Parameters of 2447 Southern Spiral Galaxies for Use in the Tully-Fisher Relation

Mathewson, D. S.; Ford, V. L.

doi:10.1086/192356

Cited by 182 publications

(252 citation statements)

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“…Empirical evidence against a systematic di †erence between barred and unbarred galaxies was presented by Bosma (1996), and more can be found in the data from Mathewson & Ford (1996). We use the apparent magnitudes in the I-band, recession velocities, and given in V m their table, convert to absolute magnitudes assuming Hubble distances (for km s~1 Mpc~1), and plot H 0 \ 60 the Tully-Fisher relation for the 2368 galaxies in their sample having recession speeds greater than 1000 km s~1 (to avoid absurdly inaccurate Hubble distances) in Figure 18a.…”

Section: General Implicationsmentioning

confidence: 99%

“…We use the apparent magnitudes in the I-band, recession velocities, and given in V m their table, convert to absolute magnitudes assuming Hubble distances (for km s~1 Mpc~1), and plot H 0 \ 60 the Tully-Fisher relation for the 2368 galaxies in their sample having recession speeds greater than 1000 km s~1 (to avoid absurdly inaccurate Hubble distances) in Figure 18a. The line is Ðtted to all the data, but the 2219 points are for "" unbarred ÏÏ galaxies and the crosses mark the 149 galaxies that Mathewson & Ford (1996) designate as barred. 4 The histograms in Figure 18b show the distributions of velocity residuals about the Ðtted line for the barred and unbarred galaxies separately (scaled so that the area under each histogram is unity), suggesting a small o †set in the sense that the barred galaxies have slightly lower at a V m given brightness.…”

Section: General Implicationsmentioning

confidence: 99%

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Constraints from Dynamical Friction on the Dark Matter Content of Barred Galaxies

Debattista

Sellwood

2000

ApJ

518

631

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We show that bars in galaxy models having halos of moderate density and a variety of velocity distributions all experience a strong drag from dynamical friction unless the halo has large angular momentum in the same sense as the disk. The frictional drag decreases the bar pattern speed, driving the corotation point out to distances well in excess of those estimated in barred galaxies. The halo angular momentum required to avoid strong braking is unrealistically large, even when rotation is conÐned to the inner halo only. We conclude, therefore, that bars are able to maintain their observed high pattern speeds only if the halo has a central density low enough for the disk to provide most of the central attraction in the inner galaxy. We present evidence that this conclusion holds for all bright galaxies.

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Section: General Implicationsmentioning

confidence: 99%

Section: General Implicationsmentioning

confidence: 99%

Constraints from Dynamical Friction on the Dark Matter Content of Barred Galaxies

Debattista

Sellwood

2000

ApJ

518

631

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“…Long-slit observations have been traditionally used to deduce the rotation curves of galaxies (e.g., Rubin, Ford & . Thonnard 1980;Rubin et al 1982;Rubin et al 1985;Mathewson, Ford & Buchhorn 1992;Persic & Salucci 1995;Mathewson & Ford 1996;Courteau 1997;Dale et al 1997Dale et al , 1998Dale et al , 1999.…”

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confidence: 99%

Hα kinematics of S4G spiral galaxies – II. Data description and non-circular motions

Erroz-Ferrer¹,

Knapen²,

Leaman³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We present a kinematical study of 29 spiral galaxies included in the Spitzer Survey of Stellar Structure in Galaxies, using Hα Fabry-Perot data obtained with the Galaxy Hα Fabry-Perot System instrument at the William Herschel Telescope in La Palma, complemented with images in the R band and in Hα. The primary goal is to study the evolution and properties of the main structural components of galaxies through the kinematical analysis of the FP data, complemented with studies of morphology, star formation and mass distribution. In this paper we describe how the FP data have been obtained, processed and analysed. We present the resulting moment maps, rotation curves, velocity model maps and residual maps. Images are available in FITS format through the NASA/IPAC Extragalactic Database and the Centre de Données Stellaires. With these data products we study the non-circular motions, in particular those found along the bars and spiral arms. The data indicate that the amplitude of the non-circular motions created by the bar does not correlate with the bar strength indicators. The amplitude of those non-circular motions in the spiral arms does not correlate with either arm class or star formation rate along the spiral arms. This implies that the presence and the magnitude of the streaming motions in the arms is a local phenomenon.

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“…Then, defining M as the absolute I-band magnitude and S as the absolute I-band surface brightness of an object, a detailed modelling of the MFB (Mathewson et al [1992]) and MF (Mathewson & Ford [1996]) data in figure 2 shows that the particular model…”

Section: A Detailed Model Of the (α Ln A) Plotmentioning

confidence: 99%

“…Figures 5, 6 and 7 show the corresponding distributions for the Dale et al ( [1997] et seq) sample, the Mathewson & Ford [1996] sample and the Courteau [1997] sample. In each of these cases, the vertical dotted lines indicate the peak centres of figure 4.…”

Section: The Ln a Frequency Diagramsmentioning

confidence: 99%

Gravitation in the Fractal D = 2 Inertial Universe: New Phenomenology in Spiral Discs and a Theoretical Basis for MOND

Roscoe

2004

General Relativity and Gravitation

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A particular interpretation of Mach's Principle led us to consider if it was possible to have a globally inertial universe that was irreducibly associated with a non-trivial global matter distribution, Roscoe [2002a]. This question received a positive answer, subject to the condition that the global matter distribution is necessarily fractal, D = 2. The purpose of the present paper is to show how general gravitational processes arise in this universe. We begin by showing how classical Newtonian gravitational processes arise from point-source perturbations of this D = 2 inertial background. We are then able to use the insights gained from this initial analysis to arrive at a general theory for arbitrary material distributions. We illustrate the process by using it to model an idealized spiral galaxy. One particular subclass of solutions, corresponding to logarithmic spirals, has already been extensively tested (Roscoe [1999a(Roscoe [ ], [2002b), and shown to resolve dynamical data over large samples of optical rotation curves (ORCs) with a very high degree of statistical precision.Whilst the primary purpose of the data analysis of Roscoe [1999a] was to test the predictions of the logarithmic spiral theory, it led directly to the discovery of a major new phenomenology in spiral discs -that of discrete dynamical classes -initially reported in Roscoe [1999b] and comprehensively confirmed in Roscoe [2002b] over four large independent samples of ORCs. In this paper, we analyse the theory more comprehensively, and show how the discrete dynamical classes phenomenology has a ready explanation in terms of an algebraic consistency condition which must necessarily be satisfied.Of equal significance, we apply the theory with complete success to the detailed modelling of a sample of eight Low Surface Brightness spirals (LSBs) which, hitherto, have been succesfully modelled only by the MOND algorithm (Modified Newtonian Dynamics, Milgrom [1983a], [1983b], [1983c). The CDM models have failed comprehensively when applied to LSBs. We are able to conclude that the essence of the MOND algorithm must be contained within the presented theory.

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Parameters of 2447 Southern Spiral Galaxies for Use in the Tully-Fisher Relation

Cited by 182 publications

References 0 publications

Constraints from Dynamical Friction on the Dark Matter Content of Barred Galaxies

Constraints from Dynamical Friction on the Dark Matter Content of Barred Galaxies

Hα kinematics of S4G spiral galaxies – II. Data description and non-circular motions

Gravitation in the Fractal D = 2 Inertial Universe: New Phenomenology in Spiral Discs and a Theoretical Basis for MOND

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