28 research outputs found
The evolution of dark matter substructure
This thesis investigates the dynamical evolution of systems orbiting within deeper potentials. Initially we use a simple satellite-halo interaction to study the dynamical processes that act on orbiting systems and we compare these results to analytical theory. Deep images of the Centaurus cluster reveal a spectacular arc of diffuse light that stretches for over 100 kpc and yet is just a few kpc wide. We use numerical simulations to show that this feature can be produced by the tidal debris of a spiral galaxy that has been disrupted by the potential of one of the central cD galaxies of the cluster. The evolution of sub-halos is then studied in a cosmological context using high resolution N-body simulations of galactic mass halos that form in a cold dark matter (CDM) simulation. CDM halos form via a complex series of mergers, accretion events and violent relaxation. Halos are non-spherical, have steep singular density profiles and contain many thousands of surviving dark matter substructure clumps. This will lead to several unique signatures for experiments that aim to detect dark matter either indirectly, through particle annihilation, or directly in a laboratory. For the first time it is possible to construct maps of the gamma-ray sky that result from the annihilation of dark matter particles within simulated dark matter halo distributions
Gamma-ray and synchrotron emission from neutralino annihilation in the Large Magellanic Cloud
We calculate the expected flux of gamma-ray and radio emission from the LMC
due to neutralino annihilation. Using rotation curve data to probe the density
profile and assuming a minimum disk, we describe the dark matter halo of the
LMC using models predicted by N-body simulations. We consider a range of
density profiles including the NFW profile, a modified NFW profile proposed by
Hayashi et al.(2003) to account for the effects of tidal stripping, and an
isothermal sphere with a core. We find that the gamma-ray flux expected from
these models may be detectable by GLAST for a significant part of the
neutralino parameter space. The prospects for existing and upcoming Atmospheric
Cherenkov Telescopes are less optimistic, as unrealistically long exposures are
required for detection. However, the effects of adiabatic compression due to
the baryonic component may improve the chances for detection by ACTs. The
maximum flux we predict is well below EGRET's measurements and thus EGRET does
not constrain the parameter space. The expected synchrotron emission generally
lies below the observed radio emission from the LMC in the frequency range of
19.7 to 8550 MHz. As long as <2x 10^-26 cm^3 s^-1 for a neutralino
mass of 50 GeV, the observed radio emission is not primarily due to neutralinos
and is consistent with the assumption that the main source is cosmic rays. We
find that the predicted fluxes, obtained by integrating over the entire LMC,
are not very strongly dependent on the inner slope of the halo profile, varying
by less than an order of magnitude for the range of profiles we considered.Comment: 24 pages, 5 figures; detailed discussion of how the neutralino
induced signals compare with the cosmic-ray induced ones was added. Main
conclusions unchanged. Matches accepted version, to appear in Astroparticle
Physic
A large HI cloud near the centre of the Virgo cluster
We report the discovery of a large HI cloud in the central regions of the
Virgo cluster. It is 110 x 25 kpc in size and contains 3.4 x 10^8 Msol of HI.
The morphology and kinematics of this cloud strongly suggest that it consists
of HI removed from the galaxy NGC 4388 by ram-pressure stripping. It is more
likely the result of an interaction of the ISM of NGC 4388 with the hot halo of
the M86 group and not with the ICM centred on M87. The large extent of the
plume suggests that gas stripped from cluster galaxies can remain neutral for
at least 10^8 yr. Locally, the column density is well above 10^20 cm^-2,
suggesting that the intra-cluster HII regions known to exist in Virgo may have
formed from gas stripped from cluster galaxies. The existence of the HI plume
suggests that stripping of infalling spirals contributes to the enrichment of
the ICM. The HI object in the Virgo cluster recently reported by Minchin et al.
may have a similar origin and may therefore not be a ``dark galaxy''.Comment: Accepted for publication in A&A. 5 pages, 2 figures. Version with
high-resolution figures at http://www.astron.nl/~oosterlo/n438
Diffuse light and building history of the galaxy cluster Abell 2667
We have searched for diffuse intracluster light in the galaxy cluster Abell
2667 (z=0.233) from HST images in three filters. We have applied to these
images an iterative multi-scale wavelet analysis and reconstruction technique,
which allows to subtract stars and galaxies from the original images. We detect
a zone of diffuse emission south west of the cluster center (DS1), and a second
faint object (ComDif), within DS1. Another diffuse source (DS2) may be
detected, at lower confidence level, north east of the center. These sources of
diffuse light contribute to 10-15% of the total visible light in the cluster.
Whether they are independent entities or are part of the very elliptical
external envelope of the central galaxy remains unclear. VLT VIMOS integral
field spectroscopy reveals a faint continuum at the positions of DS1 and ComDif
but do not allow to compute a redshift. A hierarchical substructure detection
method reveals the presence of several galaxy pairs and groups defining a
similar direction as the one drawn by the DS1-central galaxy-DS2 axis. The
analysis of archive XMM-Newton and Chandra observations shows X-ray emission
elongated in the same direction. The X-ray temperature map shows the presence
of a cool core, a broad cool zone stretching from north to south and hotter
regions towards the north east, south west and north west. This possibly
suggests shock fronts along these directions produced by infalling material.
These various data are consistent with a picture in which diffuse sources are
concentrations of tidal debris and harassed matter expelled from infalling
galaxies by tidal stripping and undergoing an accretion process onto the
central cluster galaxy; as such, they are expected to be found along the main
infall directions.Comment: Accepted for publication in Astronomy and Astrophysic
Neutralino Annihilation at the Galactic Center Revisited
The annihilation of neutralino dark matter in the Galactic Center (GC) may
result in radio signals that can be used to detect or constrain the dark matter
halo density profile or dark matter particle properties. At the Galactic
Center, the accretion flow onto the central Black Hole (BH) sustains strong
magnetic fields that can induce synchrotron emission by electrons and positrons
generated in neutralino annihilations during advection onto the BH. Here we
reanalyze the radiative processes relevant for the neutralino annihilation
signal at the GC, with realistic assumptions about the accretion flow and its
magnetic properties. We find that neglecting these effects, as done in previous
papers, leads to the incorrent electron and photon spectra. We find that the
magnetic fields associated with the flow are significantly stronger than
previously estimated. We derive the appropriate equilibrium distribution of
electrons and positron and the resulting radiation, considering adiabatic
compression in the accretion flow, inverse Compton scattering off synchrotron
photons (synchrotron self-Compton scattering), and synchrotron self-absorption
of the emitted radiation. We derive the signal for a Navarro-Frenk-White (NFW)
dark matter halo profile and a NFW profile with a dark matter spike due to the
central BH. We find that the observed radio emission from the GC is
inconsistent with the scenario in which a spiky distribution of neutralinos is
present. We discuss several important differences between our calculations and
those previously presented in the literature.Comment: 19 pages, 11 eps figures, version accepted for publication in JCA
Cusps in CDM halos
We resolve the inner region of a massive cluster forming in a cosmological
LCDM simulation with a mass resolution of 2*10^6 Msun and before z=4.4 even
3*10^5 Msun. This is a billion times less than the clusters final virial mass
and a substantial increase over current LCDM simulations. We achieve this
resolution using a new multi-mass refinement procedure and are now able to
probe a dark matter halo density profile down to 0.1 percent of the virial
radius. The inner density profile of this cluster halo is well fitted by a
power-law rho ~ r^-gamma down to the smallest resolved scale. An inner region
with roughly constant logarithmic slope is now resolved, which suggests that
cuspy profiles describe the inner profile better than recently proposed
profiles with a core. The cluster studied here is one out of a sample of six
high resolution cluster simulations of Diemand et al. (2004) and it's inner
slope of gamma = 1.2 lies close to the sample average.Comment: 10 pages,10 figures. Matches version in press. Added Figure 7 and
section 3.3. about upper limits of inner slopes, text (incl, title and
abstract) revised, conclusions unchange
Large scale diffuse light in the Coma cluster: a multi-scale approach
We have obtained wide field images of the Coma cluster in the B, V, R and I
bands with the CFH12K camera at CFHT. In order to search for large scale
diffuse emission, we have applied to these images an iterative multi scale
wavelet analysis and reconstruction technique which allowed to model all the
sources (stars and galaxies) and subtract them from the original images. We
found various concentrations of diffuse emission present in the central zone
around the central galaxies NGC4874 and NGC4889. We characterize the positions,
sizes and colors of these concentrations. Some sources do not seem to have
strong star formation, while another one probably exhibits spiral-like color.
One possible origin for the star forming diffuse emission sources is that in
the region of the two main galaxies NGC4874 and NGC4889 spiral galaxies have
recently been disrupted and star formation is still active in the dispersed
material. We also use the characteristics of the sources of diffuse emission to
trace the cluster dynamics. A scenario in which the group around NGC 4874 is
moving north is consistent with our data.Comment: 11 pages, accepted in A&A, jpg figure
The effect of dwarf galaxies disruption in semi-analytic models
We present results for a galaxy formation model that includes a simple
treatment for the disruption of dwarf galaxies by gravitational forces and
galaxy encounters within galaxy clusters. This is implemented a posteriori in a
semi-analytic model by considering the stability of cluster dark matter
sub-haloes at z=0. We assume that a galaxy whose dark matter substructure has
been disrupted will itself disperse, while its stars become part of the
population of intracluster stars responsible for the observed intracluster
light. Despite the simplicity of this assumption, our results show a
substantial improvement over previous models and indicate that the inclusion of
galaxy disruption is indeed a necessary ingredient of galaxy formation models.
We find that galaxy disruption suppresses the number density of dwarf galaxies
by about a factor of two. This makes the slope of the faint end of the galaxy
luminosity function shallower, in agreement with observations. In particular,
the abundance of faint, red galaxies is strongly suppressed. As a result, the
luminosity function of red galaxies and the distinction between the red and the
blue galaxy populations in colour-magnitude relationships are correctly
predicted. Finally, we estimate a fraction of intracluster light comparable to
that found in clusters of galaxies.Comment: 7 pages, 6 figures, accepted for publication in MNRAS, 2 figures
changed and references adde
Convergence and scatter of cluster density profiles
We present new results from a series of LCDM simulations of cluster mass
halos resolved with high force and mass resolution. These results are compared
with recently published simulations from groups using various codes including
PKDGRAV, ART, TPM, GRAPE and GADGET. Careful resolution tests show that with 25
million particles within the high resolution region we can resolve to about
0.3% of the virial radius and that convergence in radius is proportional to the
mean interparticle separation. The density profiles of 26 high resolution
clusters obtained with the different codes and from different initial
conditions agree very well. The average logarithmic slope at one percent of the
virial radius is with a scatter of . Over the entire
resolved regions the density profiles are well fitted by a smooth function that
asymptotes to a central cusp , where we find
from the mean of the fits to our six highest resolution
clusters.Comment: MNRAS accepted version. Due to an error in the initial conditions
these simulations have a lower sigma_8 than the published value, 0.7 instead
of 0.9. We thank Mike Kuhlen who helped us finding this mistake. See the
erratum at http://www-theorie.physik.unizh.ch/~diemand/proerr.pdf . Images
and movies available at http://www-theorie.physik.unizh.ch/~diemand/clusters
Bayesian Strong Gravitational-Lens Modeling on Adaptive Grids: Objective Detection of Mass Substructure in Galaxies
We introduce a new adaptive and fully Bayesian grid-based method to model
strong gravitational lenses with extended images. The primary goal of this
method is to quantify the level of luminous and dark-mass substructure in
massive galaxies, through their effect on highly-magnified arcs and Einstein
rings. The method is adaptive on the source plane, where a Delaunay
tessellation is defined according to the lens mapping of a regular grid onto
the source plane. The Bayesian penalty function allows us to recover the best
non-linear potential-model parameters and/or a grid-based potential correction
and to objectively quantify the level of regularization for both the source and
the potential. In addition, we implement a Nested-Sampling technique to
quantify the errors on all non-linear mass model parameters -- ... -- and allow
an objective ranking of different potential models in terms of the marginalized
evidence. In particular, we are interested in comparing very smooth lens mass
models with ones that contain mass-substructures. The algorithm has been tested
on a range of simulated data sets, created from a model of a realistic lens
system. One of the lens systems is characterized by a smooth potential with a
power-law density profile, twelve include a NFW dark-matter substructure of
different masses and at different positions and one contains two NFW dark
substructures with the same mass but with different positions. Reconstruction
of the source and of the lens potential for all of these systems shows the
method is able, in a realistic scenario, to identify perturbations with masses
>=10^7 solar mass when located on the Einstein ring. For positions both inside
and outside of the ring, masses of at least 10^9 solar mass are required (...).Comment: 21 pages, 15 figures, 4 tables; accepted for publication in MNRA