The Baryonic Tully-Fisher Relation of Galaxies with Extended Rotation Curves and the Stellar Mass of Rotating Galaxies

By S. McGaugh. 2005

433 citations recorded by the source corpus.

I investigate the baryonic Tully-Fisher relation for a sample of galaxies with extended 21 cm rotation curves spanning the range 20 km s-1 ≲ Vf ≤ 300 km s-1. A variety of scalings of the stellar mass-to-light ratio ϒ⋆ are considered. For each prescription for ϒ⋆, I give fits of the form ℳd = 𝒜V. Presumably, the prescription that comes closest to the correct value will minimize the scatter in the relation. The fit with minimum scatter has 𝒜 = 50 ℳ☉ km-4 s4 and x = 4. This relation holds over five decades in mass. Galaxy color, stellar fraction, and ϒ⋆ are correlated with each other and with ℳd, in the sense that more massive galaxies tend to be more evolved. There is a systematic dependence of the degree of maximality of disks on surface brightness. High surface brightness galaxies typically have ϒ⋆ ~ of the maximum disk value, while low surface brightness galaxies typically attain ~ of this amount.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/88387b3f5cb8b77e4aefc60314b738eafafb1c56

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Citations in the corpus

The Stellar Mass Tully-Fisher Relation to z = 1.2 from AEGIS (2006, methodology): “Recent local studies focus on stellar or baryonic masses (e.g., Bell & de Jong 2001; McGaugh 2005; Pizagno et al. 2005), which are easier to model than luminosity.”
THE BARYON CONTENT OF COSMIC STRUCTURES (2009, methodology): “We utilize the rotation velocities and mass estimates of McGaugh (2005), selecting only those galaxies with M∗ > Mg for Q = 1.”
THE BARYONIC TULLY–FISHER RELATION OF GAS-RICH GALAXIES AS A TEST OF ΛCDM AND MOND (2011, methodology): “My own experience with modeling adiabatic contraction (Sellwood & McGaugh 2005) leads me to expect this to be a modest effect, most likely in 12 13 the range 1 ≤ fV ≤ 1.3.”
The structure of the interstellar medium of star‐forming galaxies (2011, background): “The SMC-like runs show a similar moderate dispersion ∼6– 8 km s−1, giving V/σ ∼ 5–15, and maintain very high gas fractions ∼70–80 per cent; these properties all agree very well with typical properties for ∼109 M dwarf galaxies (see e.g. Bell & de Jong 2001; McGaugh 2005).”
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, methodology): “It appears to hold quite generally [272], even for galaxies that we would conventionally expect to deviate from it [165, 279, 276].”
Scaling Relations of Spiral Galaxies (2007, methodology): “The slope, scatter, and zero-point of blue V L relations are predominantly dominated by stellar population and dust extinction effects (e.g. Aaronson & Mould 1983; G97; Willick et al. 1997; Tully & Pierce 2000; P07) and on the techniques used to recover the major observables and fitting for fundamen”
Scaling relations and the fundamental line of the local group dwarf galaxies (2008, methodology): “The first option recognises the uncertainties of both methods of calculating c© 2006 RAS, MNRAS 000, 1–18 M∗/L (namely, the uncertainties in the SFH, and the uncertainties in extrapolating BdJ’s colour-M∗/L correlation down to dwarf galaxies), while the second method uses the full available data to ”
ELVIS: Exploring the Local Volume in Simulations (2013, background): “In reality, the gas-to-stellar-mass relation shows a considerable amount of scatter (Kannappan 2004; McGaugh 2005; Stewart et al. 2009; Huang et al. 2012b,a; Kannappan et al. 2013), and this is especially true for the faintest systems in the LG (as summarized in McConnachie 2012).”
Molecular Hydrogen and Global Star Formation Relations in Galaxies (2007, methodology): “These numbers are similar to those compiled by McGaugh (2005) for DDO 154 and, combined with the dark matter virial velocityV200 = 50km s−1 and concentrationc = 6, produce a rotational velocity of vcirc ≈ 50km s−1 (wherevcirc is defined as the maximum of rotation velocity profile) similar to the…”
The Origin and Evolution of the Mass-Metallicity Relationship for Galaxies: Results from Cosmological N-Body Simulations (2006, methodology): “As discussed in G07, at disk galaxies in our simulations fall on the Tully-Fisherz p 0 (TF) and baryonic TF relations (Giovanelli et al. 1997; McGaugh 2005) and the age-mass relation (MacArthur et al. 2004).”
DISSIPATION AND EXTRA LIGHT IN GALACTIC NUCLEI. IV. EVOLUTION IN THE SCALING RELATIONS OF SPHEROIDS (2008, background): “At z = 0, there is no significant uncertainty; various measurements (e.g. Kennicutt 1998; Bell & de Jong 2000; Kannappan 2004; McGaugh et al. 2000; McGaugh 2005) and indirect constraints from star formation and the baryonic Tully-Fisher relation (Bell et al. 2003a; Noeske et al. 2007; Calura et al.…”
A Universal Stellar Initial Mass Function? A critical look at variations in extreme environments (2010, background): “Assuming that all of the scatter is due to IMF variations (i.e. assuming zero measurement error or variations in the star-formation history of the galaxies) implies a scatter in the stellar mass associated with a given luminosity less than a factor of two (see also McGaugh 2005).”
Fitting the radial acceleration relation to individual SPARC galaxies (2018, background): “The factor X → 1 as R → ∞, but on average, 〈X〉 = 0.8 (McGaugh 2005) at the finite radii observed in spiral galaxies.”
How Stellar Feedback Simultaneously Regulates Star Formation and Drives Outflows (2015, methodology): “…was obtained by fitting a theoretically motivated functional form (Kereš et al. 2005, 2009) to a compilation of observations (Bell & de Jong 2000; McGaugh 2005; Shapley et al. 2005; Erb et al. 2006b; Erb 2008; Calura et al. 2008; Puech et al. 2008; Cresci et al. 2009; Förster Schreiber et al.…”
THE M31 VELOCITY VECTOR. II. RADIAL ORBIT TOWARD THE MILKY WAY AND IMPLIED LOCAL GROUP MASS (2012, methodology): “This can be compared to the baryonic mass ratio implied by the Tully–Fisher relation, (VM33/VM31)4 (McGaugh 2005).”