Direct determination of chromium in empty medicine capsules by tungsten coil atomic emission spectrometry

Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)

NGC 2782: a merger remnant with young stars in its gaseous tidal tail

We have searched for young star-forming regions around the merger remnant NGC 2782. By using Galaxy Evolution Explorer far-ultraviolet and near-ultraviolet imaging and H i data we found seven ultraviolet sources, located at distances greater than 26 kpc from the centre of NGC 2782, and coinciding with its western H i tidal tail. These regions were resolved in several smaller systems when Gemini/Gemini multi-object spectrograph (GMOS) r-band images were used. We compared the observed colours to stellar population synthesis models and found that these objects have ages of similar to 1 to 11 Myr and masses ranging from 103.9 to 104.6 M circle dot. By using Gemini/GMOS spectroscopic data we confirm memberships and derive high metallicities for three of the young regions in the tail (12+log(O/H) = 8.74 +/- 0.20, 8.81 +/- 0.20 and 8.78 +/- 0.20). These metallicities are similar to the value presented by the nuclear region of NGC 2782 and also similar to the value presented for an object located close to the main body of NGC 2782. The high metallicities measured for the star-forming regions in the gaseous tidal tail of NGC 2782 could be explained if they were formed out of highly enriched gas which was once expelled from the centre of the merging galaxies when the system collided. An additional possibility is that the tail has been a nursery of a few generations of young stellar systems which ultimately polluted this medium with metals, further enriching the already pre-enriched gas ejected to the tail when the galaxies collided.

Metallicities for six nearby open clusters from high-resolution spectra of giant stars [Fe/H] values for a planet search sample

We present a study of the stellar parameters and iron abundances of 18 giant stars in six open clusters. The analysis was based on high-resolution and high-S/N spectra obtained with the UVES spectrograph (VLT-UT2). The results complement our previous study where 13 clusters were already analyzed. The total sample of 18 clusters is part of a program to search for planets around giant stars. The results show that the 18 clusters cover a metallicity range between -0.23 and +0.23 dex. Together with the derivation of the stellar masses, these metallicities will allow the metallicity and mass effects to be disentangled when analyzing the frequency of planets as a function of these stellar parameters.

Elemental abundances and classification of carbon-enhanced metal-poor stars

We present a detailed study of carbon-enhanced metal-poor (CEMP) stars, based on high-resolution spectroscopic observations of a sample of 18 stars. The stellar spectra for this sample were obtained at the 4.2 m William Herschel Telescope in 2001 and 2002, using the Utrecht Echelle Spectrograph, at a resolving power R similar to 52 000 and S/N similar to 40, covering the wavelength range lambda lambda 3700-5700 angstrom. The atmospheric parameters determined for this sample indicate temperatures ranging from 4750 K to 7100 K, log g from 1.5 to 4.3, and metallicities -3.0 <= [Fe/H]<=-1.7. Elemental abundances for C, Na, Mg, Sc, Ti, Cr, Cu, Zn, Sr, Y, Zr, Ba, La, Ce, Nd, Sm, Eu, Gd, Dy are determined. Abundances for an additional 109 stars were taken from the literature and combined with the data of our sample. The literature sample reveals a lack of reliable abundance estimates for species that might be associated with the r-process elements for about 67% of CEMP stars, preventing a complete understanding of this class of stars, since [Ba/Eu] ratios are used to classify them. Although eight stars in our observed sample are also found in the literature sample, Eu abundances or limits are determined for four of these stars for the first time. From the observed correlations between C, Ba, and Eu, we argue that the CEMP-r/s class has the same astronomical origin as CEMP-s stars, highlighting the need for a more complete understanding of Eu production.

Homogeneous metallicities and radial velocities for Galactic globular clusters

Well determined radial velocities and abundances are essential for analyzing the properties of the globular cluster system of the Milky Way. However more than 50% of these clusters have no spectroscopic measure of their metallicity. In this context, this work provides new radial velocities and abundances for twenty Milky Way globular clusters which lack or have poorly known values for these quantities. The radial velocities and abundances are derived from spectra obtained at the Ca II triplet using the FORS2 imager and spectrograph at the VLT, calibrated with spectra of red giants in a number of clusters with well determined abundances. For about half of the clusters in our sample we present significant revisions of the existing velocities or abundances, or both. We also confirm the existence of a sizable abundance spread in the globular cluster M 54, which lies at the center of the Sagittarius dwarf galaxy. In addition evidence is provided for the existence of a small intrinsic internal abundance spread (sigma[Fe/H](int) approximate to 0.11-0.14 dex, similar to that of M 54) in the luminous distant globular cluster NGC 5824. This cluster thus joins the small number of Galactic globular clusters known to possess internal metallicity ([Fe/H]) spreads.

THE SLOAN DIGITAL SKY SURVEY CO-ADD: A GALAXY PHOTOMETRIC REDSHIFT CATALOG

We present and describe a catalog of galaxy photometric redshifts (photo-z) for the Sloan Digital Sky Survey (SDSS) Co-add Data. We use the artificial neural network (ANN) technique to calculate the photo-z and the nearest neighbor error method to estimate photo-z errors for similar to 13 million objects classified as galaxies in the co-add with r < 24.5. The photo-z and photo-z error estimators are trained and validated on a sample of similar to 83,000 galaxies that have SDSS photometry and spectroscopic redshifts measured by the SDSS Data Release 7 (DR7), the Canadian Network for Observational Cosmology Field Galaxy Survey, the Deep Extragalactic Evolutionary Probe Data Release 3, the VIsible imaging Multi-Object Spectrograph-Very Large Telescope Deep Survey, and the WiggleZ Dark Energy Survey. For the best ANN methods we have tried, we find that 68% of the galaxies in the validation set have a photo-z error smaller than sigma(68) = 0.031. After presenting our results and quality tests, we provide a short guide for users accessing the public data.

Sensing the "LUV" with HST+COS in Cycle 20 and beyond

New Cosmic Origins Spectrograph (COS) observing modes have extended the Hubble Space Telescope's spectral range to wavelengths between 900-1150 Å. However, the G140L/1280 and the Cycle 19 available G130M central wavelengths (1055 and 1096) that sample below 1150 Å were only available at focus positions which provided low-resolution (R<3,000). For HST Cycle 20, we introduced a new G130M/1222 central wavelength that covers 1065-1365 Å with R>10,000 everywhere, but optimized for 15000 from 1080-1200 Å. This mode places geo-coronal Lyα between the COS FUV detector segments to minimize detector gain sag. Also for Cycle 20, the resolution of the G130M/1055 and 1096 modes will be increased by a factor of 3-4 by optimizing the focus positions for these modes. This will give HST approximately the effective area of FUSE over the FUSE bandpass at 10,000. Here we present the current calibration status of the COS G130M/1055, 1096, and 1222 central wavelength settings at the original and second FUV lifetime positions with an emphasis on observing over the "Lyman UV", or "LUV", 912-1216 Å.

Results from the HST/COS FUV detector "lifetime move"

We describe the planning, implementation, and initial results of the first planned move of the default position of spectra on the Hubble Space Telescope's Cosmic Origins Spectrograph (COS) Far Ultraviolet (FUV) cross-delay line detector. This was motivated by the limited amount of charge that can be extracted from the microchannel plate due to gain sag at any one position. Operations at a new location began on July 23, 2012, with a shift of the spectrum by +3.5"(corresponding to ~ 41 pixels or ~ 1 mm) in a direction orthogonal to the spectral dispersion. Operation at this second "lifetime position" allows for spectra to be collected which are not affected by detector artifacts and loss of sensitivity due to gain sag. We discuss programs designed to enable operations at the new lifetime position; these include determinations of operational high voltage, measuring walk corrections and focus, confirming spectrum placement and aperture centering, and target acquisition performance. We also present results related to calibration of the new lifetime position, including measurements of spectral resolution and wavelength calibration, flux and flat field calibration, carryover of time-dependent sensitivity monitoring, and operations with the Bright Object Aperture (BOA).

Alpha cluster structure in 16O.

The alpha cluster phenomenon in the light nuclei structure has been the subject of a longtime investigation since the proposal of the Ikeda diagrams, however the mechanism of the cluster formation is still not completely understood. In fact, if the clusters have a fairly rigid crystal-like or a gas-like structure remains an open question. The interpretation of the Hoyle state as an α condensate brought a renewed interest to this subject, in particular to resonances analogous to the Hoyle state. In this context the study of the experimental evolution of the α-cluster phenomenon through (6Li,d) transfer reactions has been performed in São Paulo. Particularly important are the regions around the nα thresholds where the α-cluster structure states are predicted. The resonant states around the 4α threshold in the nucleus 16O are the focus of the present contribution. The 12C(6Li,d)16O reaction was measured at a bombarding energy of 25.5 MeV employing the São Paulo Pelletron-Enge-Spectrograph facility and the nuclear emulsion detection technique. Resonant states above the α threshold were measured and an energy resolution of 15-30 keV allows to define states previously unresolved. The angular distributions of the absolute cross sections were determined in a range of 4-40 degree in the center of mass system and up to 17 MeV excitation energy. The upper limit for the resonance widths in the crucial region of the 4α threshold was obtained. These values revealed to be at least a factor three smaller than the ones previously reported in the literature, indicating that the α cluster structure information on this region should be revised.

Quasi-bound alpha resonant states populated by the 12C(6Li,d) reaction.

Several narrow alpha resonant 16O states were detected through the 12C(6Li,d) reaction, in the range of 12 to 17 MeV of excitation energy. The reaction was measured at a bombarding energy of 25.5 MeV employing the São Paulo Pelletron-Enge-Spectrograph facility and the nuclear emulsion technique. Experimental angular distributions associated with four natural parity quasi-bound states ncar the 4α threshold are presented and compared to DWBA predictions.

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.

Entwicklung eines Spektralradiometers zur Bestimmung von aktinischer Strahlung und Photolysefrequenzen in bewölkter Atmosphäre

In dieser Arbeit wird ein neu entwickeltes Spektralradiometer zur Messung des solaren aktinischen Strahlungsflusses, speziell bei bewölkter Atmosphäre, vorgestellt. Das Meßsystem benutzt ein spezielles neu entwickeltes optisches Empfangssystem mit winkelunabhängiger Empfindlichkeit über den gesamten Raum (4pisr). Das Spektrometer besteht aus einem Gitterspektrographen und einer CCD-Kamera als Detektor, wodurch die schnelle simultane Messung eines Wellenlängenbereiches von 300nm bis 660nm ermöglicht wird. Zudem können Spektren von drei Empfangssystemen gleichzeitig aufgenommen werden, was zur höhenaufgelösten Messung des aktinischen Flusses verwendet wird. Photolysefrequenzen von Ozon, Stickstoffdioxid, und anderen für die troposphärische Chemie interessanten Molekülen werden mit Literaturdaten des molekularen Absorptionsquerschnitts und der Quantenausbeute und dem gemessenen aktinischen Strahlungsfluß berechnet. Zudem werden anhand von Spektren des aktinischen Flusses, die bei der Feldmeßkampagne BERLIOZ (BERLIn OZonexperiment) und bei Feldmessungen an einem 107m hohen Turm auf einem Berg (753m NN, Hunsrück) aufgenommen wurden, die Effekte unterschiedlicher Bewölkungssituationen untersucht. Als Ergebnis dieser Arbeit wurden verschiedene wellenlängenabhängige Effekte deutlich: bei partieller Bewölkung ist der aktinische Fluß am Erdboden gegenüber dem wolkenfreien Fall teilweise reduziert, aber auch erhöht, wobei diese Effekte mit zunehmender Wellenlänge größer werden. Oberhalb von Wolken ist der aktinische Fluß gegenüber dem wolkenfreien Fall erhöht. Dieser Effekt nimmt mit abnehmender Wellenlänge zu.

Surface-plasmon optical and electrochemical characterization of biofunctional surface architectures

The development and characterization of biomolecule sensor formats based on the optical technique Surface Plasmon Resonance (SPR) Spectroscopy and electrochemical methods were investigated. The study can be divided into two parts of different scope. In the first part new novel detection schemes for labeled targets were developed on the basis of the investigations in Surface-plamon Field Enhanced Spectroscopy (SPFS). The first one is SPR fluorescence imaging formats, Surface-plamon Field Enhanced Fluorescence Microscopy (SPFM). Patterned self assembled monolayers (SAMs) were prepared and used to direct the spatial distribution of biomolecules immobilized on surfaces. Here the patterned monolayers would serve as molecular templates to secure different biomolecules to known locations on a surface. The binding processed of labeled target biomolecules from solution to sensor surface were visually and kinetically recorded by the fluorescence microscope, in which fluorescence was excited by the evanescent field of propagating plasmon surface polaritons. The second format which also originates from SPFS technique, Surface-plamon Field Enhanced Fluorescence Spectrometry (SPFSm), concerns the coupling of a fluorometry to normal SPR setup. A spectrograph mounted in place of photomultiplier or microscope can provide the information of fluorescence spectrum as well as fluorescence intensity. This study also firstly demonstrated the analytical combination of surface plasmon enhanced fluorescence detection with analyte tagged by semiconducting nano- crystals (QDs). Electrochemically addressable fabrication of DNA biosensor arrays in aqueous environment was also developed. An electrochemical method was introduced for the directed in-situ assembly of various specific oligonucleotide catcher probes onto different sensing elements of a multi-electrode array in the aqueous environment of a flow cell. Surface plasmon microscopy (SPM) is utilized for the on-line recording of the various functionalization steps. Hybridization reactions between targets from solution to the different surface-bound complementary probes are monitored by surface-plasmon field-enhanced fluorescence microscopy (SPFM) using targets that are either labeled with organic dyes or with semiconducting quantum dots for color-multiplexing. This study provides a new approach for the fabrication of (small) DNA arrays and the recording and quantitative evaluation of parallel hybridization reactions. In the second part of this work, the ideas of combining the SP optical and electrochemical characterization were extended to tethered bilayer lipid membrane (tBLM) format. Tethered bilayer lipid membranes provide a versatile model platform for the study of many membrane related processes. The thiolipids were firstly self-assembled on ultraflat gold substrates. Fusion of the monolayers with small unilamellar vesicles (SUVs) formed the distal layer and the membranes thus obtained have the sealing properties comparable to those of natural membranes. The fusion could be monitored optically by SPR as an increase in reflectivity (thickness) upon formation of the outer leaflet of the bilayer. With EIS, a drop in capacitance and a steady increase in resistance could be observed leading to a tightly sealing membrane with low leakage currents. The assembly of tBLMs and the subsequent incorporation of membrane proteins were investigated with respect to their potential use as a biosensing system. In the case of valinomycin the potassium transport mediated by the ion carrier could be shown by a decrease in resistance upon increasing potassium concentration. Potential mediation of membrane pores could be shown for the ion channel forming peptide alamethicin (Alm). It was shown that at high positive dc bias (cis negative) Alm channels stay at relatively low conductance levels and show higher permeability to potassium than to tetramethylammonium. The addition of inhibitor amiloride can partially block the Alm channels and results in increase of membrane resistance. tBLMs are robust and versatile model membrane architectures that can mimic certain properties of biological membranes. tBLMs with incorporated lipopolysaccharide (LPS) and lipid A mimicking bacteria membranes were used to probe the interactions of antibodies against LPS and to investigate the binding and incorporation of the small antimicrobial peptide V4. The influence of membrane composition and charge on the behavior of V4 was also probed. This study displays the possibility of using tBLM platform to record and valuate the efficiency or potency of numerous synthesized antimicrobial peptides as potential drug candidates.

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.

Homogeneous analysis of a sample of Open Clusters in the context of the BOCCE project and the Gaia-ESO Survey

The open clusters (OC) are gravitationally bound systems of a few tens or hundreds of stars. In our Galaxy, the Milky Way, we know about 3000 open clusters, of very different ages in the range of a few millions years to about 9 Gyr. OCs are mainly located in the Galactic thin disc, with distances from the Galactic centre in the range 4-22 kpc and a height scale on the disc of about 200 pc. Their chemical properties trace those of the environment in which they formed and the metallicity is in the range -0.5<[Fe/H]<+0.5 dex. Through photometry and spectroscopy it is possible to study relatively easily the properties of the OCs and estimate their age, distance, and chemistry. For these reasons they are considered primary tracers of the chemical properties and chemical evolution of the Galactic disc. The main subject of this thesis is the comprehensive study of several OCs. The research embraces two different projects: the Bologna Open Cluster Chemical Evolution project (BOCCE) and the Gaia-ESO Survey. The first is a long-term programme, aiming at studying the chemical evolution of the Milky Way disc by means of a homogeneous sample of OCs. The latter is a large public spectroscopy survey, conducted with the high-resolution spectrograph FLAMES@VLT and targeting about 10^5 stars in different part of the Galaxy and 10^4 stars in about 100 OCs. The common ground between the two projects is the study of the properties of the OCs as tracers of the disc's characteristics. The impressive scientific outcome of the Gaia-ESO Survey and the unique framework of homogeneity of the BOCCE project can propose, especially once combined together, a much more accurate description of the properties of the OCs. In turn, this will give fundamental constraints for the interpretation of the properties of the Galactic disc.