More examples of structure formation in the Lemaitre-Tolman model

In continuing our earlier research, we find the formulae needed to determine the arbitrary functions in the Lemaitre-Tolman model when the evolution proceeds from a given initial velocity distribution to a final state that is determined either by a density distribution or by a velocity distribution. In each case the initial and final distributions uniquely determine the L-T model that evolves between them, and the sign of the energy-function is determined by a simple inequality. We also show how the final density profile can be more accurately fitted to observational data than was done in our previous paper. We work out new numerical examples of the evolution: the creation of a galaxy cluster out of different velocity distributions, reflecting the current data on temperature anisotropies of CMB, the creation of the same out of different density distributions, and the creation of a void. The void in its present state is surrounded by a nonsingular wall of high density.Comment: LaTeX 2e with eps figures. 30 pages, 11 figures, 30 figure files. Revision matches published versio

Alkemio: association of chemicals with biomedical topics by text and data mining

The PubMed(R) database of biomedical citations allows the retrieval of scientific articles studying the function of chemicals in biology and medicine. Mining millions of available citations to search reported associations between chemicals and topics of interest would require substantial human time. We have implemented the Alkemio text mining web tool and SOAP web service to help in this task. The tool uses biomedical articles discussing chemicals (including drugs), predicts their relatedness to the query topic with a naïve Bayesian classifier and ranks all chemicals by P-values computed from random simulations. Benchmarks on seven human pathways showed good retrieval performance (areas under the receiver operating characteristic curves ranged from 73.6 to 94.5%). Comparison with existing tools to retrieve chemicals associated to eight diseases showed the higher precision and recall of Alkemio when considering the top 10 candidate chemicals. Alkemio is a high performing web tool ranking chemicals for any biomedical topics and it is free to non-commercial users. Availability: http://cbdm.mdc-berlin.de/∼medlineranker/cms/alkemio

Satellites and haloes of dwarf galaxies

We study the abundance of satellite galaxies as a function of primary stellar mass using the Sloan Digital Sky Survey/Data Release 7 (SDSS/DR7) spectroscopic catalogue. In contrast with previous studies, which focused mainly on bright primaries, our central galaxies span a wide range of stellar mass, 107.5 ⩽ Mpri*/M⊙ ⩽ 1011, from dwarfs to central cluster galaxies. Our analysis confirms that the average number of satellites around bright primaries, when expressed in terms of satellite-to-primary stellar mass ratio (msat*/M*pri), is a strong function of Mpri*. On the other hand, satellite abundance is largely independent of primary mass for dwarf primaries (Mpri* < 1010 M⊙). These results are consistent with galaxy formation models in the Λ cold dark matter (ΛCDM) scenario. We find excellent agreement between SDSS data and semianalytic mock galaxy catalogues constructed from the Millennium-II Simulation. Satellite galaxies trace dark matter substructure in ΛCDM, so satellite abundance reflects the dependence on halo mass, M200, of both substructure and galaxy stellar mass (M*). Since dark matter substructure is almost scale free, the dependence of satellite abundance on primary mass results solely from the well-defined characteristic mass in the galaxy mass-halo mass relation. On dwarf galaxy scales, where models predict a power-law scaling, M*∝M2.5200, similarity is preserved and satellite abundance is independent of primary mass. For primaries brighter than the characteristic mass of the M*–M200 relation, satellite abundance increases strongly with primary mass. Our results provide strong support for the steep, approximately power-law dependence of dwarf galaxy mass on halo mass envisioned in ΛCDM galaxy formation models

Fracturas diafisarias de húmero en adultos: estudio retrospectivo de 53 casos

Se estudian retrospectivamente 53 pacientes adultos con fractura diafisaria de húmero, 36 de los cuales siguieron el tratamiento ortopédico funcional. En otros 17 casos, pacientes politraumatizados o con fracturas de tercio medio transversas, realizamos tratamiento quirúrgico. La edad media de los pacientes fue 48 ± 2 2 años. Se afectó más el lado derecho, siendo el antecedente etiológico más frecuente el accidente casual. No hubo diferencia entre el tiempo de consolidación con el tratamiento ortopédico-funcional (60 ± 14 días) y el tratamiento quirúrgico (56 ±1 2 días). Como complicaciones hubo 7 pseudoartrosis (4 tras tratamiento ortopédico-funcional y 3 tratamiento quirúrgico). La edad media de los pacientes con pseudoartrosis fue superior a la de los pacientes con consolidación completa. Ocho casos cursaron con lesión del nervio radial, obteniendo una recuperación funcional del 100% en un tiempo medio de 38 ± 30 semanas. Valorando los resultados con arreglo a los criterios de Gayet, hemos obtenido un 80% de buenos y muy buenos resultados con tratamiento ortopédico funcional y un 70% con tratamiento quirúrgico.Fifty three adult patients with fracture of the humeral shaft were retrospectively studied. Orthopaedic-functional treatment was applied in 36 cases. Seventeen patients with either multiple injuries or transverse middle-shaft fractures were surgically treated. The mean age of patients was 48 ± 21 years. Right side was most frecuently affected and casual fall was the predominated etiology. There were no differences regarding the average consolidation period between fractures treated conservatively (60 ± 14 days) and those undergoing surgery (56 ± 12 days). As complications, there were 7 monounions (4 conservative and 3 operative treatment). The mean age of patients with non-unions was higther than those with complete fracture consolidation. Radial nerve injury was seen in 8 cases. In all there patients, a complete functional were recovery was obtained with a mean average time of 38 ± 30 weeks. When evaluating functional results according to Gayet, satisfactory results were found in 80 per cent of patients with conservative treatment and 70 per cent of those surgically treated

Aplasia del arco posterior del Atlas

Las anomalías congénitas del arco posterior del Atlas son poco frecuentes. Se presenta el caso de una paciente, que tras sufrir un accidente se diagnosticó de aplasia parcial del atlas. Esta lesión es considerada como una variante anatómica benigna de la región cráneovertebral. Se expone el desarrollo y el significado de esta anomalía.Congenital anomalies of the posterior arch of the atlas are uncommon. This paper presents the case of a patient who, as result of an accident, was diagnosed as having a congenital partial agenesia of the posterior arch of the atlas. This finding is considered as a benign anatomical variation of the craniovertebral junction region. The development and clinical significance of this anomaly are discussed

On the Sunyaev-Zel'dovich effect from dark matter annihilation or decay in galaxy clusters

We revisit the prospects for detecting the Sunyaev Zel'dovich (SZ) effect induced by dark matter (DM) annihilation or decay. We show that with standard (or even extreme) assumptions for DM properties, the optical depth associated with relativistic electrons injected from DM annihilation or decay is much smaller than that associated with thermal electrons, when averaged over the angular resolution of current and future experiments. For example, we find: $\tau_{\rm DM} \sim 10^{-9}-10^{-5}$ (depending on the assumptions) for \mchi = 1 GeV and a density profile $\rho\propto r^{-1}$ for a template cluster located at 50 Mpc and observed within an angular resolution of $10"$, compared to $\tau_{\rm th}\sim 10^{-3}-10^{-2}$. This, together with a full spectral analysis, enables us to demonstrate that, for a template cluster with generic properties, the SZ effect due to DM annihilation or decay is far below the sensitivity of the Planck satellite. This is at variance with previous claims regarding heavier annihilating DM particles. Should DM be made of lighter particles, the current constraints from 511 keV observations on the annihilation cross section or decay rate still prevent a detectable SZ effect. Finally, we show that spatial diffusion sets a core of a few kpc in the electron distribution, even for very cuspy DM profiles, such that improving the angular resolution of the instrument, e.g. with ALMA, does not necessarily improve the detection potential. We provide useful analytical formulae parameterized in terms of the DM mass, decay rate or annihilation cross section and DM halo features, that allow quick estimates of the SZ effect induced by any given candidate and any DM halo profile.Comment: 27 p, 6 figs, additional section on spatial diffusion effects. Accepted for publication in JCA

The missing massive satellites of the Milky Way

Recent studies suggest that only three of the 12 brightest satellites of the Milky Way (MW) inhabit dark matter haloes with maximum circular velocity, Vmax, exceeding ∼30 km s−1. This is in apparent contradiction with the Λ cold dark matter (CDM) simulations of the Aquarius Project, which suggest that MW-sized haloes should have at least eight subhaloes with Vmax > 30 km s−1. The absence of luminous satellites in such massive subhaloes is thus puzzling and may present a challenge to the ΛCDM paradigm. We note, however, that the number of massive subhaloes depends sensitively on the (poorly known) virial mass of the MW, and that their scarcity makes estimates of their abundance from a small simulation set like Aquarius uncertain. We use the Millennium Simulation series and the invariance of the scaled subhalo velocity function (i.e. the number of subhaloes as a function of ν, the ratio of the subhalo Vmax to the host halo virial velocity, V200) to secure improved estimates of the abundance of rare massive subsystems. In the range 0.1 ν) is approximately Poisson distributed about an average given by 〈Nsub〉 = 10.2 (ν/0.15)−3.11. This is slightly lower than that in Aquarius haloes, but consistent with recent results from the Phoenix Project. The probability that a ΛCDM halo has three or fewer subhaloes with Vmax above some threshold value, Vth, is then straightforward to compute. It decreases steeply both with decreasing Vth and with increasing halo mass. For Vth = 30 km s−1, ∼40 per cent of Mhalo = 1012 M⊙ haloes pass the test; fewer than ∼5 per cent do so for Mhalo ≳ 2 × 1012 M⊙ and the probability effectively vanishes for Mhalo ≳ 3 × 1012 M⊙. Rather than a failure of ΛCDM, the absence of massive subhaloes might simply indicate that the MW is less massive than is commonly thought

Módulo para la enseñanza de la energía solar como una propuesta interdisciplinar para la enseñanza de las ciencias en niveles de educación básica y media en Colombia.

In this paper we present an analysis of results obtained with a didactic proposal based on a module for teaching solar energy concepts in basic and high school levels in Colombia. First, the importance of teaching topics related to solar energy in the school is highlighted, then a brief explanation of the content of this module is made and finally an analysis of results obtained after presenting and testing the proposal with classmates.En el presente documento se hace un análisis de los resultados obtenidos con la propuesta del módulo didáctico para la enseñanza de la energía solar en niveles de educación básica y media en Colombia. Primero se resalta la importancia de enseñar temas relacionados con la energía solar en la escuela, luego se hace una breve explicación del contenido de este módulo y finalmente se hace un análisis de resultados obtenidos después de presentar y poner a prueba la propuesta con los compañeros de clase

Implication of the PAMELA antiproton data for dark matter indirect detection at LHC

Since the PAMELA results on the "anomalously" high positron fraction and the lack of antiproton excess in our Galaxy, there has been a tremendous number of studies advocating new types of dark matter, with larger couplings to electrons than to quarks. This raises the question of the production of dark matter particles (and heavy associated coloured states) at LHC. Here, we explore a very simple benchmark dark matter model and show that, in spite of the agreement between the PAMELA antiproton measurements and the expected astrophysical secondary background, there is room for large couplings of a WIMP candidate to heavy quarks. Contrary to what could have been naively anticipated, the PAMELA pbar/p measurements do not challenge dark matter model building, as far as the quark sector is concerned. A quarkophillic species is therefore not forbidden.Owing to these large couplings, one would expect that a new production channel opens up at the LHC, through quark--quark and quark--gluon interactions. Alas, when the PDF of the quark is taken into account, prospects for a copious production fade away.Comment: 7 pages, 2 figures, captions of some figures modified, main conclusion unchange

Gamma rays from dark matter annihilation in the Draco and observability at ARGO

The CACTUS experiment recently observed a gamma ray excess above 50 GeV from the direction of the Draco dwarf spheroidal galaxy. Considering that Draco is dark matter dominated the gamma rays may be generated through dark matter annihilation in the Draco halo. In the framework of the minimal supersymmetric extension of the standard model we explore the parameter space to account for the gamma ray signals at CACTUS. We find that the neutralino mass is constrained to be approximately in the range between 100 GeV ~ 400 GeV and a sharp central cuspy of the dark halo profile in Draco is necessary to explain the CACTUS results. We then discuss further constraints on the supersymmetric parameter space by observations at the ground based ARGO detector. It is found that the parameter space can be strongly constrained by ARGO if no excess from Draco is observed above 100 GeV.Comment: 15 pages, 4 figure