The SAURON project - XIX. Optical and near-infrared scaling relations of nearby elliptical, lenticular and Sa galaxies

Abstract

We present ground‐based MDM Observatory V‐band and Spitzer/InfraRed Array Camera 3.6‐m‐band photometric observations of the 72 representative galaxies of the SAURON survey. Galaxies in our sample probe the elliptical E, lenticular S0 and spiral Sa populations in the nearby Universe, both in field and cluster environments. We perform aperture photometry to derive homogeneous structural quantities. In combination with the SAURON stellar velocity dispersion measured within an effective radius (σe), this allows us to explore the location of our galaxies in the colour–magnitude, colour–σe, Kormendy, Faber–Jackson and Fundamental Plane scaling relations. We investigate the dependence of these relations on our recent kinematical classification of early‐type galaxies (i.e. slow/fast rotators) and the stellar populations. Slow rotator and fast rotator E/S0 galaxies do not populate distinct locations in the scaling relations, although slow rotators display a smaller intrinsic scatter. We find that Sa galaxies deviate from the colour–magnitude and colour–σe relations due to the presence of dust, while the E/S0 galaxies define tight relations. Surprisingly, extremely young objects do not display the bluest (V−[3.6]) colours in our sample, as is usually the case in optical colours. This can be understood in the context of the large contribution of thermally pulsing asymptotic giant branch stars to the infrared, even for young populations, resulting in a very tight (V−[3.6])–σe relation that in turn allows us to define a strong correlation between metallicity and σe. Many Sa galaxies appear to follow the Fundamental Plane defined by E/S0 galaxies. Galaxies that appear offset from the relations correspond mostly to objects with extremely young populations, with signs of ongoing, extended star formation. We correct for this effect in the Fundamental Plane, by replacing luminosity with stellar mass using an estimate of the stellar mass‐to‐light ratio, so that all galaxies are part of a tight, single relation. The new estimated coefficients are consistent in both photometric bands and suggest that differences in stellar populations account for about half of the observed tilt with respect to the virial prediction. After these corrections, the slow rotator family shows almost no intrinsic scatter around the best‐fitting Fundamental Plane. The use of a velocity dispersion within a small aperture (e.g. Re/8) in the Fundamental Plane results in an increase of around 15 per cent in the intrinsic scatter and an average 10 per cent decrease in the tilt away from the virial relation.

No evidence for small disk-like bulges in a sample of late-type spirals

“…The Pearson correlation coefficient is ρ = −0.8, reflecting a tight correlation between galaxies properties in this plane. The scatter increases in the low-σ end of the relation, showing a trend mimicking the expected down-bending of the FJR (Falcón-Barroso et al 2011). This regime of the FJR is populated by the small bulges of the comparison sample.…”

“…The FJR (Faber & Jackson 1976;Falcón-Barroso et al 2011) states that brighter galaxies exhibit larger velocity dispersion. …”

Formation and evolution of dwarf early-type galaxies in the Virgo cluster

“…Another novelty of this work is the way the velocity dispersion is computed for dwarf galaxies. As previously suggested (Zaritsky et al 2006(Zaritsky et al , 2008Falcón-Barroso et al 2011), the velocity dispersion is best measured within the half light radius including both the rotation and the random motions of the stars, so that it represents the kinetic energy of the systems.…”

The Stellar Initial Mass Function in Early-Type Galaxies From Absorption Line Spectroscopy. Ii. Results

“…A number of recent papers have pointed to fragmentation in supersonically turbulent molecular clouds as the key physical 8 The stellar mass within r e /8 is estimated by combining the best-fit M/L K ratios, the total K-band luminosities from Cappellari et al (2011), and the Sérsic indices from Falcón-Barroso et al (2011). The latter quantity is used to estimate the fraction of the total light contained within r e /8.…”