The Tully-Fisher Relation and its Residuals for a Broadly Selected Sample of Galaxies

By J. Pizagno, F. Prada, D. Weinberg, Hans-Walter Rix, R. Pogge, E. Grebel, D. Harbeck, M. Blanton, J. Brinkmann, J. A. P. A. S. University and 7 more. 2006

149 citations recorded by the source corpus.

We measure the relation between galaxy luminosity and disk circular velocity (the Tully-Fisher [TF] relation), in the g, r, i, and z bands, for a broadly selected sample of galaxies from the Sloan Digital Sky Survey, with the goal of providing well-defined observational constraints for theoretical models of galaxy formation. The input sample of 234 galaxies has a roughly flat distribution of absolute magnitudes in the range -18.5 > Mr > -22, and our only morphological selection is an isophotal axis ratio cut b/a < 0.6 to allow accurate inclination corrections. Long-slit spectroscopy from the Calar Alto and MDM observatories yields usable Hα rotation curves for 162 galaxies (69%), with a representative color and morphology distribution. We define circular velocities V80 by evaluating the rotation curve at the radius containing 80% of the i-band light. Observational errors, including estimated distance errors due to peculiar velocities, are small compared to the intrinsic scatter of the TF relation. The slope of the forward TF relation steepens from -5.5 ± 0.2 mag (log10 km s-1)-1 in the g band to -6.6 ± 0.2 mag (log10 km s-1)-1 in the z band. The intrinsic scatter is σ ≈ 0.4 mag in all bands, and residuals from either the forward or inverse relations have an approximately Gaussian distribution. We discuss how Malmquist-type biases may affect the observed slope, intercept, and scatter. The scatter is not dominated by rare outliers or by any particular class of galaxies, although it drops slightly, to σ ≈ 0.36 mag, if we restrict the sample to nearly bulgeless systems. Correlations of TF residuals with other galaxy properties are weak: bluer galaxies are significantly brighter than average in the g-band TF relation but only marginally brighter in the i band; more concentrated (earlier type) galaxies are slightly fainter than average, and the TF residual is virtually independent of half-light radius, contrary to the trend expected for gravitationally dominant disks. The observed residual correlations do not account for most of the intrinsic scatter, implying that this scatter is instead driven largely by variations in the ratio of dark to luminous matter within the disk galaxy population.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/9c09ae6eeb54fe88ffb122d2bd73898b4993eff6

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Citations in the corpus

The formation of disc galaxies in a ΛCDM universe (2010, methodology): “These are compared to the observed TF relation from the SDSS (Pizagno et al. 2007).”
Constraints on star formation driven galaxy winds from the mass–metallicity relation at z= 0 (2010, background): “…therein), we have verified that equation (17) yields a Tully-Fisher relation (Tully & Fisher 1977) consistent with the more recent calibrations by Pizagno et al. (2007), as long as the dynamical contribution of the dark matter within a few optical radii is less than the onepredicted by a pure…”
THE SMALL SCATTER OF THE BARYONIC TULLY–FISHER RELATION (2015, methodology): “Studies based on Hα (Pizagno et al. 2007) or CO (Ho 2007) observations may present similar issues, since Hα and CO discs are typically less extended than H I discs and their maximum velocities may not be tracing Vf .”
Dark halo response and the stellar initial mass function in early-type and late-type galaxies (2010, methodology): “A fit to the Verheijen (2001) and Pizagno et al. (2007) galaxies (solid blue line in Fig.”
THE EPOCH OF DISK SETTLING: z ∼ 1 TO NOW (2012, background): “…tried to minimize scatter by selecting galaxies which are morphologically well-ordered disks (e.g., Verheijen 1997, Kassin, de Jong, & Weiner 2006, Pizagno et al. 2007 and references therein for low redshift, and e.g., Conselice et al. 2005, Miller et al. 2011 and references therein for z .”
Hierarchical formation of bulgeless galaxies – II. Redistribution of angular momentum via galactic fountains (2011, methodology): “We plot the observed Tully-Fisher relation using data from Pizagno et al. (2007) who plot the SDSS i-band magnitudes against V80, the rotation velocity at the radius which encompass 80% of the i-band flux (open squares).”
The properties of the star-forming interstellar medium at z = 0.84-2.23 from HiZELS : mapping the internal dynamics and metallicity gradients in high-redshift disc galaxies. (2012, methodology): “The z = 0 stellar-mass Tully–Fisher relation is well established (Bell & de Jong 2001; Pizagno et al. 2007; Meyer et al. 2008), and in Fig.”
Galacticus: A Semi-Analytic Model of Galaxy Formation (2010, result): “Figure 12 shows the SDSS color-magnitude diagram (colored shading) derived by Weinmann et al. (2006) which clearly shows these two populations.”
Integral field spectroscopy with SINFONI of VVDS galaxies I. Galaxy dynamics and mass assembly at 1.2 < z < 1.6 (2009, methodology): “Puech et al. (2008) used a subsample of SDSS sample (Pizagno et al. 2007) to derive a local reference TFR.”
NEW CONSTRAINTS ON THE EVOLUTION OF THE STELLAR-TO-DARK MATTER CONNECTION: A COMBINED ANALYSIS OF GALAXY–GALAXY LENSING, CLUSTERING, AND STELLAR MASS FUNCTIONS FROM z = 0.2 to z = 1 (2011, methodology): “…data in combination with a compilation of prior work on the SHMR to place constraints on Vopt/V200 for late-type galaxies (the requirement that the Pizagno et al. 2007 galaxies have sufficiently extended Hα emission to yield a useful rotation curve implies that this is primarily a late-type…”
The kinematic connection between galaxies and dark matter haloes (2010, background): “However, a large scatter in Vopt/V200 may be difficult to reconcile with the small scatter (≃ 0.05 dex in velocity) in the observed (Vopt − Mstar) TF relation (Courteau et al. 2007; Pizagno et al. 2007).”
ON THE INTERPLAY BETWEEN STAR FORMATION AND FEEDBACK IN GALAXY FORMATION SIMULATIONS (2014, methodology): “…of preferentially low angular momentum gas via stellar feedback can remedy this problem (e.g. Governato et al. 2007; Agertz et al. 2011; Brook et al. 2012; Übler et al. 2014), hence bringing simulated galaxies closer to the observed Tully-Fisher relation (Tully & Fisher 1977; Pizagno et al. 2007).”
The Tully-Fisher relations of early-type spiral and S0 galaxies (2010, methodology): “These scatters are broadly consistent with dedicated studies of the spiral TFR scatter (e.g. Pizagno et al. 2007), which is perhaps somewhat surprising given the expected poor quality of our distance estimates and the importance and uncertainty of internal extinction in edge-on spirals.”
The Aquila comparison project: the effects of feedback and numerical methods on simulations of galaxy formation (2011, methodology): “7, where we compare data compiled by Dutton et al. (2011) from Pizagno et al. (2007), Verheijen (2001) and Courteau et al. (2007) with the 13 simulated galaxies.”
A DIRECT MEASUREMENT OF THE BARYONIC MASS FUNCTION OF GALAXIES AND IMPLICATIONS FOR THE GALACTIC BARYON FRACTION (2012, background): “The triangles correspond to disc galaxies for which Mh was determined from their rotation speed (Geha et al. 2006; Pizagno et al. 2007; Springob et al. 2007).”
Scaling Relations of Spiral Galaxies (2007, background): “…L relation has been examined at nearly all optical-IR wavelengths (e.g. Strauss & Willick 1995; Verheijen 2001, hereafter V01; Masters et al. 2006; Pizagno et al. 2007, hereafter P07), comparatively few analyses of the RL relation of spiral galaxies have been reported so far (Salpeter & Hoffman…”
Physical properties and environments of nearby galaxies (2009, background): “The higher scatter value from Pizagno et al. (2007) occurs because they use a wider range of morphological types, in particular including “peculiar” systems and barred galaxies.”
GALAXIES IN ΛCDM WITH HALO ABUNDANCE MATCHING: LUMINOSITY–VELOCITY RELATION, BARYONIC MASS–VELOCITY RELATION, VELOCITY FUNCTION, AND CLUSTERING (2010, methodology): “In order to convert the I-band luminosities measured by Springob et al. (2007) to the r band, we cross-referenced their data with the sample of Pizagno et al. (2007) and used the median (r − I ) colors of the galaxies present in both catalogs.”