THE SLOAN LENS ACS SURVEY. X. STELLAR, DYNAMICAL, AND TOTAL MASS CORRELATIONS OF MASSIVE EARLY-TYPE GALAXIES

By M. Auger, T. Treu, A. Bolton, R. Gavazzi, Leon V. E. Koopmans, P. J. Marshall, L. A. Moustakas, S. Burles. 2010

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We use stellar masses, surface photometry, strong-lensing masses, and stellar velocity dispersions (σe/2) to investigate empirical correlations for the definitive sample of 73 early-type galaxies (ETGs) that are strong gravitational lenses from the SLACS survey. The traditional correlations (fundamental plane (FP) and its projections) are consistent with those found for non-lens galaxies, supporting the thesis that SLACS lens galaxies are representative of massive ETGs (dimensional mass Mdim = 1011–1012 M☉). The addition of high-precision strong-lensing estimates of the total mass allows us to gain further insights into their internal structure: (1) the average slope of the total mass-density profile ( ) is 〈γ′〉 = 2.078 ± 0.027 with an intrinsic scatter of 0.16 ± 0.02; (2) γ′ correlates with effective radius (re) and central mass density, in the sense that denser galaxies have steeper profiles; (3) the dark matter (DM) fraction within re/2 is a monotonically increasing function of galaxy mass and size (due to a mass-dependent central cold DM distribution or due to baryonic DM—stellar remnants or low-mass stars—if the initial mass function is non-universal and its normalization increases with mass); (4) the dimensional mass Mdim ≡ 5reσ2e/2/G is proportional to the total (lensing) mass M , and both increase more rapidly than stellar mass M* (M ); (5) the mass plane (MP), obtained by replacing surface brightness with surface mass density in the FP, is found to be tighter and closer to the virial relation than the FP and the M*P, indicating that the scatter of those relations is dominated by stellar population effects; (6) we construct the fundamental hyper-plane by adding stellar masses to the MP and find the M* coefficient to be consistent with zero and no residual intrinsic scatter. Our results demonstrate that the dynamical structure of ETGs is not scale invariant and that it is fully specified by M , re, and σe/2. Although the basic trends can be explained qualitatively in terms of varying star formation efficiency as a function of halo mass and as the result of dry and wet mergers, reproducing quantitatively the observed correlations and their tightness may be a significant challenge for galaxy formation models.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/4c752b5b531932d066d3bcb3c6134a3678e056d0

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In Astronomy and Astrophysics

1. M. Cappellari
2. C. Conroy
3. P. Hopkins
4. L. Hernquist
5. P. V. van Dokkum
6. T. Naab
7. T. Treu
8. A. Dekel

In Instrumentation

1. M. Cappellari
2. C. Conroy
3. P. V. van Dokkum
4. T. Treu
5. T. Naab
6. L. Hernquist
7. P. Hopkins
8. M. Franx

Citations in the corpus

• Mass-sheet degeneracy, power-law models and external convergence: Impact on the determination of the Hubble constant from gravitational lensing (2013, positive): “In general, the velocity dispersion measurement in individual systems is derived with typically 10% uncertainty, which translates into an uncertainty of the same order on the logarithmic slope of the profile (e.g. Koopmans 2004; Auger et al. 2010; Agnello et al. 2013).”
• Dark halo response and the stellar initial mass function in early-type and late-type galaxies (2010, methodology): “The trend of increasing dark matter fractions in higher mass (or luminosity) early-type galaxies, for a universal IMF, is well established (e.g., Padmanabhan et al. 2004; Gallazzi et al. 2006; Tortora et al. 2009; Auger et al. 2010b, Napolitano et al. 2010).”
• The stellar IMF in early-type galaxies from a non-degenerate set of optical line indices (2013, background): “E-mail: spiniello@astro.rug.nl ter (DM) fraction in the internal region of these systems increases with the mass of the galaxy (e.g. Zaritsky et al. 2006; Auger et al. 2010; Treu et al. 2010; Barnabè et al. 2011).”
• Galaxy Masses: A Review (2013, methodology): “Regarding the total mass density profile, Koopmans et al. (2009) and Auger et al. (2010b) found that inside one effective radius massive elliptical galaxies with Meff ≥ 3 · 1010 M are well-approximated by a power-law ellipsoid with an average logarithmic density slope of 〈γ′LD〉 ≡ −d log(ρtot)/d…”
• THE POPULATION OF GALAXY–GALAXY STRONG LENSES IN FORTHCOMING OPTICAL IMAGING SURVEYS (2015, methodology): “The sample has been used to constrain the masses and density profiles of galaxies (Auger et al. 2010; Barnabè et al. 2011), the dark sub-halo population (Vegetti et al. 2014), cosmological parameters (Collett & Auger 2014; Oguri et al. 2012; Suyu et al. 2014), the high redshift luminosity function…”
• Two-dimensional kinematics of SLACS lenses – III. Mass structure and dynamics of early-type lens galaxies beyond z ≃ 0.1 (2011, methodology): “…by previous analyses of the SLACS systems (Koopmans et al. 2006; Gavazzi et al. 2007; Czoske et al. 2008; Barnabè et al. 2009a; Koopmans et al. 2009; Auger et al. 2010a), as well as a number of stellar dynamics (e.g. Gerhard et al. 2001), gravitational lensing (e.g. Dye et al.2008; Tu et al.…”
• THE DENSITY PROFILES OF MASSIVE, RELAXED GALAXY CLUSTERS. II. SEPARATING LUMINOUS AND DARK MATTER IN CLUSTER CORES (2012, methodology): “Auger et al. (2010b) probe the SLACS samples of earlytype lenses using strong and weak lensing and stellar kinematics (see also Gavazzi et al. 2007; Treu et al. 2010).”
• TWO ACCURATE TIME-DELAY DISTANCES FROM STRONG LENSING: IMPLICATIONS FOR COSMOLOGY (2012, background): “Various studies have shown that the power-law profile provides accurate descriptions of lens galaxies (e.g., Gavazzi et al. 2007; Humphrey & Buote 2010; Koopmans et al. 2009; Auger et al. 2010; Barnabè et al. 2011).”
• H0LiCOW - IV. Lens mass model of HE 0435-1223 and blind measurement of its time-delay distance for cosmology (2016, methodology): “With reasonable assumptions about the lens galaxy’s mass profile, these degeneracies can be reduced by augmenting the lensing data with stellar kinematics measurements of the lens galaxy (e.g., Treu & Koopmans 2002; Koopmans et al. 2003; Auger et al. 2010; Suyu et al. 2014).”
• Galaxy clustering in the CFHTLS-Wide: the changing relationship between galaxies and haloes since z ~ 1.2 (2011, methodology): “Several methodologies exist to estimate halo masses: for example, using satellite kinematics (More et al. 2011), X-ray temperatures (Peterson & Fabian 2006; Cattaneo et al. 2009), or gravitational lensing (Heymans et al. 2006; Mandelbaum et al. 2006; Auger et al. 2010; Leauthaud et al. 2012b).”
• The ATLAS3D project XV: benchmark for early-type galaxies scaling relations from 260 dynamical models: mass-to-light ratio, dark matter, fundamental plane and mass plane (2012, methodology): “A similar study was performed by Bolton et al. (2007, 2008), and updated by Auger et al. (2010b), using masses derived from strong lensing analysis.”
• H0LiCOW – I. H0 Lenses in COSMOGRAIL's wellspring: program overview (2016, methodology): “…lens modeling techniques (Suyu et al. 2009; Suyu & Halkola 2010; Suyu et al. 2012b, Suyu et al. in preparation) and kinematic modeling methods (Auger et al. 2010; Sonnenfeld et al. 2012) to obtain the lens mass distribution with a few percent uncertainty (e.g., Suyu et al. 2013, 2014).”
• Inference of the cold dark matter substructure mass function at z = 0.2 using strong gravitational lenses (2014, methodology): “A measure of the slope of the mass density profile γ was also derived by Koopmans et al. (2009) and Auger et al. (2010), using a combination of lensing and the stellar velocity dispersion for each galaxy.”
• TDCOSMO. I. An exploration of systematic uncertainties in the inference of $H_0$ from time-delay cosmography (2019, background): “About 90% of galaxy-scale lenses are early-type galaxies (Auger et al. 2009), which satisfy very tight correlations between their observable properties (Auger et al. 2010).”