The SBF Survey of Galaxy Distances. IV. SBF Magnitudes, Colors, and Distances

By J. Tonry, A. Dressler, J. Blakeslee, E. Ajhar, A. Fletcher, G. Luppino, M. Metzger, C. B. Moore. 2000

1,029 citations recorded by the source corpus.

We report data for I-band surface brightness fluctuation (SBF) magnitudes, (V-I) colors, and distance moduli for 300 galaxies. The survey contains E, S0, and early-type spiral galaxies in the proportions of 49 : 42 : 9 and is essentially complete for E galaxies to Hubble velocities of 2000 km s-1, with a substantial sampling of E galaxies out to 4000 km s-1. The median error in distance modulus is 0.22 mag. We also present two new results from the survey. (1) We compare the mean peculiar flow velocity (bulk flow) implied by our distances with predictions of typical cold dark matter transfer functions as a function of scale, and we find very good agreement with cold, dark matter cosmologies if the transfer function scale parameter Γ and the power spectrum normalization σ8 are related by σ8Γ-0.5 ≈ 2 ± 0.5. Derived directly from velocities, this result is independent of the distribution of galaxies or models for biasing. This modest bulk flow contradicts reports of large-scale, large-amplitude flows in the ~200 Mpc diameter volume surrounding our survey volume. (2) We present a distance-independent measure of absolute galaxy luminosity, and show how it correlates with galaxy properties such as color and velocity dispersion, demonstrating its utility for measuring galaxy distances through large and unknown extinction.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/3572c7eec785eb7941b6054cadf654b2eba39627

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Citations in the corpus

Observed and Physical Properties of Core-Collapse Supernovae (2002, background): “For five objects it is possible to assign the SN host galaxy to a galaxy group with surface brightness fluctuation (SBF) distances (Tonry et al. 2001) in the F00 Cepheid scale (adopting an uncertainty of 1 Mpc to account for cluster depth).”
HST STIS Spectroscopy of the Triple Nucleus of M31: Two Nested Disks in Keplerian Rotation around a Supermassive Black Hole (2005, background): “Considering, in addition to M31, only the two closest other supermassive BHs, i.e., M32 and the Galaxy, we get the following: M32 has bulge 75 km s 1, a predicted M ¼ 2:6 ; 106 M , and an observed M ¼ (2:9 0:6) ; 106 M (Verolme et al. 2002; corrected to distance 0.81 Mpc from Tonry et al. 2001).”
On the X-ray, optical emission line and black hole mass properties of local Seyfert galaxies ! (2006, neutral): “…in HFS97; Col. (3): Hubble type; Col. (4) total apparent B magnitude of the galaxy; Col. (5): galaxy distances; Col. (6): references on distances: (a) Tonry et al. (2001); (b) Tully (1988); (c) Paturel et al. (2002); (d) Cecil et al. (2002); (e) Stetson et al. (2001); (f) Merritt & Ferrarese…”
X-Ray Luminosity Function and Total Luminosity of Low-Mass X-Ray Binaries in Early-Type Galaxies (2003, background): “We take the distance from the surface brightness fluctuation results by Tonry et al. (2001).”
The Tully-Fisher relations of early-type spiral and S0 galaxies (2010, methodology): “As described in WBC09, we use surface brightness fluctuation (SBF) estimates where available (NGC 1381 from Jensen et al. 2003 and NGC 1596 from Tonry et al. 2001) and the Virgo cluster distance where appropriate (NGC 4469 and c© 2010 RAS, MNRAS 000, 1–17”
THE ACS FORNAX CLUSTER SURVEY. V. MEASUREMENT AND RECALIBRATION OF SURFACE BRIGHTNESS FLUCTUATIONS AND A PRECISE VALUE OF THE FORNAX–VIRGO RELATIVE DISTANCE (2009, methodology): “The ensuing ground-based SBF Survey of Galaxy Distances (Tonry et al. 1997, 2001) determined distances to some 300 early-type galaxies and spiral bulges.”
The SAURON project - IV. The mass-to-light ratio, the virial mass estimator and the Fundamental Plane of elliptical and lenticular galaxies (2005, methodology): “TheM/L measurements are inversely proportional to the assumed distance, which is taken from Tonry et al. (2001) and was adjusted to the new Cepheids zeropoint of Freedman etal.”
The SAURON project – IX. A kinematic classification for early‐type galaxies (2007, methodology): “Bothhave very similar total luminosity,V − I colour (Tonry et al. 2001) and gas content (Paper V).”
Cosmic Dawn (CoDa): the first radiation-hydrodynamics simulation of reionization and galaxy formation in the Local Universe (2015, methodology): “In essence, the method takes as its input, galaxy observations of the local universe today: galaxy catalogs with distances and peculiar velocities, galaxy group catalogs, such as the MARKIII (Willick et al. 1997), SBF (Tonry et al. 2001) and the Karachentsev catalog (Karachentsev et al. 2004).”
The ACS Virgo Cluster Survey. I. Introduction to the Survey (2004, methodology): “Similar conclusions were later reached by Lauer et al. (1995) using V-band HST images for 45 early-type galaxies with distances in the range 3– 280 Mpc.”
The very local Hubble flow (2002, background): “Tonry et al. (2001) determined its distance as 3.26±0.15 Mpc based on fluctuations of its surface brightness.”
The search for failed supernovae with the Large Binocular Telescope: first candidates (2014, neutral): “…et al. 2000; (10) Theureau et al. 2007; (11) Kanbur et al. 2003; (12) Dopita et al. 2010; (13) Herrnstein et al. 1999; (14) Thim et al. 2004; (15) Annibali et al. 2008; (16) Karachentsev et al. 2006; (17) Tonry et al. 2001; (18) Poznanski et al. 2009; (19) Karachentsev et al. 2000.”
The Coincidence of Nuclear Star Clusters and Active Galactic Nuclei (2008, methodology): “For the Virgo cluster galaxies, a distance of 16.5 Mpc was assumed (Tonry et al. 2001; Mei et al. 2007).”
High-Frequency VLBI Imaging of the Jet Base of M87 (2007, methodology): “Throughout this paper, a BH mass of 3 ;109 M at a distance of 16 Mpc (Whitmore et al. 1995; Tonry et al. 2001) is adopted for M87.”
How Large Are the Bars in Barred Galaxies (2005, methodology): “…group as one of Martin’s galaxies: NGC 4236 is in the same group as NGC 2403 (M81), which has an HST Cepheid distance, while NGC 5236 is in the same group as NGC 5253 (D = 4.2 Mpc from Cepheids; Saha et al. 1995) and NGC 5128 (D = 4.2 Mpc from surfacebrightness fluctuations; Tonry et al. 2001).”
Globular Cluster Systems in Brightest Cluster Galaxies: Bimodal Metallicity Distributions and the Nature of the High-Luminosity Clusters (2005, methodology): “…and 3268 are a rare example of a co-dominant central pair), (3) the redshift cz of the galaxy, corrected where possible to the CMB reference frame (Tonry et al. 2001), (4) the galaxy luminosity MTV as listed in the NASA Extragalactic Database (NED), (5) the foreground reddening, from Schlegel et…”
The ACS Virgo Cluster Survey. VII. Resolving the Connection between Globular Clusters and Ultracompact Dwarf Galaxies (2005, background): “The arrow in each panel indicates the fitted half-light radius, demonstrating the large spatial extent of these objects: hrhi ¼ 0B3, or ’24 pc for our adopted M87 distance of 16.1 Mpc (Tonry et al. 2001).”