1,103 research outputs found
The Tilt of the Fundamental Plane of Elliptical Galaxies: I. Dynamical and Structural Effects
In this paper we explore several structural and dynamical effects on the
projected velocity dispersion as possible causes of the fundamental plane (FP)
tilt of elliptical galaxies. Specifically, we determine the size of the
systematic trend along the FP in the orbital radial anisotropy, in the dark
matter (DM) content and distribution relative to the bright matter, and in the
shape of the light profile that would be needed to produce the tilt, under the
assumption of a constant stellar mass to light ratio. Spherical, non rotating,
two--components models are constructed, where the light profiles resemble the
law. For the investigated models anisotropy cannot play a major role
in causing the tilt, while a systematic increase in the DM content and/or
concentration may formally produce it. Also a suitable variation of the shape
of the light profile can produce the desired effect, and there may be some
observational hints supporting this possibility. However, fine tuning is always
required in order to produce the tilt, while preserving the {\it tightness} of
the galaxies distribution about the FP.Comment: 12 pages MNRAS-TeX (mn.tex v1.5 incl.), 6 figures (.ps included)
uuencoded, gzip'ed tar file, accepted by MNRA
Star formation in early-type galaxies: the role of stellar winds and kinematics
Early-type galaxies (ETGs) host a hot ISM produced mainly by stellar winds,
and heated by Type Ia supernovae and the thermalization of stellar motions.
High resolution 2D hydrodynamical simulations showed that ordered rotation in
the stellar component results in the formation of a centrifugally supported
cold equatorial disc. In a recent numerical investigation we found that
subsequent generations of stars are formed in this cold disc; this process
consumes most of the cold gas, leaving at the present epoch cold masses
comparable to those observed. Most of the new stellar mass formed a few Gyrs
ago, and resides in a disc.Comment: 2 pages, 1 figure, to appear in proceedings of IAU Symposium 315,
"From Interstellar Clouds to Star-Forming Galaxies: Universal Processes?", P.
Jablonka, F. Van der Tak & P. Andre', ed
Exact solutions for the spatial de Vaucouleurs and Sersic laws and related quantities
Using the Mathematica package, we find exact analytical expressions for the
so-called de-projected De Vaucouleurs and Sersic laws as well as for related
spatial (3D) quantities, such the mass, gravitational potential, the total
energy and the central velocity dispersion, generally involved in astronomical
calculations expressed in terms of the Meijer G functions.Comment: 11 pages, accepted in A
Effects of tidal interactions on the gas flows of elliptical galaxies
During a Hubble time, cluster galaxies may undergo several mutual encounters
close enough to gravitationally perturb their hot, X-ray emitting gas flows. We
ran several 2D, time dependent hydrodynamical models to investigate the effects
of such perturbations on the gas flow inside elliptical galaxies. In
particular, we studied in detail the modifications occurring in the scenario
proposed by D'Ercole et al. (1989), in which the galactic interstellar medium
produced by the aging galactic stellar population, is heated by SNIa at a
decreasing rate. We find that, although the tidal interaction in our models
lasts less than 1 Gyr, its effect extends over several Gyrs. The tidally
induced turbulent flows create dense filaments which cool quickly and accrete
onto the galactic center, producing large spikes in the global Lx. Once this
mechanism starts, it is fed by gravity and amplified by SNIa. In cooling flow
models without supernovae the amplitude of the Lx fluctuations due to the tidal
interaction is substantially reduced. We conclude that, if SNIa significantly
contribute to the energetics of the gas flows in ellipticals, then the observed
spread in the Lx-Lb diagram may be caused, at least in part, by this mechanism.
On the contrary, tidal interactions cannot be responsible for the observed
spread if the pure cooling flow scenario applies (abridged).Comment: 21 pages, 8 figures, to be published in ApJ (main journal
The Effect of the AGN Feedback on the Interstellar Medium of Early-Type Galaxies: 2D Hydrodynamical Simulations of the Low-Rotation Case
We present 2D hydrodynamical simulations for the evolution of early-type
galaxies containing central massive black holes (MBHs), starting at age 2 Gyr.
The code contains accurate and physically consistent radiative and mechanical
AGN wind feedback, with parsec-scale central resolution. Mass input comes from
stellar evolution; energy input includes Type Ia and II supernova and stellar
heating; star-formation is included. Realistic, axisymmetric dynamical models
for the galaxies are built solving the Jeans' equations. The lowest mass models
(Mstar = 8 10^{10}Msun) develop global outflows sustained by SNIa's heating,
ending with a significantly lower amount of hot gas and new stars. In more
massive models, nuclear outbursts last to the present epoch, with large and
frequent fluctuations in nuclear emission and from the gas (Lx). Each burst
last ~ 10^{7.5} yr, during which (for r < 2-3 kpc) cold, inflowing, and hot,
outflowing gas phases coexist. The Lx-T relation for the gas matches that of
local galaxies. AGN activity causes positive feedback for star formation.
Roughly half of the total mass loss is recycled into new stars (DeltaMstar),
just ~ 3% of it is accreted on the MBH, the remainder being ejected from the
galaxy. The ratio between the mass of gas expelled to that in to new stars, the
load factor, is ~0.6. Rounder galaxies shapes lead to larger final MBH masses,
DeltaMstar, and Lx. Almost all the time is spent at very low nuclear
luminosities, yet one quarter of the total energy is emitted at an Eddington
ratio > 0.1. The duty-cycle of AGN activity approximates 4% (Abridged).Comment: 26 pages, 15 figure, submitted to ApJ. Comments welcom
Radiative feedback from massive black holes in elliptical galaxies. AGN flaring and central starburst fueled by recycled gas
The importance of the radiative feedback from massive black holes at the
centers of elliptical galaxies is not in doubt, given the well established
relations among electromagnetic output, black hole mass and galaxy optical
luminosity. We show how this AGN radiative output affects the hot ISM of an
isolated elliptical galaxy with the aid of a high-resolution hydrodynamical
code, where the cooling and heating functions include photoionization plus
Compton heating. We find that radiative heating is a key factor in the
self-regulated coevolution of massive black holes and their host galaxies and
that 1) the mass accumulated by the central black hole is limited by feedback
to the range observed today, and 2) relaxation instabilities occur so that duty
cycles are small enough (~0.03) to account for the very small fraction of
massive ellipticals observed to be in the "on" -QSO- phase, when the accretion
luminosity approaches the Eddington luminosity. The duty cycle of the hot
bubbles inflated at the galaxy center during major accretion episodes is of the
order of 0.1-0.4. Major accretion episodes caused by cooling flows in the
recycled gas produced by normal stellar evolution trigger nuclear starbursts
coincident with AGN flaring. During such episodes the central sources are often
obscured; but overall, in the bursting phase (1<z<3), the duty cycle of the
black hole in its "on" phase is of the order of percents and it is unobscured
approximately one-third of the time. Mechanical energy output from
non-relativistic gas winds integrates to 2.3 10^{59} erg, with most of it
caused by broadline AGN outflows. [abridged]Comment: ApJ resubmitted. 48 pages, 14 figures (some of them new, bitmapped,
low resolution). New references added, typos correcte
Cooling flows and quasars: different aspects of the same phenomenon? I. Concepts
We present a new class of solutions for the gas flows in elliptical galaxies
containing massive central black holes (BH). Modified King model galaxies are
assumed. Two source terms operate: mass loss from evolving stars, and a
secularly declining heating by SNIa. Relevant atomic physical processes are
modeled in detail. Like the previous models investigated by Ciotti et al.
(1991), these new models first evolve through three consecutive evolutionary
stages: wind, outflow, and inflow. At this point the presence of the BH alters
dramatically the subsequent evolution, because the energy emitted by the BH can
heat the surrounding gas to above virial temperatures, causing the formation of
a hot expanding central bubble. Short and strong nuclear bursts of radiation
are followed by longer periods during which the X-ray galaxy emission comes
from the coronal gas (Lx). The range and approximate distribution spanned by Lx
are found to be in accordance with observations of X-ray early type galaxies.
Moreover, although high accretion rates occur during bursting phases when the
central BH has a luminosity characteristic of QSOs, the total mass accreted is
very small when compared to that predicted by stationary cooling-flow solutions
and computed masses are in accord with putative BH nuclear masses. In the
bursting phases Lx is low and the surface brightness profile is very low
compared to pre-burst or to cooling flow models. We propose that these new
models, while solving some long-standing problems of the cooling flow scenario,
can provide a unified description of QSO-like objects and X-ray emitting
elliptical galaxies, these being the same objects observed at two different
evolutionary phases.Comment: 10 pages, ApJ LaTeX, plus 5 .eps figures and TeX-macro aasms4.sty -
revised version - in press on ApJ Letter
Decoupled and inhomogeneous gas flows in S0 galaxies
A recent analysis of the "Einstein" sample of early-type galaxies has
revealed that at any fixed optical luminosity Lb S0 galaxies have lower mean
X-ray luminosity Lx per unit Lb than ellipticals. Following a previous
analytical investigation of this problem (Ciotti & Pellegrini 1996), we have
performed 2D numerical simulations of the gas flows inside S0 galaxies in order
to ascertain the effectiveness of rotation and/or galaxy flattening in reducing
the Lx/Lb ratio. The flow in models without SNIa heating is considerably
ordered, and essentially all the gas lost by the stars is cooled and
accumulated in the galaxy center. If rotation is present, the cold material
settles in a disk on the galactic equatorial plane. Models with a time
decreasing SNIa heating host gas flows that can be much more complex. After an
initial wind phase, gas flows in energetically strongly bound galaxies tend to
reverse to inflows. This occurs in the polar regions, while the disk is still
in the outflow phase. In this phase of strong decoupling, cold filaments are
created at the interface between inflowing and outflowing gas. Models with more
realistic values of the dynamical quantities are preferentially found in the
wind phase with respect to their spherical counterparts of equal Lb. The
resulting Lx of this class of models is lower than in spherical models with the
same Lb and SNIa heating. At variance with cooling flow models, rotation is
shown to have only a marginal effect in this reduction, while the flattening is
one of the driving parameters for such underluminosity, in accordance with the
analytical investigation.Comment: 32 pages LaTex file, plus 5 .ps figures and macro aasms4.sty --
Accepted on Ap
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