A spectroscopic and photometric study of MSP companions in Galactic Globular Clusters

This Thesis is devoted to the study of the optical companions of Millisecond Pulsars in Galactic Globular Clusters (GCs) as a part of a large project started at the Department of Astronomy of the Bologna University, in collaboration with other institutions (Astronomical Observatory of Cagliari and Bologna, University of Virginia), specifically dedicated to the study of the environmental effects on passive stellar evolution in galactic GCs. Globular Clusters are very efficient “Kilns” for generating exotic object, such as Millisecond Pulsars (MSP), low mass X-ray binaries(LMXB) or Blue Straggler Stars (BSS). In particular MSPs are formed in binary systems containing a Neutron Star which is spun up through mass accretion from the evolving companion (e.g. Bhattacharia & van den Heuvel 1991). The final stage of this recycling process is either the core of a peeled star (generally an Helium white dwarf) or a very light almos exhausted star, orbiting a very fast rotating Neutron Star (a MSP). Despite the large difference in total mass between the disk of the Galaxy and the Galactic GC system (up a factor 103), the percentage of fast rotating pulsar in binary systems found in the latter is very higher. MSPs in GCs show spin periods in the range 1.3 ÷ 30ms, slowdown rates ˙P 1019 s/s and a lower magnetic field, respect to ”normal” radio pulsars, B 108 gauss . The high probability of disruption of a binary systems after a supernova explosion, explain why we expect only a low percentage of recycled millisecond pulsars respect to the whole pulsar population. In fact only the 10% of the known 1800 radio pulsars are radio MSPs. Is not surprising, that MSP are overabundant in GCs respect to Galactic field, since in the Galactic Disk, MSPs can only form through the evolution of primordial binaries, and only if the binary survives to the supernova explosion which lead to the neutron star formation. On the other hand, the extremely high stellar density in the core of GCs, relative to most of the rest of the Galaxy, favors the formation of several different binary systems, suitable for the recycling of NSs (Davies at al. 1998). In this thesis we will present the properties two millisecond pulsars companions discovered in two globular clusters, the Helium white dwarf orbiting the MSP PSR 1911-5958A in NGC 6752 and the second case of a tidally deformed star orbiting an eclipsing millisecond pulsar, PSR J1701-3006B in NGC6266

A spectroscopic and photometric study of stellar populations in a sample of clusters in the Magellanic Clouds

This Ph.D. Thesis has been carried out in the framework of a long-term and large project devoted to describe the main photometric, chemical, evolutionary and integrated properties of a representative sample of Large and Small Magellanic Cloud (LMC and SMC respectively) clusters. The globular clusters system of these two Irregular galaxies provides a rich resource for investigating stellar and chemical evolution and to obtain a detailed view of the star formation history and chemical enrichment of the Clouds. The results discussed here are based on the analysis of high-resolution photometric and spectroscopic datasets obtained by using the last generation of imagers and spectrographs. The principal aims of this project are summarized as follows: • The study of the AGB and RGB sequences in a sample of MC clusters, through the analysis of a wide near-infrared photometric database, including 33 Magellanic globulars obtained in three observing runs with the near-infrared camera SOFI@NTT (ESO, La Silla). • The study of the chemical properties of a sample of MCs clusters, by using optical and near-infrared high-resolution spectra. 3 observing runs have been secured to our group to observe 9 LMC clusters (with ages between 100 Myr and 13 Gyr) with the optical high-resolution spectrograph FLAMES@VLT (ESO, Paranal) and 4 very young (<30 Myr) clusters (3 in the LMC and 1 in the SMC) with the near-infrared high-resolution spectrograph CRIRES@VLT. • The study of the photometric properties of the main evolutive sequences in optical Color- Magnitude Diagrams (CMD) obtained by using HST archive data, with the final aim of dating several clusters via the comparison between the observed CMDs and theoretical isochrones. The determination of the age of a stellar population requires an accurate measure of the Main Sequence (MS) Turn-Off (TO) luminosity and the knowledge of the distance modulus, reddening and overall metallicity. For this purpose, we limited the study of the age just to the clusters already observed with high-resolution spectroscopy, in order to date only clusters with accurate estimates of the overall metallicity.

Mechanismen der Aktivierung und Detoxifizierung von Aflatoxin B 1 in verschiedenen Leberzelltypen von Ratten, Mäusen und Waldmurmeltieren

Zusammenfassung: Die Applikation des Mykotoxins Aflatoxin B1 (AFB1) führt in der Ratte zu Lebertumoren hepatozellulären Ursprungs, während bisher keine transformierende Wirkung dieses Mykotoxins auf Kupffer- und Endothelzellen (Nichtparenchymzellen, NPC) nachgewiesen werden konnte. Diese Resistenzmechanismen der NPC gegenüber AFB1 wurden im ersten Teil dieser Arbeit untersucht. AFB1 ist per se inaktiv, wird jedoch durch Verstoffwechselung in den chemisch reaktiven, an DNA bindenden Metaboliten AFB1-8,9-Epoxid überführt. Daneben stellt die enzymatische Hydroxylierung von AFB1 am Kohlenstoff-9a zum Aflatoxin M1 eine Detoxifizierung dar. Durch HPLC-Analyse der AFB1-Metabolite konnte gezeigt werden, daß in Nichtparenchymzellen (NPC) das Verhältnis von 9a-Hydroxylierung zu 8,9-Epoxidierung höher als in Parenchymzellen (PC) ist. Die AFB1-9a-hydroxylase fördert insbesondere in den NPC der Leber die Bildung des weniger gentoxischen Metaboliten AFM1 und konkurriert daher um die Aktivierung von AFB1 zum mutagenen und kanzerogenen 8,9-Epoxid. Dieser metabolische Unterschied scheint also einen Beitrag zur Resistenz der NPC der Leber gegenüber der hepatokanzerogenen Wirkung von AFB1 zu leisten. Da ein Synergismus zwischen der AFB1-Exposition und einer Infektion mit dem Hepatitis B-Virus (HBV) beim Menschen bezüglich des Auftretens von hepatozellulären Karzinomen zu bestehen scheint, wurde im zweiten Teil dieser Arbeit untersucht, ob die metabolische Aktivierung von AFB1 durch eine HBV-Infektion verstärkt wird. In einem Vergleich der Biotransformation von AFB1 mit mikrosomalen Leberfraktionen von transgenen HBV-Mäusen und Kontrollmäusen wurde keine signifikanten Unterschiede festgestellt. Dagegen wurde bei Virus-infizierten Waldmurmeltieren eine deutlich reduzierte Bildung des AFB1-8,9-Epoxids beobachtet. Es konnte z.T. ein Zusammenhang zwischen den verschiedenen Stadien der Leberschädigung und den Metabolismusraten festgestellt werden, wobei die metabolische Aktivierung mit zunehmender Leberschädigung abzunehmen scheint. Auch hinsichtlich der Aktivitäten verschiedener Cytochrom P450 abhängiger Monooxygenasen wurde eine weitgehende Übereinstimmung mit den durch HPLC ermittelten Metabolitenprofilen des AFB1 beobachtet. Diese Studien mit subzellulären Leberfraktion der transgenen HBV-Mäusen und der Waldmurmeltieren zeigen, daß die Interaktion zwischen Hepatitis und AFB1 nicht mit der verstärkten metabolischer Aktivierung von AFB1 zu erklären ist. TGF-ß1, aus der Gruppe der Cytokine, wird als Mediator bei Entzündungsprozessen in der Leber so z.B. im Verlauf einer Virushepatitis freigesetzt. Aufgrund der besonderen Bedeutung des murinen CYP2A5 (ortholog zum humanen CYP2A6) bei der Aktivierung von AFB1 wurde der Einfluß von TGF-ß1 auf CYP2A5 in Primärkulturen von Maushepatozyten untersucht. Durch Messung der Aktivität der Cumarin-7-hydroxylase sowie durch Bestimmung der Proteinmenge von CYP2A5 mittels Western Blotting konnte zunächst die Induzierbarkeit des CYP2A5-Isoenzyms durch Phenobarbital in kultivierten Hepatozyten der Maus gezeigt werden. Nur bei einer niedrigen TGF-ß1-Konzentration wurde eine leicht erhöhte Expression von CYP2A5 festgestellt, ansonsten führte die Behandlung der kultivierten Maushepatozyten mit TGF-ß1 zu einer dosisabhängigen Verminderung der Expression von CYP2A5.

Synthese und Charakterisierung von Poly(tert-butylacrylat)- und Polyacrylsäure-Sternpolymeren

Sternpolymere aus Poly(tert.-butylacrylat)-Armen und einem Mikrogel-Core aus Ethylenglykoldimethacrylat wurden nach der arm-first Strategie hergestellt. Diese weisen eine enge Armzahlverteilung auf. Mit sinkender Precursorlänge, mit steigendem Verhältnis [bifunktionelles Monomer]/[Initiator], sowie mit zunehmender Reaktionszeit und Gesamtkonzentration nimmt die mittlere Armzahl fn zu. Die Sternbildung verläuft ähnlich einer Polykondensation. Die Molekulargewichte wurden mittels GPC gekoppelt mit einem online-Viskosimeter und einem online-Vielwinkellichtstreudetektor (MALLS) bestimmt.Die intrinsischen Viskositäten der Sternpolymere sind sehr niedrig. Für Armzahlen f ca. 8 erhält man ein Maximum in der doppellogarithmischen Auftragung der intrinsischen Viskosität und des Molekulargewichts. Die Trägheitsradien nehmen nur wenig mit dem Molekulargewicht zu. Die erhaltenen Koeffizienten liegen im von Daoud und Cotton vorhergesagten Bereich. Die Schrumpfungsfaktoren sinken auf g ca. 0,2 bzw. g' ca. 0,25. Aus den Poly(tert.-butylacrylat)-Sternpolymeren wurden durch Verseifung mit HBr in Methanol Polyacrylsäure-Sternpolymere hergestellt, welche ebenfalls mittels GPC-Viskosimetrie und GPC-MALLS charakterisiert wurden. Für die ionischen Sternpolymere findet man deutlich höhere Schrumpfungsfaktoren, kein Maximum in der intrinsischen Viskosität und höhere Exponenten als von Daoud und Cotton vorhergesagt. Erklärt wurde dies mit der hohen Segmentdichte in Sternpolymeren, die bei den ionischen Sternpolymeren zu einer hohen Ladungsdichte führt. Dadurch müssen sich die Arme stärker strecken als bei nicht-ionischen Sternen und es resultieren größere Moleküldimensionen.

Millimeter characteristics of Galactic and extragalactic starbursts

The goal of the thesis was to compare Galactic and extragalactic star-forming environments, to understand whether we can derive scaling relations for the extragalactic star formation from our understanding of the Galactic star formation; and to analyze the effect of the angular resolution of the observations and the molecular tracer used in extragalactic studies. It is therefore necessary to perform observations at the same linear resolution in both cases. With this in mind we have started a program aimed at comparing properties of mini-starburst regions in our Galaxy and starbursts in nearby galaxies at similar linear resolutions.

A panchromatic view of the evolution of supermassive black holes

This PhD Thesis is devoted to the accurate analysis of the physical properties of Active Galactic Nuclei (AGN) and the AGN/host-galaxy interplay. Due to the broad-band AGN emission (from radio to hard X-rays), a multi-wavelength approach is mandatory. Our research is carried out over the COSMOS field, within the context of the XMM-Newton wide-field survey. To date, the COSMOS field is a unique area for comprehensive multi-wavelength studies, allowing us to define a large and homogeneous sample of QSOs with a well-sampled spectral coverage and to keep selection effects under control. Moreover, the broad-band information contained in the COSMOS database is well-suited for a detailed analysis of AGN SEDs, bolometric luminosities and bolometric corrections. In order to investigate the nature of both obscured (Type-2) and unobscured (Type-1) AGN, the observational approach is complemented with a theoretical modelling of the AGN/galaxy co-evolution. The X-ray to optical properties of an X-ray selected Type-1 AGN sample are discussed in the first part. The relationship between X-ray and optical/UV luminosities, parametrized by the spectral index αox, provides a first indication about the nature of the central engine powering the AGN. Since a Type-1 AGN outshines the surrounding environment, it is extremely difficult to constrain the properties of its host-galaxy. Conversely, in Type-2 AGN the host-galaxy light is the dominant component of the optical/near-IR SEDs, severely affecting the recovery of the intrinsic AGN emission. Hence a multi-component SED-fitting code is developed to disentangle the emission of the stellar populationof the galaxy from that associated with mass accretion. Bolometric corrections, luminosities, stellar masses and star-formation rates, correlated with the morphology of Type-2 AGN hosts, are presented in the second part, while the final part concerns a physically-motivated model for the evolution of spheroidal galaxies with a central SMBH. The model is able to reproduce two important stages of galaxy evolution, namely the obscured cold-phase and the subsequent quiescent hot-phase.

Dynamics of the halo gas in disc galaxies

This Thesis studies the dynamics of hot and cold gas outside the plane in galaxies like the Milky-Way (extra-planar gas) and focuses on the interaction between disc and halo material. Stationary models for the cold phase of the extra-planar gas are presented. They show that the kinematics of this phase must be influenced by the interaction with an ambient medium that we identify as the hot cosmological corona that surrounds disc galaxies. To study this interaction a novel hydrodynamical code has been implemented and a series of hydrodynamical simulations has been run to investigate the mass and momentum exchange between the cold extra-planar gas clouds and the hot corona. These simulations show that the coronal gas can condense efficiently in the turbulent wakes that form behind the cold clouds and it can be accreted by the disc to sustain star formation. They also predict that the corona cannot be a static structure but it must rotate and lag by approximately 80-120 km/s with respect to the disc. Implications of the results of this Thesis for the evolution of star-forming galaxies and for the large-scale dynamics of galactic coronae are also briefly discussed.

Hydrodynamical simulations of galaxy clusters in dark energy cosmologies

In this work we investigate the influence of dark energy on structure formation, within five different cosmological models, namely a concordance $\Lambda$CDM model, two models with dynamical dark energy, viewed as a quintessence scalar field (using a RP and a SUGRA potential form) and two extended quintessence models (EQp and EQn) where the quintessence scalar field interacts non-minimally with gravity (scalar-tensor theories). We adopted for all models the normalization of the matter power spectrum $\sigma_{8}$ to match the CMB data. For each model, we perform hydrodynamical simulations in a cosmological box of $(300 \ {\rm{Mpc}} \ h^{-1})^{3}$ including baryons and allowing for cooling and star formation. We find that, in models with dynamical dark energy, the evolving cosmological background leads to different star formation rates and different formation histories of galaxy clusters, but the baryon physics is not affected in a relevant way. We investigate several proxies for the cluster mass function based on X-ray observables like temperature, luminosity, $M_{gas}$, and $Y_{X}$. We confirm that the overall baryon fraction is almost independent of the dark energy models within few percentage points. The same is true for the gas fraction. This evidence reinforces the use of galaxy clusters as cosmological probe of the matter and energy content of the Universe. We also study the $c-M$ relation in the different cosmological scenarios, using both dark matter only and hydrodynamical simulations. We find that the normalization of the $c-M$ relation is directly linked to $\sigma_{8}$ and the evolution of the density perturbations for $\Lambda$CDM, RP and SUGRA, while for EQp and EQn it depends also on the evolution of the linear density contrast. These differences in the $c-M$ relation provide another way to use galaxy clusters to constrain the underlying cosmology.

Galaxy evolution in the VIMOS public extragalactic redshift survey (VIPERS)

In this work I present the first measurements of the galaxy stellar mass function (GSMF) from the first public release of the VIPERS catalogue, containing ∼55,000 objects. First, I present the survey design, its scientific goal, the redshift measurements and validation. Then, I provide details about the estimate of galaxy stellar masses, star formation rates, and other physical quantities. I derive the GSMF of different galaxy types (e.g. active and passive galaxies) and as a function of the environment (defined through the local galaxy density contrast). These estimates represent new observational evidence useful to characterise the mechanism of galaxy evolution.

Extracting evolutionary information from the spectral decomposition of early-type galaxies.

Holding the major share of stellar mass in galaxies and being also old and passively evolving, early-type galaxies (ETGs) are the primary probes in investigating these various evolution scenarios, as well as being useful means to provide insights on cosmological parameters. In this thesis work I focused specifically on ETGs and on their capability in constraining galaxy formation and evolution; in particular, the principal aims were to derive some of the ETGs evolutionary parameters, such as age, metallicity and star formation history (SFH) and to study their age-redshift and mass-age relations. In order to infer galaxy physical parameters, I used the public code STARLIGHT: this program provides a best fit to the observed spectrum from a combination of many theoretical models defined in user-made libraries. the comparison between the output and input light-weighted ages shows a good agreement starting from SNRs of ∼ 10, with a bias of ∼ 2.2% and a dispersion 3%. Furthermore, also metallicities and SFHs are well reproduced. In the second part of the thesis I performed an analysis on real data, starting from Sloan Digital Sky Survey (SDSS) spectra. I found that galaxies get older with cosmic time and with increasing mass (for a fixed redshift bin); absolute light-weighted ages, instead, result independent from the fitting parameters or the synthetic models used. Metallicities, instead, are very similar from each other and clearly consistent with the ones derived from the Lick indices. The predicted SFH indicates the presence of a double burst of star formation. Velocity dispersions and extinctiona are also well constrained, following the expected behaviours. As a further step, I also fitted single SDSS spectra (with SNR∼ 20), to verify that stacked spectra gave the same results without introducing any bias: this is an important check, if one wants to apply the method at higher z, where stacked spectra are necessary to increase the SNR. Our upcoming aim is to adopt this approach also on galaxy spectra obtained from higher redshift Surveys, such as BOSS (z ∼ 0.5), zCOSMOS (z 1), K20 (z ∼ 1), GMASS (z ∼ 1.5) and, eventually, Euclid (z 2). Indeed, I am currently carrying on a preliminary study to estabilish the applicability of the method to lower resolution, as well as higher redshift (z 2) spectra, just like the Euclid ones.

The relationship between coagulation and the extend of surgery and postoperative infection in surgical infants below 6 months of age

AIM: First to assess coagulation changes after surgery in children below 6 months of age. Second to detect differences attributable to the extent of surgery and postoperative infection. MATERIALS AND METHODS: Blood counts, haemoglobin concentration (Hb), haematocrit (Ht), prothrombine time (PT), activated partial thromboplastine time (aPTT) and thrombelastography (TEG) were studied pre- and 2+/-1/2 d postoperatively. Patients were divided in 3 groups. I: minor surgery without access to the abdomen or thorax (n=51); II: abdominal or thoracic interventions (n=24); III: abdominal surgery with postoperative sepsis (n=11). RESULTS: Preoperative values of Hb, Ht and INR were related to the age of the infant. Postoperatively clot strength and formation rate increased in gr. I (p<0.05). In gr. II, clot formation was initiated earlier (p<0.05) even though PT decreased (p<0.05). In group III, patients postoperatively developed a tendency for hypocoagulability in all TEG-parameters, but not in plasmatic coagulation. Postoperative TEG measurements were significantly inferior in gr. III when compared to gr. I and II. CONCLUSION: Our findings suggest activation of whole blood coagulation in the uncomplicated postoperative period despite of a decrease in plasmatic coagulation. In sepsis, only thrombelastography, but not plasmatic coagulation was affected.

Effects of growth hormone (GH) replacement therapy on low-density lipoprotein apolipoprotein B100 kinetics in adult patients with GH deficiency: a stable isotope study

GH replacement therapy has been shown to improve the dyslipidemic condition in a substantial proportion of patients with adult GH deficiency. The mechanisms are not yet fully elucidated. Low-density lipoprotein (LDL) apolipoprotein B100 (apoB) formation and catabolism are important determinants of plasma cholesterol concentrations. This study examined the effect of GH replacement therapy on LDL apoB metabolism using a stable isotope turnover technique. LDL apoB kinetics was determined in 13 adult patients with GH deficiency before and after 3 months GH/placebo treatment in a randomized, double-blind, placebo-controlled study. LDL apoB (13)C-leucine enrichment was determined by isotope-ratio mass spectrometry. Plasma volume was assessed by standardized radionuclide dilution technique. GH replacement therapy significantly decreased LDL cholesterol, LDL apoB concentrations, and LDL apoB pool size compared with placebo. Compared with baseline, GH replacement therapy resulted in a significant increase in plasma volume and fractional catabolic rate, whereas LDL formation rate remained unchanged. LDL lipid content did not significantly change after GH and placebo. This study suggests that short-term GH replacement therapy decreases the LDL apoB pool by increasing removal of LDL particles without changing LDL composition or LDL apoB production rate. In addition, it is possible that the beneficial effects of GH on the cardiovascular system contribute to these findings.

Assessment of BoviPureTM for the In Vitro Production of Bovine Embryos

The objective of this study was to examine the potential utility of a commercially available sperm separation and purification product for the in vitro production of bovine embryos. Bovine oocytes were purchased from a commercial supplier, and matured oocytes were randomly allocated to one of two treatments. Oocytes were co-incubated with frozen-thawed semen washed twice with BoviPureTM (BoviPure group) or with modified Brackett-Oliphant medium (control group). After a 6-hour insemination period, oocytes were cultured in vitro for 8 days. Cleavage rate of embryos was determined 48 hours post-insemination, and blastocyst formation rate was assessed on day 8 of culture. The experiment was replicated three times, and data were analyzed using chi-square analysis. Washing of sperm in BoviPureTM had no effect (P>.05) on either cleavage rate (77.2%) or blastocyst development (21.6%) when compared with controls (71.9% and 17.1%, respectively). These results indicate that, under conditions of our study, the washing of sperm with BoviPureTM did not significantly enhance the ability to produce bovine embryos in vitro.

Alveolar bone regeneration in response to local application of calcitriol in vitamin D deficient rats

AIM Vitamin D deficiency is considered to diminish bone regeneration. Yet, raising the serum levels takes months. A topic application of the active vitamin D metabolite, calcitriol, may be an effective approach. Thus, it becomes important to know the effect of vitamin D deficiency and local application on alveolar bone regeneration. MATERIAL AND METHODS Sixty rats were divided into three groups; two vitamin depletion groups and a control group. Identical single defects (2 mm diameter) were created in the maxilla and mandible treated with calcitriol soaked collagen in one deficiency group while in the other two groups not. Histomorphometric analysis and micro CTs were performed after 1 and 3 weeks. Serum levels of 25(OH)D3 and PTH were determined. RESULTS Bone formation rate significantly increased within the observation period in all groups. Bone regeneration was higher in the maxilla than in the mandible. However, bone regeneration was lower in the control group compared to vitamin depletion groups, with no significant effects by local administration of calcitriol (micro CT mandible p = 0.003, maxilla p < 0.001; histomorphometry maxilla p = 0.035, mandible p = 0.18). CONCLUSION Vitamin D deficiency not necessarily impairs bone regeneration in the rat jaw and a single local calcitriol application does not enhance healing.