Dissertations / Theses on the topic 'Tully-Fisher relation'

In this thesis are presented the Tully-Fisher (TF) relations for a sample of 99 galaxies within the four nearby dusters; Coma, Abell 2199. Abell 2634 and Abell 194. Each cluster was compromised of two samples. The first sample was drawn from either Zwicky or UGC catalogues based on a combination of magnitude, type and ellipticity. These provided spiral duster member candidates over the entire duster region to a magnitude limit of 16 in the b-band. The second sample was selected from published photographic plate scans of the central areas of each duster. This sample had a fainter magnitude limit of 18 b-band mags but covered a much smaller area (approx. 2ºx2º). The galaxies were observed over two observing runs in May and August of 1993 on the JKT and INT Isaac Newton Group Telescopes simultaneously. I-band CCD images and optical long-slit spectra were taken of 65% of the sdected objects. Isophotal ellipse fitting of the images was used to produce surface brightness profiles. From these, isophotal magnitudes and diameters woe extracted. From, consideration of the surface brightness, ellipticity and position angle a "disk region" of each profile was selected and used to calculate extrapolated total magnitudes. Gaussian fitting of Ha emission lines of the long-split spectra produced optical rotation curves for each galaxy. Maximum rotation velocities were calculated from these curves. Corrections found in the literature were applied to the total magnitude and rotation velocity of each galaxy. These compensated for internal dust extinction and the inclination of the disk to the line-of sight. Numerical simulations of the fitting procedures demonstrated that an inverse regression of log-rotation velocity on magnitude provided a fit tothe relationship free from selection bias. Residuals around this fit woe used to choose forms of the corrections that produced the minimum scatter. A fullerror budget was compiled and an error weighted fit to the data yielded relationships with a mean scatter of 0.35 mags rms. A combination of all sources of measurement error, considering inter-correlation, produced a value of 027 mags rms, as an estimate of the contribution to the scatter. It was shown that uncertain cluster membership was not a significant source of scatter. In addition, the "expanding duster" model correction suggested in the literature did not significantly reduce the scatter. The most important source of scatter in the relationship was found to be the symmetry and extent of rotation curves used. A significant correlation was shown to exist between rotation curve extent in terms of disk scale lengths and the TF fit residuals. When only the highest quality data were used, the typical scatter was reduced to 020 mags rms. Consideration of the remaining measurement errors produced an upper limit of 0.12 mags rms for the intrinsic scatter within the TF relation. Monte-Carlo modelling indicated that the observed difference in TF slope between the Coma and Abell 2634 samples was significant, The possibility that this difference is the result of systematic errors in the dataset was ruled out It is concluded that the change in gradients is due to real variations in the underlying slope influenced by differences in duster environment.

Ce travail de thèse s’inscrit dans le projet à long terme COSFLOS qui a pour but de comprendre l’évolution des structures de l’univers local. Pour cela nous utilisons la relation de Tully-Fisher qui permet de mesurer des distances indépendamment de la loi de Hubble pour des galaxies spirales dans un rayon de 80 Mpc. Mon travail a consisté à collecter, mesurer et analyser les données nécessaires pour cette relation également appelée Luminosity LineWidth (LLW). Cette relation relie la luminosité intrinsèque d’une galaxie à la vitesse maximale de rotation de son gaz neutre. La meilleure façon d’obtenir cette vitesse est de mesurer la largeur de la raie de l’hydrogène neutre (HI) à 21 cm. J’ai effectué de nouvelles observations ainsi que de nouvelles mesures au sein de ce programme, qui aujourd’hui compte 15411 profils HI dans la base de données EDD. J’ai également amélioré l’interface graphique du logiciel de photométrie ARCHANGEL qui nous permet d’obtenir les magnitudes apparentes afin de calculer les distances. Nous verrons que nous avons porté une grande attention sur le calcul du paramètre d’inclinaison de la galaxie observée. Enfin, parmi tous les échantillons en notre possession, j’ai choisi d’étudier plus en détail l’amas de galaxies d’Antlia qui permettra une calibration de la pente de la LLW. Ce travail a commencé par la sélection des candidates, a continué avec les observations puis les mesures et pour se finir sur la détermination des distances nécessaires à la calibration de la relation de Tully-Fisher
This phD thesis is part of the COSFLOS’project. Its goal is to understand the galaxy structure evolution in the local universe. For this purpose, we make use of the Tully-Fisher relation in order to measure the distances for galaxies within 80 Mpc. My research area in the project is to collect, measure and analyze the data needed for the Luminosity LineWidth (LLW). This relation is a direct link between intrinsic luminosity of a spiral galaxy and its maximal gas rotation velocity. The best way to compute this velocity is to measure HI linewidth. Including my new observations and measurements, the current extragalactic database EDD contains 15 411 HI profiles. To obtain the apparent magnitude needed for the distances, I improve the ARCHANGEL software, implementing new displays. We took a great care to a special parameter : the inclination of observed galaxy. Finally, I present the Antlia cluster, one of the cluster I use to calibrate the slope of the LLW. I start with the candidates selection, then with observations to finally obtain the distances for the calibration

Ce travail de thèse s'inscrit dans le projet à long terme COSFLOS qui a pour but de comprendre l'évolution des structures de l'univers local. Pour cela nous utilisons la relation de Tully-Fisher qui permet de mesurer des distances indépendamment de la loi de Hubble pour des galaxies spirales dans un rayon de 80 Mpc. Mon travail a consisté à collecter, mesurer et analyser les données nécessaires pour cette relation également appelée Luminosity LineWidth (LLW). Cette relation relie la luminosité intrinsèque d'une galaxie à la vitesse maximale de rotation de son gaz neutre. La meilleure façon d'obtenir cette vitesse est de mesurer la largeur de la raie de l'hydrogène neutre (HI) à 21 cm. J'ai effectué de nouvelles observations ainsi que de nouvelles mesures au sein de ce programme, qui aujourd'hui compte 15411 profils HI dans la base de données EDD. J'ai également amélioré l'interface graphique du logiciel de photométrie ARCHANGEL qui nous permet d'obtenir les magnitudes apparentes afin de calculer les distances. Nous verrons que nous avons porté une grande attention sur le calcul du paramètre d'inclinaison de la galaxie observée. Enfin, parmi tous les échantillons en notre possession, j'ai choisi d'étudier plus en détail l'amas de galaxies d'Antlia qui permettra une calibration de la pente de la LLW. Ce travail a commencé par la sélection des candidates, a continué avec les observations puis les mesures et pour se finir sur la détermination des distances nécessaires à la calibration de la relation de Tully-Fisher

In this thesis we use the Tully-Fisher relation (TFR), the correlation between a galaxy's luminosity and its rotation velocity, to probe the luminous and dark matter in galaxies over the last ≈ 8 Gyr. First, we use samples of galaxies spatially resolved in Hα emission with integral field unit observations from the K-band Multi-Object Spectrograph (KMOS) Redshift One Spectroscopic Survey (KROSS) at z ≈ 1 and the Sydney-Australian-Astronomical-Observatory Multi- object Integral-Field Spectrograph (SAMI) Galaxy Survey at z ≈ 0. We match the data quality, analysis methods and sample selection between the two surveys to conduct a direct comparison of the absolute K-band magnitude (MK) and stellar mass (M_*) TFRs at z ≈ 1 and z ≈ 0, free of any difference in biases between them. We measure no evolution of the MK TFR zero-point for star- forming disk-like galaxies since z ≈ 1, but an increase by 0.2 ± 0.2 dex of the M_* TFR zero-point for the same galaxies over the same period. This implies the total mass-to-stellar mass ratio of those galaxies has decreased by a factor of ≈ 0.4 since z ≈ 1 at fixed rotation velocity, whilst their K-band stellar mass-to- light ratio has increased by a factor of ≈ 1.6. Moderate rates of star formation in galaxies and continued gas accretion since z ≈ 1 can explain these changes. Second, we take a step toward an independent measure of the TFR evolution over the same period using carbon monoxide (CO) emission from galaxies as an alternative kinematic tracer. We present the M_* and Wide-Field Infrared Survey Explorer absolute Band 1 magnitude (MW1) TFRs for galaxies from the CO Legacy Database for the Galex Arecibo SDSS Survey (COLD GASS) as z ≈ 0 benchmarks that are pre-requisites to extend the CO TFR to z ≳ 1. We find no significant offsets between the COLD GASS TFR zero-points and those of similar z ≈ 0 studies. The slope of the M_* COLD GASS TFR agrees with those of similar z ≈ 0 studies, but the MW1 TFR slope is slightly shallower than previous studies at a similar redshift. We attribute this to the fact that the COLD GASS sample comprises galaxies of various (late-type) morphologies. Nevertheless, our work provides a robust reference point with which to compare future CO TFR studies.

Cette thèse présente une étude exhaustive de la relation Tully-Fisher (TF) appliquée aux galaxies spirales de champ. Mon échantillon (KLUN) compte 6620 galaxies de type Sa à Sdm ; il a été collecté à partir de nouvelles observations et de la base LEDA, et étudié en détail, en particulier en terme de complétude et d'homogénéité. Il permet d'analyser les différents aspects de la relation TF en bande B, en utilisant en parallèle les relations en diamètre, en magnitude, directe ou inverse. J’expose une version généralisée de la méthode des distances normalisées de Bottinelli et al (1986), ou toutes les variations du biais de Malmquist dans l'espace des paramètres observables sont maintenant prises en compte. Sa validation en termes statistiques conduit à une nouvelle méthode de correction du biais, qui permet d'étudier le champ des vitesses particulières jusqu'à des distances de 200 Mpc. Je montre par ailleurs que l'introduction de paramètres supplémentaires, tels que le type morphologique ou la brillance superficielle moyenne, permet de réduire la dispersion de la relation TF, et d'étendre le domaine des distances non-biaisées. J’obtiens ainsi une valeur statistiquement fiable de la constante de Hubble Ho à partir d'un échantillon non-biaisé de 600 galaxies de champ (z ≤ 0. 02), en parfait accord avec les résultats obtenus a plus grandes distances (z ≤ 0. 1) à partir des supernovæ de type Ia. Cette valeur de Ho = 55 ± 5 km s-1 Mpc-1 ne dépend plus que de la calibration primaire (distances céphéides). J’évalue indépendamment la vitesse de chute du groupe local vers Virgo (VGL=200 ± 30 km s-1), confirme l'existence d'une anomalie locale du champ des vitesses, et mets en valeur un mouvement de chute important au voisinage des amas de Persée-Poissons et Hydra, à la fois à l'arrière et à l'avant de ces concentrations. Le fort puit de potentiel attendu dans la région du grand attracteur n'est pas confirmé
This thesis presents an exhaustive study of the Tully-Fisher (TF) relation on the basis of the largest available sample of field spiral galaxies. This co-called KLUN sample, containing 6620 galaxies from type Sa to Sdm, has been collected from LEDA data base and studied in detail for completeness and homogeneity. It allows to investigate the various aspects of the B-band TF relation both with diameter and magnitude, direct or inverse relations. I report on an advanced version of the normalized distance method (Bottinelli et al. 1986), now taking into account all the variations of the Malmquist bias the observable parameters space. Its validation in statistical terms leads to work out a new bias correction method allowing to study the peculiar velocity field up to 200 Mpc. In addition, I show that introducing additional parameters such as morphological type or mean surface brightness reduces the TF intrinsic scatter and allows to extend the unbiased distance range. Then, a statistically reliable value of the Hubble constant Ho is obtained from an unbiased subsample of 600 field galaxies (z ≤ 0. 02), in perfect agreement with the results derived at greater distance from type Ia supernovae (up to z=0. 1). This value H0=55 ± 5 km s-1 Mpc-1 depends only on the primary calibration, i. E. Cepheid distances. I give an independent estimate of the Local Group infall toward Virgo (Vgl=200 ± 300 km s-1), confirm the existence of a Local Anomaly of the velocity field limited too Leo spur and Sculptor cloud, and show evidence for an infall pattern (front and back side infall) in the vinicity of some great mass concentrations such as Hydra or Perseus-Pisces clusters. The prominent bulk flow expected in the direction of the Great Attractor is not confirmed

In this thesis, we investigate the flow field in and around the major large-scale structures in the southern Zone of Avoidance as derived from peculiar motions of galaxies. The peculiar velocities were derived from a galaxy sample based on the systematic deep Parkes HI Zone of Avoidance survey (HIZOA) using a newly optimized Near InfraRed (NIR) Tully-Fisher (TF) relation. The NIR imaging data of the HIZOA galaxies were obtained with the Infrared Survey Facility (IRSF) on the 1.4-m telescope at the South African Astronomical Observatory, which allows simultaneous three-colour (J; H; and Ks) imaging. We first calibrate the NIR Tully-Fisher relation for isophotal magnitudes, using the same 888 calibrator galaxies that were used for the derivation of the 2MASS TF relation for total magnitudes. The isophotal NIR TF relation allows for a significant improvement in the scatter of low surface brightness galaxies, and galaxies obscured by dust. We also simulate the effect of dust extinction on the shape of galaxies and derive a correction model. We show the ability of this model to reproduce the intrinsic axial ratio from the observed parameters up to extinction levels of AV ~ 11 mag. We present new narrow-band HI 21-cm observations for 394 selected galaxies from the HIZOA survey with improved velocity resolution. These new observations with high resolution allow a robust measurement of five different types of linewidth. We used a Bayesian mixture model to derive conversion equations between these five widths, which will be used to combine data sets of differently-derived linewidths. We present deep near-infrared (J; H; and Ks bands) observations of 1108 detections from the HIZOA survey. The average seeing, sky background and the isophotal magnitude errors are 1:38 arcsec, 20:1 mag, and 0:02 mag respectively, which are of sufficient accuracy for a Tully-Fisher analysis. Through comparisons with 2MASS and UKIDSS images we demonstrate the reliability of the IRSF photometry. We use these data and the isophotal Tully-Fisher relation to measure distances and peculiar velocities for 287 galaxies, which covers the whole southern ZOA. We derive the HI mass function to make predictions for the Malmquist bias, thus enabling us to correct the measured distances accordingly. The slope of the HI mass function agrees with both HIPASS Bright Galaxy Catalog (BGC) and ALFALFA, whereas the characteristic HI mass aligns more closely with ALFALFA than the HIPASS BGC. We map the velocity field around the major large-scale structures in the southern ZOA, such as the Great Attractor (GA), the Local Void (LV), and the Puppis region. In the GA region, we find a clear infall into the GA from both sides. Our analysis of the LV shows that the void galaxies are moving away from the center which confirms the recent results which show the draining of the LV. We also find outflow from the Puppis region. We present comparisons between the velocity field derived in this thesis, the 2MASS TullyFisher observations (2MTF), the 2MASS Redshift Survey (2MRS), as well as the IRAS Point Source Catalog Redshift Survey (PSCz) reconstructions. We find good agreement at low redshift with the 2MTF observations, better than the 2MRS and the PSCz reconstructions. At high redshift, our results disagree with the 2MTF observations, the 2MRS, and the PSCz reconstructions.

This thesis aims at using the Infrared Survey Facility (IRSF) JHKₛ bands, Two Micron All Sky Survey (2MASS) JHKₛ bands and Wide Field Infrared Survey Explorer (WISE) W1-W4 bands isophotal magnitudes to understand the cosmic flow associated with Zone of Avoidance (ZoA) galaxies.

During the last few decades, it has been discovered that most of the material in the Universe is invisible. Since it interacts only gravitationally with the rest of the Universe components. From the latest measurements of WMAP satellite we know that the Universe consists of 4% Baryons, 22% Cold Dark Matter, 74% Dark Energy. Now it is clear a wonderful time to study cosmology. Using the latest technological advances we have obtained detailed picture of the early Universe and maps of the distribution of matter on the largest scales in the Universe today. And we have a physical model for the origin and evolution of the Universe. However on the small scales there are still a lot of open issues. The mass distribution in spiral galaxies is an interesting question that is tightly band to the galaxy formation and evolution process.

Cette thèse est consacrée à l'étude de la formation et de l'évolution des galaxies. La mise à disposition de la communauté par l'ESO du spectrographe à multi-intégrales de champ FLAMES/GIRAFFE représente une opportunité unique d'étudier la dynamique des galaxies à z<1, et de pouvoir ainsi relier les populations distantes aux populations locales. Nous présentons dans un premier temps les résultats obtenus grâce à cet instrument dans le cadre du temps garanti de l'Observatoire de Paris (GEPI). Ces résultats montrent que la fraction de galaxies n'ayant pas encore atteint leur équilibre dynamique à z~0.6 est importante. Cette fraction est encore plus importante parmi les galaxies compactes lumineuses (LCGs), ce qui supporte l'hypothèse selon laquelle ces galaxies sont des systèmes en cours de fusion. Jusqu'à présent, l'utilisation de la spectroscopie à fente ne permettait pas de distinguer efficacement les systèmes relaxés des systèmes non relaxés, ce qui explique les désaccords concernant l'évolution de la relation de Tully-Fisher. Les résultats présentés dans cette thèse montrent en effet une non évolution de cette relation dans le plan vitesse-masse stellaire. Enfin, GIRAFFE avec son mode IFU montre la pertinence de la cartographie physico-chimique du milieu interstellaire dans la compréhension des mécanismes liés aux processus de formation stellaire dans les galaxies distantes. L'extension des méthodes de spectroscopie intégrale de champ à z>1 requiert d'explorer leur couplage avec des techniques d'optique adaptative. Le projet FALCON (à la fois dédié aux VLTs et aux ELTs) propose une nouvelle voie prometteuse dans cette direction en introduisant le concept d'optique adaptative multi-objets (MOAO). Dans ce concept, seules les zones d'intérêt scientifique sont corrigées et analysées, ce qui nécessite le développement de systèmes miniaturisés de correction de front d'onde ainsi que d'une stratégie de commande originale en boucle ouverte.

Cette thèse présente les résultats concernant la structure, les relations d'échelle et la cinématique de 48 galaxies au sein de 22 groupes compacts de Hickson, sachant que pour 35 d'entre elles au sein de 12 groupes, ce travail présente des cartes monochromatiques, de vitesses et de dispersion de vitesses originales pour la ligne H. Les différents paramètres cinématiques et les courbes de rotation ont été déduits de ces cartes de vitesses ainsi que d'images dans le domaine optique. En utilisant les vitesses maximales de rotation (déduites des courbes de rotation), les luminosités tant dans le domaine visible que dans le domaine de l'infrarouge et les masses stellaires et baryoniques, il a été possible d'étudier les relations de Tully Fisher (TF) pour ces galaxies dans les groupes compacts. La comparaison de ces résultats avec ceux obtenus pour un échantillon de galaxies de champs, a montré que les galaxies dans des groupes compacts suivent la même relation de TF, définie pour un échantillon de galaxies dans un environnement moins dense. Toutefois, certaines galaxies de faible masse présentent des luminosités élevées pour leurs vitesses de rotation maximales. Les sursauts de formation stellaire, ainsi que l'activité nucléaire au sein de ces galaxies, paraissent être les facteurs principaux pouvant expliquer pourquoi les galaxies de faible masse dans les groupes compacts ne se retrouvent pas sur la relation de TF définie pour les galaxies de champs. Ce résultat indique que les vitesses maximales de rotation ne sont pas modifiées pour des galaxies en interactions et qu'il n'y a pas de perte de masse significative pour ces galaxies, à l'intérieur du R25. L'utilisation des courbes de rotation pour étudier la distribution de masse pour ces galaxies a révélé que ces dernières montrent un degré élevé de dissymétrie lié à des phénomènes d'interactions entre galaxies. Ces phénomènes, en plus de perturber les courbes de rotation, ont pour effet, d'expulser une partie du gaz neutre dans le milieu intra-groupe. L'utilisation de données dans le domaine ultra violet (UV) a montré la présence de plusieurs systèmes stellaires jeunes au sein du milieu intergalactique des groupes compacts. Ces systèmes peuvent devenir des galaxies satellites ou simplement se dissoudre dans le milieu intra-groupe
This thesis presents results on the kinematics, scaling relations and structures of 48 galaxies in 22 compact groups. For 35 galaxies in 12 compact groups, velocity fields, monochromatic maps (derived from Hα observations) and velocity dispersion maps are presented for the first time. By using these data, it was possible to determine the kinematic and morphological parameters, the rotation curves and to derive the Tully-Fisher relation for the galaxies in dense environments. By using the maximum rotational velocity for each galaxy (derived from its rotation curve) and its optical and near-infrared luminosity and mass, the different Tully-Fisher relations for galaxies in compact groups were derived. Comparing these results with the results displayed by galaxies in less dense environments, it was found that galaxies in compact groups agrees with the Tully-Fisher relation defined by non-interacting galaxies. However, some of the low-mass galaxies are off the Tully-Fisher relation, having too high luminosities for their maximum rotational velocities. This scenario can be explained by a burst of star formation and/or by nuclear activity. We conclude that the maximum rotational velocities of compact groups galaxies are not affected during galaxy-galaxy interactions which implies that there is no significant mass stripping in galaxies of compact groups inside their optical radius. The mass distribution of galaxies in compact groups indicates that the rotation curves of these galaxies are highly asymmetric. The asymmetry could be produced by interactions between galaxies. These interactions, besides affecting the shape of the rotation curve, can eject some neutral gas from the disk of the interacting galaxies into the intragroup medium. By using ultraviolet data, we find several young star-forming regions in the intragroup medium of compact groups. It is still an open question wether these young stellar systems can survive and become new members of the group or if they will fall back onto their parent galaxies

We examine the Einstein equation coupled to the Klein-Gordon equation for a complex-valued scalar field. These two equations together are known as the Einstein-Klein-Gordon system. In the low-field, non-relativistic limit, the Einstein-Klein-Gordon system reduces to the Poisson-Schrödinger system. We describe the simplest solutions of these systems in spherical symmetry, the spherically symmetric static states, and some scaling properties they obey. We also describe some approximate analytic solutions for these states.

The EKG system underlies a theory of wave dark matter, also known as scalar field dark matter (SFDM), boson star dark matter, and Bose-Einstein condensate (BEC) dark matter. We discuss a possible connection between the theory of wave dark matter and the baryonic Tully-Fisher relation, which is a scaling relation observed to hold for disk galaxies in the universe across many decades in mass. We show how fixing boundary conditions at the edge of the spherically symmetric static states implies Tully-Fisher-like relations for the states. We also catalog other ``scaling conditions'' one can impose on the static states and show that they do not lead to Tully-Fisher-like relations--barring one exception which is already known and which has nothing to do with the specifics of wave dark matter.

Dissertation

The ultimate goal of this thesis is to better understand the large-scale motions in the universe on scales beyond the Local-Supercluster, and also to better understand the Tully-Fisher relation as a distance indicator. Sixteen clusters of galaxies in redshifts range from 3000-10000 kms(-1) are studied as test points of the large-scale velocity field, using the I-band Tully-Fisher relation as distance indicator. A complete observational procedure and techniques of measuring cluster distance using the Tully-Fisher relation is investigated in detail, which involves many general topics in the photometric studies of galaxies. Major discussions and results in the thesis are summarized as: 1. CCD surface photometry is described in detail. Errors and various effects (extinction, cosmological and seeing) on surface photometry are discussed. I-band surface photometry is carried out for some 280 galaxies in the thesis sample. 2. The problem of internal absorption in spiral galaxies is investigated; new magnitude and isophotal-diameter corrections for internal absorption are derived. 3. Different techniques for deriving cluster distances using Tully-Fisher relation are compared; distance bias due to sample selection effects is discussed at length; a Maximum-Likelihood method is given which is able to handle the sample selection effects. 4. Global photometric properties of the cluster galaxies are examined; the problem of second parameter in the TF relation is investigated; a physical explanation for the TF relation and its dispersion is proposed. 5. The peculiar velocity field as traced by the sample clusters is found to be highly non-random, and appears to be a coherent flow towards the general direction of the Great Attractor, with a flow amplitude of some 400~600 kms(-1) at the position of the Local Group.

We have compiled a large sample of 3041 spiral galaxies with multi-band $gri$ photometry from the the Sloan Digital Sky Survey (SDSS) Data Release 7 archive. We compare our own extracted photometry with data products provided through the SDSS pipeline algorithms. This comparison benefits from an extensive compilation of galaxy rotational velocities, $V$, derived from HI linewidths. Galaxy sizes and luminosities can thus be compared against an unbiased and independent metric. We find the SDSS radial ($R$), and luminous, ($L$), data products to be unreliable for the construction of tight scaling relations of $R$ and $L$ with velocity ($V$). We use our own robust scaling parameters to yield the tightest $VRL$ relations possible. We further compile the largest scaling relation of galaxy baryonic mass (stars + gas) with velocity to find that the relation is not tighter, and thus no more significant, than the luminous $VL$ relation.
Thesis (Master, Physics, Engineering Physics and Astronomy) -- Queen's University, 2010-09-17 16:23:20.649