The Carnegie-Irvine Galaxy Survey. Iii. the Three-Component Structure of Nearby Elliptical Galaxies
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DRAFT VERSION 6 Preprint typeset using LATEX style emulateapj v. 26/01/00 THE CARNEGIE-IRVINE GALAXY SURVEY. III. THE THREE-COMPONENT STRUCTURE OF NEARBY ELLIPTICAL GALAXIES 1 2 3 2 4 5 6 SONG HUANG (黄崧) , , LUIS C. HO , CHIEN Y. PENG ,ZHAO-YU LI (李兆聿) , AND AARON J. BARTH Draft version 6 ABSTRACT Motivated by recent developments in our understanding of the formation and evolution of massive galaxies, we explore the detailed photometric structure of a representative sample of 94 bright, nearby elliptical galaxies, using high-quality optical images from the Carnegie-Irvine Galaxy Survey. The sample spans a range of environ- 10.2 12.0 ments and stellar masses, from M∗ = 10 to 10 M⊙. We exploit the unique capabilities of two-dimensional image decomposition to explore the possibility that local elliptical galaxies may contain photometrically distinct substructure that can shed light on their evolutionary history. Compared with the traditional one-dimensional ap- proach, these two-dimensional models are capable of consistently recovering the surface brightness distribution and the systematic radial variation of geometric informationat the same time. Contrary to conventionalperception, we find that the global light distribution of the majority (>75%) of elliptical galaxies is not well described by a single Sérsic function. Instead, we propose that local elliptical∼ galaxies generically contain three subcomponents: a compact (Re <1 kpc) inner component with luminosity fraction f 0.1 − 0.15; an intermediate-scale (Re 2.5 ≈ ≈ kpc) middle component∼ with f 0.2 − 0.25; and a dominant ( f =0.6), extended (Re 10 kpc) outer envelope. All subcomponents have average≈ Sérsic indices n 1 − 2, significantly lower than the≈ values typically obtained from single-component fits. The individual subcomponents≈ follow well-defined photometric scaling relations and the stellar mass-size relation. We discuss the physical nature of the substructures and their implications for the formation of massive elliptical galaxies. Subject headings: galaxies: elliptical and lenticular, cD — galaxies: formation — galaxies: photometry — galaxies: structure — galaxies: surveys 1. INTRODUCTION ness profile of elliptical galaxies was found to deviate system- The formation and evolution of massive elliptical galaxies, as atically from de Vaucouleurs’ profile (Kormendy 1977; King 1978; Lauer 1985). These observations showed that elliptical fundamentally important areas in astrophysics, are extensively galaxies have a variety of inner profiles that cannot be accom- studied using different observational constraints. Among them, the photometric analysis of their morphological structure re- modated by de Vaucouleurs’ law. Beginning in the late 1980s, it was realized that the more mains one of the most efficient and straightforward methods. flexible R1/n Sérsic (1968) profile does a much better job of Since different physical processes can result in different stellar configurations, the surface brightness distribution of a galaxy, describing the surface brightness profile of elliptical galaxies (Capaccioli 1989; Caon et al. 1993). Over a large radial range, as the first-order proxy of the underlying stellar mass distribu- nearby elliptical galaxies were found to be well fit by Sérsic tion, provides an important archaeological record of its evolu- tionary history. profiles with 2.5 < n < 10 (e.g., Caon et al. 1994; Bertin et al. 2002; Kormendy et al. 2009, hereinafter K09). Compared With their nearly featureless morphologies, elliptical galax- ∼ ∼ to other types of galaxies, ellipticals have significantly larger ies traditionally have been viewed as structurally simple ob- jects. Historically, the surface brightness profile of luminous Sérsic indices, reflecting their high degree of central concen- tration. As the detailed properties of the Sérsic function be- elliptical galaxies was described by an R1/4 law (de Vaucouleurs 1948, 1953). This simple profile reflects the high central con- came better understood, both theoretically (Ciotti 1991; Hjorth centration and large radial extension of the light distribution & Madsen 1995; Ciotti & Bertin 1999; Lima Neto et al. 1999) and observationally (Graham & Driver 2005), a variety of stud- of massive elliptical galaxies. As an empirical surface bright- ness model, de Vaucouleurs profile was embraced by different ies have explored empirical correlations between the Sérsic in- theories for elliptical galaxy formation. Both the dissipational dex and other key structural parameters (e.g., Caon et al. 1993; Trujillo et al. 2001; Graham et al. 2005). Modern numerical monolithic collapse model (e.g., Larson 1974) and the initially dissipationless disk merger model (e.g., van Albada 1982; Carl- simulations of galaxy formation that invoke either dissipational berg 1986) predicted that the density profile of the final prod- monolithic collapse (Nipoti et al. 2006) or dissipational merg- ing (Aceves et al. 2006; Naab & Trujillo 2006) can recover the uct should be very similar to the R1/4 law. With the advent of more accurate photometric data, however, the surface bright- variety of Sérsic shapes observed in ellipticals. Neither monolithic collapse nor dissipational mergers pro- 1School of Astronomy and Space Science, Nanjing University, Nanjing 210093, China 2The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA 3Key Laboratory of Modern Astronomy and Astrophysics, Nanjing University, Nanjing 210093, China 4Giant Magellan Telescope Organization, 251 South Lake Avenue, Suite 300, Pasadena, CA 91101, USA 5Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, China 6Department of Physics and Astronomy, 4129 Frederick Reines Hall, University of California, Irvine, CA 92697-4575, USA 1 2 HUANG ET AL. vides an adequate description of the full evolutionary process 1988), as are embedded nuclear stellar disks (Carter 1978; Ben- of massive elliptical galaxies. Recent observations show that der 1988; Franx et al. 1989; Peletier et al. 1990; Ledo et al. massive, quiescent early-type galaxies have been in place since 2010). These substructures are often attributed to merger or z 2.5 (Cimatti et al. 2004, 2008; McCarthy et al. 2004). accretion events. Even when the overall light distribution of el- High-redshift≈ massive galaxies have a great diversity in prop- lipticals appears smooth, it is not uncommon to see isophotal erties. Of particular interest is the population of “red nuggets,” twists (Kormendy 1982; Fasano & Bonoli 1989), which often which appear to be nascent, evolutionary precursors of local cannot be explained as an artifact of dust absorption. Nieto et giant ellipticals. On average, these quiescent galaxies have al. (1992) suggested that structural subcomponents may give smaller size (Daddi et al. 2005; Trujillo et al. 2006; Toft et al. rise to the isophotal twists observed in ellipticals. 2007; van der Wel et al. 2008; van Dokkum et al. 2008, 2009; The innermost regions of nearby elliptical galaxies contain Damjanov et al. 2009; Cassata et al. 2010, 2011; Szomoru et photometricially distinct components. This was recognized al. 2012) and possibly higher central stellar velocity dispersion even from ground-based images (Lauer 1985; Kormendy 1985) (Cappellari et al. 2009; Cenarro & Trujillo 2009; van Dokkum and has been fully elaborated with higher resolution data from et al. 2009; Onodera et al. 2010; van de Sande et al. 2011) HST (e.g., Jaffe et al. 1994; Lauer et al. 1995, 2007; Côté than local elliptical galaxies of the same stellar mass. On av- et al. 2006; Ferrarese et al. 2006). Depending on the relative erage the massive early-type galaxy population appears to re- steepness of the inner luminosity profile compared to the global quire a doubling in stellar mass and tripling in size during the one, the central regions of nearby elliptical galaxies have been epoch between z =2.0 and 1.0 (van Dokkum et al. 2010; see classified into “core” and “power law” (or “extra-light”) types, also Cimatti et al. 2012). Stacking analysis of large samples whose incidence depends strongly on galaxy luminosity (Faber of early-type galaxies at different redshift bins (Bezanson et al. et al. 1997; Lauer et al. 2007; K09): steep power-law cusps 2009; van Dokkum et al. 2010) and deep near-infrared images are found mostly in lower-luminosity systems, whereas lower of individual objects (Szomoru et al. 2012) reveal that high- density cores reside exclusively in the most massive, luminous redshift red nuggets differ from local ellipticals in two ways: ellipticals. Various empirical functions have been used to de- they lack an extended outer envelope while at the same time scribe these inner “deviations” of the surface brightness profile. their inner stellar mass density is higher. These observational The most popularhas been the “Nuker” law (Lauer et al. 1995), constraints strongly challenge theoretical scenarios wherein ei- but other forms have been used (Ferrarese et al. 1994; Graham ther dissipational collapse or gas-rich major mergers dominate et al. 2003; Trujillo et al. 2004; Côté et al. 2006; Hopkins et al. during the main phases of elliptical galaxy formation. Dis- 2009a). sipational processes lead to greater central concentration, not At the another extreme end in scale, the most luminous envelope building as required by the observed dramatic size members of the elliptical galaxy family are known to have ex- growth. Whatever