The Baryonic Tully-Fisher Relation

McGaugh, Stacy S.; Schombert, James M.; Bothun, G. D.; Blok, W. J. G. de

doi:10.1086/312628

Cited by 742 publications

(890 citation statements)

References 27 publications

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“…Among these relations, the Baryonic Tully-Fisher relation (hereafter BTFR, e.g. McGaugh et al 2000;Bell & de Jong 2001;Gurovich et al 2004;McGaugh 2005;Pfenniger & Revaz 2005;Begum et al 2008;Trachternach et al 2009;Stark et al 2009;Gurovich et al 2010;Zaritsky et al 2014), extension of the Tully-Fisher relation (hereafter TF, e.g. Tully & Fisher 1977;Pierce & Tully 1988;Teerikorpi 1995;Giovanelli et al 1997b;Courteau & Rix 1999;Tully & Pierce 2000;Giovanelli et al 1997a;Karachentsev et al 2002;Bedregal et al 2006;Noordermeer & Verheijen 2007;Springob et al 2007;Williams et al 2010;Tully & Courtois 2012;Mocz et al 2012;Rawle et al 2013;Torres-Flores et al 2013;Sorce et al 2013Sorce et al , 2014b to the low luminosity galaxies, is often used to constrain and test galaxy formation and evolution models, with various computational methods, in the ΛCDM scenario as well as in alternative theories (e.g.…”

Section: Introductionmentioning

confidence: 99%

The baryonic Tully–Fisher relation cares about the galaxy sample

Sorce¹,

Guo²

2016

Mon. Not. R. Astron. Soc.

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The Baryonic Tully-Fisher relation (BTFR) is a clear manifestation of the underlying physics of galaxy formation. As such, it is used to constrain and test galaxy formation and evolution models. Of particular interest, apart from the slope of the relation, is its intrinsic scatter. In this paper, we use the eagle simulation to study the dependence of the BTFR on the size of the simulated galaxy sample. The huge number of datapoint available in the simulation is indeed not available with current observations. Observational studies that computed the BTFR used various (small) size samples with the only obligation to have galaxies spanning over a large range of masses and rotation rates. Accordingly, to compare observational and theoretical results, we build a large number of various size datasets using the same criterion and derive the BTFR for all of them. Unmistakably, their is an effect of the number of galaxies used to derive the relation. The smaller the number, the larger the standard deviation around the average slope and intrinsic scatter of a given size sample of galaxies. This observation allows us to alleviate the tensions between observational measurements and ΛCDM predictions. Namely, the size of the observational samples adds up to the complexity in comparing observed and simulated relations to discredit or confirm ΛCDM. Similarly, samples, even large, that do not reflect the galaxy distribution give on average biased results. Large size samples reproducing the underlying distribution of galaxies constitute a supplementary necessity to compare efficiently observations and simulations.

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Section: Introductionmentioning

confidence: 99%

The baryonic Tully–Fisher relation cares about the galaxy sample

Sorce¹,

Guo²

2016

Mon. Not. R. Astron. Soc.

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“…For example, estimates of dust reddening, even if small, are needed to correctly interpret the stellar populations inferred from broadband colors and spectroscopic measurements (e.g., Bell et al 2000). It has been found that many of the lowest luminosity LSB galaxies deviate from the standard optical Tully-Fisher relation in the sense that they rotate faster than predicted for their luminosities (e.g., Matthews, van Driel, & Gallagher 1998 ;Stil 1999 ;McGaugh et al 2000), while more luminous LSB galaxies seem to follow the same Tully-Fisher relation as higher surface brightness galaxies (e.g., Zwaan et al 1995 ;Sprayberry et al 1995). This appears to have important implications for galaxy formation models (e.g., van den Bosch 2000) and for establishing the possible existence of a "" baryonic ÏÏ Tully-Fisher relation (e.g., Matthews et al 1998 ;McGaugh et al 2000) ; however, the internal extinction corrections appropriate for the LSB galaxies used in these analyses remains a point of contention (e.g., Han 1992 ;Rhee 1996 ;Matthews et al 1998 ;Pierni 1999).…”

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confidence: 99%

Modeling the Interstellar Medium of Low Surface Brightness Galaxies: Constraining Internal Extinction, Disk Color Gradients, and Intrinsic Rotation Curve Shapes

Matthews

Wood

2001

Astrophysical Journal

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We use a combination of three-dimensional Monte Carlo radiative transfer techniques and multiwavelength (BRHK, Ha) imaging data to investigate the nature of the interstellar medium (ISM) in the edge-on, low surface brightness (LSB) galaxy UGC 7321. Using realistic models that incorporate multiple scattering e †ects and clumping of the stars and the interstellar material, we explore the distribution and opacity of the interstellar material (gas]dust) and its e †ects on the observed stellar disk luminosity proÐles, color gradients, and rotation curve shape. We Ðnd that UGC 7321 contains a small but nonnegligible dusty component to its ISM, yielding a B-band optical depth from disk edge to q6 e,B D 4.0 center. A signiÐcant fraction (D50%^10%) of the interstellar material in the innermost regions of UGC 7321 appears to be contained in a clumpy medium, indicating that LSB galaxies can support a modest, multiphase ISM structure. In spite of the clear presence of dust, we conclude that the large radial optical color gradients observed in UGC 7321 and other similar LSB spiral galaxies cannot be accounted for by dust and must result primarily from signiÐcant stellar population and/or metallicity gradients. We show that realistic optical depth e †ects will have little impact on the observed rotation curves of edge-on disk galaxies and cannot explain the linear, slowly rising rotation curves seen in some edge-on LSB spirals. Projection e †ects create a far larger uncertainty in recovering the true underlying rotation curve shape of galaxies viewed at inclinations i Z 85¡.

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“…Moreover, the relation is essentially one between the total baryonic mass of a galaxy and the asymptotic flat rotational velocity-not the peak rotation velocity but the velocity at large distance. This is the most immediate prediction [23,24].…”

Section: The Basics Of Mondmentioning

confidence: 84%

Modified Gravity Without Dark Matter

Sanders¹

2007

Lecture Notes in Physics

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On an empirical level, the most successful alternative to dark matter in bound gravitational systems is the modified Newtonian dynamics, or MOND, proposed by Milgrom. Here I discuss the attempts to formulate MOND as a modification of General Relativity. I begin with a summary of the phenomenological successes of MOND and then discuss the various covariant theories that have been proposed as a basis for the idea. I show why these proposals have led inevitably to a multi-field theory. I describe in some detail TeVeS, the tensor-vector-scalar theory proposed by Bekenstein, and discuss its successes and shortcomings. This lecture is primarily pedagogical and directed to those with some, but not a deep, background in General Relativity

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The Baryonic Tully-Fisher Relation

Cited by 742 publications

References 27 publications

The baryonic Tully–Fisher relation cares about the galaxy sample

The baryonic Tully–Fisher relation cares about the galaxy sample

Modeling the Interstellar Medium of Low Surface Brightness Galaxies: Constraining Internal Extinction, Disk Color Gradients, and Intrinsic Rotation Curve Shapes

Modified Gravity Without Dark Matter

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