The Centers of Early-Type Galaxies with HST. IV. Central Parameter Relations.

Abstract

We analyze Hubble Space Telescope surface-brightness profiles of 61 elliptical galaxies and spiral bulges (hereafter "hot" galaxies). The profiles are parameterized by break radius r b and break surface brightness I b . These are combined with central velocity dispersions, total luminosities, rotation velocities, and isophote shapes to explore correlations among central and global properties. Luminous hot galaxies (M V < −22) have cuspy cores with steep outer power-law profiles that break at r ≈ r b to shallow inner profiles I ∝ r −γ with γ ≤ 0.3. Break radii and core luminosities for these objects are approximately proportional to effective radii and total luminosities. Scaling relations are presented for several core parameters as a function of total luminosity. Cores follow a fundamental plane that parallels the global fundamental plane for hot galaxies but is 30% thicker. Some of this extra thickness may be due to the effect of massive black holes (BHs) on central velocity dispersions. Faint hot galaxies (M V > −20.5) show steep, largely featureless power-law profiles that lack cores. Measured values of r b and I b for these galaxies are limits only. At a limiting radius of 10 pc, the centers of power-law galaxies are up to 1000 times denser in mass and luminosity than the cores of large galaxies. At intermediate magnitudes (−22 < M V < −20.5), core and power-law galaxies coexist, and there is a range in r b at a given luminosity of at least two orders of magnitude. Here, central properties correlate strongly with global rotation and shape: core galaxies tend to be boxy and slowly rotating, whereas power-law galaxies tend to be disky and rapidly rotating. A search for inner disks was conducted to test a claim in the literature, based on a smaller sample, that power laws originate from edge-on stellar disks. We find only limited evidence for such disks and believe that the difference between core and power-law profiles reflects a real difference in the spatial distribution of the luminous spheroidal component of the galaxy. The dense power-law centers of disky, rotating galaxies are consistent with their formation in gas-rich mergers. The parallel proposition, that cores are the by-products of gas-free stellar mergers, is less compelling for at least two reasons: (1) dissipationless hierarchical clustering does not appear to produce core profiles like those seen; (2) core galaxies accrete small, dense, gas-free galaxies at a rate sufficient to fill in their low-density cores if the satellites survived and sank to the center (whether the satellites survive is still an open question). An alternative model for core formation involves the orbital decay of massive black holes (BHs) that are accreted in mergers: the decaying BHs may heat and eject stars from the center, eroding a power law if any exists and scouring out a core. An average BH mass per spheroid of 0.002 times the stellar mass yields cores in fair agreement with observed cores and is consistent with the energetics of AGNs and the kinematic detection of...

The dynamical evolution of massive black hole binaries I. Hardening in a fixed stellar background

“…This is a much stronger anisotropy than is predicted by models like the adiabatic-growth model for the formation of massive black holes. The adiabatic growth of a bh in an initially isotropic galaxy leads to a final anisotropy of at most β = −0.3 Our mass-ejection results support the suggestion of Ebisuzaki et al (1991) and Faber et al (1996) that bh binaries can explain the weak density cusps in large elliptical galaxies. If these galaxies contain massive bhs, and if they have formed through mergers of smaller galaxies also containing massive bhs, the binaries that result will clear out the central region.…”

“…If binary mergers are frequent they will be the most interesting source of gravitational radiation for the planned space-based detector LISA (Haehnelt, 1994;Bender et al, 1995). Lastly, the evolution of bh binaries may explain why the density profiles of elliptical galaxies fall into two classes, with small galaxies having strong density cusps and large galaxies having weaker cusps (Ebisuzaki et al, 1991;Faber et al, 1996).…”

The Kinematics of Core and Cusp Galaxies: Comparing HST Imaging and Integral-Field Observations

“…There are 33 galaxies in the SAURON sample of 48 elliptical and lenticular galaxies with known values for their inner profile slope, which separates them in "core" and "power-law" galaxies [6,14,13,11]. From the point of view of their stellar kinematics (see [4]) early-type galaxies appear in two broad flavours, depending on whether they exhibit clear large-scale rotation or not.…”

Structural properties of dwarf ellipticals and the connection with (ordinary) elliptical galaxies

“…(ii) Using HST data from the Nuker team (Faber et al 1997), the M -µ 0 relation is now much better defined than it was twenty years ago, especially at the bright end. Furthermore, the increased number of galaxies around the alleged transition magnitude of −18 B-mag has also improved our understanding of what is going on.…”

“…The central surface brightness values obtained from Sérsic models fitted to luminous (MB −20.5 mag) E galaxies follow this same relation (Jerjen & Binggeli 1997), although they were not used to define it. The symbols are the same as in Figure 1, with the additional open circles representing the so-called "power-law" E galaxies from Faber et al (1997), and the filled circles representing the "core" E galaxies from these same authors.…”