405 research outputs found
The Dark Matter Density in the Solar Neighborhood reconsidered
Both the gas flaring and the dip in the rotation curve, which was recently
reconfirmed with precise measurements using the VERA VLBI array in Japan,
suggest doughnut-like substructure in the dark matter (DM) halo. A global fit
to all available data shows that the data are indeed best described by an NFW
DM profile complemented by two doughnut-like DM substructures with radii of 4.2
and 12.4 kpc, which coincide with the local dust ring and the Monocerus ring of
stars, respectively. Both regions have been suggested as regions with tidal
streams from "shredded" satellites. If real, the radial extensions of these
nearby ringlike structures enhance the local dark matter density by a factor of
four to about 1.3 GeV/cm.
It is shown that i) this higher DM density is perfectly consistent with the
local gravitational potential determining the surface density and the local
matter density (Oort limit), ii) previous determinations of the surface density
were biased by the assumption of a smoothly varying DM halo and iii) the
s-shaped gas flaring is explained. Such a possible enhancement of the local DM
density is of great interest for direct DM searches and would change the
directional dependence for indirect DM searches.Comment: 14 pages, 4 figures, extended version, accepted for publication in
JCA
On determining the shape of matter distributions
A basic property of objects, like galaxies and halos that form in
cosmological structure formation simulations, is their shape. Here, we
critically investigate shape determination methods that are commonly used in
the literature. It is found that using an enclosed integration volume and
weight factors r^{-2} and r_{ell}^{-2} (elliptical radius) for the contribution
of each particle or volume element in the shape tensor leads to biased axis
ratios and smoothing of details when calculating the local shape as a function
of distance from the center. To determine the local shape of matter
distributions as a function of distance for well resolved objects (typically
more than O(10^4) particles), we advocate a method that (1) uses an ellipsoidal
shell (homoeoid) as an integration volume without any weight factors in the
shape tensor and (2) removes subhalos.Comment: 8 pages, 6 figures, submitted to ApJ
Direct Formation of Supermassive Black Holes via Multi-Scale Gas Inflows in Galaxy Mergers
Observations of distant bright quasars suggest that billion solar mass
supermassive black holes (SMBHs) were already in place less than a billion
years after the Big Bang. Models in which light black hole seeds form by the
collapse of primordial metal-free stars cannot explain their rapid appearance
due to inefficient gas accretion. Alternatively, these black holes may form by
direct collapse of gas at the center of protogalaxies. However, this requires
metal-free gas that does not cool efficiently and thus is not turned into
stars, in contrast with the rapid metal enrichment of protogalaxies. Here we
use a numerical simulation to show that mergers between massive protogalaxies
naturally produce the required central gas accumulation with no need to
suppress star formation. Merger-driven gas inflows produce an unstable, massive
nuclear gas disk. Within the disk a second gas inflow accumulates more than 100
million solar masses of gas in a sub-parsec scale cloud in one hundred thousand
years. The cloud undergoes gravitational collapse, which eventually leads to
the formation of a massive black hole. The black hole can grow to a billion
solar masses in less than a billion years by accreting gas from the surrounding
disk.Comment: 26 pages, 4 Figures, submitted to Nature (includes Supplementary
Information
On relaxation processes in collisionless mergers
We analyze N-body simulations of halo mergers to investigate the mechanisms
responsible for driving mixing in phase-space and the evolution to dynamical
equilibrium. We focus on mixing in energy and angular momentum and show that
mixing occurs in step-like fashion following pericenter passages of the halos.
This makes mixing during a merger unlike other well known mixing processes such
as phase mixing and chaotic mixing whose rates scale with local dynamical time.
We conclude that the mixing process that drives the system to equilibrium is
primarily a response to energy and angular momentum redistribution that occurs
due to impulsive tidal shocking and dynamical friction rather than a result of
chaotic mixing in a continuously changing potential. We also analyze the merger
remnants to determine the degree of mixing at various radii by monitoring
changes in radius, energy and angular momentum of particles. We confirm
previous findings that show that the majority of particles retain strong memory
of their original kinetic energies and angular momenta but do experience
changes in their potential energies owing to the tidal shocks they experience
during pericenter passages. Finally, we show that a significant fraction of
mass (~ 40%) in the merger remnant lies outside its formal virial radius and
that this matter is ejected roughly uniformly from all radii outside the inner
regions. This highlights the fact that mass, in its standard virial definition,
is not additive in mergers. We discuss the implications of these results for
our understanding of relaxation in collisionless dynamical systems.Comment: Version accepted for Publication in Astrophysical Journal, March 20,
2007, v685. Minor changes, latex, 14 figure
Are Great Disks Defined by Satellite Galaxies in Milky-Way Type Halos Rare in CDM model?
We study the spatial distribution of satellite galaxies by assuming that they
follow the dark matter distribution. This assumption is supported by
semi-analytical studies based on high-resolution numerical simulations. We find
that for a Milky-Way type halo, if only a dozen satellite galaxies are
observed, then they can lie on a ``great'' disk with an rms height of about 40
kpc. The normal to the plane is roughly isotropic on the sky. These results are
consistent with the observed properties of the satellite galaxies in the Milky
Way. If, however, the satellite galaxies follow the distribution of
substructure selected by present mass, then great disks similar to the one in
the Milky Way are rare and difficult to reproduce, in agreement with the
conclusion reached by Kroupa et al. (2004).Comment: Major revised, new figure and text added, to appear in A&
The Robustness of Dark Matter Density Profiles in Dissipationless Mergers
We present a comprehensive series of dissipationless N-body simulations to
investigate the evolution of density distribution in equal-mass mergers between
dark matter (DM) halos and multicomponent galaxies. The DM halo models are
constructed with various asymptotic power-law indices ranging from steep cusps
to core-like profiles and the structural properties of the galaxy models are
motivated by the LCDM paradigm of structure formation. The adopted force
resolution allows robust density profile estimates in the inner ~1% of the
virial radii of the simulated systems. We demonstrate that the central slopes
and overall shapes of the remnant density profiles are virtually identical to
those of the initial systems suggesting that the remnants retain a remarkable
memory of the density structure of their progenitors, despite the relaxation
that accompanies merger activity. We also find that halo concentrations remain
approximately constant through hierarchical merging involving identical systems
and show that remnants contain significant fractions of their bound mass well
beyond their formal virial radii. These conclusions hold for a wide variety of
initial asymptotic density slopes, orbital energies, and encounter
configurations, including sequences of consecutive merger events, simultaneous
mergers of severals ystems, and mergers of halos with embedded cold baryonic
components in the form of disks, spheroids, or both. As an immediate
consequence, the net effect of gas cooling, which contracts and steepens the
inner density profiles of DM halos, should be preserved through a period of
dissipationless major merging. Our results imply that the characteristic
universal shape of DM density profiles may be set early in the evolution of
halos.Comment: Accepted for publication in ApJ, 20 pages, 10 figures, LaTeX (uses
emulateapj.cls
The impact of baryon physics on the structure of high-redshift galaxies
We study the detailed structure of galaxies at redshifts z > 2 using
cosmological simulations with improved modeling of the interstellar medium and
star formation. The simulations follow the formation and dissociation of
molecular hydrogen, and include star formation only in cold molecular gas. The
molecular gas is more concentrated towards the center of galaxies than the
atomic gas, and as a consequence, the resulting stellar distribution is very
compact. For halos with total mass above 10^{11} Mo, the median half-mass
radius of the stellar disks is 0.8 kpc at z = 3. The vertical structure of the
molecular disk is much thinner than that of the atomic neutral gas. Relative to
the non-radiative run, the inner regions of the dark matter halo change shape
from prolate to mildly oblate and align with the stellar disk. However, we do
not find evidence for a significant dark disk of dark matter around the stellar
disk. The outer halo regions retain the orientation acquired during accretion
and mergers, and are significantly misaligned with the inner regions. The
radial profile of the dark matter halo contracts in response to baryon
dissipation, establishing an approximately isothermal profile throughout most
of the halo. This effect can be accurately described by a modified model of
halo contraction. The angular momentum of a fixed amount of inner dark matter
is approximately conserved over time, while in the dissipationless case most of
it is transferred outward during mergers. The conservation of the dark matter
angular momentum provides supporting evidence for the validity of the halo
contraction model in a hierarchical galaxy formation process.Comment: 17 pages, 18 figures, submitted to Ap
The sizes of mini-voids in the local universe: an argument in favor of a warm dark matter model?
Using high-resolution simulations within the Cold and Warm Dark Matter models
we study the evolution of small scale structure in the Local Volume, a sphere
of 8 Mpc radius around the Local Group. We compare the observed spectrum of
mini-voids in the Local Volume with the spectrum of mini-voids determined from
the simulations. We show that the \LWDM model can easily explain both the
observed spectrum of mini-voids and the presence of low-mass galaxies observed
in the Local Volume, provided that all haloes with circular velocities greater
than 20 km/s host galaxies. On the contrary within the LCDM model the
distribution of the simulated mini-voids reflects the observed one if haloes
with maximal circular velocities larger than 35 km/s host galaxies. This
assumption is in contradiction with observations of galaxies with circular
velocities as low as 20 km/s in our Local Universe. A potential problem of the
LWDM model could be the late formation of the haloes in which the gas can be
efficiently photo-evaporated. Thus star formation is suppressed and low-mass
haloes might not host any galaxy at all.Comment: 13 pages, 10 figures, version 2, subsection 3.1 added, accepted to
MNRA
Dark Matter Direct Detection with Non-Maxwellian Velocity Structure
The velocity distribution function of dark matter particles is expected to
show significant departures from a Maxwell-Boltzmann distribution. This can
have profound effects on the predicted dark matter - nucleon scattering rates
in direct detection experiments, especially for dark matter models in which the
scattering is sensitive to the high velocity tail of the distribution, such as
inelastic dark matter (iDM) or light (few GeV) dark matter (LDM), and for
experiments that require high energy recoil events, such as many directionally
sensitive experiments. Here we determine the velocity distribution functions
from two of the highest resolution numerical simulations of Galactic dark
matter structure (Via Lactea II and GHALO), and study the effects for these
scenarios. For directional detection, we find that the observed departures from
Maxwell-Boltzmann increase the contrast of the signal and change the typical
direction of incoming DM particles. For iDM, the expected signals at direct
detection experiments are changed dramatically: the annual modulation can be
enhanced by more than a factor two, and the relative rates of DAMA compared to
CDMS can change by an order of magnitude, while those compared to CRESST can
change by a factor of two. The spectrum of the signal can also change
dramatically, with many features arising due to substructure. For LDM the
spectral effects are smaller, but changes do arise that improve the
compatibility with existing experiments. We find that the phase of the
modulation can depend upon energy, which would help discriminate against
background should it be found.Comment: 34 pages, 16 figures, submitted to JCAP. Tables of g(v_min), the
integral of f(v)/v from v_min to infinity, derived from our simulations, are
available for download at http://astro.berkeley.edu/~mqk/dmdd
Prospects for CDM sub-halo detection using high angular resolution observations
In the CDM scenario, dark matter halos are assembled hierarchically from
smaller subunits. A long-standing problem with this picture is that the number
of sub-halos predicted by CDM simulations is orders of magnitudes higher than
the known number of satellite galaxies in the vicinity of the Milky Way. A
plausible way out of this problem could be that the majority of these sub-halos
somehow have so far evaded detection. If such "dark galaxies" do indeed exist,
gravitational lensing may offer one of the most promising ways to detect them.
Dark matter sub-halos in the 1e6 - 1e10 solar mass range should cause strong
gravitational lensing on (sub)milliarcsecond scales. We study the feasibility
of a strong lensing detection of dark sub-halos by deriving the image
separations expected for density profiles favoured by recent simulations and
comparing these to the angular resolution of both existing and upcoming
observational facilities. We find that there is a reasonable probability to
detect sub-halo lensing effects in high resolution observations at radio
wavelengths, such as produced by the upcoming VSOP-2 satellite, and thereby
test the existence of dark galaxies.Comment: 9 pages, 5 figures, Proceedings for "The Universe under the
Microscope" (AHAR 2008), held in Bad Honnef (Germany) in April 2008, to be
published in Journal of Physics: Conference Series by Institute of Physics
Publishing, R. Schoedel, A. Eckart, S. Pfalzner, and E. Ros (eds.
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