THE BARYONIC TULLY–FISHER RELATION OF GAS-RICH GALAXIES AS A TEST OF ΛCDM AND MOND

By S. McGaugh. 2011

366 citations recorded by the source corpus.

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 Mb = AV 4 f with A = 47 ± 6 M ☉ km−4 s4. 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 to relate halo properties to those of the galaxies they host. 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.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/73ae1484625891acba30f74f295c5ac04765c6cd

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Nuclear and High Energy Physics

Citations in the corpus

Understanding the shape and diversity of dwarf galaxy rotation curves in ΛCDM (2016, background): “The Baryonic Tully-Fisher Relation (BTFR) is a well-known correlation between the total baryonic mass of galaxies (stars plus gas; Mb) and their peak rotation velocity (Vf ; e.g. McGaugh et al. 2000; McGaugh & Wolf 2010; McGaugh 2012; Lelli et al. 2016).”
3D BAROLO: a new 3D algorithm to derive rotation curves of galaxies (2015, methodology): “The TFR is a severe testing ground for galaxy formation: current observations show a slope L (or Mbar) ∝ Vα with α ∼ 4 (e.g. Verheijen 2001; McGaugh 2012) and these relations strongly constrain models in the standard ΛCDM picture (e.g. Mo, Mao & White 1998; Bullock et al. 2001).”
Galaxies as simple dynamical systems: observational data disfavor dark matter and stochastic star formation (2014, methodology): “The extreme correlation between the density of dark matter and that of baryons as evidenced by low-surface brightness galaxies has been used as an argument against the SMoC by McGaugh [55], and that observed disk galaxies are much simpler than expected in the SMoC has been demonstrated by Disney et ”
THE SMALL SCATTER OF THE BARYONIC TULLY–FISHER RELATION (2015, methodology): “The presumed fb −Mb and fV −Mb relations are set by the galaxy formation process and must induce scatter on the observed BTFR.”
Dark matter, dark energy, and alternate models: A review (2017, result): “Modified potentials of MONG, may encounter some problems with Tully-Fisher law, which is an empirical relation between the intrinsic luminosity of a spiral galaxy and the rotation velocity, 4vµL , whereas, MOND is consistent with this law (McGaugh, 2012).”
THIRD-EPOCH MAGELLANIC CLOUD PROPER MOTIONS. II. THE LARGE MAGELLANIC CLOUD ROTATION FIELD IN THREE DIMENSIONS (2013, methodology): “As with high-mass galaxies, the scatter is below what is expected from initial conditions in cosmological models, implying the need for some feedback process that is correlated with the galaxy potential (Eisenstein & Loeb 1996; McGaugh 2012).”
Towards a more realistic population of bright spiral galaxies in cosmological simulations (2013, methodology): “Only a minority of galaxies lies within 1σ of these observations and the powerlaw slope constituted by our model sample is closer to 3 as advocated by Avila-Reese et al. (2008) and not 4 as found by McGaugh (2012).”
Theory of dark matter superfluidity (2015, background): “ses, which are inherently stochastic, result in such a tight correlation across dierent galaxy types? Indeed, recent hydrodynamical simulations [7] show considerably larger scatter than observations [4]. Another set of challenges comes from dwarf satellite galaxies in the Local Group. Dwarf satellit”
COLOR–MASS-TO-LIGHT-RATIO RELATIONS FOR DISK GALAXIES (2014, methodology): “Using the calibration based on gas rich galaxies of McGaugh (2012), we have checked the implied NIR mass-to-light ratios for those galaxies discussed here for which adequate kinematic data exist.”
A BUDGET AND ACCOUNTING OF METALS AT z ∼ 0: RESULTS FROM THE COS-HALOS SURVEY (2013, background): “In Figure 3 we show the atomic plus molecular gas mass measurements from McGaugh (2005, 2012) and Leroy et al. (2008), adding star-forming (NUV − r < 4) galaxies from the COLDGASS sample (Saintonge et al. 2011).”
Modified Newtonian Dynamics (MOND): Observational Phenomenology and Relativistic Extensions (2011, result): “Line-widths give a systematically different estimate of the slope of the BTFR than Vf , even for the same galaxies [277, 341, 476], and they cannot be related at all to the circular velocity of the potential at the virial radius, nor to the prediction of MOND (Sect.”
The unexpected diversity of dwarf galaxy rotation curves (2015, methodology): “…at 2 kpc comparable to the maximum (Vmax ∼ 62 km s−1, Vcirc(2 kpc) ∼ 58 km s−1), which indicates an enclosed mass of ∼2.3 × 109 M , or about twice as much as the total baryonic mass of the galaxy, according to the baryonic Tully–Fisher relation; Mbar/M = 102.3 (Vmax/ km s−1)3.82 (McGaugh 2012).”
The Dark Matter Crisis: Falsification of the Current Standard Model of Cosmology (2012, methodology): “…depends solely 6 Galaxies having such a well defined BTF relation is a major challenge for the SMoC (e.g. McGaugh 2011; Piontek & Steinmetz 2011; McGaugh 2012; Desmond 2012): For each individual DM halo of a givenDMmass (i.e. for a givenVc), the assembly history is different, and a wide range…”
Small scale problems of the $\Lambda$CDM model: a short review (2016, background): “oes. The tightness of the observed BTFR is therefore difﬁcult to explain in the LCDM model, contrary to the fundamental acceleration scale included in the MOdiﬁed Newtonian Dynamic (MOND) proposition [68]. Indeed, [119] claim that observation of a select sample of disk galaxies, assuming constant st”
The current status of galaxy formation (2012, methodology): “The observed slope is approximately 4, similar to what is found for MOND (Milgrom, 1983), whereas ΛCDM (without feedback) gives a slope of 3 (McGaugh, 2011, 2012), but fails to account for the observed dispersion and curvature.”
The VPOS: a vast polar structure of satellite galaxies, globular clusters and streams around the Milky Way (2012, methodology): “In the MOND-framework, the more massive, ”classical” dSph satellites naturally obey the Tully-Fisher relation (Tully & Fisher 1977), as it is a basic consequence of a MONDian gravity law (Milgrom 1983; McGaugh 2012; Famaey & McGaugh 2011).”