SFI++ I: A New I-Band Tully-Fisher Template, the Cluster Peculiar Velocity Dispersion, and H0

By Karen L. Masters, C. Springob, M. Haynes, R. Giovanelli. 2006

132 citations recorded by the source corpus.

The SFI++ consists of ~5000 spiral galaxies that have measurements suitable for the application of the I-band Tully-Fisher (TF) relation. This sample builds on the SCI and SFI samples published in the 1990s but includes significant amounts of new data, as well as improved methods for parameter determination. We derive a new I-band TF relation from a subset of this sample, which consists of 807 galaxies in the fields of 31 nearby clusters and groups. This sample constitutes the largest ever available for the calibration of the TF template and extends the range of line widths over which the template is reliably measured. Careful accounting is made of observational and sample biases such as incompleteness, finite cluster size, galaxy morphology, and environment. We find evidence for a type-dependent TF slope that is shallower for early-type than for late-type spirals. The line-of-sight cluster peculiar velocity dispersion is measured for the sample of 31 clusters. This value is directly related to the spectrum of initial density fluctuations and thus provides an independent verification of the best-fit WMAP cosmology and an estimate of Ω0.6σ8 = 0.52 ± 0.06. We also provide an independent measure of the TF zero point using 17 galaxies in the SFI++ sample for which Cepheid distances are available. In combination with the "basket-of-clusters" template relation these calibrator galaxies provide a measure of H0 = 74 ± 2 (random) ±6 (systematic) km s-1 Mpc-1.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/8febc0294e9b1d313a0b93485b3f940c03c92f37

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Citations in the corpus

Cosmological parameters from the comparison of peculiar velocities with predictions from the 2M++ density field (2014, methodology): “…on Spiral Cluster I-band (SCI) and Spiral Field I-band (SFI) samples and uses a mixture of 21-cm line profile widths and optical rotation curves in determining the I-band Tully-Fisher (TF) relation from a subset of 807 galaxies in the fields of 31 clusters and groups Masters et al. (2006).”
SFI++. II. A New I-Band Tully-Fisher Catalog, Derivation of Peculiar Velocities, and Data Set Properties (2007, methodology): “The actual calculation of morphological corrections for the construction of the template in Masters et al. (2006) was done correctly, but the processing of parameters into data tables done for this paper included an error in this correction.”
THE 2MASS REDSHIFT SURVEY—DESCRIPTION AND DATA RELEASE (2011, background): “25 to the SFI++ peculiar velocity survey (Masters et al. 2006; Springob et al. 2007a) to place constraints on the bias between galaxies and dark matter halos, as well as β = f(Ω)/b (where f is the rate of growth of structure and b is the bias factor) and σ8 (which measures the amplitude of the…”
The Hubble Constant from Infrared Surface Brightness Fluctuation Distances (2021, background): “Estimates of this small-scale peculiar velocity “noise” σp range from 100 to 300 km s−1, depending on the sample considered (Masters et al. 2006; Hoffman et al. 2015; Graziani et al. 2019).”
COSMICFLOWS-2: THE DATA (2013, methodology): “As an aside, we note that an absolute zero point for the TFR distances by the Cornell group was given by Masters et al. (2006) based on the HST key project scale but with a reduced sample of Cepheid PLR calibrators.”
THE LOW-LUMINOSITY END OF THE RADIUS–LUMINOSITY RELATIONSHIP FOR ACTIVE GALACTIC NUCLEI (2013, background): “…NGC 3783 would generally be expected to have peculiar velocities affecting its perceived recessional velocity at only the ∼10% level (∼300 km s−1, e.g., Masters et al. 2006; Bahcall & Oh 1996), a severe underesti mate given the 50% discrepancy between the group-averaged distance estimate and the…”
Local gravity versus local velocity: solutions for β and non-linear bias (2010, methodology): “We use the published SFI++ magnitudes and velocity widths, and derive our own peculiar velocities, rather than taking the published distances as given.”
The Mass Function of Active Black Holes in the Local Universe (2007, methodology): “In particular, weuse the best-fit Tully-Fisher relation from Masters et al. (2006) for their “in+” sample, and we neglect variations in the relation with Hubble type.”
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”
REVERBERATION MEASUREMENTS OF THE INNER RADIUS OF THE DUST TORUS IN 17 SEYFERT GALAXIES (2014, background): “Since the values presented for the peculiar velocity dispersion, σ2pec, differ slightly (e.g., Watkins 1997; Gibbons et al. 2001; Radburn-Smith et al. 2004; Masters et al. 2006), we assumed σpec = 200 km s −1 and 300 km s−1 to estimate the uncertainty of MV caused by peculiar velocity.”
Cosmic flows on 100 h−1 Mpc scales: standardized minimum variance bulk flow, shear and octupole moments (2009, background): “This compilation, which we label “COMPOSITE”, consists of a number of surveys, the largest of which is the SFI++ peculiar velocity survey of spirals in the field and in groups (Masters et al. 2006; Springob et al. 2007; Springob et al. 2009).”
The Megamaser Cosmology Project. XIII. Combined Hubble Constant Constraints (2020, background): “Typical values for galaxy peculiar velocities lie in the range ∼150–250 km s−1 (e.g., Davis et al. 1997; Zaroubi et al. 2001; Masters et al. 2006; Hoffman et al. 2015), so we conservatively take the upper end of this range and add σpec = 250 km s −1 in quadrature to our velocity uncertainties.”
The Tully-Fisher Relation and its Residuals for a Broadly Selected Sample of Galaxies (2006, background): “Since large samples of galaxies ( 2000) have been observed for TF studies in the past (see, e.g., Courteau et al. 2003; Masters et al. 2006 and references therein), it may be possible to construct such a sample largely from archival data, if the data quality can be made sufficiently homogeneous and…”
Physical properties and environments of nearby galaxies (2009, background): “Recent compilations (Verheijen 2001; Kannappan, Fabricant & Franx 2002; Masters et al. 2006; Pizagno et al. 2007; Courteau et al. 2007) find α ∼ 0.27–0.35, with a scatter equivalent to about 0.15–0.4 mag in the luminosity direction.”
OVERVIEW OF THE SDSS-IV MaNGA SURVEY: MAPPING NEARBY GALAXIES AT APACHE POINT OBSERVATORY (2014, methodology): “In addition to obtaining definitive measures of scaling relations like Tully–Fisher (e.g., Masters et al. 2006; Reyes et al. 2011), MaNGA’s unique strength in providing multiple kinematic tracers across a long, uniformly calibrated wavelength range raises a potentially transformative but more…”