheric-pressure, excited helium species and primary reagent ions are generated which exit the discharge region through a capillary electrode, forming the so-called afterglow region where desorption and ionization of the analytes occurs. Commonly, fragmentation of the analytes during ionization is reported to occur only to a minimum extent, predominantly resulting in the formation of quasimolecular ions, i.e. [M+H]+ and [M–H]– in the positive and the negative ion mode, respectively. Thus, identification and detection of signals and their corresponding compounds is facilitated in the acquired mass spectra. The focus of the first part of this study lies on the application, characterization and assessment of FAPA–MS in the offline mode, i.e. desorption and ionization of the analytes from surfaces. Experiments in both positive and negative ion mode revealed ionization patterns for a variety of compound classes comprising alkanes, alcohols, aldehydes, ketones, carboxylic acids, organic peroxides, and alkaloids. Besides the always emphasized detection of quasimolecular ions, a broad range of signals for adducts and losses was found. Additionally, the capabilities and limitations of the technique were studied in three proof-of-principle applications. In general, the method showed to be best suited for polar analytes with high volatilities and low molecular weights, ideally containing nitrogen- and/or oxygen functionalities. However, for compounds with low vapor pressures, containing long carbon chains and/or high molecular weights, desorption and ionization is in direct competition with oxidation of the analytes, leading to the formation of adducts and oxidation products which impede a clear signal assignment in the acquired mass spectra. Nonetheless, FAPA–MS showed to be capable of detecting and identifying common limonene oxidation products in secondary OA (SOA) particles on a filter sample and, thus, is considered a suitable method for offline analysis of OA particles. In the second as well as the subsequent parts, FAPA–MS was applied online, i.e. for real time analysis of OA particles suspended in air. Therefore, the acronym AeroFAPA–MS (i.e. Aerosol FAPA–MS) was chosen to refer to this method. After optimization and characterization, the method was used to measure a range of model compounds and to evaluate typical ionization patterns in the positive and the negative ion mode. In addition, results from laboratory studies as well as from a field campaign in Central Europe (F–BEACh 2014) are presented and discussed. During the F–BEACh campaign AeroFAPA–MS was used in combination with complementary MS techniques, giving a comprehensive characterization of the sampled OA particles. For example, several common SOA marker compounds were identified in real time by MSn experiments, indicating that photochemically aged SOA particles were present during the campaign period. Moreover, AeroFAPA–MS was capable of detecting highly oxidized sulfur-containing compounds in the particle phase, presenting the first real-time measurements of this compound class. Further comparisons with data from other aerosol and gas-phase measurements suggest that both particulate sulfate as well as highly oxidized peroxyradicals in the gas phase might play a role during formation of these species. Besides applying AeroFAPA–MS for the analysis of aerosol particles, desorption processes of particles in the afterglow region were investigated in order to gain a more detailed understanding of the method. While during the previous measurements aerosol particles were pre-evaporated prior to AeroFAPA–MS analysis, in this part no external heat source was applied. Particle size distribution measurements before and after the AeroFAPA source revealed that only an interfacial layer of OA particles is desorbed and, thus, chemically characterized. For particles with initial diameters of 112 nm, desorption radii of 2.5–36.6 nm were found at discharge currents of 15–55 mA from these measurements. In addition, the method was applied for the analysis of laboratory-generated core-shell particles in a proof-of-principle study. As expected, predominantly compounds residing in the shell of the particles were desorbed and ionized with increasing probing depths, suggesting that AeroFAPA–MS might represent a promising technique for depth profiling of OA particles in future studies.

Juice of Bryophyllum pinnatum (Lam.) inhibits oxytocin-induced increase of the intracellular calcium concentration in human myometrial cells

http://www.ncbi.nlm.nih.gov/pubmed/20381326

Everolimus augments the effects of sorafenib in a syngeneic orthotopic model of hepatocellular carcinoma

Sorafenib targets the Raf/mitogen-activated protein kinase, VEGF, and platelet-derived growth factor pathways and prolongs survival patients in advanced hepatocellular carcinoma (HCC). Everolimus inhibits the mammalian target of rapamycin, a kinase overactive in HCC. To investigate whether the antitumor effects of these agents are additive, we compared a combined and sequential treatment regimen of everolimus and sorafenib with monotherapy. After hepatic implantation of Morris Hepatoma (MH) cells, rats were randomly allocated to everolimus (5 mg/kg, 2×/week), sorafenib (7.5 mg/kg/d), combined everolimus and sorafenib, sequential sorafenib (2 weeks) then everolimus (3 weeks), or control groups. MRI quantified tumor volumes. Erk1/2, 4E-BP1, and their phosphorylated forms were quantified by immunoblotting. Angiogenesis was assessed in vitro by aortic ring and tube formation assays, and in vivo with Vegf-a mRNA and vascular casts. After 35 days, tumor volumes were reduced by 60%, 85%, and 55%, relative to controls, in everolimus, the combination, and sequential groups, respectively (P < 0.01). Survival was longest in the combination group (P < 0.001). Phosphorylation of 4E-BP1 and Erk1/2 decreased after everolimus and sorafenib, respectively. Angiogenesis decreased after all treatments (P < 0.05), although sorafenib increased Vegf-a mRNA in liver tumors. Vessel sprouting was abundant in control tumors, lower after sorafenib, and absent after the combination. Intussusceptive angiogenic transluminal pillars failed to coalesce after the combination. Combined treatment with everolimus and sorafenib exerts a stronger antitumoral effect on MH tumors than monotherapy. Everolimus retains antitumoral properties when administered sequentially after sorafenib. This supports the clinical use of everolimus in HCC, both in combination with sorafenib or after sorafenib.

A protective antiarrhythmic role of ursodeoxycholic acid in an in vitro rat model of the cholestatic fetal heart

Intrahepatic cholestasis of pregnancy may be complicated by fetal arrhythmia, fetal hypoxia, preterm labor, and, in severe cases, intrauterine death. The precise etiology of fetal death is not known. However, taurocholate has been demonstrated to cause arrhythmia and abnormal calcium dynamics in cardiomyocytes. To identify the underlying reason for increased susceptibility of fetal cardiomyocytes to arrhythmia, we studied myofibroblasts (MFBs), which appear during structural remodeling of the adult diseased heart. In vitro, they depolarize rat cardiomyocytes via heterocellular gap junctional coupling. Recently, it has been hypothesized that ventricular MFBs might appear in the developing human heart, triggered by physiological fetal hypoxia. However, their presence in the fetal heart (FH) and their proarrhythmogenic effects have not been systematically characterized. Immunohistochemistry demonstrated that ventricular MFBs transiently appear in the human FH during gestation. We established two in vitro models of the maternal heart (MH) and FH, both exposed to increasing doses of taurocholate. The MH model consisted of confluent strands of rat cardiomyocytes, whereas for the FH model, we added cardiac MFBs on top of cardiomyocytes. Taurocholate in the FH model, but not in the MH model, slowed conduction velocity from 19 to 9 cm/s, induced early after depolarizations, and resulted in sustained re-entrant arrhythmias. These arrhythmic events were prevented by ursodeoxycholic acid, which hyperpolarized MFB membrane potential by modulating potassium conductance. CONCLUSION: These results illustrate that the appearance of MFBs in the FH may contribute to arrhythmias. The above-described mechanism represents a new therapeutic approach for cardiac arrhythmias at the level of MFB.