Pulsating variable stars as tracers of galactic structure and interaction mechanisms

My PhD project has been focused on the study of the pulsating variable stars in two ultra-faint dwarf spheroidal satellites of the Milky Way, namely, Leo IV and Hercules; and in two fields of the Large Magellanic Cloud (namely, the Gaia South Ecliptic Pole calibration field, and the 30 Doradus region) that were repeatedly observed in the KS band by the VISTA Magellanic Cloud (VMC, PI M.R. Cioni) survey of the Magellanic System.

GM-CSF (granulocyte-macrophage colony-stimulating factor): Modulation der durch UV-B-Strahlung induzierten Hautkarzinogenese

UV-B-Strahlung, die durch die fortschreitende Zerstörung der Ozonschicht zunimmt, ist hauptsächlich für das Entstehen von Basaliomen und Plattenepithelkarzinomen verantwort-lich, an denen jedes Jahr etwa 2-3 Millionen Menschen weltweit erkranken. UV-B indu-zierte Hautkarzinogenese ist ein komplexer Prozess, bei dem vor allem die mutagenen und immunsuppressiven Wirkungen der UV-B-Strahlung von Bedeutung sind. Die Rolle von GM-CSF in der Hautkarzinogenese ist dabei widersprüchlich. Aus diesem Grund wurde die Funktion von GM-CSF in vivo in der UV-B induzierten Hautkarzinogenese mittels zwei bereits etablierter Mauslinien untersucht: Erstens transgene Mäuse, die einen GM-CSF Antagonisten unter der Kontrolle des Keratin-10-Promotors in den suprabasalen Schichten der Epidermis exprimieren und zweitens solche, die unter dem Keratin-5-Promotor murines GM-CSF in der Basalschicht der Epidermis überexprimieren. Eine Gruppe von Tieren wurde chronisch, die andere akut bestrahlt. Die konstitutionelle Verfassung der Tiere mit erhöhter GM-CSF-Aktivität in der Haut war nach chronischer UV-B-Bestrahlung insgesamt sehr schlecht. Sie wiesen deshalb eine stark erhöhte Mortali-tät auf. Dies ist sowohl auf die hohe Inzidenz als auch dem frühen Auftreten der benignen und malignen Läsionen zurückzuführen. Eine verminderte GM-CSF Aktivität verzögerte dagegen die Karzinomentwicklung und erhöhte die Überlebensrate leicht. GM-CSF wirkt auf verschiedenen Ebenen tumorpromovierend: Erstens erhöht eine gesteigerte Mastzell-anzahl in der Haut der GM-CSF überexprimierenden Tiere per se die Suszeptibilität für Hautkarzinogenese. Zweitens stimuliert GM-CSF die Keratinozytenproliferation. Dadurch kommt es nach UV-B-Bestrahlung zu einer prolongierten epidermalen Hyperproliferation, die zur endogenen Tumorpromotion beiträgt, indem sie die Bildung von Neoplasien unter-stützt. Der Antagonist verzögert dagegen den Proliferationsbeginn, die Keratinozyten blei-ben demzufolge länger in der G1-Phase und der durch UV-B verursachte DNA-Schaden kann effizienter repariert werden. Drittens kann GM-CSF die LCs nicht als APCs aktivie-ren und eine Antitumorimmunität induzieren, da UV-B-Strahlung zur Apoptose von LCs bzw. zu deren Migration in Richtung Lymphknoten führt. Zusätzlich entwickeln GM-CSF überexprimierende Tiere in ihrer Haut nach UV-B-Bestrahlung ein Millieu von antago-nistisch wirkenden Zytokinen, wie TNF-a, TGF-b1 und IL-12p40 und GM-CSF, die proinflammatorische Prozesse und somit die Karzinomentwicklung begünstigen. Der Anta-gonist hemmt nach UV-B-Bestrahlung die Ausschüttung sowohl von immunsuppressiven Zytokinen, wie etwa TNF-a, als auch solchen, die die Th2-Entwicklung unterstützen, wie etwa IL-10 und IL-4. Dies wirkt sich negativ auf die Karzinomentwicklung aus.

Chemical and kinematical properties of Blue Straggler stars in Galactic globular clusters

Blue straggler stars (BSSs) are brighter and bluer (hotter) than the main-sequence (MS) turnoff and they are known to be more massive than MS stars.Two main scenarios for their formation have been proposed:collision-induced stellar mergers (COL-BSSs),or mass-transfer in binary systems (MT-BSSs).Depleted surface abundances of C and O are expected for MT-BSSs,whereas no chemical anomalies are predicted for COL-BSSs.Both MT- and COL-BSSs should rotate fast, but braking mechanisms may intervene with efficiencies and time-scales not well known yet,thus preventing a clear prediction of the expected rotational velocities.Within this context,an extensive survey is ongoing by using the multi-object spectrograph FLAMES@VLT,with the aim to obtain abundance patterns and rotational velocities for representative samples of BSSs in several Galactic GCs.A sub-population of CO-depleted BSSs has been identified in 47 Tuc,with only one fast rotating star detected.For this PhD Thesis work I analyzed FLAMES spectra of more than 130 BSSs in four GCs:M4,NGC 6397,M30 and ω Centauri.This is the largest sample of BSSs spectroscopically investigated so far.Hints of CO depletion have been observed in only 4-5 cases (in M30 and ω Centauri),suggesting either that the majority of BSSs have a collisional origin,or that the CO-depletion is a transient phenomenon.Unfortunately,no conclusions in terms of formation mechanism could be drawn in a large number of cases,because of the effects of radiative levitation. Remarkably,however,this is the first time that evidence of radiative levitation is found in BSSs hotter than 8200 K.Finally, we also discovered the largest fractions of fast rotating BSSs ever observed in any GCs:40% in M4 and 30% in ω Centauri.While not solving the problem of BSS formation,these results provide invaluable information about the BSS physical properties,which is crucial to build realistic models of their evolution.

COSMIC-LAB: Unexpected Results from High-resolution Spectra of AGB Stars in Globular Clusters

We have used high-resolution spectra, acquired with UVES@ESO-VLT, to determine the chemical abundances of different samples of AGB and RGB stars in 4 Galactic globular clusters, namely 47Tuc, NGC3201, M22 and M62. For almost all the analyzed AGB stars we found a clear discrepancy between the iron abundance measured from neutral lines and that obtained from single ionized lines, while this discrepancy is not obtained for the RGB samples observed in the same clusters and analyzed with the same procedure. Such a behavior exactly corresponds to what expected in the case of Non-Local Thermodynamical Equilibrium (NLTE) in the star atmosphere. These results have a huge impact on the proper determination of GC chemistry. In fact, one of the most intriguing consequences is that, at odds with previous claims, no iron spread is found in NGC3201 and M22 if the iron abundance is obtained from ionized lines only.

Planck stars: theory and phenomenology

General Relativity (GR) is one of the greatest scientific achievements of the 20th century along with quantum theory. Despite the elegance and the accordance with experimental tests, these two theories appear to be utterly incompatible at fundamental level. Black holes provide a perfect stage to point out these difficulties. Indeed, classical GR fails to describe Nature at small radii, because nothing prevents quantum mechanics from affecting the high curvature zone, and because classical GR becomes ill-defined at r = 0 anyway. Rovelli and Haggard have recently proposed a scenario where a negative quantum pressure at the Planck scales stops and reverts the gravitational collapse, leading to an effective “bounce” and explosion, thus resolving the central singularity. This scenario, called Black Hole Fireworks, has been proposed in a semiclassical framework. The purpose of this thesis is twofold: - Compute the bouncing time by means of a pure quantum computation based on Loop Quantum Gravity; - Extend the known theory to a more realistic scenario, in which the rotation is taken into account by means of the Newman-Janis Algorithm.

La popolazione di Blue Straggler Stars in due ammassi globulari della Grande Nube di Magellano

Le Blue Straggler Stars (BSS) sono la popolazione di oggetti esotici piu' comune e numerosa negli ammassi globulari. Nel diagramma colore-magnitudine le BSS definiscono una sequenza più brillante e blu del punto di turn-off della Sequenza Principale, simulando una popolazione più giovane delle stelle dell'ammasso.  Osservazioni hanno dimostrato che le BSS hanno una massa significativamente più grande (1.2-1.7 Msun) di quella delle stelle di un ammasso globulare. Per questa proprietà, la distribuzione radiale delle BSS e' un utile strumento per tracciare empiricamente lo stato di evoluzione dinamica degli ammassi stellari. Il lavoro di tesi si è concentrato sullo studio della popolazione di BSS di due ammassi globulari della Grande Nube di Magellano: NGC2257 e NGC1754. Applicando metodi di indagine già usati per sistemi stellari della Via Lattea, abbiamo derivato le eta' dinamiche di questi due sistemi e le abbiamo confrontate con stime teoriche.

Coatings ibridi organici-inorganici ottenuti mediante processo sol-gel e contenenti assorbitori di radiazioni uv

In questo progetto di tesi si è cercato il modo di rendere più efficace la resistenza dei materiali plastici alla fotodegradazione indotta dai raggi ultravioletti, attraverso l’utilizzo di coatings ibridi organici-inorganici preparati utilizzando il processo sol-gel. Tali rivestimenti in grado di migliorare la resistenza superficiale potrebbero essere applicati a diversi materiali ed in particolare ai policarbonati che per le loro eccellenti proprietà di trasparenza vengono molto utilizzati in illuminotecnica ed altre applicazioni per l’esterno. In particolare il lavoro ha riguardato lo studio e l’utilizzo di due assorbitori UV di tipo fenolico, il 2,2’-diidrossi-4-metossibenzofenone e il 2,2’,4,4’-tetraidrossibenzofenone. Si è provato a non collocare semplicemente tali assorbitori all’interno del coating sol-gel ma a legarli covalentemente al network tridimensionale di silani auspicando una migliore resistenza alla fotodegradazione UV-indotta. Il nostro interesse si è concentrato soprattutto sul 2,2’,4,4’-tetraidrossibenzofenone, in quanto abbiamo visto che una sua funzionalizzazione rispetto all’altro assorbitore UV risulta più semplice ed efficace.

UV Responses in Native Hawaiians or Other Pacific Islanders and Asians Residing in Hawaiʻi and in Maryland

Background: UV exposure causes a wide range of skin damage including cutaneous melanoma. The mechanisms of cellular and molecular damage as well as erythemal and pigmentation responses to UV exposure have largely been studied in the White population. Methods: This study systematically investigates responses to UV exposure in the Native Hawaiian and Pacific Islanders (NHPI) and Asian populations living in Hawai’i (A/HI) as well as in Asians living in Maryland (A/MD). Results: Our analyses indicate that the NHPI population is less sensitive to UV exposure than the A/HI population. Comparisons between the two Asian groups suggest that, despite slightly but not statistically different baseline constitutive pigmentation (pre-UV exposure), the A/HI and A/MD had similar UV sensitivity, measured as minimal erythemal dose (MED). However, the A/MD population had higher levels of oxy-hemoglobin at doses of 2.0, 2.8 and 4.0 MED. Unexpectedly the A/MD subjects retained higher levels of pigmentation 2 weeks post UV exposure. Conclusion: This study provides insight into UV responses of the inhabitants of Hawai’i and shows that such responses are statistically significant for relatively small samples of Native Hawaiian and Pacific Islanders, and for Asians living in Hawai’i and Asians living in Maryland.

Homeopathic Preparations of Quartz, Sulfur and Copper Sulfate Assessed by UV-Spectroscopy

Homeopathic preparations are used in homeopathy and anthroposophic medicine. Although there is evidence of effectiveness in several clinical studies, including double-blinded randomized controlled trials, their nature and mode of action could not be explained with current scientific approaches yet. Several physical methods have already been applied to investigate homeopathic preparations but it is yet unclear which methods are best suited to identify characteristic physicochemical properties of homeopathic preparations. The aim of this study was to investigate homeopathic preparations with UV-spectroscopy. In a blinded, randomized, controlled experiment homeopathic preparations of copper sulfate (CuSO(4); 11c-30c), quartz (SiO(2); 10c-30c, i.e., centesimal dilution steps) and sulfur (S; 11×-30×, i.e., decimal dilution steps) and controls (one-time succussed diluent) were investigated using UV-spectroscopy and tested for contamination by inductively coupled plasma mass spectrometry (ICP-MS). The UV transmission for homeopathic preparations of CuSO(4) preparations was significantly lower than in controls. The transmission seemed to be also lower for both SiO(2) and S, but not significant. The mean effect size (95% confidence interval) was similar for the homeopathic preparations: CuSO(4) (pooled data) 0.0544% (0.0260-0.0827%), SiO(2) 0.0323% (-0.0064% to 0.0710%) and S 0.0281% (-0.0520% to 0.1082%). UV transmission values of homeopathic preparations had a significantly higher variability compared to controls. In none of the samples the concentration of any element analyzed by ICP-MS exceeded 100 ppb. Lower transmission of UV light may indicate that homeopathic preparations are less structured or more dynamic than their succussed pure solvent.

Vibronic Spectra of Jet-Cooled 2-Aminopurine center dot H2O Clusters Studied by UV Resonant Two-Photon Ionization Spectroscopy and Quantum Chemical Calculations

For understanding the major- and minor-groove hydration patterns of DNAs and RNAs, it is important to understand the local solvation of individual nucleobases at the molecular level. We have investigated the 2-aminopurine center dot H2O. monohydrate by two-color resonant two-photon ionization and UV/UV hole-burning spectroscopies, which reveal two isomers, denoted A and B. The electronic spectral shift delta nu of the S-1 <- S-0 transition relative to bare 9H-2-aminopurine (9H-2AP) is small for isomer A (-70 cm(-1)), while that of isomer B is much larger (delta nu = 889 cm(-1)). B3LYP geometry optimizations with the TZVP basis set predict four cluster isomers, of which three are doubly H-bonded, with H2O acting as an acceptor to a N-H or -NH2 group and as a donor to either of the pyrimidine N sites. The "sugar-edge" isomer A is calculated to be the most stable form with binding energy D-e = 56.4 kJ/mol. Isomers B and C are H-bonded between the -NH2 group and pyrimidine moieties and are 2.5 and 6.9 kJ/mol less stable, respectively. Time-dependent (TD) B3LYP/TZVP calculations predict the adiabatic energies of the lowest (1)pi pi* states of A and B in excellent agreement with the observed 0(0)(0) bands; also, the relative intensities of the A and B origin bands agree well with the calculated S-0 state relative energies. This allows unequivocal identification of the isomers. The R2PI spectra of 9H-2AP and of isomer A exhibit intense low-frequency out-of-plane overtone and combination bands, which is interpreted as a coupling of the optically excited (1)pi pi* state to the lower-lying (1)n pi* dark state. In contrast, these overtone and combination bands are much weaker for isomer B, implying that the (1)pi pi* state of B is planar and decoupled from the (1)n pi* state. These observations agree with the calculations, which predict the (1)n pi* above the (1)pi pi* state for isomer B but below the (1)pi pi* for both 9H-2AP and isomer A.