Studies of the temporal evolution of young stars and their associated properties rely upon the ability of astronomers to determine ages and masses of objects in different evolutionary states. The best method for determining the age and mass of a young stellar object is to place the object on the Hertzsprung-Russell (HR) diagram and to compare to theoretical evolutionary tracks. Accurate ages allow the investigation of the temporal evolution of properties associated with stellar youth (accretion rates, X-ray activity, circumstellar excess, etc...). One property intimately linked with stellar youth is the presence (or absence) of an optically thick primordial circumstellar disk. Objects in "young" star forming regions are more likely to show evidence for a disk than objects in "older" clusters. Within a single cluster, the picture is not as clear. There exist objects in very young clusters (~1 Myr) which show no evidence for circumstellar disks, and there exist objects in very old clusters (~10 Myr), which show evidence for robust disks, suggesting a variable other than stellar age is driving the evolution of the disks. To investigate whether these outliers are due to age spreads, initial conditions, or simply appear anomalous due to erroneous age determinations, we must determine better placements in the HR diagram by carefully transforming observable quantities (spectral type and apparent magnitude) into the quantities necessary for comparison evolutionary models (effective temperature and luminosity). In the Ophiuchus star forming region, I investigate whether or not objects with disks are younger than disk-less objects. I find no difference in the ages of the two populations, but the systematic and random uncertainties are large enough to mask all but the largest age differences. In the hope of better determining the physical parameters of young stellar objects, I embark on a spectral synthesis campaign to produce comparison synthetic spectra which account for the effects of magnetic fields. This requires the modification of the MOOG spectral synthesis program to handle the full Stokes vector treatment for polarized radiation through a magnetized medium. I create a grid of synthetic spectra covering ranges in effective temperature, surface gravity, and average magnetic field strength relevant for studies of young stellar objects, and develop a Chi-squared minimization routine to determine the best fit synthetic spectrum for a given observed spectrum at an arbitrary resolving power. This grid of synthetic spectra will be an invaluable complement to future near infrared, large band-pass, high-resolving power spectrographs (i.e. IGRINS). In addition to these observational and theoretical attempts to reduce systematic errors, I also helped to develop a suite of silicon and KRS-5 grisms for use in the FORCAST instrument, a mid infrared camera on the SOFIA telescope. These grisms will afford the imaging instrument a mid infrared spectroscopic capability at wavelengths normally inaccessible from the ground. I also report on my work to help write FG Widget, the quick-look reduction software package developed to support grism observations. / text

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O σκοπός της εργασίας αυτής ήταν η σύνθεση νέων αστεροειδών τριπολυμερών, τύπου An(B-C)n διαφόρων μοριακών δομών, με την τεχνική του «ζωντανού» ανιονικού πολυμερισμού. Αναπτύχθηκε μια μεθοδολογία τεσσάρων διαδοχικών σταδίων σε αντίδραση διαλείποντος έργου η οποία δίνει προϊόντα καθορισμένης μοριακής αρχιτεκτονικής. Η μέθοδος αυτή είναι επέκταση της μεθόδου in-out που χρησιμοποιήθηκε για την σύνθεση ετεροκλαδικών συμπολυμερών αστεροειδών τύπου ΑnBn. Τα νέα αστεροειδή τριπολυμερή Αn(B-C)n αποτελούνται από ένα πυρήνα διασταυρομένων μονομερών από τον οποίο εξέρχονται δύο ειδών κλάδοι θεωρητικά ίσου αριθμού, ήτοι κλάδοι ομοπολυμερούς Α και κλάδοι δι-συσταδικού συμπολυμερούς (B-C). Για το σκοπό αυτό χρησιμοποιήθηκε μια ποικιλία μονομερών και παραγόντων συνένωσης προκειμένου να επιτύχουμε το επιθυμητό αποτέλεσμα. Χρησιμοποιήθηκαν διφορετικοί πυρήνες των αστεροειδών τόσο στη φύση (διβίνυλοβενζόλιο, διμεθακρυλικός αιθυλενο-γλυκολεστέρας) όσο και στις διαστάσεις (μίγμα διβίνυλοβενζολίου/στυρενίου) προκειμένου να μελετηθεί η επίδραση που φέρουν. Η μεθοδολογία που χρησιμοποιήθηκε δίνει τη δυνατότητα του σταδιακού χαρακτηρισμού των προϊόντων ο οποίος ήταν ουσιώδης για τον τελικό χαρακτηρισμό των τριπολυμερών. Για το μοριακό χαρακτηρισμό πρόδρομων και τελικών πολυμερών χρησιμοποιήθηκαν οι τεχνικές της χρωματογραφίας αποκλεισμού μεγεθών, της στατικής σκέδασης φωτός και η φασματοσκοπία του πυρηνικού μαγνητικού συντονισμού (1H-NMR). Επιπλέον για λόγους σύγκρισης ιδιοτήτων μεταξύ γραμμικών και αστεροειδών, συντέθηκαν γραμμικά ABC τριπολυμερή χρησιμοποιώντας την μέθοδο της διαδοχικής προσθήκης. Τα τελικά πολυμερή καθαρίστηκαν από τυχόν προσμίξεις με την τεχνική της soxhlet και χρησιμοποιώντας ως διαλύτη κυκλοεξάνιο. Μελετήθηκαν οι μηχανικές ιδιότητες των ετεροκλαδικών αστεροειδών συμπολυμερών σε σύγκριση με τα αντίστοιχα γραμμικά τριπολυμερή, με σκοπό να διερευνηθεί η επίδραση της αρχιτεκτονικής στις ιδιότητες αυτές. Επιπλέον εξετάσθηκε και ο μικροφασικός διαχωρισμός τόσο των γραμμικών όσο και των αστεροειδών τριπολυμερών και ο ρόλος που παίζουν η αρχιτεκτονική και τα μοριακά χαρακτηριστικά των πολυμερών. Η πραγματοποίηση πειραμάτων δυναμικής μηχανικής ανάλυσης καθώς και διαφορικής θερμιδομετρίας σάρωσης σε αστεροειδή πολυμερή πολύστυρενίου, πολύ(μεθακρυλικού εξυλεστέρα) και πολύ(μεθακρυλικού μεθυλεστέρα) και στα αντίστοιχα γραμμικά τους πολυμερή οδήγησαν σε ενδιαφέρον συμπεράσματα. Έγινε σαφές πως η δομή και το μοριακό βάρος επηρεάζουν τις ιδιότητες των πολυμερών. / The subject of this research was the synthesis of star-shaped terpolymers An(B-C)n, using the anionic living polymerization. A 4-step methodology in patch reaction was developed which gives polymers of specific molecular structure. This method is expansion of the in-out method which is used to synthesize heteroarm-star copolymers AnBn. The new star terpolymers consist of a core from cross-linked monomers from which derive two kind of branches theoretically equal in number. One is branches of homopolymer A and the other is branches of diblock copolymer (B-C). For this aim a variety of monomers and cross-linking agents was used. Different cores were made on the nature (DVB,EGDMA) and the size (DVB/St) in order to investigate their effect. Through the synthetic methodology we were able to molecular characterize each step which was vital for the final polymer. The polymers were well characterized through specific techniques. In order to measure the molar mass (Mw and Mn) and the polydispersity, I (Mw/Mn), we used Size Exclusion Chromatography (SEC) technique. The number of the branches was calculated by the Static Light Scattering (SLS) technique. Nuclear Magnetic Resonance spectroscopy (1 H-NMR) was used to calculate the percentage of each homopolymer to the terpolymer. Moreover in order to compare the properties of star and linear terpolymers, ABC linear terpolymers were synthesized by sequential addition. The final polymers were purified through the soxhlet technique with cycloexane. The properties of heteroarm star-like terpolymers were studied comparing with that of the corresponding linear terpolymers (the block and arm lengths were equal) in order to understand the effect of the macromolecular architecture on these properties. Moreover the microphase separation was examined in order to study the effect of the architecture and the molecular characteristics on the terpolymers. The Dynamic Mechanical Analysis (DMA) and Differential Scanning Calorimetry (DSC) experiments on linear and star terpolymers with polystyrene (PS), poly(hexylmethacrylate) (PHMA) and poly(methylmethacrylate) (PMMA) result in interesting conclusions. These conclusions gave us a clear proof that the molecular characteristics and the architecture of the polymers infect their properties.

Dense cluster environment influences the properties of galaxies and their evolution. In order to understand this environmental effect and how it evolves with time, we study the infrared (IR) properties of galaxies in three rich clusters. The IR luminosities provide us with extinction-free measurements of the star formation rates (SFRs) of these cluster galaxies. We find a strong evolution in the IR luminosity function (LF) of two z ∼ 0:8 clusters when compared to two local clusters. The evolution rate of the IR LF found in these clusters is consistent with the evolution in field IR LFs. The similar evolution rate found in very different environments favors some internal mechanism, e.g., the gradual consumption of the gas fuel in galaxies, as being responsible for much of the star formation evolution. The mass-normalized integrated SFRs within 0.5R₂₀₀ of these clusters also shows an evolution trend, ∝ (1 + z)5. But this evolution has large scatter and may be affected by the mass selection effect of the sample. In the dense cluster core regions (r < 0.3 Mpc), we find evidence for enhanced SFR suppression. A substantial fraction of members in MS 1054-03 (z ∼ 0.8) are still forming stars actively. This cannot be explained by the scenario where the cluster is only passively accreting star-forming galaxies from the surrounding field, after which their star formation is quenched quickly. We also study the extended IR emission from the intracluster dust (ICD) in A2029. We only find weak signals at 24 and 70 μm and obtain upper limits for the ICD emission.

Flygbranschen är en bransch som är mycket känslig för omvärldsfaktorer. De senaste årens konjunkturnedgång, terrorattentat, epidemier, höga oljepriser samt rådande konkurrenstryck har resulterat i stora lönsamhetsproblem för många flygbolag. Ett sätt att bli mer konkurrenskraftig och förbättra sin position på marknaden är att samarbeta i form av en strategisk allians. Idag finns det tre allianser i flygbranschen: Star Alliance, Oneworld och Skyteam. Den första globala alliansen var Star Alliance som bildades 1997. Företag har under många år samarbetat i olika former. Vissa forskare anser att ett företag inte längre kan välja mellan konkurrens eller samarbete, utan att det handlar om att kombinera de båda strategierna. Denna undersökning avser att ta reda på hur en strategisk flygallians påverkar ett flygbolag. För att avgränsa studien valdes SAS och dess samarbete inom Star Alliance som undersökningsobjekt. Studiens syfte är således att genom en fallstudie undersöka hur ett nätverksbolag har påverkats av att ingå i en strategisk flygallians. Två intervjuer har genomförts, en med en person anställd på SAS med tidigare förflutet i Star Alliance och en med en konsult med mångårig erfarenhet av resebranschen. Resultatet visar att alliansamarbetet inneburit en rad fördelar för SAS. Konkurrensen har mildrats, kostnader reducerats, intäkter och utvecklingsmöjligheter ökat. En av nackdelarna med att ingå i en strategisk allians är att beslutsprocesserna förlängs. Något som SAS dock inte upplever som ett problem då medlemskapet i alliansen varit av stor betydelse för dem. De slutsatser vi har dragit av denna undersökning är att de nämnda fördelarna med allianssamarbete kan ha ett högt pris då det kostar att vara medlem. Vi tror dock att det kan vara värt att betala en summa då samarbetet kan vara av betydelse för flygbolagets överlevnad. Då flygbolagen även samarbetar med flygbolag utanför alliansen ifrågasätter vi strategisk allians som den enda samarbetsformen för att uppnå minskad konkurrens, kostnadsreduceringar, ökade intäkter och utvecklingsmöjligheter.

Cholesterol and fatty acyl-coenzymeA thioesters are signalling molecules with role in regulation of genes involved in lipid and glucose transport and metabolism. The studies described herein focused on three proteins that bind lipids and have different cellular functions: steroidogenic acute regulatory protein (StAR), hepatocyte nuclear factor-4a (HNF-4a) and acyl-CoA binding protein (ACBP). First, StAR mediates delivery of cholesterol to inner mitochondrial membrane in steroidogenesis by a poorly understood mechanism. In our studies, fluorescent NBD-cholesterol binding assays demonstrate that StAR binds cholesterol at two binding sites with 32 nM Kds and circular dichroism spectra show that cholesterol binding results in changes of StAR secondary structure. Fluorescent sterol exchange assays between donor and acceptor mitochondrial membranes indicate that StAR significantly increased the formation of rapidly transferable cholesterol domains. Second, HNF-4a, a nuclear receptor, had been shown to bind fatty acyl-CoAs as natural ligands with apparent low affinities obtained with radiolabeled ligand binding assays. Our fluorescence spectroscopy studies demonstrate that HNF-4a ligand binding domain (HNF-4aLBD) binds acyl-CoAs at a single binding site with Kds of 1.6-4 nM. Fluorescence resonance energy transfer (FRET) between HNF-4aLBD tryptophan residues and cis-parinaroyl-CoA yielded an intermolecular distance of 42 Â thus pointing to direct molecular interaction. Third, although ACBP has been detected in the nucleus, it is not known whether ACBP may directly and/or functionally interact with a nuclear acyl-CoA binding protein such as HNF-4a to regulate transcription. Our present studies in vitro and in intact cultured cells, including circular dichroism of HNF-4a in the presence of ACBP, coimmunoprecipitation of HNF-4a/ACBP complexes, ACBP and HNF-4a colocalization in nuclei of cells by confocal microscopy demonstrate a physical association of ACBP and HNF-4a. FRET microscopy data indicated an intermolecular distance of 53 Â between ACBP and HNF-4a in rat hepatoma cells. Functional assays (transactivation of an HNF4a-dependent reporter gene) showed significant increase in the presence of ACBP in two different cell lines. Expression of ACBP anti-sense RNA decreased HNF-4a-mediated transactivation, pointing to a role of ACBP in co-regulating HNF-4a-dependent transcription.

It has become clear that the global star formation rate in the Universe has been decreasing since at least z~1, and blue, star-forming galaxies are transformed into red, passive galaxies through one or more processes. The origin of this decline and transformation remains unclear. The role environment plays in all this is especially uncertain. Despite the observed domination of a passive population in the cores of clusters, in contrast to the more actively star-forming field population, whether or not, and how environment affects the properties of galaxies when they fall into clusters is an unsettled question. In this thesis, we look into these issues by examining both the passive and star-forming galaxies, from the cores out to the infall regions, in a large sample of clusters at 0.15<z<0.36 we detected from the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS). We find that in the cores of clusters, the red-sequence galaxies are a mixture of two populations, indicated by the inflexion in their luminosity function. There is no strong evolution in the shape of the red-sequence between z~0.4 and z~0.2; however, from z~0.2 to today, there is a rapid increase in the number of faint galaxies on the red-sequence relative to the bright ones, suggesting a rapid quenching of the faint galaxies in cluster cores within the last few billion years. At z~0.2, we find that the red fraction (star-forming fraction), at all stellar mass explored (9.0<log10(M*/M_solar)<11.5), shows no dependence on the distance from cluster centres, in the range 3<r<7Mpc; but within the inner 3 Mpc, we see a clear increase (decrease) in the red fraction (star-forming fraction). Also, for the lowest stellar mass galaxies, their red fraction has increased by a factor of 2 from z~0.3 to z~0.2 (over 1 Gyr), and yet we do not detect any difference between the star formation properties of the star-forming galaxies in clusters at all radii and that in the field. This suggests that for the low mass galaxies, it is likely that a mechanism that truncates star formation rapidly (within 1 Gyr) is at work. In the outskirts of the clusters, despite the low density contrast with the field, the red fraction is still higher than that in the field, suggesting that those galaxies have had their star formation quenched relative to the field population, supporting the pre-processing scenario.

(Abridged) Physical processes regulating star formation in satellite galaxies represent an area of ongoing research, but the projected nature of observed coordinates makes separating different populations of satellites (with different processes at work) difficult. The present-day phase space coordinates of a satellite galaxy carry information about its orbital history, which can then be compared to its star formation history (SFH). This is expected to reveal both a trigger time and timescale for environmental quenching. Finally, this can be related back to the physical process(es) regulating star formation in high density environments. We use merger trees from the MultiDark Run 1 N-body simulation to compile a catalogue of satellite orbits in cluster environments. We parameterize the orbital history by the time since crossing within 2.5 virial radii of the cluster centre and use our catalogue to estimate the probability density over a range of this parameter given a set of projected phase space coordinates. We show that different populations of satellite haloes occupy (semi-)distinct regions of (projected) phase space. We generalize this result by producing a probability distribution function (PDF) of possible infall times at every point in projected phase space. We apply our method to determining the infall time PDFs of a large sample of observed cluster satellite candidates from the Sloan Digital Sky Survey. We use galaxy colour as a proxy for SFH and model the distribution of satellite galaxy colours as two gaussian populations. We derive a Markov chain Monte-Carlo method to obtain the colour distribution as a function of the time since infall into the cluster environment. Our implementation of this method is still being tuned, but we use a second simpler (but much cruder) method to obtain an estimate of the evolution of the colour distribution. Our results are suggestive of a quenching process that begins within perhaps ±1 Gyr of virial radius crossing and which slows after pericentric passage. We stress that results obtained with this second method come with important caveats.

Baigiamojo bakalauro darbo tema yra žmogaus, kaip asmens pasąmonėje suformuotas ryšis su žvaigždėmis. Siekiama išanalizuoti žvaigždžių svarbą pačiam žmogui ir asmens istoriškumą su dangaus kūnais. Žmogaus istoriškumo, sąsajų su žvaigždėmis, erdvės pojūčio užuominų ieškoma lietuvių ir užsienio menininkų darbuose. Remiantis surinkta medžiaga, pateikiama tolimesnė darbo eiga, eskizai, technikos pasirinkimas. / Topic of the bachelor paper is the relation of human as a person with stars formed in his subconsciousness. It is striven to analyse the significance of stars to the man himself and the personal historical background with regard to heavenly bodies. Allusions with regard to historical background of the man, links with stars, sense of space are sought in pieces by Lithuanian and foreign artists. Referring to the material collected, further work process is provided along with sketches and the selection of technique.

The object of this dissertation is to provide an observational study of the effects of interstellar magnetic fields on star-formation regions. This is part of a long-standing research project that uses the techniques of radio astronomy to measure magnetic field strengths in the interstellar medium of our galaxy. Interstellar magnetic fields are believed to play a crucial role in the star-formation process therefore a comprehensive study of magnetic fields is necessary in understanding the origins of stars. These projects use observational data obtained from the Very Large Array (VLA) in Socorro, NM. The data reveal interstellar magnetic field strengths via the Zeeman effect in radio frequency spectral lines. This information provides an estimate of the magnetic energy in star-forming interstellar clouds in the Galaxy, and comparisons can be made with these energies and the energies of self-gravitation and internal motions. From these comparisons, a better understanding of the role of magnetic fields in the origins of stars will emerge. The regions observed include the giant molecular clouds and star-forming regions of Cygnus X and NGC 6334. NGC 6334 A is a compact HII region at the center of what is believed to be a large, rotating molecular torus (based on studies by Kramer et al. (1997)). This is a continuing study based on initial measurements of the HI and OH Zeeman effect (Sarma et al. (2000)). The current study includes OH observations performed by the VLA at a higher spatial resolution than previously published data, and allows for a better analysis of the spatial variations of the magnetic field. A new model of the region is also developed based on OH opacity studies, dust continuum maps, radio spectral lines, and infrared (IR) maps. The VLA has been used to study the Zeeman effect in the 21cm HI line seen in absorption against radio sources in the Cygnus-X region. These sources are mostly galactic nebulae or HII regions, and are bright and compact in this region of the spectrum. HI absorption lines are strong against these regions and the VLA is capable of detecting the weak Zeeman effect within them.