The baryonic Tully-Fisher relation and its implication for dark matter halos

Trachternach, C.; Blok, de Erwin; McGaugh, Stacy S.; Hulst, van der Thijs; Dettmar, R.‐J.

doi:10.1051/0004-6361/200811136

Cited by 100 publications

(139 citation statements)

References 47 publications

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“…Pfenniger & Revaz (2005) showed that a marginal improvement in the scatter of the BTFR of McGaugh et al (2000) could be obtained by treating η as a free parameter and suggested that the best-fit value (η ≈ 3) implied additional dark baryonic mass in the disk. In more accurate data, the scatter is consistent with being caused entirely by observational uncertainties (Verheijen 2001;McGaugh 2005b;Stark et al 2009;Trachternach et al 2009;McGaugh 2011), nullifying this motivation for dark baryons.…”

Section: Other Forms Of Gasmentioning

confidence: 76%

“…The latter is a flux-weighted integral over the velocity field and lacks the clear physical meaning of a rotation curve. It is, however, readily obtained from single disk 21 cm observations, whereas obtaining and analyzing interferometric data cubes is considerably more effort intensive (e.g., de Blok et al 2008;Trachternach et al 2009). …”

Section: Rotation Velocitymentioning

confidence: 99%

“…In general, these corrections turn out to be rather small (cf. Tully & Fouque 1985;Oh et al 2008;Trachternach et al 2009;Dalcanton & Stilp 2010), as the typical velocity dispersion of low-mass galaxies is ∼8 km s −1 (Kuzio de Naray et al 2009). Since the correction to the circular velocity occurs in quadrature, it is only somewhat important in the slowest rotators.…”

Section: Rotation Velocitymentioning

confidence: 99%

“…More importantly, physics should not distinguish between mass in stars and mass in other forms. Adding the observed gas mass to the stellar mass results in a baryonic Tully-Fisher relation (BTFR) that is linear (in log space) over many decades in mass (Verheijen 2001;Bell & de Jong 2001;Gurovich et al 2004;McGaugh 2005b;Pfenniger & Revaz 2005;Begum et al 2008a;Stark et al 2009;Trachternach et al 2009;Gurovich et al 2010). The BTFR appears to be the fundamental physical relation underpinning the empirical Tully-Fisher relation.…”

Section: Introductionmentioning

confidence: 99%

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The Baryonic Tully–fisher Relation of Gas-Rich Galaxies as a Test of Λcdm and Mond

McGaugh

2012

434

459

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The baryonic Tully-Fisher relation (BTFR) is an empirical relation between baryonic mass and rotation velocity in disk galaxies. It provides tests of galaxy formation models in ΛCDM and of alternative theories like modified Newtonian dynamics (MOND). Observations of gas-rich galaxies provide a measure of the slope and normalization of the BTFR that is more accurate (if less precise) than that provided by star-dominated spirals, as their masses are insensitive to the details of stellar population modeling. Recent independent data for such galaxies are consistent with M b = AV 4 f with A = 47 ± 6 M km −4 s 4 . This is equivalent to MOND with a 0 = 1.3 ± 0.3 Å s −2 . The scatter in the data is consistent with being due entirely to observational uncertainties. It is unclear why the physics of galaxy formation in ΛCDM happens to pick out the relation predicted by MOND. We introduce a feedback efficacy parameter E to relate halo properties to those of the galaxies they host. E correlates with star formation rate and gas fraction in the sense that galaxies that have experienced the least star formation have been most impacted by feedback.

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Section: Other Forms Of Gasmentioning

confidence: 76%

Section: Rotation Velocitymentioning

confidence: 99%

Section: Rotation Velocitymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

The Baryonic Tully–fisher Relation of Gas-Rich Galaxies as a Test of Λcdm and Mond

McGaugh

2012

434

459

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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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The isolated elliptical galaxy NGC 5812–MOND or dark matter?

Richtler,

Salinas,

Lane

et al. 2023

Astron Nachr

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There exist isolated elliptical galaxies, whose dynamics can be modeled without resorting to dark matter or MOND, for example, NGC 7507. Such objects lack understanding within the current framework of galaxy formation. The isolated elliptical NGC 5812 is another object to investigate a possible role of isolation. We use globular clusters (GCs) and the galaxy light itself as dynamical tracers to constrain its mass profile. We employ Gemini/GMOS mask spectroscopy, apply the GMOS reduction procedures provided within IRAF, measure GC velocities by cross correlation methods and extract the line‐of‐sight kinematics of galaxy spectra using the tool pPXF. We identify 28 GCs with an outermost galactocentric distance of 20 kpc, for which velocities could be obtained. Furthermore, 16 spectra of the integrated galaxy light out to 6 kpc have been used to model the central kinematics. These spectra provide evidence for a disturbed velocity field, which is plausible given the disturbed morphology of the galaxy. We construct spherical Jeans models for the galaxy light and apply tracer mass estimators for the globular clusters. With the assumptions inherent to the mass estimators, MOND is compatible with the mass out to 20 kpc. However, a dark matter free galaxy is not excluded, given the uncertainties related to a possible nonsphericity and a possible nonequilibrium state. We find one globular cluster with an estimated mass of , the first Ultra Compact Dwarf in an isolated elliptical. We put NGC 5812 into the general context of dark matter or alternative ideas in elliptical galaxies. The case for a MONDian phenomenology also among early‐type galaxies has become so strong that deviating cases appear astrophysically more interesting than agreements. The baryonic Tully Fisher relation (BTFR) as predicted by MOND is observed in some samples of early‐type galaxies, in others not. However, in cases of galaxies that deviate from the MONDian prediction, data quality and data completeness are often problematic.

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The baryonic Tully-Fisher relation and its implication for dark matter halos

Cited by 100 publications

References 47 publications

The Baryonic Tully–fisher Relation of Gas-Rich Galaxies as a Test of Λcdm and Mond

The Baryonic Tully–fisher Relation of Gas-Rich Galaxies as a Test of Λcdm and Mond

The baryonic Tully–Fisher relation cares about the galaxy sample

The isolated elliptical galaxy NGC 5812–MOND or dark matter?

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