Dynamical and Chemical Structure of Galactic Halos

This doctoral dissertation presents studies of the formation and evolution of galaxies, through observations and simulations of galactic halos. The halo is the component of galaxies which hosts some of the oldest objects we know of in the cosmos; it is where clues to the history of galaxies are found, for example, by how the chemical structure is related to the dynamics of objects in the halo. The dynamical and chemical structure of halos, both in the Milky Way’s own halo, and in two elliptical galaxies, is the underlying theme in the research. I focus on the density falloff and chemistry of the two external halos, and on the dynamics, density falloff, and chemistry of the Milky Way halo. I first study galactic halos via computer simulations, to test the long- term stability of an anomalous feature recently found in kinematics of the Milky Way’s metal-poor stellar halo. I find that the feature is transient, making its origin unclear. I use a second set of simulations to test if an initially strong relation between the dynamics and chemistry of halo glob-ular clusters in a Milky Way-type galaxy is affected by a merging satellite galaxy, and find that the relation remains strong despite a merger in which the satellite is a third of the mass of the host galaxy. From simulations, I move to observing halos in nearby galaxies, a challenging procedure as most of the light from galaxies comes from the disk and bulge components as opposed to the halo. I use Hubble Space Tele scope observations of the halo of the galaxy M87 and, comparing to similar observations of NGC 5128, find that the chemical structure of the inner halo is similar for both of these giant elliptical galaxies. I use Very Large Telescope observations of the outer halo of NGC 5128 (Centaurus A) and, because of the difficultly in resolving dim extragalac- tic stellar halo populations, I introduce a new technique to subtract the contaminating background galaxies. A transition from a metal-rich stellar halo to a metal-poor has previously been discovered in two different types of galaxies, the disk galaxy M31 and the classic elliptical NGC 3379. Unexpectedly, I discover in this third type of galaxy, the merger remnant NGC 5128, that the density of metal-rich and metal-poor halo stars falls at the same rate within the galactocentric radii of 8 − 65 kpc, the limit of our observations. This thesis presents new results which open opportunities for future investigations.

Biosynthesis of Yersinia enterocolitica serotype O:3 lipopolysaccharide outer core

Lipopolysacharide (LPS) present on the outer leaflet of Gram-negative bacteria is important for the adaptation of the bacteria to the environment. Structurally, LPS can be divided into three parts: lipid A, core and O-polysaccharide (OPS). OPS is the outermost and also the most diverse moiety. When OPS is composed of identical sugar residues it is called homopolymeric and when it is composed of repeating units of oligosaccharides it is called heteropolymeric. Bacteria synthesize LPS at the inner membrane via two separate pathways, Lipid A-core via one and OPS via the other. These are ligated together in the periplasmic space and the completed LPS molecule is translocated to the surface of the bacteria. The genes directing the OPS biosynthesis are often clustered and the clusters directing the biosynthesis of heteropolymeric OPS often contain genes for i) the biosynthesis of required NDP-sugar precursors, ii) glycosyltransferases needed to build up the repeating unit, iii) translocation of the completed O-unit to the periplasmic side of the inner membrane (flippase) and iv) polymerization of the repeating units to complete OPS. The aim of this thesis was to characterize the biosynthesis of the outer core (OC) of Yersinia enterocolitica serotype O:3 (YeO3). Y. enterocolitica is a member of the Gram-negative Yersinia genus and it causes diarrhea followed sometimes by reactive arthritis. The chemical structure of the OC and the nucleotide sequence of the gene cluster directing its biosynthesis were already known; however, no experimental evidence had been provided for the predicted functions of the gene products. The hypothesis was that the OC biosynthesis would follow the pathway described for heteropolymeric OPS, i.e. a Wzy-dependent pathway. In this work the biochemical activities of two enzymes involved in the NDP-sugar biosynthesis was established. Gne was determined to be a UDP-N-acetylglucosamine-4-epimerase catalyzing the conversion of UDP-GlcNAc to UDP-GalNAc and WbcP was shown to be a UDP-GlcNAc- 4,6-dehydratase catalyzing the reaction that converts UDP-GlcNAc to a rare UDP-2-acetamido- 2,6-dideoxy-d-xylo-hex-4-ulopyranose (UDP-Sugp). In this work, the linkage specificities and the order in which the different glycosyltransferases build up the OC onto the lipid carrier were also investigated. In addition, by using a site-directed mutagenesis approach the catalytically important amino acids of Gne and two of the characterized glycosyltranferases were identified. Also evidence to show the enzymes involved in the ligations of OC and OPS to the lipid A inner core was provided. The importance of the OC to the physiology of Y. enterocolitica O:3 was defined by determining the minimum requirements for the OC to be recognized by a bacteriophage, bacteriocin and monoclonal antibody. The biological importance of the rare keto sugar (Sugp) was also shown. As a conclusion this work provides an extensive overview of the biosynthesis of YeO3 OC as it provides a substantial amount of information of the stepwise and coordinated synthesis of the Ye O:3 OC hexasaccharide and detailed information of its properties as a receptor.

Multifrequency VLBI Observations of Selected Active Galactic Nuclei

In this dissertation, active galactic nuclei (AGN) are discussed, as they are seen with the high-resolution radio-astronomical technique called Very Long Baseline Interferometry (VLBI). This observational technique provides very high angular resolution (_ 10−300 = 1 milliarcsecond). VLBI observations, performed at different radio frequencies (multi-frequency VLBI), allow to penetrate deep into the core of an AGN to reveal an otherwise obscured inner part of the jet and the vicinity of the AGN’s central engine. Multi-frequency VLBI data are used to scrutinize the structure and evolution of the jet, as well as the distribution of the polarized emission. These data can help to derive the properties of the plasma and the magnetic field, and to provide constraints to the jet composition and the parameters of emission mechanisms. Also VLBI data can be used for testing the possible physical processes in the jet by comparing observational results with results of numerical simulations. The work presented in this thesis contributes to different aspects of AGN physics studies, as well as to the methodology of VLBI data reduction. In particular, Paper I reports evidence of optical and radio emission of AGN coming from the same region in the inner jet. This result was obtained via simultaneous observations of linear polarization in the optical and in radio using VLBI technique of a sample of AGN. Papers II and III describe, in detail, the jet kinematics of the blazar 0716+714, based on multi-frequency data, and reveal a peculiar kinematic pattern: plasma in the inner jet appears to move substantially faster that that in the large-scale jet. This peculiarity is explained by the jet bending, in Paper III. Also, Paper III presents a test of the new imaging technique for VLBI data, the Generalized Maximum Entropy Method (GMEM), with the observed (not simulated) data and compares its results with the conventional imaging. Papers IV and V report the results of observations of the circularly polarized (CP) emission in AGN at small spatial scales. In particular, Paper IV presents values of the core CP for 41 AGN at 15, 22 and 43 GHz, obtained with the help of the standard Gain transfer (GT) method, which was previously developed by D. Homan and J.Wardle for the calibration of multi-source VLBI observations. This method was developed for long multi-source observations, when many AGN are observed in a single VLBI run. In contrast, in Paper V, an attempt is made to apply the GT method to single-source VLBI observations. In such observations, the object list would include only a few sources: a target source and two or three calibrators, and it lasts much shorter than the multi-source experiment. For the CP calibration of a single-source observation, it is necessary to have a source with zero or known CP as one of the calibrators. If the archival observations included such a source to the list of calibrators, the GT could also be used for the archival data, increasing a list of known AGN with the CP at small spatial scale. Paper V contains also calculation of contributions of different sourced of errors to the uncertainty of the final result, and presents the first results for the blazar 0716+714.

Muukalainen aviovuoteessa : I married a monster for outer space (1958) ja invaasioelokuvan sukupuolittuneet todellisuudet

Teemanumero 1/2011 : Kauhut ja pelot.

Plan B from Outer Space - InsomniaGame-pelin suunnittelu ja toteutus 2010–2011

InsomniaGame oli Turun yliopiston digitaalisen kulttuurin oppiaineen ja Insomnia verkkopeliyhdistyksen yhteistyössä vuosina 2010 ja 2011 toteuttama pelikonseptikokeilu. InsomniaGame oli osa laajempaa ”CoEx: Yhteisöllistä tekemistä tukevat tilat kokemusten jakamisessa” kaksivuotista (1.10.2009–31.12.2011) hanketta, jonka toteuttivat yhteistyössä Turun yliopiston Porin yksikkö, Tampereen teknillisen yliopiston Porin yksikkö ja Tampereen yliopisto. Hankkeen tavoitteena oli toteuttaa sosiaalista mediaa, yhteisöllisyyttä ja lisättyä todellisuutta hyödyntäviä virtuaalisia ja julkisia tiloja, joissa käyttäjät voivat jakaa kokemuksia. Tutkimus on luonteeltaan soveltava pro gradu -tutkielma, joka sisältää kaksi vuotta kestäneen ja kaksi pelisovellusta sisältävän työosuuden. InsomniaGame koostui erilaisista pelaajien suorittamista tehtävistä, pelialustasta sekä taustatarinasta. Päätutkimuskysymykset ovat: Mitkä tekijät vaikuttivat pelisuunnitteluprosessiin ja miten? Työ esittelee InsomniaGame-pelin kehityksen. Erityistarkastelussa ovat suunnitteluprosessin ja pelin sisällölliset muutokset sekä niihin vaikuttaneet tekijät. Pelin kehitys perustui pääasiassa erilaisiin dokumentteihin, joita käytettiin suunnittelun apuvälineenä sekä viestinnässä projektin eri toimijoiden kesken. Tutkimus pyrkii syntyneiden dokumenttien sekä pelisuunnittelijoiden muistin perusteella rekonstruoimaan InsomniaGame-pelisovelluksen kehityskaaren. InsomniaGamen kehityksessä oli monia tekijöitä, jotka muuttuivat sen kehityskaaren aikana. Itse pelin sisältö, kuten myös suunnittelutapa, muuttuivat kahden vuoden aikana huomattavasti. Pelillä oli myös monia erityispiirteitä, jotka tekevät sen kehityksestä ainutlaatuisen, sillä esimerkiksi pelin testaaminen yhtenä kokonaisuutena oli mahdotonta. Lisäksi peli oli tutkimus- ja yhteistyöprojekti, jossa oli mukana monia eri toimijoita ja erityisesti tutkimuksessa korostuu yhteistyökumppani Insomnia verkkopeliyhdistyksen osallisuus. InsomniaGamen kummankaan vuoden toteutus ei sujunut odotetulla tavalla, mikä osaltaan vaikutti etenkin jälkimmäisen vuoden pelin suunnitteluun. Varsinainen suunnittelutyö kuitenkin eteni ensimmäisenä vuonna käytetyn mallin mukaisesti, mutta kuitenkin niin että alkuperäiset oletukset pelisuunnittelusta ja lopputuloksesta muuttuivat. Tämän vuoksi peliprojektia voi paikoitellen luonnehtia jopa kaoottiseksi, ja erityisesti toteutusvaiheessa jouduttiin luomaan nopealla aikataululla uusia toimintamalleja. Työ toimii mallina tuleville peliprojekteille, mutta erityisen tärkeää olisi luoda yhtenäinen kehitysalusta vastaavanlaisia projekteja varten.

Solar Twins and Solar Analogues in Galactic Surveys.

The Sun is a crucial benchmark for how we see the universe. Especially when it comes to the visible range of the spectrum, stars are commonly compared to the Sun, as it is the most thoroughly studied star. In this work I have focussed on two aspects of the Sun and how it is used in modern astronomy. Firstly, I try to answer the question on how similar to the Sun another star can be. Given the limits of observations, we call a solar twin a star that has the same observed parameters as the Sun within its errors. These stars can be used as stand-in suns when doing observations, as normal night-time telescopes are not built to be pointed at the Sun. There have been many searches for these twins and every one of them provided not only information on how close to the Sun another star can be, but also helped us to understand the Sun itself. In my work I have selected _ 300 stars that are both photometrically and spectroscopically close to the Sun and found 22 solar twins, of which 17 were previously unknown and can therefore help the emerging picture on solar twins. In my second research project I have used my full sample of 300 solar analogue stars to check the temperature and metallicity scale of stellar catalogue calibrations. My photometric sample was originally drawn from the Geneva-Copenhagen-Survey (Nordström et al. 2004; Holmberg et al. 2007, 2009) for which two alternative calibrations exist, i.e. GCS-III (Holmberg et al. 2009) and C11 (Casagrande et al. 2011). I used very high resolution spectra of solar analogues, and a new approach to test the two calibrations. I found a zero–point shift of order of +75 K and +0.10 dex in effective temperature and metallicity, respectively, in the GCS-III and therefore favour the C11 calibration, which found similar offsets. I then performed a spectroscopic analysis of the stars to derive effective temperatures and metallicities, and tested that they are well centred around the solar values.