Готові списки джерел за темами / Tully-Fisher relation

Добірка наукової літератури з теми "Tully-Fisher relation"

Автор: Grafiati

Опубліковано: 14 березня 2023

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Статті в журналах з теми "Tully-Fisher relation"

Tully, Richard. "Tully-Fisher relation." Scholarpedia 2, no. 12 (2007): 4485. http://dx.doi.org/10.4249/scholarpedia.4485.

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M. ALI, AKRAM. "TULLY - FISHER RELATION PROOFING." Journal of University of Anbar for Pure Science 3, no. 3 (December 1, 2009): 177–83. http://dx.doi.org/10.37652/juaps.2009.15642.

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Gurovich, Sebastián, Stacy S. McGaugh, Ken C. Freeman, Helmut Jerjen, Lister Staveley-Smith, and W. J. G. De Blok. "The Baryonic Tully–Fisher Relation." Publications of the Astronomical Society of Australia 21, no. 4 (2004): 412–14. http://dx.doi.org/10.1071/as04038.

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AbstractWe validate the baryonic Tully–Fisher (TF) relation by exploring the Tully–Fisher (TF) and BTF properties of optically and Hi-selected disk galaxies. The data includes galaxies from Sakai et al. (2000) calibrator sample, McGaugh et al. (2000: M2000) I-band sample, and 18 newly acquired Hi-selected field dwarf galaxies observed with the ANU 2.3-m telescope and the ATNF Parkes telescope (Gurovich 2005a).As in M2000, we re-cast the TF and BTF relations as relationships between baryon mass and W20. First we report some numerical errors in M2000. Then, we calculate weighted bi-variate linear fits to the data, and finally we compare the fits of the intrinsically fainter dwarfs with the brighter galaxies of Sakai et al. (2000). With regards to the local calibrator disk galaxies of Sakai et al. (2000), our results suggest that the BTF relation is indeed tighter than the TF relation and that the slopes of the BTF relations are statistically flatter than the equivalent TF relations. Further, for the fainter galaxies which include the I-band M2000 and Hi-selected galaxies of Gurovich's sample, we calculate a break from a simple power law model because of what appears to be real cosmic scatter. Not withstanding this point, the BTF models are marginally better models than the equivalent TF ones with slightly smaller Χred2 values.

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McGaugh, S. S., J. M. Schombert, G. D. Bothun, and W. J. G. de Blok. "The Baryonic Tully-Fisher Relation." Astrophysical Journal 533, no. 2 (April 20, 2000): L99—L102. http://dx.doi.org/10.1086/312628.

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Meyer, Martin J., Martin A. Zwaan, Rachel L. Webster, and Stephen E. Schneider. "Tully-Fisher Relations from an HI-Selected Sample." Symposium - International Astronomical Union 220 (2004): 411–12. http://dx.doi.org/10.1017/s0074180900183731.

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The Tully-Fisher relation is of interest because of its use as a secondary distance measure and the constraints it places on the physics of rotationally supported galaxies. We use data from the HI Parkes All-Sky Survey Catalogue to study and apply the Tully-Fisher relation on a sample of galaxies selected on their HI properties. the issues of third parameter dependencies and intrinsic scatter of the Tully-Fisher relation are investigated.

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de Oliveira, Claudia Mendes, Sergio Torres-Flores, Philippe Amram, Henri Plana, and Benoit Epinat. "3D Studies of Galaxies in Compact Groups." Proceedings of the International Astronomical Union 10, S309 (July 2014): 175–77. http://dx.doi.org/10.1017/s1743921314009612.

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AbstractFabry-Perot data of compact group galaxies have been used to show that the Tully-Fisher relation in any photometric band, for galaxies with vmax > 100 km/s, is very similar to that for galaxies in other less dense environments. In the low-luminosity end, however, a few compact group galaxies fall above the relation apparently because they are too bright for their mass. Here we show that if the mass is properly computed from spectral energy distribution fitting or mass modelling, for the low-luminosity galaxies, their positions in the stellar-mass or baryonic Tully-Fisher relation are what is expected for a normal Tully-Fisher relation and the outlying positions observed in the B and K Tully-Fisher relation could be explained by brightening of the low-luminosity interacting galaxies due to strong star formation or AGN activity.

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Pfenniger, D., and Y. Revaz. "The Baryonic Tully-Fisher relation revisited." Astronomy & Astrophysics 431, no. 2 (February 2005): 511–16. http://dx.doi.org/10.1051/0004-6361:20041660.

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Andersen, David R., and Matthew A. Bershady. "A Face-on Tully-Fisher Relation." Astrophysical Journal 599, no. 2 (December 12, 2003): L79—L82. http://dx.doi.org/10.1086/381292.

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Ferrero, Ismael, and Mario G. Abadi. "Redshift evolution of Tully-Fisher relation." Proceedings of the International Astronomical Union 11, S321 (March 2016): 126. http://dx.doi.org/10.1017/s1743921316009054.

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AbstractUsing the eagle cosmological simulation of galaxy formation we test the ability of the ΛCDM cosmological model to reproduce the Tully-Fisher relation (TFR) and its redshift evolution. We find that our simulated galaxies follow a TFR that is in good agreement with observed results up to z = 1, indicating no evolution in the slope and a weak decrease in the zero-point.

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Mould, Jeremy, Mingsheng Han, and Greg Bothun. "Nonlinearity of the Tully-Fisher relation." Astrophysical Journal 347 (December 1989): 112. http://dx.doi.org/10.1086/168101.

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Дисертації з теми "Tully-Fisher relation"

Young, Paul. "The Tully-Fisher relation in nearby clusters." Thesis, Durham University, 1996. http://etheses.dur.ac.uk/5097/.

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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.

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Barden, Marco. "The Evolution of the Tully-Fisher Relation at Redshift z~1." Diss., lmu, 2004. http://nbn-resolving.de/urn:nbn:de:bvb:19-29114.

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Bonhomme, Nicolas. "Cosmographie de l’univers local : analyse de données pour la relation de Tully-Fisher." Thesis, Lyon 1, 2010. http://www.theses.fr/2010LYO10048/document.

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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

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Bonhomme, Nicolas. "Cosmographie de l'univers local : analyse de données pour la relation de Tully-Fisher." Phd thesis, Université Claude Bernard - Lyon I, 2010. http://tel.archives-ouvertes.fr/tel-00522062.

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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

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Tiley, Alfred. "Probing the evolution of galaxies since z ~ 1 with the Tully-Fisher relation." Thesis, University of Oxford, 2016. https://ora.ox.ac.uk/objects/uuid:1169c5e2-5962-47a4-8c9f-f58fcf93bf68.

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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.

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Han, Mingsheng Mould Jeremy Mould Jeremy. "The I-band Tully-Fisher relation and large-scale motions in the universe /." Diss., Pasadena, Calif. : California Institute of Technology, 1991. http://resolver.caltech.edu/CaltechETD:etd-06222007-113504.

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Theureau, Gilles. "L'échelle des distances extragalactiques : la relation Tully-Fisher et la constante de Hubble Ho." Observatoire de Paris (1667-....), 1997. https://hal.science/tel-02153817.

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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

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Iodice, Enrichetta. "Formation Scenarios for Polar Ring Galaxies." Doctoral thesis, SISSA, 2001. http://hdl.handle.net/20.500.11767/4321.

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Soliman, Khaled Said Ahmed. "Peculiar flow fields in the zone of avoidance from the near-infrared Tully-Fisher relation." Doctoral thesis, University of Cape Town, 2017. http://hdl.handle.net/11427/25463.

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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.

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Pizagno, James Lawrence II. "The Tully-Fisher Relation, its residuals, and a comparison to theoretical predictions for a broadly selected sample of galaxies." The Ohio State University, 2006. http://rave.ohiolink.edu/etdc/view?acc_num=osu1154980670.

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Частини книг з теми "Tully-Fisher relation"

Lorenzo, M. Fernández, J. Cepa, A. Bongiovanni, H. Castañeda, A. M. Pérez García, M. A. Lara López, M. Pović, and M. Sánchez Portal. "Evolution of the Tully–Fisher Relation." In Astrophysics and Space Science Proceedings, 291. Berlin, Heidelberg: Springer Berlin Heidelberg, 2010. http://dx.doi.org/10.1007/978-3-642-11250-8_45.

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Bottinelli, L., L. Gouguenheim, G. Paturel, and P. Teerikorpi. "Malmquist bias in “Tully-Fisher” relation." In New Aspects of Galaxy Photometry, 223–26. Berlin, Heidelberg: Springer Berlin Heidelberg, 1985. http://dx.doi.org/10.1007/bfb0030946.

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Rosenberg, Jessica L. "2MASS and the Tully-Fisher Relation." In The Impact of Near-Infrared Sky Surveys on Galactic and Extragalactic Astronomy, 247–53. Dordrecht: Springer Netherlands, 1998. http://dx.doi.org/10.1007/978-94-011-5026-2_29.

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Giraud, E. "Distance Moduli from the Tully-Fisher Relation." In Observational Cosmology, 199–205. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3853-3_17.

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Evrard, August E. "The Tully-Fisher Relation: A Numerical Simulator’s Perspective." In Galaxy Scaling Relations: Origins, Evolution and Applications, 25–29. Berlin, Heidelberg: Springer Berlin Heidelberg, 1997. http://dx.doi.org/10.1007/978-3-540-69654-4_3.

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Bothun, G. D. "Minimizing the Scatter in the Tully-Fisher Relation." In Galaxy Distances and Deviations from Universal Expansion, 87–92. Dordrecht: Springer Netherlands, 1986. http://dx.doi.org/10.1007/978-94-009-4702-3_16.

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van der Kruit, P. C., and A. J. Pickles. "Applications of the Tully-Fisher Relation at High Redshift." In Astrophysics and Space Science Library, 339–47. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2919-7_39.

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Dale, Daniel A., Riccardo Giovanelli, Martha P. Haynes, Marco Scodeggio, Luis Campusano, and Eduardo Hardy. "The I-Band Tully-Fisher Relation at Intermediate Redshifts." In Galaxy Scaling Relations: Origins, Evolution and Applications, 341–43. Berlin, Heidelberg: Springer Berlin Heidelberg, 1997. http://dx.doi.org/10.1007/978-3-540-69654-4_41.

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Bernstein, Gary M., Puragra Guhathakurta, and Somak Raychaudhury. "How Good Is the Near-Infrared Tully-Fisher Relation?" In Spiral Galaxies in the Near-IR, 200–209. Berlin, Heidelberg: Springer Berlin Heidelberg, 1996. http://dx.doi.org/10.1007/978-3-540-49739-4_29.

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Bottinelli, L., P. Fouqué, L. Gouguenheim, G. Paturel, and P. Teerikorpi. "Malmquist Bias and Virgocentric Model in Tully-Fisher Relation." In Galaxy Distances and Deviations from Universal Expansion, 73–76. Dordrecht: Springer Netherlands, 1986. http://dx.doi.org/10.1007/978-94-009-4702-3_13.

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Тези доповідей конференцій з теми "Tully-Fisher relation"

Yegorova, Irina, and Paolo Salucci. "The Tully Fisher relation of spiral galaxies." In Baryons in Dark Matter Halos. Trieste, Italy: Sissa Medialab, 2004. http://dx.doi.org/10.22323/1.014.0084.

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Kobayashi, Masato, and Tsutomu Takeuchi. "Baryonic Tully-Fisher relation and star formation rate." In The Life Cycle of Dust in the Universe: Observations, Theory, and Laboratory Experiments. Trieste, Italy: Sissa Medialab, 2014. http://dx.doi.org/10.22323/1.207.0076.

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Spekkens, Kristine, Robert Minchin, and Emmanuel Momjian. "The Baryonic Tully-Fisher Relation and Dark Matter in Nearby Spirals." In THE EVOLUTION OF GALAXIES THROUGH THE NEUTRAL HYDROGEN WINDOW. AIP, 2008. http://dx.doi.org/10.1063/1.2973614.

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Saburova, A., I. Chilingarian, A. Kasparova, O. Sil’chenko, I. Katkov, K. Grishin, and R. Uklein. "Observational insights on the formation scenarios of giant low surface brightness galaxies." In ASTRONOMY AT THE EPOCH OF MULTIMESSENGER STUDIES. Proceedings of the VAK-2021 conference, Aug 23–28, 2021. Crossref, 2022. http://dx.doi.org/10.51194/vak2021.2022.1.1.161.

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Анотація:

Giant low surface brightness galaxies (gLSBGs) with the disk radii of up to 130 kpc represent a challenge for currentlyaccepted theories of galaxy formation and evolution, because it is diﬃcult to build-up such large dynamically cold systemsvia mergers preserving extended disks. We summarize the in-depth study of the sample of 7 gLSBGs based on the resultsof the performed spectral long-slit observations at BTA SAO RAS, surface photometry and Hi data available in literature.Our study revealed that most gLSBGs do not deviate from the Tully-Fisher relation. We discovered compact elliptical (cE)satellites in 2 out of these 7 galaxies. Provided the low statistical frequencies of gLSBGs and cEs, the chance alignment isimprobable, so it can indicate that gLSBGs and cE are evolutionary connected and gives evidence in favor of the majormerger formation scenario. Other formation paths of gLSBGs are also discussed.

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Williams, Michael J., Martin Bureau, Michele Cappellari, Victor P. Debattista, and C. C. Popescu. "Dark Matter and the Tully-Fisher Relations of Spiral and S0 Galaxies." In HUNTING FOR THE DARK: THE HIDDEN SIDE OF GALAXY FORMATION. AIP, 2010. http://dx.doi.org/10.1063/1.3458559.

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