384 research outputs found
Characteristic Scales in Galaxy Formation
Recent data, e.g. from SDSS and 2dF, reveal a robust bi-modality in the
distribution of galaxy properties, with a characteristic transition scale at
stellar mass M_*~3x10^{10} Msun (near L_*), corresponding to virial velocity
V~100 km/s. Smaller galaxies tend to be blue disks of young populations. They
define a "fundamental line" of decreasing surface brightness, metallicity and
velocity with decreasing M_*, which extends to the smallest dwarf galaxies.
Galaxies above the critical scale are dominated by red spheroids of old
populations, with roughly constant high surface brightens and metallicity, and
they tend to host AGNs. A minimum in the virial M/L is obtained at the same
magic scale. This bi-modality can be the combined imprint of several different
physical processes. On smaller scales, disks are built by cold flows, and
supernova feedback is effective in regulating star formation. On larger scales,
the infalling gas is heated by a virial shock and star formation can be
suppressed by AGN feedback. Another feedback mechanism -- gas evaporation due
to photo-ionization -- may explain the existence of totally dark halos below
V~30 km/s. The standard cooling barriers are responsible for the loose upper
and lower bounds for galaxies: 10 < V < 300 km/s.Comment: 10 pages, 5 figures, LaTeX (svmult.cls, physprbb.sty), to be
published in ESO/USM/MPE Venice Workshop on Multiwavelength Mapping of Galaxy
Formation and Evolution, eds. R. Bender and A. Renzini. Also
http://phys.huji.ac.il/~dekel/scales/scales.ps.g
Dynamics of Cosmic Flows
CONTENTS: 1. INTRODUCTION 2. GRAVITATIONAL INSTABILITY 3. MEASURING PECULIAR
VELOCITIES 4. ANALYSIS OF OBSERVED PECULIAR VELOCITIES 5. PREDICTED MOTIONS
FROM THE GALAXY DISTRIBUTION 6. TESTING BASIC HYPOTHESES 7. THE INITIAL
FLUCTUATIONS 8. THE VALUE OF OMEGA 9. DISCUSSION: ARE THE HYPOTHESES JUSTIFIED?
REFERENCESComment: A review for Ann. Rev. of Astron. and Astrophys. 32 (October 1994).
46 pages, 10 figures built-in, compressed and uuencoded PostScript (1.58
Mbyte). (Also available by anonymous ftp from venus.huji.ac.il as
pub/dekel/reviews/annrev9.uu, or text and figures separately as annrev7.uu
with fig*.ps) (HUJI-AST-94-002
Cosmological Implications of Large-Scale Flows
Cosmological implications of the observed large-scale peculiar velocities are
reviewed, alone or combined with redshift surveys and CMB data. The latest
version of the POTENT method for reconstructing the underlying
three-dimensional velocity and mass-density fields is described. The initial
fluctuations and the nature of the dark matter are addressed via statistics
such as bulk flow and mass power spectrum. The focus is on constraining the
mass density parameter , directly or via the parameter which
involves the unknown relation between galaxies and mass. The acceptable range
for is found to be . The range of estimates is likely
to reflect non-trivial features in the galaxy biasing scheme, such as scale
dependence. Similar constraints on and from global measures
are summarized.Comment: 40 pages, 15 figures, LaTex (aaspp4.sty), to appear in the
proceedings of the 3rd ESO-VLT Workshop on ``Galaxy Scaling Relations:
Origins, Evolution and Applications", ed. L. da Costa (Springer
Cosmic Flows 99: Conference Summary
I address the following issues: All bulk velocity measurements (but one) are
consistent with our standard gravitational instability theory. New accurate
data and reconstruction methods allow high-resolution dynamical analysis
nearby, revealing Virgo, Ursa Major and Fornax as attractors. Large
peculiar-velocity surveys enable robust reconstruction of the dynamical fields
on the Great-Attractor scale. A decomposition of the velocity field into its
local and tidal components indicates the presence of big perturbations further
away. Cluster velocities start exploring very large scales, revealing Coma,
Shapely and other mass enhancements, and constraining a possible local Hubble
bubble. Supernovae type Ia (SNIa) are very promising for cosmic flow analysis.
Peculiar velocities do provide unique valuable constraints on cosmological
parameters, e.g., 0.3<Omega_m<1 (95% confidence) independent of biasing.
Jointly with other data they can confine other parameters such as Omega_Lambda,
h, sigma_8, n, and the biasing. Nontrivial features of the biasing scheme can
explain much of the span of estimates for beta. Quantitative error analysis is
essential in our maturing field; every method ought to be calibrated with
suitable mock catalogs, that are offered as benchmarks.Comment: 8 pages LaTeX, 8 embedded figures. paspconf.sty. Higher quality figs
from ftp://alf.fiz.huji.ac.il/pub/dekel/vic99/ as adekel*_l.ps.gz (*=1-8). In
"Cosmic Flows: Towards an Understanding of Large-Scale Structure", eds S.
Courteau, M.A. Strauss, & J.A. Willick, ASP Conf. Serie
Galaxy Biasing: Nonlinear, Stochastic and Measurable
I describe a general formalism for galaxy biasing (Dekel & Lahav 1998) and
its application to measurements of beta (=Omega^0.6/b), e.g. via direct
comparisons of light and mass and via redshift distortions. The linear and
deterministic relation g=b*d between the density fluctuation fields of galaxies
g and mass d is replaced by the conditional distribution P(g|d) of these as
random fields, smoothed at a given scale and at a given time. The mean biasing
and its nonlinearity are characterized by the conditional mean =b(d)*d and
the local scatter by the conditional variance s_b^2(d). This scatter arises
from hidden effects on galaxy formation and from shot noise. For applications
involving second-order local moments, the biasing is defined by three natural
parameters: the slope b_h of the regression of g on d (replacing b), a
nonlinearity parameter b_t, and a scatter parameter s_b. The ratio of variances
b_v^2 and the correlation coefficient r mix these parameters. The nonlinearity
and scatter lead to underestimates of order b_t^2/b_h^2 and s_b^2/b_h^2 in the
different estimators of beta, which may partly explain the range of estimates.
Local stochasticity affects the redshift-distortion analysis only by limiting
the useful range of scales. In this range, for linear stochastic biasing, the
analysis reduces to Kaiser's formula for b_h (not b_v) independent of the
scatter. The distortion analysis is affected by nonlinearity but in a weak way.
Estimates of the nontrivial features of the biasing scheme are made based on
simulations and toy models, and a new method for measuring them via
distribution functions is proposed.Comment: 13 pages, LaTeX (conf_iap.sty enclosed), 2 figures (Postscript), to
appear in the XIV IAP meeting on Wide Field Surveys in Cosmology, eds. Y.
Mellier & S. Colombi (Gif-sur-Yvette: Editions Frontieres
Virial shocks in galactic haloes?
We investigate the conditions for the existence of an expanding virial shock
in the gas falling within a spherical dark-matter halo. The shock relies on
pressure support by the shock-heated gas behind it. When the radiative cooling
is efficient compared to the infall rate the post-shock gas becomes unstable;
it collapses inwards and cannot support the shock.
We find for a monoatomic gas that the shock is stable when the post-shock
pressure and density obey gamma effective>10/7, with gamma effective begin the
time depended equivalent to the adiabatic index. We express the effective gamma
in terms of r, u and rho at the shock to obtain a simple condition for shock
stability. This result is confirmed by hydrodynamical simulations, using an
accurate spheri-symmetric Lagrangian code. When the stability analysis is
applied in cosmology, we find that a virial shock does not develop in most
haloes that form before z ~ 2, and it never forms in haloes less massive than a
few 10^11 solar masses. In such haloes the infalling gas is never heated to the
virial temperature, and it does not need to cool radiatively before it drops
into a disc. Instead, the gas collapses at T ~ 10^4K directly into the disc.
This should have nontrivial effects on the star-formation rate and on the gas
removal by supernova-driven winds. Instead of radiating soft x rays, this gas
would emit lyman alpha thus helping explain the low flux of soft x-ray
background and the lyman alpha emitters observed at high redshift.Comment: 17 pages, 13 eps figs, latex, mn2e, accepted by MNRAS - minor
additions to the discussio
An analytic solution for the minimal bathtub toy model: challenges in the star-formation history of high-z galaxies
We study the minimal ``bathtub" toy model as an analytic tool for capturing
key processes of galaxy evolution and identifying robust successes and
challenges in reproducing observations at high redshift. The source and sink
terms of the continuity equations for gas and stars are expressed in simple
terms from first principles. The assumed dependence of star-formation rate
(SFR) on gas mass self-regulates the system into a unique asymptotic behavior,
which is approximated by an analytic quasi-steady-state solution (QSS). We
address the validity of the QSS at different epochs independent of earlier
conditions. At high z, where the accretion is assumed to consist of gas only,
the specific SFR is robustly predicted to be sSFR = [(1+z)/3]^{5/2} Gyr^{-1},
slightly higher than the cosmological specific accretion rate, in agreement
with observations at z=3-8. The gas fraction is expected to decline slowly, and
the observations constrain the SFR efficiency per dynamical time to
epsilon=0.02. The stellar-to-virial mass ratio f_sv is predicted to be constant
in time, and the observed value requires an outflow mass-lading factor of
eta=1-3, depending on the penetration efficiency of gas into the galaxy.
However, at z=2, where stars are also accreted through mergers, the simplest
model has an apparent difficulty in matching observations. The model that
maximizes the sSFR, with the outflows fully recycled, falls short by a factor 3
in sSFR, and overestimates f_sv. With strong outflows, the model can reproduce
the observed f_sv but at the expense of underestimating the sSFR by an order of
magnitude. We discuss potential remedies including a bias due to the exclusion
of quenched galaxies.Comment: 14 pages, 3 figure
Stochastic Nonlinear Galaxy Biasing
We propose a general formalism for galaxy biasing and apply it to methods for
measuring cosmological parameters, such as regression of light versus mass, the
analysis of redshift distortions, measures involving skewness and the cosmic
virial theorem. The common linear and deterministic relation g=b*d between the
density fluctuation fields of galaxies g and mass d is replaced by the
conditional distribution P(g|d) of these random fields, smoothed at a given
scale at a given time. The nonlinearity is characterized by the conditional
mean =b(d)*d, while the local scatter is represented by the conditional
variance s_b^2(d) and higher moments. The scatter arises from hidden factors
affecting galaxy formation and from shot noise unless it has been properly
removed. For applications involving second-order local moments, the biasing is
defined by three natural parameters: the slope b_h of the regression of g on d,
a nonlinearity b_t, and a scatter s_b. The ratio of variances b_v^2 and the
correlation coefficient r mix these parameters. The nonlinearity and the
scatter lead to underestimates of order b_t^2/b_h^2 and s_b^2/b_h^2 in the
different estimators of beta (=Omega^0.6/b_h). The nonlinear effects are
typically smaller. Local stochasticity affects the redshift-distortion analysis
only by limiting the useful range of scales, especially for power spectra. In
this range, for linear stochastic biasing, the analysis reduces to Kaiser's
formula for b_h (not b_v), independent of the scatter. The distortion analysis
is affected by nonlinear properties of biasing but in a weak way. Estimates of
the nontrivial features of the biasing scheme are made based on simulations and
toy models, and strategies for measuring them are discussed. They may partly
explain the range of estimates for beta.Comment: 28 pages, LaTeX (aaspp4.sty), 1 figure (2 ps files), minor revision
Phase-Space Structure & Substructure of Dark Halos
A method is presented for computing the 6-D phase-space density f(x,v) and
its PDF v(f) in an N-body system. It is based on Delaunay tessellation,
yielding v(f) with a fixed smoothing window over a wide f range, independent of
the sampling resolution. It is found that in a gravitationally relaxed halo
built by hierarchical clustering, v(f) is a robust power law, v(f) f^{-2.5 \pm
0.05}, over more than 4 decades in f, from its virial level to the current
resolution limit. This is valid for halos of different sizes in the LCDM
cosmology, indicating insensitivity to the initial-fluctuation power spectrum
as long as the small-scale fluctuations were not completely suppressed. By
mapping f in position space, we find that the high-f contributions to v(f) come
from the "cold" subhalos within the parent halo rather than the halo central
region and its global spherical profile. The f in subhalos near the halo virial
radius is more than 100 times higher than at the halo center, and it decreases
gradually with decreasing radius. This indicates phase mixing due to mergers
and tidal effects involving puffing up and heating. The phase-space structure
provides a sensitive tool for studying the evolution of subhalos during the
buildup of halos. One wishes to understand why the substructure adds up to the
universal power law in v(f). It seems that the f^{-2.5} behavior is related to
the hierarchical clustering process and is not a general result of violent
relaxation.Comment: 12 pages, LaTeX using newpasp.sty, to be published in Satellites and
Tidal Streams, eds. D. Martinez-Delgado & F. Prada, ASP Conference Serie
Cosmological Parameters and Power Spectrum from Peculiar Velocities
The power spectrum of mass density fluctuations is evaluated from the Mark
III and the SFI catalogs of peculiar velocities by a maximum likelihood
analysis, using parametric models for the power spectrum and for the errors.
The applications to the two different data sets, using generalized CDM models
with and without COBE normalization, give consistent results. The general
result is a relatively high amplitude of the power spectrum, with \sigma_8
\Omega_m^{0.6} = 0.8+/-0.2 at 90% confidence. Casting the results in the
\Omega_m - \Omega_\Lambda plane, yields complementary constraints to those of
the high-redshift supernovae, together favoring a nearly flat, unbound and
accelerating universe with comparable contributions from \Omega_m and
\Omega_\Lambda. Further implications on the cosmological parameters, arising
from a joint analysis of the velocities together with small-scale CMB
anisotropies and the high-redshift supernovae, are also briefly described.Comment: 8 pages, 3 figures. To appear in Proceedings of the Cosmic Flows
Workshop, Victoria, B.C., Canada, July 1999, eds. S. Courteau, M. Strauss,
and J. Willic
- …