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

By M. Cappellari, Nicholas Scott, K. Alatalo, L. Blitz, M. Bois, Frédéric Bournaud, M. Bureau, A. Crocker, Roger Davies, T. Davis and 14 more. 2012

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We study the volume-limited and nearly mass-selected (stellar mass M-stars greater than or similar to 6 x 10(9) M circle dot) ATLAS(3D) sample of 260 early-type galaxies (ETGs, ellipticals Es and lenticulars S0s). We construct detailed axisymmetric dynamical models (Jeans Anisotropic MGE), which allow for orbital anisotropy, include a dark matter halo and reproduce in detail both the galaxy images and the high-quality integral-field stellar kinematics out to about 1R(e), the projected half-light radius. We derive accurate total mass-to-light ratios (M/L)(e) and dark matter fractions f(DM), within a sphere of radius centred on the galaxies. We also measure the stellar (M/L)(stars) and derive a median dark matter fraction f(DM) = 13 per cent in our sample. We infer masses M-JAM equivalent to L x (M/L)(e) approximate to 2 x M-1/2, where M-1/2 is the total mass within a sphere enclosing half of the galaxy light. We find that the thin two-dimensional subset spanned by galaxies in the (M-JAM, sigma(e), R-e(maj)) coordinates system, which we call the Mass Plane (MP) has an observed rms scatter of 19 per cent, which implies an intrinsic one of 11 per cent. Here, is the major axis of an isophote enclosing half of the observed galaxy light, while Sigma(e) is measured within that isophote. The MP satisfies the scalar virial relation M-JAM proportional to sigma R-2(e)e(maj) within our tight errors. This show that the larger scatter in the Fundamental Plane (FP) (L, Sigma(e), R-e) is due to stellar population effects [including trends in the stellar initial mass function (IMF)]. It confirms that the FP deviation from the virial exponents is due to a genuine (M/L)(e) variation. However, the details of how both R-e and Sigma(e) are determined are critical in defining the precise deviation from the virial exponents. The main uncertainty in masses or M/L estimates using the scalar virial relation is in the measurement of R-e. This problem is already relevant for nearby galaxies and may cause significant biases in virial mass and size determinations at high redshift. Dynamical models can eliminate these problems. We revisit the (M/L)(e)-Sigma(e) relation, which describes most of the deviations between the MP and the FP. The best-fitting relation is (M/L)(e) sigma(0.72)(e) (r band). It provides an upper limit to any systematic increase of the IMF mass normalization with Sigma(e). The correlation is more shallow and has smaller scatter for slow rotating systems or for galaxies in Virgo. For the latter, when using the best distance estimates, we observe a scatter in (M/L)(e) of 11 per cent, and infer an intrinsic one of 8 per cent. We perform an accurate empirical study of the link between Sigma(e) and the galaxies circular velocity V-circ within 1R(e) (where stars dominate) and find the relation max (V-circ) approximate to 1.76 x Sigma(e), which has an observed scatter of 7 per cent. The accurate parameters described in this paper are used in the companion Paper XX (Cappellari et al.) of this series to explore the variation of global galaxy properties, including the IMF, on the projections of the MP.

Subfields: Astronomy and Astrophysics, Instrumentation

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In Astronomy and Astrophysics

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

In Instrumentation

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

Citations in the corpus

• The AIMSS Project I: bridging the star cluster, galaxy divide (2014, methodology): “The quoted central (Re/8) velocity dispersions are from Cappellari et al. (2013a).”
• Improving the full spectrum fitting method: accurate convolution with Gauss-Hermite functions (2016, methodology): “Dynamical models based on IFS kinematics allow one to infer galaxy mass distributions to study scaling relations (e.g. Cappellari et al. 2013a; Scott et al. 2015), the stellar and dark matter content (e.g. Cappellari et al. 2012, 2015), or measure black hole masses (e.g. Krajnović et al. 2009;…”
• Mass-sheet degeneracy, power-law models and external convergence: Impact on the determination of the Hubble constant from gravitational lensing (2013, background): “In fact, from our understanding of the physical properties of galaxies, one would not expect the density profile in the central kiloparsecs region where the lensing effects occur to be a perfect power law (e.g. van de Ven et al. 2009; Cappellari et al. 2013, but see also Remus et al. 2013).”
• THE SMALL SCATTER OF THE BARYONIC TULLY–FISHER RELATION (2015, methodology): “(6) We use the LTS LINEFIT algorithm (Cappellari et al. 2013), which performs a least-square minimization considering errors in both variables and allowing for intrinsic scatter.”
• The fast molecular outflow in the Seyfert galaxy IC 5063 as seen by ALMA (2015, background): “Solid-body rotation is not expected in the central regions of a massive early-type galaxy such as IC 5063 (e.g. Cappellari et al. 2013, see also Fig.”
• One Law to Rule Them All: The Radial Acceleration Relation of Galaxies (2016, methodology): “2.2.1): one at small radii from JAM modelling of IFU data (Cappellari et al. 2013) and one at large radii from H I data (den Heijer et al. 2015).”
• Fitting the radial acceleration relation to individual SPARC galaxies (2018, methodology): “We used the LTS_LINEFIT program (Cappellari et al. 2013) to fit the linear relation log(Mb) = n log(Vf) + log(A).”
• Structure and Kinematics of Early-Type Galaxies from Integral Field Spectroscopy (2016, methodology): “The dynamical models of the IFS ATLAS3D data are taken from Cappellari et al. (2013b), while the combined lensing and dynamics models were based on the SLACS lens models of Treu et al. (2010), but were redone using axisymmetric JAM models for maximum consistency between the two sets of…”
• An Older, More Quiescent Universe from Panchromatic SED Fitting of the 3D-HST Survey (2018, methodology): “IR spectroscopy (van Dokkum & Conroy 2010; Conroy & van Dokkum 2012), dynamical modeling (Cappellari et al. 2013), and gravitational lens analysis (Treu et al. 2010) all independently suggest that ellipticals with higher velocity dispersions have increasingly “bottom-heavy” IMFs, though there…”
• The ATLAS3D project - XXIX. The new look of early-type galaxies and surrounding fields disclosed by extremely deep optical images (2014, background): “7 tabulated in Table 1, column 10 of Cappellari et al. (2013).”
• The ATLAS3D Project – XXX. Star formation histories and stellar population scaling relations of early-type galaxies (2015, methodology): “The mass MJAM is derived applying equation 3 of Cappellari et al. (2013b), using the (M/L)JAM and r-band luminosity given in table 1 of Cappellari et al. (2013a), columns 6 and 15, respectively.”
• Galaxy Masses: A Review (2013, methodology): “Cappellari et al. (2013b) find this dark matter fraction to be consistent with predictions for the same galaxies inferred by linking NFW halos to the real galaxies and assuming halo masses via the halo abundance matching technique (e.g. Behroozi et al. 2010).”
• Coevolution (Or Not) of Supermassive Black Holes and Host Galaxies (2013, methodology): “Figure 11 Comparison of our adopted σe (Tables 2 and 3) to (left) the central velocity dispersion as tabulated in HyperLeda and to (right) the σe value tabulated by the SAURON/ATLAS3D teams (Emsellem et al. 2007; Cappellari et al. 2013).”
• THE SINFONI BLACK HOLE SURVEY: THE BLACK HOLE FUNDAMENTAL PLANE REVISITED AND THE PATHS OF (CO)EVOLUTION OF SUPERMASSIVE BLACK HOLES AND BULGES (2016, methodology): “In principle, stellar-population M/L determinations could be uncertain, because they depend on the proper choice of the stellar initial mass function (Thomas et al. 2011; Cappellari et al. 2013) and internal dust corrections, see discussion in Rusli et al. (2013a).”
• The ATLAS3D Project – XXVIII. Dynamically driven star formation suppression in early-type galaxies (2014, methodology): “This average fraction appearsto decrease with increasing galaxy bulge fraction (Cappellari et al. 2013a, hereafter Paper XX; see also Saintonge et al. 2012).”