Observational effects of stellar rotation on Be stars' disks

Be stars are known to be fast rotators. At high rotation rates a profound modification of the radiation field reaching the circumstellar environment is expected. The origin of this modification is the decrease of the effective gravity on stellar surface leading to the stellar geometrical flattening and the gravity darkening effect predicted by Von Zeipel. Making use of the radiative transfer code HDUST we discuss the consequences of such stellar rotation on the structure of Be star disks based on the Viscous Decretion Disk model. Observational predictions are also made, as SED, IR-excess and Hydrogen line profiles. The modified illumination of the circumstellar disk generates significant changes in these quantities. Ascertaining these changes is useful to set some of the fundamental parameters of the Be system and to unveil the role of stellar rotation over the stellar evolution.

The Gemini planet-finding campaign: the frequency of giant planets aroud debris disk stars

We have completed a high-contrast direct imaging survey for giant planets around 57 debris disk stars as part of the Gemini NICI Planet-Finding Campaign. We achieved median H-band contrasts of 12.4 mag at 0.''5 and 14.1 mag at 1'' separation. Follow-up observations of the 66 candidates with projected separation <500 AU show that all of them are background objects. To establish statistical constraints on the underlying giant planet population based on our imaging data, we have developed a new Bayesian formalism that incorporates (1) non-detections, (2) single-epoch candidates, (3) astrometric and (4) photometric information, and (5) the possibility of multiple planets per star to constrain the planet population. Our formalism allows us to include in our analysis the previously known β Pictoris and the HR 8799 planets. Our results show at 95% confidence that <13% of debris disk stars have a ≥5 M Jup planet beyond 80 AU, and <21% of debris disk stars have a ≥3 M Jup planet outside of 40 AU, based on hot-start evolutionary models. We model the population of directly imaged planets as d 2 N/dMdavpropm α a β, where m is planet mass and a is orbital semi-major axis (with a maximum value of a max). We find that β < –0.8 and/or α > 1.7. Likewise, we find that β < –0.8 and/or a max < 200 AU. For the case where the planet frequency rises sharply with mass (α > 1.7), this occurs because all the planets detected to date have masses above 5 M Jup, but planets of lower mass could easily have been detected by our search. If we ignore the β Pic and HR 8799 planets (should they belong to a rare and distinct group), we find that <20% of debris disk stars have a ≥3 M Jup planet beyond 10 AU, and β < –0.8 and/or α < –1.5. Likewise, β < –0.8 and/or a max < 125 AU. Our Bayesian constraints are not strong enough to reveal any dependence of the planet frequency on stellar host mass. Studies of transition disks have suggested that about 20% of stars are undergoing planet formation; our non-detections at large separations show that planets with orbital separation >40 AU and planet masses >3 M Jup do not carve the central holes in these disks.

The Gemini NICI planet-finding campaign: the frequency of giant planets around young B and A stars

We have carried out high contrast imaging of 70 young, nearby B and A stars to search for brown dwarf and planetary companions as part of the Gemini NICI Planet-Finding Campaign. Our survey represents the largest, deepest survey for planets around high-mass stars (≈1.5-2.5 M ☉) conducted to date and includes the planet hosts β Pic and Fomalhaut. We obtained follow-up astrometry of all candidate companions within 400 AU projected separation for stars in uncrowded fields and identified new low-mass companions to HD 1160 and HIP 79797. We have found that the previously known young brown dwarf companion to HIP 79797 is itself a tight (3 AU) binary, composed of brown dwarfs with masses 58$^{+21}_{-20}$ M Jup and 55$^{+20}_{-19}$ M Jup, making this system one of the rare substellar binaries in orbit around a star. Considering the contrast limits of our NICI data and the fact that we did not detect any planets, we use high-fidelity Monte Carlo simulations to show that fewer than 20% of 2 M ☉ stars can have giant planets greater than 4 M Jup between 59 and 460 AU at 95% confidence, and fewer than 10% of these stars can have a planet more massive than 10 M Jup between 38 and 650 AU. Overall, we find that large-separation giant planets are not common around B and A stars: fewer than 10% of B and A stars can have an analog to the HR 8799 b (7 M Jup, 68 AU) planet at 95% confidence. We also describe a new Bayesian technique for determining the ages of field B and A stars from photometry and theoretical isochrones. Our method produces more plausible ages for high-mass stars than previous age-dating techniques, which tend to underestimate stellar ages and their uncertainties.

Genomic characterization of the italian wolf (Canis lupus): the genes involved in black coat colour determination and application of microarray technique for snps detection.

This study provides a comprehensive genetic overview on the endangered Italian wolf population. In particular, it focuses on two research lines. On one hand, we focalised on melanism in wolf in order to isolate a mutation related with black coat colour in canids. With several reported black individuals (an exception at European level), the Italian wolf population constituted a challenging research field posing many unanswered questions. As found in North American wolf, we reported that melanism in the Italian population is caused by a different melanocortin pathway component, the K locus, in which a beta-defensin protein acts as an alternative ligand for the Mc1r. This research project was conducted in collaboration with Prof. Gregory Barsh, Department of Genetics and Paediatrics, Stanford University. On the other hand, we performed analysis on a high number of SNPs thanks to a customized Canine microarray useful to integrate or substitute the STR markers for genotyping individuals and detecting wolf-dog hybrids. Thanks to DNA microchip technology, we obtained an impressive amount of genetic data which provides a solid base for future functional genomic studies. This study was undertaken in collaboration with Prof. Robert K. Wayne, Department of Ecology and Evolutionary Biology, University of California, Los Angeles (UCLA).

Molekulare Untersuchung des Wolf-Hirschhorn-Syndroms

Das Wolf-Hirschhorn-Syndrom (WHS) ist ein komplexes und variables Fehlbildungs- Retardierungssyndrom, das durch Deletion in der distalen Chromosomenregion 4p16.3 hervorgerufen wird und dessen Ätiologie und Pathogenese bisher weitgehend unverstanden sind. Die Zielsetzung in der vorliegenden Arbeit bestand in der Identifizierung und vorläufigen Charakterisierung neuer Gene, die an der Entstehung des Syndroms beteiligt sein könnten. Die Wolf-Hirschhorn-Syndrom-kritische Region (WHSCR) konnte zu Beginn der vorliegenden Arbeit auf einen ca. 2 Mb großen Bereich zwischen den Markern D4S43 und D4S142 eingegrenzt werden. Für die Identifizierung neuer Gene wurden zunächst drei größere genomische Cosmid-/PAC-Contigs (I-III) im Bereich der Marker D4S114 bis D4S142 erstellt und mittels Exonamplifikation auf transkribierte Bereiche (Exons) untersucht. Es konnten insgesamt 67 putative 'Exons' isoliert werden, von denen einige bereits bekannten Genen (ZNF141, PDEB, MYL5, GAK, DAGK4 und FGFR3) entsprechen. Zwei dieser Gene konnten im Rahmen dieser Arbeit erstmals (DAGK4) bzw. genauer (GAK) in die distale Region 4p16.3 kartiert werden. Die restlichen Exons können aufgrund von Homologievergleichen und/oder EST-cDNA-Homologien vermutlich neuen Genen oder auch Pseudogenen (z. B. YWEE1hu) zugeordnet werden. Durch die im Verlaufe der vorliegenden Arbeit publizierte weitere Eingrenzung der WHSCR auf einen 165 Kb-großen Bereich proximal des FGFR3-Gens konzentrierten sich weitere Untersuchungen auf die detaillierte Analyse der WHSCR zwischen dem Marker D4S43 und FGFR3. Mit Hilfe von Exonamplifikation bzw. computergestützter Auswertung vorliegender Sequenzdaten aus diesem Bereich ('GRAIL', 'GENSCAN' und Homologievergleiche in den EST-Datenbanken des NCBI) konnten mehrere neue Gene identifiziert werden. In distaler-proximaler Reihenfolge handelt es sich dabei um die Gene LETM1, 51, 43, 45, 57 und POL4P. LETM1 kodiert für ein putatives Transmembran-Protein mit einem Leucin-Zipper- und zwei EF-Hand-Motiven und könnte aufgrund seiner möglichen Beteiligung an der Ca2+-Homeostase und/oder der Signal-transduktion zu Merkmalen des WHS (Krampfanfällen, mentale Retardierung und muskuläre Hypotonie) beitragen. Das Gen 51 entspricht einem in etwa zeitgleich durch Stec et al. (1998) und Chesi et al. (1998) als WHSC1 bzw. MMSET bezeichnetem Gen und wurde daher nicht weiter charakterisiert. Es wird genauso wie das Gen 43, das zeitgleich von Wright et al. (1999b) als WHSC2 beschrieben werden konnte und eine mögliche Rolle bei der Transkriptionselongation spielt, ubiquitär exprimiert. Das in der vorliegenden Arbeit identifizierte Gen 45 zeigt demgegenüber ein ausgesprochen spezifisches Expressionsmuster (in Nervenzellen des Gehirns sowie in Spermatiden). Dies stellt zusammen mit der strukturellen Ähnlichkeit des putativen Genprodukts zu Signalmolekülen einen interessanten Zusammenhang zu Merkmalen des WHS (beispielsweise Kryptorchismus, Uterusfehlbildungen oder auch neurologische Defekte) her. Demgegenüber handelt es sich bei dem Gen 57 möglicherweise um ein trunkiertes Pseudogen des eRFS-Gens auf Chromosom 6q24 (Wallrapp et al., 1998). Das POL4P-Gen schließlich stellt allein aufgrund seiner genomischen Lokalisation sowie seiner möglichen Funktion (als DNA-Polymerase-ähnliches Gen) kein gutes Kandidatengen für spezifische Merkmale des Syndroms dar und wurde daher nicht im Detail charakterisiert. Um die Beteiligung der Gene an der Ätiologie und Pathogenese des Syndroms zu verstehen, ist die Entwicklung eines Mausmodells (über das Einfügen gezielter Deletionen in das Mausgenom) geplant. Um dies zu ermöglichen, wurde in der vorliegenden Arbeit die Charakterisierung der orthologen Region bei der Maus vorgenommen. Zunächst wurden die orthologen Gene der Maus (Letm1, Whsc1, Gen 43 (Whsc2h), Gen 45 und Pol4p) identifiziert. Durch die Erstellung sowie die genaue Kartierung eines murinen genomischen P1/PAC-Klon-Contigs konnte gezeigt werden, daß die murinen Gene Fgfr3, Letm1, Whsc1, Gen 43 (Whsc2h), Gen 45 und Pol4p sowie einige weitere der überprüften EST-cDNA-Klone der Maus in einem durchgehenden Syntänieblock zwischen Mensch (POL4P bis FGFR3) und Maus (Mmu 5.20) enthalten sind, der in seiner genomischen Ausdehnung in etwa den Verhältnissen beim Menschen (zwischen POL4P und FGFR3) entspricht.

Laser guide stars wavefront sensors for the EELT

The Adaptive Optics is the measurement and correction in real time of the wavefront aberration of the star light caused by the atmospheric turbulence, that limits the angular resolution of ground based telescopes and thus their capabilities to deep explore faint and crowded astronomical objects. The lack of natural stars enough bright to be used as reference sources for the Adaptive Optics, over a relevant fraction of the sky, led to the introduction of artificial reference stars. The so-called Laser Guide Stars are produced by exciting the Sodium atoms in a layer laying at 90km of altitude, by a powerful laser beam projected toward the sky. The possibility to turn on a reference star close to the scientific targets of interest has the drawback in an increased difficulty in the wavefront measuring, mainly due to the time instability of the Sodium layer density. These issues are increased with the telescope diameter. In view of the construction of the 42m diameter European Extremely Large Telescope a detailed investigation of the achievable performances of Adaptive Optics becomes mandatory to exploit its unique angular resolution . The goal of this Thesis was to present a complete description of a laboratory Prototype development simulating a Shack-Hartmann wavefront sensor using Laser Guide Stars as references, in the expected conditions for a 42m telescope. From the conceptual design, through the opto-mechanical design, to the Assembly, Integration and Test, all the phases of the Prototype construction are explained. The tests carried out shown the reliability of the images produced by the Prototype that agreed with the numerical simulations. For this reason some possible upgrades regarding the opto-mechanical design are presented, to extend the system functionalities and let the Prototype become a more complete test bench to simulate the performances and drive the future Adaptive Optics modules design.

Ecological genetics and conservation genomics of wolf (Canis lupus)

In the present work, we apply both traditional and Next Generation Sequencing (NGS) tools to investigate some of the most important adaptive traits of wolves (Canis lupus). In the first part, we analyze the variability of three Major Histocompatibility Complex (MHC) class II genes in the Italian wolf population, also studying their possible role in mating choice and their influence on fitness traits. In the second section, as part of a larger canid genome project, we will exploit NGS data to investigate the transcript-level differences between the wolf and the dog genome that can be correlated to domestication.

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.

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.

Landscape ecology and genetics of the wolf in Italy

This PhD Thesis includes five main parts on diverse topics. The first two parts deal with the trophic ecology of wolves in Italy consequently to a recent increase of wild ungulates abundance. Data on wolf diet across time highlighted how wild ungulates are important food resource for wolves in Italy. Increasing wolf population, increasing numbers of wild ungulates and decreasing livestock consume are mitigating wolf-man conflicts in Italy in the near future. In the third part, non-invasive genetic sampling techniques were used to obtain genotypes and genders of about 400 wolves. Thus, wolf packs were genetically reconstructed using diverse population genetic and parentage software. Combining the results on pack structure and genetic relatedness with sampling locations, home ranges of wolf packs and dispersal patterns were identified. These results, particularly important for the conservation management of wolves in Italy, illustrated detailed information that can be retrieved from genetic identification of individuals. In the fourth part, wolf locations were combined with environmental information obtained as GIS-layers. Modern species distribution models (niche models) were applied to infer potential wolf distribution and predation risk. From the resulting distribution maps, information pastures with the highest risk of depredation were derived. This is particularly relevant as it allows identifying those areas under danger of carnivore attack on livestock. Finally, in the fifth part, habitat suitability models were combined with landscape genetic analysis. On one side landscape genetic analyses on the Italian wolves provided new information on the dynamics and connectivity of the population and, on the other side, a profound analysis of the effects that habitat suitability methods had on the parameterization of landscape genetic analyses was carried out to contributed significantly to landscape genetic theory.

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.