51 research outputs found
From cusps to cores: a stochastic model
The cold dark matter model of structure formation faces apparent problems on
galactic scales. Several threads point to excessive halo concentration,
including central densities that rise too steeply with decreasing radius. Yet,
random fluctuations in the gaseous component can 'heat' the centres of haloes,
decreasing their densities. We present a theoretical model deriving this effect
from first principles: stochastic variations in the gas density are converted
into potential fluctuations that act on the dark matter; the associated force
correlation function is calculated and the corresponding stochastic equation
solved. Assuming a power law spectrum of fluctuations with maximal and minimal
cutoff scales, we derive the velocity dispersion imparted to the halo particles
and the relevant relaxation time. We further perform numerical simulations,
with fluctuations realised as a Gaussian random field, which confirm the
formation of a core within a timescale comparable to that derived analytically.
Non-radial collective modes enhance the energy transport process that erases
the cusp, though the parametrisations of the analytical model persist.
In our model, the dominant contribution to the dynamical coupling driving the
cusp-core transformation comes from the largest scale fluctuations. Yet, the
efficiency of the transformation is independent of the value of the largest
scale and depends weakly (linearly) on the power law exponent; it effectively
depends on two parameters: the gas mass fraction and the normalisation of the
power spectrum. This suggests that cusp-core transformations observed in
hydrodynamic simulations of galaxy formation may be understood and parametrised
in simple terms, the physical and numerical complexities of the various
implementations notwithstanding.Comment: Minor revisions to match version to appear in MNRAS; Section~2.3
largely rewritten for clarit
Reproducing the Stellar Mass/Halo Mass Relation in Simulated LCDM Galaxies: Theory vs Observational Estimates
We examine the present-day total stellar-to-halo mass (SHM) ratio as a
function of halo mass for a new sample of simulated field galaxies using fully
cosmological, LCDM, high resolution SPH + N-Body simulations.These simulations
include an explicit treatment of metal line cooling, dust and self-shielding,
H2 based star formation and supernova driven gas outflows. The 18 simulated
halos have masses ranging from a few times 10^8 to nearly 10^12 solar masses.
At z=0 our simulated galaxies have a baryon content and morphology typical of
field galaxies. Over a stellar mass range of 2.2 x 10^3 to 4.5 x 10^10 solar
masses, we find extremely good agreement between the SHM ratio in simulations
and the present-day predictions from the statistical Abundance Matching
Technique presented in Moster et al. (2012). This improvement over past
simulations is due to a number systematic factors, each decreasing the SHM
ratios: 1) gas outflows that reduce the overall SF efficiency but allow for the
formation of a cold gas component 2) estimating the stellar masses of simulated
galaxies using artificial observations and photometric techniques similar to
those used in observations and 3) accounting for a systematic, up to 30 percent
overestimate in total halo masses in DM-only simulations, due to the neglect of
baryon loss over cosmic times. Our analysis suggests that stellar mass
estimates based on photometric magnitudes can underestimate the contribution of
old stellar populations to the total stellar mass, leading to stellar mass
errors of up to 50 percent for individual galaxies. These results highlight the
importance of using proper techniques to compare simulations with observations
and reduce the perceived tension between the star formation efficiency in
galaxy formation models and in real galaxies.Comment: Submitted to ApJ 9 pages, 5 figure
High-resolution mass models of dwarf galaxies from LITTLE THINGS
We present high-resolution rotation curves and mass models of 26 dwarf galaxies from LITTLE THINGS. LITTLE THINGS is a high-resolution Very Large Array HI survey for nearby dwarf galaxies in the local volume within 11 Mpc. The rotation curves of the sample galaxies derived in a homogeneous and consistent manner are combined with Spitzer archival 3.6 micron and ancillary optical U, B, and V images to construct mass models of the galaxies. We decompose the rotation curves in terms of the dynamical contributions by baryons and dark matter halos, and compare the latter with those of dwarf galaxies from THINGS as well as Lambda CDM SPH simulations in which the effect of baryonic feedback processes is included. Being generally consistent with THINGS and simulated dwarf galaxies, most of the LITTLE THINGS sample galaxies show a linear increase of the rotation curve in their inner regions, which gives shallower logarithmic inner slopes alpha of their dark matter density profiles. The mean value of the slopes of the 26 LITTLE THINGS dwarf galaxies is alpha =-0.32 +/- 0.24 which is in accordance with the previous results found for low surface brightness galaxies (alpha = -0.2 +/- 0.2) as well as the seven THINGS dwarf galaxies (alpha =-0.29 +/- 0.07). However, this significantly deviates from the cusp-like dark matter distribution predicted by dark-matter-only Lambda CDM simulations. Instead our results are more in line with the shallower slopes found in the Lambda CDM SPH simulations of dwarf galaxies in which the effect of baryonic feedback processes is included. In addition, we discuss the central dark matter distribution of DDO 210 whose stellar mass is relatively low in our sample to examine the scenario of inefficient supernova feedback in low mass dwarf galaxies predicted from recent Lambda SPH simulations of dwarf galaxies where central cusps still remain.Peer reviewe
In-spiraling Clumps in Blue Compact Dwarf Galaxies
Giant star-formation clumps in dwarf irregular galaxies can have masses
exceeding a few percent of the galaxy mass enclosed inside their orbital radii.
They can produce sufficient torques on dark matter halo particles, halo stars,
and the surrounding disk to lose their angular momentum and spiral into the
central region in 1 Gyr. Pairs of giant clumps with similarly large relative
masses can interact and exchange angular momentum to the same degree. The
result of this angular momentum loss is a growing central concentration of old
stars, gas, and star formation that can produce a long-lived starburst in the
inner region, identified with the BCD phase. This central concentration is
proposed to be analogous to the bulge in a young spiral galaxy. Observations of
star complexes in five local BCDs confirm the relatively large clump masses
that are expected for this process. The observed clumps also seem to contain
old field stars, even after background light subtraction, in which case the
clumps may be long-lived. The two examples with clumps closest to the center
have the largest relative clump masses and the greatest contributions from old
stars. An additional indication that the dense central regions of BCDs are like
bulges is the high ratio of the inner disk scale height to the scale length,
which is comparable to 1 for four of the galaxies.Comment: 15 pages, 2 figures, accepted by ApJ 1/5/201
Ductal carcinoma in situ and sentinel lymph node metastasis in breast cancer
<p>Abstract</p> <p>Background</p> <p>The impact of sentinel lymph node biopsy on breast cancer mimicking ductal carcinoma in situ (DCIS) is a matter of debate.</p> <p>Methods</p> <p>We studied the rate of occurrence of sentinel lymph node metastasis in 255 breast cancer patients with pure DCIS showing no invasive components on routine pathological examination. We compared this to the rate of occurrence in 177 patients with predominant intraductal-component (IDC) breast cancers containing invasive foci equal to or less than 0.5 cm in size.</p> <p>Results</p> <p>Most of the clinical and pathological baseline characteristics were the same between the two groups. However, peritumoral lymphatic permeation occurred less often in the pure DCIS group than in the IDC-predominant invasive-lesion group (1.2% vs. 6.8%, p = 0.002). One patient (0.39%) with pure DCIS had two sentinel lymph nodes positive for metastasis. This rate was significantly lower than that in patients with IDC-predominant invasive lesions (6.2%; p < 0.001).</p> <p>Conclusions</p> <p>Because the rate of sentinel lymph node metastasis in pure DCIS is very low, sentinel lymph node biopsy can safely be omitted.</p
Inducible nitric oxide synthase expression in gastric adenocarcinoma: impact on lymphangiogenesis and lymphatic metastasis
Constraints and consequences of reducing small scale structure via large dark matter-neutrino interactions
Etude et realisation d'un detecteur a avalanche a plaques paralleles destine a des mesures de temps de vol et de localisation
SIGLET 55078 / INIST-CNRS - Institut de l'Information Scientifique et TechniqueFRFranc
The connection between the cusp-to-core transformation and observational universalities of DM haloes
Observations have revealed interesting universal properties of dark matter
(DM) halos especially around low-mass galaxies. Strigari et al. (2008) showed
that DM halos have common enclosed masses within 300pc (Strigari relation).
Kormendy & Freeman (2004) reported DM halos having almost identical central
surface densities (the relation). In addition, there exists a
core-cusp problem, a discrepancy of the central density distribution between
simulated halos and observations. We investigate whether a scenario where cuspy
halos transform into cores by some dynamical processes can also explain their
universal structural properties. It is shown that a cusp-to-core transformation
model naturally reproduces the relation and that Strigari
relation follows from the relation for dwarf galaxies. We also
show that the central densities of cored dark halos provide valuable
information about their formation redshifts.Comment: 5 pages, 3 figures, accepted for publication in MNRAS Letter
On the tidal formation of dark matter-deficient galaxies
Previous studies have shown that dark matter-deficient galaxies (DMDG) such as NGC 1052-DF2 (hereafter DF2) can result from tidal stripping. An important question, though, is whether such a stripping scenario can explain DF2’s large specific frequency of globular clusters (GCs). After all, tidal stripping and shocking preferentially remove matter from the outskirts. We examine this using idealized, high-resolution simulations of a regular dark matter-dominated galaxy that is accreted on to a massive halo. As long as the initial (pre-infall) dark matter halo of the satellite is cored, which is consistent with predictions of cosmological, hydrodynamical simulations, the tidal remnant can be made to resemble DF2 in all its properties, including its GC population. The required orbit has a pericentre at the 8.3 percentile of the distribution for subhaloes at infall, and thus is not particularly extreme. On this orbit the satellite loses 98.5 (30) per cent of its original dark matter (stellar) mass, and thus evolves into a DMDG. The fraction of GCs that is stripped off depends on the initial radial distribution. If, at infall, the median projected radius of the GC population is roughly two times that of the stars, consistent with observations of isolated galaxies, only ∼20 per cent of the GCs are stripped off. This is less than for the stars, which is due to dynamical friction counteracting the tidal stirring. We predict that, if indeed DF2 was crafted by strong tides, its stellar outskirts should have a very shallow metallicity gradient
- …