46 research outputs found
Investigating the retention of intermediate-mass black holes in star clusters using N-body simulations
Contrary to supermassive and stellar-mass black holes (SBHs), the existence
of intermediate-mass black holes (IMBHs) with masses ranging between 10^{2-5}
Msun has not yet been confirmed. The main problem in the detection is that the
innermost stellar kinematics of globular clusters (GCs) or small galaxies, the
possible natural loci to IMBHs, are very difficult to resolve. However, if
IMBHs reside in the centre of GCs, a possibility is that they interact
dynamically with their environment. A binary formed with the IMBH and a compact
object of the GC would naturally lead to a prominent source of gravitational
radiation, detectable with future observatories. We use N-body simulations to
study the evolution of GCs containing an IMBH and calculate the gravitational
radiation emitted from dynamically formed IMBH-SBH binaries and the possibility
that the IMBH escapes the GC after an IMBH-SBH merger. We run for the first
time direct-summation integrations of GCs with an IMBH including the dynamical
evolution of the IMBH with the stellar system and relativistic effects, such as
energy loss in gravitational waves (GWs) and periapsis shift, and gravitational
recoil. We find in one of our models an intermediate mass-ratio inspiral
(IMRI), which leads to a merger with a recoiling velocity higher than the
escape velocity of the GC. The GWs emitted fall in the range of frequencies
that a LISA-like observatory could detect, like the European eLISA or in
mission options considered in the recent preliminary mission study conducted in
China. The merger has an impact on the global dynamics of the cluster, as an
important heating source is removed when the merged system leaves the GC. The
detection of one IMRI would constitute a test of GR, as well as an irrefutable
proof of the existence of IMBHs.Comment: Accepted for publication by A&A, minor modification
Evaluation of the Parasight Platform for Malaria Diagnosis
The World Health Organization estimates that nearly 500 million malaria tests are performed annually. While microscopy and rapid diagnostic tests (RDTs) are the main diagnostic approaches, no single method is inexpensive, rapid, and highly accurate. Two recent studies from our group have demonstrated a prototype computer vision platform that meets those needs. Here we present the results from two clinical studies on the commercially available version of this technology, the Sight Diagnostics Parasight platform, which provides malaria diagnosis, species identification, and parasite quantification. We conducted a multisite trial in Chennai, India (Apollo Hospital [n = 205]), and Nairobi, Kenya (Aga Khan University Hospital [n = 263]), in which we compared the device to microscopy, RDTs, and PCR. For identification of malaria, the device performed similarly well in both contexts (sensitivity of 99% and specificity of 100% at the Indian site and sensitivity of 99.3% and specificity of 98.9% at the Kenyan site, compared to PCR). For species identification, the device correctly identified 100% of samples with Plasmodium vivax and 100% of samples with Plasmodium falciparum in India and 100% of samples with P. vivax and 96.1% of samples with P. falciparum in Kenya, compared to PCR. Lastly, comparisons of the device parasite counts with those of trained microscopists produced average Pearson correlation coefficients of 0.84 at the Indian site and 0.85 at the Kenyan site
Unlocking the secrets of stellar haloes using combined star counts and surface photometry
The stellar haloes of galaxies can currently be studied either through
observations of resolved halo stars or through surface photometry. Curiously,
the two methods appear to give conflicting results, as a number of surface
photometry measurements have revealed integrated colours that are too red to be
reconciled with the halo properties inferred from the study of resolved stars.
Several explanations for this anomaly have been proposed - including dust
photoluminescence, extinction of extragalactic background light and a
bottom-heavy stellar initial mass function. A decisive test is, however, still
lacking. Here, we explain how observations of the halo of a nearby galaxy,
involving a combination of both surface photometry and bright star counts, can
be used to distinguish between the proposed explanations. We derive the
observational requirements for this endeavour and find that star counts in
filters VI and surface photometry in filters VIJ appears to be the optimal
strategy. Since the required halo star counts are already available for many
nearby galaxies, the most challenging part of this test is likely to be the
optical surface photometry, which requires several nights of exposure time on a
4-8 m telescope, and the near-IR surface photometry, which is most readily
carried out using the upcoming James Webb Space Telescope.Comment: 14 pages, 4 figures; v.2 matches published version (minor changes
only
Age and metallicity gradients in early-type galaxies: A dwarf to giant sequence
We studied the stellar populations of 40 early-type galaxies using medium
resolution long-slit spectroscopy along their major axes (and along the minor
axis for two of them), from 10^7 Msol to 10^12 Msol (-9.2 > M_B > -22.4 mag).
All the studied galaxies lie on the mass-metallicity and age-mass relations.
The transition type dwarfs deviate from the latter relation having younger mean
age, and the low-mass dwarf spheroidals have older ages, marking a
discontinuity in the relation, possibly due to selection effects.
In all mass regimes, the mean metallicity gradients are approximately -0.2
and the mean age gradients +0.1 dex per decade of radius. The individual
gradients are widely spread: and . We do not find evidence for a correlation
between the metallicity gradient and luminosity, velocity dispersion, central
age or age gradient. Likewise, we do not find a correlation between the age
gradient and any other parameter in bright early-type galaxies. In faint
early-types with mag, on the other hand, we find a
correlation between the age gradient and luminosity: the age gradient becomes
more positive for fainter galaxies.
We conclude that various physical mechanisms can lead to similar gradients
and that these gradients are robust against the environmental effects. In
particular, the gradients observed in dwarfs galaxies certainly survived the
transformation of the progenitors through tidal harassment or/and ram-pressure
stripping. The diversity of metallicity gradients amongst dwarf elliptical
galaxies may reflect a plurality of progenitors' morphologies. The dwarfs with
steep metallicity gradients could have originated from blue compact dwarfs and
those with flat profiles from dwarf irregulars and late type spirals.
(Abridged)Comment: 31 pages, 16 figures. Accepted for publications in MNRA
The Demography of Super-Massive Black Holes: Growing Monsters at the Heart of Galaxies
Supermassive black holes (BHs) appear to be ubiquitous at the center of all
galaxies which have been observed at high enough sensitivities and resolution
with the Hubble Space Telescope. Their masses are found to be tightly linked
with the masses and velocity dispersions of their host galaxies. On the other
hand, BHs are widely held to constitute the central engines of quasars and
active galactic nuclei (AGN) in general. It is however still unclear how BHs
have grown, and whether they have co-evolved with their hosts. In this Review I
discuss how, in ways independent of specific models, constraints on the growth
history of BHs and their host galaxies have been set by matching the statistics
of local BHs to the emissivity, number density, and clustering properties of
AGNs at different cosmological epochs. I also present some new results obtained
through a novel numerical code which evolves the BH mass function and
clustering adopting broad distributions of Eddington ratios. I finally review
BH evolution in a wider cosmological context, connecting BH growth to galaxy
evolution.Comment: 70 pages. New Astronomy Reviews, in pres
Formation of galaxies in {\Lambda}CDM cosmologies. I. The fine structure of disc galaxies
We present a detailed analysis of the global and fine structure of four
middle-mass disc galaxies obtained from simulations in a CDM scenario.
These objects have photometric D/T ratios in good agreement with those observed
for late-type spirals, as well as kinematic properties in agreement with the
observational Tully-Fisher relation. We identify the different dynamical
components at z=0 on the basis of both orbital parameters and the binding
energy of stars in the galaxy. In this way, we recognize a slowly rotating
centrally concentrated spheroid, and two disc components supported by rotation:
a thin disc with stars in nearly circular orbits, and a thick disc with orbital
parameters transitional between the thin disc and the spheroid. The spheroidal
component is composed mainly by old, metal-poor and {\alpha}-enhanced stars.
The distribution of metals in this component shows, however, a clear bimodality
with a low-metallicity peak, which could be related to a classical bulge, and a
high-metallicity peak, which could be related to a pseudo-bulge. The thin disc
appears in our simulations as the youngest and most metal-rich component. The
radial distribution of ages and colours in this component are U-shaped: the new
stars are forming in the inner regions, and then migrate through secular
processes. Finally, we also find a thick disc containing about 16% of the total
stellar mass and with properties that are intermediate between those of the
thin disc and the spheroid. Its low-metallicity stars are {\alpha}-enhanced
when compared to thin disc stars of the same metallicity. The structural
parameters (e.g., the scale height) of the simulated thick discs suggest that
such a component could result from the combination of different thickening
mechanisms that include merger-driven processes, but also long-lived internal
perturbations of the thin disc. [Abridged]Comment: 23 pages, 16 figures, accepted for publication in MNRAS, references
fixe
A clinical evaluation of an ex vivo organ culture system to predict patient response to cancer therapy
IntroductionEx vivo organ cultures (EVOC) were recently optimized to sustain cancer tissue for 5 days with its complete microenvironment. We examined the ability of an EVOC platform to predict patient response to cancer therapy.MethodsA multicenter, prospective, single-arm observational trial. Samples were obtained from patients with newly diagnosed bladder cancer who underwent transurethral resection of bladder tumor and from core needle biopsies of patients with metastatic cancer. The tumors were cut into 250 μM slices and cultured within 24 h, then incubated for 96 h with vehicle or intended to treat drug. The cultures were then fixed and stained to analyze their morphology and cell viability. Each EVOC was given a score based on cell viability, level of damage, and Ki67 proliferation, and the scores were correlated with the patients’ clinical response assessed by pathology or Response Evaluation Criteria in Solid Tumors (RECIST).ResultsThe cancer tissue and microenvironment, including endothelial and immune cells, were preserved at high viability with continued cell division for 5 days, demonstrating active cell signaling dynamics. A total of 34 cancer samples were tested by the platform and were correlated with clinical results. A higher EVOC score was correlated with better clinical response. The EVOC system showed a predictive specificity of 77.7% (7/9, 95% CI 0.4–0.97) and a sensitivity of 96% (24/25, 95% CI 0.80–0.99).ConclusionEVOC cultured for 5 days showed high sensitivity and specificity for predicting clinical response to therapy among patients with muscle-invasive bladder cancer and other solid tumors
Light-front holographic QCD and emerging confinement
In this report we explore the remarkable connections between light-front dynamics, its holographic mapping to gravity in a higher-dimensional anti-de Sitter (AdS) space, and conformal quantum mechanics. This approach provides new insights into the origin of a fundamental mass scale and the physics underlying confinement dynamics in QCD in the limit of massless quarks. The result is a relativistic light-front wave equation for arbitrary spin with an effective confinement potential derived from a conformal action and its embedding in AdS space. This equation allows for the computation of essential features of hadron spectra in terms of a single scale. The light-front holographic methods described here give a precise interpretation of holographic variables and quantities in AdS space in terms of light-front variables and quantum numbers. This leads to a relation between the AdS wave functions and the boost-invariant light-front wave functions describing the internal structure of hadronic bound-states in physical space-time. The pion is massless in the chiral limit and the excitation spectra of relativistic light-quark meson and baryon bound states lie on linear Regge trajectories with identical slopes in the radial and orbital quantum numbers. In the light-front holographic approach described here currents are expressed as an infinite sum of poles, and form factors as a product of poles. At large q(2) the form factor incorporates the correct power-law fall-off for hard scattering independent of the specific dynamics and is dictated by the twist. At low q2 the form factor leads to vector dominance. The approach is also extended to include small quark masses. We briefly review in this report other holographic approaches to QCD, in particular top-down and bottom-up models based on chiral symmetry breaking. We also include a discussion of open problems and future applications. (C)) 2015 Elsevier B.V. All rights reserved
Galaxy bulges and their massive black holes: a review
With references to both key and oft-forgotten pioneering works, this article
starts by presenting a review into how we came to believe in the existence of
massive black holes at the centres of galaxies. It then presents the historical
development of the near-linear (black hole)-(host spheroid) mass relation,
before explaining why this has recently been dramatically revised. Past
disagreement over the slope of the (black hole)-(velocity dispersion) relation
is also explained, and the discovery of sub-structure within the (black
hole)-(velocity dispersion) diagram is discussed. As the search for the
fundamental connection between massive black holes and their host galaxies
continues, the competing array of additional black hole mass scaling relations
for samples of predominantly inactive galaxies are presented.Comment: Invited (15 Feb. 2014) review article (submitted 16 Nov. 2014). 590
references, 9 figures, 25 pages in emulateApJ format. To appear in "Galactic
Bulges", E. Laurikainen, R.F. Peletier, and D.A. Gadotti (eds.), Springer
Publishin
Erratum: Global, regional, and national comparative risk assessment of 84 behavioural, environmental and occupational, and metabolic risks or clusters of risks for 195 countries and territories, 1990–2017: a systematic analysis for the Global Burden of Disease Study 2017
Interpretation: By quantifying levels and trends in exposures to risk factors and the resulting disease burden, this assessment offers insight into where past policy and programme efforts might have been successful and highlights current priorities for public health action. Decreases in behavioural, environmental, and occupational risks have largely offset the effects of population growth and ageing, in relation to trends in absolute burden. Conversely, the combination of increasing metabolic risks and population ageing will probably continue to drive the increasing trends in non-communicable diseases at the global level, which presents both a public health challenge and opportunity. We see considerable spatiotemporal heterogeneity in levels of risk exposure and risk-attributable burden. Although levels of development underlie some of this heterogeneity, O/E ratios show risks for which countries are overperforming or underperforming relative to their level of development. As such, these ratios provide a benchmarking tool to help to focus local decision making. Our findings reinforce the importance of both risk exposure monitoring and epidemiological research to assess causal connections between risks and health outcomes, and they highlight the usefulness of the GBD study in synthesising data to draw comprehensive and robust conclusions that help to inform good policy and strategic health planning