Scaling Relations of Spiral Galaxies

By S. Courteau, A. Dutton, Frank C. van den Bosch, L. MacArthur, A. Dekel, D. H. Mcintosh, D. Dale. 2007

187 citations recorded by the source corpus.

We construct a large data set of global structural parameters for 1300 field and cluster spiral galaxies and explore the joint distribution of luminosity L, optical rotation velocity V, and disk size R at I and 2MASS K bands. The I- and K-band velocity-luminosity (VL) relations have log slopes of 0.29 and 0.27, respectively, with σln(VL) ~ 0.13, and show a small dependence on color and morphological type in the sense that redder, earlier type disk galaxies rotate faster than bluer, later type disk galaxies for most luminosities. The VL relation at I and K bands is independent of surface brightness, size, and light concentration. The log slope of the I- and K-band size-luminosity (RL) relations is a strong function of morphology and varies from 0.25 to 0.5, with a mean of 0.32 for all Hubble types. At most luminosities, early-type disk galaxies have shorter scale lengths than later type ones. The average dispersion σln(RL) decreases from 0.33 at I band to 0.29 at K, likely due to the 2MASS selection bias against lower surface brightness galaxies. The VL and RL residuals are largely uncorrelated with each other with a correlation coefficient r = -0.16 and Δ log V|L/Δ log R|L = -0.07 ± 0.01; the RV - RL residuals show a weak positive correlation with r = 0.53. These correlations suggest that scatter in luminosity is not a significant source of the scatter in the VL and RL relations. We discuss in two Appendices various pitfalls of standard analytical derivations of galaxy scaling relations, including the Tully-Fisher relation with different slopes. Our galaxy database is available at http://www.astro.queensu.ca/~courteau/data/VRL2007.dat.

Subfields: Astronomy and Astrophysics, Ecology, Instrumentation

View Paper: https://www.semanticscholar.org/paper/15fa52ef9cf6d824bf37e12226ade0ac3813d00c

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 Ecology

In Instrumentation

Citations in the corpus

Dark halo response and the stellar initial mass function in early-type and late-type galaxies (2010, methodology): “However, the data set compiled by Courteau et al. (2007b) has a TF relation (as calculated by Dutton et al. 2007, dashed line in Fig.”
On the origin of the galaxy star‐formation‐rate sequence: evolution and scatter (2009, background): “There is a significant scatter ( 0.14–0.2 dex) in the sizes of galactic stellar disks at a given stellar mass or luminosity (e.g. Shen et al. 2003; Courteau et al. 2007), which corresponds to a scatter in disk surface density of 0.28–0.4 dex.”
A REVISED PARALLEL-SEQUENCE MORPHOLOGICAL CLASSIFICATION OF GALAXIES: STRUCTURE AND FORMATION OF S0 AND SPHEROIDAL GALAXIES (2011, background): “…1979; Kent 1985; Byun & Freeman 1995; Scorza & Bender 1995; Baggett et al. 1998; GIM2D: Simard et al. 2002; GALFIT: Peng et al. 2002; BUDA: de Souza et al. 2004; Laurikainen et al. 2005, 2007; Courteau et al. 2007; GASP2D: Méndez-Abreu et al. 2008; Fisher & Drory 2008; Weinzirl et al. 2009).”
Physical properties and environments of nearby galaxies (2009, methodology): “They occupy a different place in the size-luminosity relation, one that overlaps considerably with the ellipticals (§5; see also Courteau et al. 2007).”
HOW DO DISKS SURVIVE MERGERS? (2008, background): “…further check that these are indeed real disks, Figure 5 plots the disks in disk-dominated simulation remnants on the baryonic Tully-Fisher and stellar size-mass relations observed for disks of similar morphology (see e.g. Bell & de Jong 2001; McGaugh 2005; Shen et al. 2003; Courteau et al. 2007).”
Physical Models of Galaxy Formation in a Cosmological Framework (2014, background): “1.1.4 Structural Scaling Relations Both disks and spheroids exhibit correlations between their stellar mass or luminosity, their radial size, and their internal velocity (Bernardi et al. 2010, Courteau et al. 2007, Faber & Jackson 1976, Kormendy 1977, Shen et al. 2003, Tully & Fisher 1977).”
The impact of baryonic physics on the structure of dark matter haloes: the view from the FIRE cosmological simulations (2015, methodology): “They derived the TFR using the data from Courteau et al. (2007) and with the best fit: c© 0000 RAS, MNRAS 000, 000–000 c© 0000 RAS, MNRAS 000, 000–000 log10 V2.”
THE BARYONIC TULLY–FISHER RELATION OF GAS-RICH GALAXIES AS A TEST OF ΛCDM AND MOND (2011, methodology): “This leads to Tully-Fisher relations with different slopes and scatter depending on the band-pass used to measure the luminosity (e.g., Tully et al. 1998; Verheijen 2001; Courteau et al. 2007; Noordermeer & Verheijen 2007; Masters et al. 2008).”
PROBING THE INTERGALACTIC MEDIUM/GALAXY CONNECTION. V. ON THE ORIGIN OF Lyα AND O vi ABSORPTION AT z < 0.2 (2011, background): “4c (Courteau et al. 2007), we would infer that rvir scales as rvir ∝ L 0.3.”
MaGICC discs: matching observed galaxy relationships over a wide stellar mass range (2012, methodology): “The values of scale-length (S) are used for the ‘size’ of the galaxy in this paper, to make consistent with the observational data with which comparison is made (Courteau et al. 2007).”
GALAXIES IN ΛCDM WITH HALO ABUNDANCE MATCHING: LUMINOSITY–VELOCITY RELATION, BARYONIC MASS–VELOCITY RELATION, VELOCITY FUNCTION, AND CLUSTERING (2010, background): “Consid ering the correlation between the central surface brightness and disk scale length found by Courteau et al. (2007), the most lu minous disks appear to have scale lengths as large as 15 kpc, whereas according to Courteau (1997) their rotation curves peak at about 1 scale length.”
The Tully-Fisher relations of early-type spiral and S0 galaxies (2010, background): “In the spirit of Courteau & Rix (1999) and Courteau et al. (2007), the possibility that the luminous component of the dynamical mass is smaller or more concentrated in S0s at a given velocity can be tested directly by measuring the size of our galaxies.”
FORMING REALISTIC LATE-TYPE SPIRALS IN A ΛCDM UNIVERSE: THE ERIS SIMULATION (2011, background): “Its value also agrees with the scaling relations of spiral galaxies (Courteau et al. 2007).”
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).”
MORPHOLOGIES OF ∼190,000 GALAXIES AT z = 0–10 REVEALED WITH HST LEGACY DATA. I. SIZE EVOLUTION (2015, result): “The α measurements of local spiral and/or disk galaxies are comparable to α ∼ 0.27 (Shen et al. 2003; Courteau et al. 2007; de Jong & Lacey 2000).”
Evolution of magnetic fields in galaxies and future observational tests with the Square Kilometre Array (2008, background): “Late-type disk galaxies of a disk scale length >∼10 kpc are rare as verified by analyses of I-band images (Courteau et al. 2007).”
THE EXTRAGALACTIC DISTANCE DATABASE (2009, background): “Then there are four catalogs identified with Courteau, distinguished by the four sources of data used in the study of Courteau et al. (2007).”
Inclination- and dust-corrected galaxy parameters: bulge-to-disc ratios and size–luminosity relations (2008, methodology): “We first compare our K-band results with Courteau et al. (2007) who presented K-band galaxy luminosity-size relations for 360 2MASS galaxies binned into different galaxy types.”