603 research outputs found
On Borel Probability Measures and Noncooperative Game Theory
In this paper the well-known minimax theorems of Wald, Ville and VonNeumann are generalized under weaker topological conditions onthepayoff function Æ’ and/or extended to the larger set of the Borelprobabilitymeasures instead of the set of mixed strategies.minimax theory;infinite dimensional separation;Borel measures;noncooperative game theory;weak compactness
The Role of Starbursts in the Formation of Galaxies & Active Galactic Nuclei
Starbursts are episodes of intense star-formation in the central regions of
galaxies, and are the sites of roughly 25% of the high-mass star-formation in
the local universe. In this contribution I review the role starbursts play in
the formation and evolution of galaxies, the intergalactic medium, and active
galactic nuclei. Four major conclusions are drawn. 1) Starburst galaxies are
good analogues (in fact, the only plausible local analogues) to the known
population of star-forming galaxies at high-redshift. 2) Integrated over cosmic
time, supernova-driven galactic-winds (`superwinds') play an essential role in
the evolution of galaxies and the inter-galactic medium. 3) Circumnuclear
starbursts are an energetically-significant component of the Seyfert
phenomenon. 4) The evolution of the population of the host galaxies of
radio-quiet quasars is significantly different than that of powerful radio
galaxies, and is at least qualitatively consistent with the standard picture of
the hierarchical assembly of massive galaxies at relatively late times.Comment: 16 pages, 4 figures, Royal Society discussion meeting `The formation
of galaxies
On Borel Probability Measures and Noncooperative Game Theory
In this paper the well-known minimax theorems of Wald, Ville and Von
Neumann are generalized under weaker topological conditions onthe
payoff function Æ’ and/or extended to the larger set of the Borel
probabilitymeasures instead of the set of mixed strategies
A halo expansion technique for approximating simulated dark matter haloes
We apply a basis function expansion method to create a time-evolving density/potential approximation of the late growth of simulated N-body dark matter haloes. We demonstrate how the potential of a halo from the Aquarius Project can be accurately represented by a small number of basis functions, and show that the halo expansion (HEX) method provides a way to replay simulations. We explore the level of accuracy of the technique as well as some of its limitations. We find that the number of terms included in the expansion must be large enough to resolve the large-scale distribution and shape of the halo but, beyond this, additional terms result in little further improvement. Particle and subhalo orbits can be integrated in this realistic, time-varying halo potential approximation, at much lower cost than the original simulation, with high fidelity for many individual orbits, and a good match to the distributions of orbital energy and angular momentum. Statistically, the evolution of structural subhalo properties, such as mass, half-mass radius and characteristic circular velocity, are very well reproduced in the HEX approximation over several Gyr. We demonstrate an application of the technique by following the evolution of an orbiting subhalo at much higher resolution than can be achieved in the original simulation. Our method represents a significant improvement over commonly used techniques based on static analytical descriptions of the halo potential
A G1-like globular cluster in NGC 1023
The structure of a very bright (MV = -10.9) globular cluster in NGC 1023 is
analyzed on two sets of images taken with the Hubble Space Telescope. From
careful modeling of King profile fits to the cluster image, a core radius of
0.55+/-0.1 pc, effective radius 3.7+/-0.3 pc and a central V-band surface
brightness of 12.9+/-0.5 mag / square arcsec are derived. This makes the
cluster much more compact than Omega Cen, but very similar to the brightest
globular cluster in M31, G1 = Mayall II. The cluster in NGC 1023 appears to be
very highly flattened with an ellipticity of about 0.37, even higher than for
Omega Cen and G1, and similar to the most flattened clusters in the Large
Magellanic Cloud.Comment: 14 pages, 3 figures, 1 table. Accepted for AJ, Oct 200
Physical Bias of Galaxies From Large-Scale Hydrodynamic Simulations
We analyze a new large-scale (Mpc) numerical hydrodynamic
simulation of the popular CDM cosmological model, including in our
treatment dark matter, gas and star-formation, on the basis of standard
physical processes. The method, applied with a numerical resolution of
kpc (which is still quite coarse for following individual galaxies,
especially in dense regions), attempts to estimate where and when galaxies
form. We then compare the smoothed galaxy distribution with the smoothed mass
distribution to determine the "bias" defined as on scales large compared with the code
numerical resolution (on the basis of resolution tests given in the appendix of
this paper). We find that (holding all variables constant except the quoted
one) bias increases with decreasing scale, with increasing galactic age or
metallicity and with increasing redshift of observations. At the Mpc
fiducial comoving scale bias (for bright regions) is 1.35 at reaching to
3.6 at , both numbers being consistent with extant observations. We also
find that Mpc voids in the distribution of luminous objects are
as observed (i.e., observed voids are not an argument against CDM-like models)
and finally that the younger systems should show a colder Hubble flow than do
the early type galaxies (a testable proposition). Surprisingly, little
evolution is found in the amplitude of the smoothed galaxy-galaxy correlation
function (as a function of {\it comoving} separation). Testing this prediction
vs observations will allow a comparison between this work and that of Kauffmann
et al which is based on a different physical modelingmethod.Comment: in press, ApJ, 26 latex pages plus 7 fig
Early structure in Lambda CDM
We use a novel technique to simulate the growth of one of the most massive progenitors of a supercluster region from redshift z 80, when its mass was about 10 M, until the present day. Our nested sequence of N-body resimulations allows us to study in detail the structure both of the dark matter object itself and of its environment. Our effective resolution is optimal at redshifts of 49, 29, 12, 5 and 0 when the dominant object has mass 1.2 × 105, 5 × 107, 2 × 1010, 3 × 1012 and 8 × 1014 h1 M, respectively, and contains 106 simulation particles within its virial radius. Extended Press–Schechter (EPS) theory correctly predicts both this rapid growth and the substantial overabundance of massive haloes we find at early times in regions surrounding the dominant object. Although the large-scale structure in these regions differs dramatically from a scaled version of its present-day counterpart, the internal structure of the dominant object is remarkably similar. Molecular hydrogen cooling could start as early as z 49 in this object, while cooling by atomic hydrogen becomes effective at z 39. If the first stars formed in haloes with virial temperature 2000 K, their comoving abundance at z= 49 should be similar to that of dwarf galaxies today, while their comoving correlation length should be 2.5 h1 Mpc
Simulations of AGN feedback in galaxy clusters and groups: impact on gas fractions and the Lx-T scaling relation
Recently, rapid observational and theoretical progress has established that
black holes (BHs) play a decisive role in the formation and evolution of
individual galaxies as well as galaxy groups and clusters. In particular, there
is compelling evidence that BHs vigorously interact with their surroundings in
the central regions of galaxy clusters, indicating that any realistic model of
cluster formation needs to account for these processes. This is also suggested
by the failure of previous generations of hydrodynamical simulations without BH
physics to simultaneously account for the paucity of strong cooling flows in
clusters, the slope and amplitude of the observed cluster scaling relations,
and the high-luminosity cut-off of central cluster galaxies. Here we use
high-resolution cosmological simulations of a large cluster and group sample to
study how BHs affect their host systems. We focus on two specific properties,
the halo gas fraction and the X-ray luminosity-temperature scaling relation,
both of which are notoriously difficult to reproduce in self-consistent
hydrodynamical simulations. We show that BH feedback can solve both of these
issues, bringing them in excellent agreement with observations, without
alluding to the `cooling only' solution that produces unphysically bright
central galaxies. By comparing a large sample of simulated AGN-heated clusters
with observations, our new simulation technique should make it possible to
reliably calibrate observational biases in cluster surveys, thereby enabling
various high-precision cosmological studies of the dark matter and dark energy
content of the universe.Comment: 4 pages, 2 figures, minor revisions, ApJL in pres
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