Measurement of transverse energy-energy correlations in multi-jet events in pp collisions at s√=7 TeV using the ATLAS detector and determination of the strong coupling constant αs(mZ)

High transverse momentum jets produced in pp collisions at a centre of mass energy of 7 TeV are used to measure the transverse energy--energy correlation function and its associated azimuthal asymmetry. The data were recorded with the ATLAS detector at the LHC in the year 2011 and correspond to an integrated luminosity of 158 pb−1. The selection criteria demand the average transverse momentum of the two leading jets in an event to be larger than 250 GeV. The data at detector level are well described by Monte Carlo event generators. They are unfolded to the particle level and compared with theoretical calculations at next-to-leading-order accuracy. The agreement between data and theory is good and provides a precision test of perturbative Quantum Chromodynamics at large momentum transfers. From this comparison, the strong coupling constant given at the Z boson mass is determined to be αs(mZ)=0.1173±0.0010 (exp.) +0.0065−0.0026 (theo.).

Measurement of colour flow with the jet pull angle in t(t)over-bar events using the ATLAS detector at root s=8 TeV

The distribution and orientation of energy inside jets is predicted to be an experimental handle on colour connections between the hard--scatter quarks and gluons initiating the jets. This Letter presents a measurement of the distribution of one such variable, the jet pull angle. The pull angle is measured for jets produced in tt¯ events with one W boson decaying leptonically and the other decaying to jets using 20.3 fb−1 of data recorded with the ATLAS detector at a centre--of--mass energy of s√=8 TeV at the LHC. The jet pull angle distribution is corrected for detector resolution and acceptance effects and is compared to various models.

Measurements of the top quark branching ratios into channels with leptons and quarks with the ATLAS detector

A measurement of the inclusive cross section for top quark pair production in pp collisions using events with an isolated lepton (muon or electron) and a τ lepton decaying to hadrons (τhad) is reported. Measurements of the branching ratios of top quark decays into leptons and jets using events with tt¯ (top antitop) pairs are also reported. Events were recorded with the ATLAS detector at the LHC in pp collisions at a center-of-mass energy of 7 TeV. The collected data sample corresponds to an integrated luminosity of 4.6 fb−1. The inclusive cross section measured using events with an isolated lepton and a τhad is σtt¯=183±9(stat.)±23(syst.)±3(lumi.)pb. The measured top quark branching ratios agree with the Standard Model predictions within the measurement uncertainties of a few percent.

Estudios sobre la Formación y Evolución Estelar

La evolución estelar, si bien en sus aspectos más generales aparecen como bien comprendida de acuerdo a ciertos lineamientos teóricos, presenta en contrapartida etapas enigmáticas y detalles particulares que aún no han sido develados en su totalidad. Entre estos últimos aspectos podríamos incluir: a) Evolución de sistemas binarios cerrados, en los que la pérdida del momentro angular y la transferencia de masa entre las componentes altera sus características iniciales; b) Evolución de la secuencia principal y de las gigantes en cúmulos abiertos, efectos del "fogonazo de helio", pérdida de masa, efectos de la metalicidad, frecuencia de binarias, etcétera. c) Evolución retardada en algunas estrellas denominadas "Blue Stragglers" por uno o más motivos aún no establecidos definitivamente, aunque las evidencias observacionales apuntan a la binaridad como la causa principal de este fenómeno; d) Tasa de formación de estrellas, función inicial de masas, etapas previas a la secuencia principal. (...) Algunas etapas particulares en la evolución de las estrellas son el principal objetivo del presente proyecto. Esto incluye los sistemas binarios cerrados con probables pérdidas de momento angular y transferencia de masa; estrellas evolutivamente rezagadas (blue stragglers) en cúmulos abiertos a fin de determinar las causas de su anormalidad; estrellas de secuencia principal y gigantes rojas en agregados estelares de nuestra galaxia, con el propósito de determinar sus parámetros fundamentales como distancias, edades, metalicidades, probabilidades de pertenencia, etc.; estrellas en etapas de formación, tendiendo a investigar sus características primordiales tales como su variabilidad fotomátrica, la existencia de jets y discos circumestelares y la distribución estadística inicial de masas estelares. Se utilizan para ello las más modernas técnicas observacionales (espectroscópicas y fotométricas) a fin de aportar datos específicos de los diferentes objetos investigados. Finalmente estos datos son cotejados con las predicciones teóricas más actuales de las diferentes etapas de la evolución estelar.

A Grid Supercomputing Enviroment for High Demand Computational Applications

Despite the huge increase in processor and interprocessor network performace, many computational problems remain unsolved due to lack of some critical resources such as floating point sustained performance, memory bandwidth, etc... Examples of these problems are found in areas of climate research, biology, astrophysics, high energy physics (montecarlo simulations) and artificial intelligence, among others. For some of these problems, computing resources of a single supercomputing facility can be 1 or 2 orders of magnitude apart from the resources needed to solve some them. Supercomputer centers have to face an increasing demand on processing performance, with the direct consequence of an increasing number of processors and systems, resulting in a more difficult administration of HPC resources and the need for more physical space, higher electrical power consumption and improved air conditioning, among other problems. Some of the previous problems can´t be easily solved, so grid computing, intended as a technology enabling the addition and consolidation of computing power, can help in solving large scale supercomputing problems. In this document, we describe how 2 supercomputing facilities in Spain joined their resources to solve a problem of this kind. The objectives of this experience were, among others, to demonstrate that such a cooperation can enable the solution of bigger dimension problems and to measure the efficiency that could be achieved. In this document we show some preliminary results of this experience and to what extend these objectives were achieved.

Impacto de la circulación ecuatorial en la zona mínima de oxógeno presente en el norte del Ecosistema de la Corriente del Humboldt

El Norte del Ecosistema de la Corriente Humboldt (NECH) constituye una de las mayores zonas de afloramiento, localizada en el borde oriental del Pacifico Sur, la cual presenta características particulares, entre las que destacan una alta producción primaria y la presencia de una de las zonas mínimas de oxigeno (ZMO) más intensas en el océano abierto. La ZMO presente en esta zona es producto de la alta demanda de oxígeno durante la remineralización de la materia orgánica, el largo tiempo de residencia de sus aguas y su poca ventilación. En el presente estudio nos enfocamos en estudiar la influencia de cambios en la ventilación en la ZMO del NECH, tomando como las principales fuentes de aporte de oxígeno en esta zona a la Corriente Sub-superficial Ecuatorial (EUC) y las Contracorrientes Sub-superficiales del Sur (SSCCs) o también conocidas como los Jets de Tsuchiya. Utilizamos el modelo acoplado físico-biogeoquímico ROMS-PISCES, para observar la sensibilidad de la ZMO a diferentes condiciones de la circulación ecuatorial provenientes de dos modelos oceánicos de circulación general (SODA y MERCATOR). Los resultados muestran que el flujo de oxígeno a los 88ºW disminuye latitudinalmente de la EUC a los SSCCs; además, se observa que la ZMO desaparece de los 4ºN - 4ºS en la simulación que presenta una circulación más intensa (RPSoda) por lo que se puede concluir que una intensificación de la circulación ecuatorial afectaría principalmente a la zona ecuatorial y no frente a Perú, debido a que una mayor ventilación sería compensada con un mayor consumo de oxigeno durante la remineralización, producto de una alta productividad generada por un mayor flujo de nutrientes.

A numerical model for the gamma-ray emission of the microquasar LS 5039

The possible association between the microquasar LS 5039 and the EGRET source 3EG J1824-1514 suggests that microquasars could also be sources of high energy gamma-rays. In this paper, we explore, with a detailed numerical model, if this system can produce the emission detected by EGRET (>100 MeV) through inverse Compton (IC) scattering. Our numerical approach considers a population of relativistic electrons entrained in a cylindrical inhomogeneous jet, interacting with both the radiation and the magnetic fields, taking into account the Thomson and Klein-Nishina regimes of interaction. The computed spectrum reproduces the observed spectral characteristics at very high energy.

Hints for a fast precessing relativistic radio jet in LS I+61·303

Here we discuss two consecutive MERLIN observations of the X-ray binary LS I +61◦303. The first observation shows a double-sided jet extending up to about 200 AU on both sides of a central source. The jet shows a bent S-shaped struct ure similar to the one displayed by the well-known precessing jet of SS 433. The precession suggested in the first MERLIN image becomes evident in the second one, showing a one-sided bent jet significantly rotated with respect to the jet of the day before. We conclude that the derived precession of the relativistic (β=0.6) jet explains puzzling previous VLBI results. Moreover , the fact that the precession is fast could be the explanation of the never understood short term (days) variability of the associated gamma-ray source 2CG 135 + 01 / 3EG J0241 + 6103.

VLA multifrequency observations of RSCVn binaries

We present multiepoch Very Large Array (VLA) observations at 1.4 GHz, 4.9 GHz, 8.5 GHz and 14.9 GHz for a sample of eight RS CVn binary systems. Circular polarization measurements of these systems are also reported. Most of the fluxes observed are consistent with incoherent emission from mildly relativistic electrons. Several systems show an increase of the degree of circular polarization with increasing frequency in the optically thin regime, in conflict with predictions by gyrosynchrotron models. We observed a reversal in the sense of circular polarization with increasing frequency in three non-eclipsing systems: EI Eri, DM Uma and HD 8358. We find clear evidence for coherent plasma emission at 1.4 GHz in the quiescent spectrum of HD 8358 during the helicity reversal. The degrees of polarization of the other two systems could also be accounted for by a coherent emission process. The observations of ER Vul revealed two U-shaped flux spectra at the highest frequencies. The U-shape of the spectra may be accounted for by an optically thin gyrosynchrotron source for the low frequency part whereas the high frequency part is dominated by a thermal emission component.

A search for microquasar candidates at low galactic latitudes

Recent studies of relativistic jet sources in the Galaxy, also known as microquasars, have been very useful in trying to understand the accretion/ejection processes that take place near compact objects. However, the number of sources involved in such studies is still small. In an attempt to increase the number of known microquasars we have carried out a search for new Radio Emitting X-ray Binaries (REXBs). These sources are the ones to be observed later with VLBI techniques to unveil their possible microquasar nature. To this end, we have performed a cross-identification between the X-ray ROSAT all sky survey Bright Source Catalog (RBSC) and the radio NRAO VLA Sky Survey (NVSS) catalogs under very restrictive selection criteria for sources with |b|<5 degrees. We have also conducted a deep observational radio and optical study for six of the selected candidates. At the end of this process two of the candidates appear to be promising, and deserve additional observations aimed to confirm their proposed microquasar nature.

Microquasars as high energy gamma-ray sources

Galactic microquasars are certainly one of the most recent additions to the field of high energy astrophysics and have attracted increasing interest over the last decade. However, the high energy part of the spectrum of microquasars is the most poorly known, mainly due the lack of sensitive instrumentation in the past. Microquasars are now primary targets for all of the observatories working in the X-ray and gamma-ray domains. They also appear as the possible counterparts for some of the unidentified sources of high-energy gamma-rays detected by the experiment EGRET on board the satellite COMPTON-GRO. This paper provides a general review of the main observational results obtained up to now as well as a summary of the scenarios for production of high-energy gamma-rays at the present moment.

High-energy gamma-ray emission from microquasars: LS 5039 and LS I+61303

The possible associations between the microquasars LS 5039 and LS I +61 303 and the EGRET sources 3EG J1824-1514 and 3EG J0241+6103 suggest that microquasars could also be sources of high-energy gamma-rays. In this work, we present a detailed numerical inverse Compton (IC) model, based on a microquasar scenario, that reproduces the high-energy gamma-ray spectra and variability observed by EGRET for the mentioned sources. Our model considers a population of relativistic electrons entrained in a cylindrical inhomogeneous jet that interact through IC scattering with both the radiation and the magnetic fields.

Exploring the high frequency emission of radio loud X-ray binaries

We report millimetre-wave continuum observations of the X-ray binaries Cygnus X-3, SS 433, LSI+61 303, Cygnus X-1 and GRS 1915+105. The observations were carried out with the IRAM 30 m-antenna at 250 GHz (1.25 mm) from 1998 March 14 to March 20. These millimetre measurements are complemented with centimetre observations from the Ryle Telescope, at 15 GHz (2.0 cm) and from the Green Bank Interferometer at 2.25 and 8.3 GHz (13 and 3.6 cm). Both Cygnus X-3 and SS 433 underwent moderate flaring events during our observations, whose main spectral evolution properties are described and interpreted. A significant spectral steepening was observed in both sources during the flare decay, that is likely to be caused by adiabatic expansion, inverse Compton and synchrotron losses. Finally, we also report 250 GHz upper limits for three additional undetected X-ray binary stars: LSI+65 010, LSI+61 235 and X Per.

Search for very high energy gamma-ray emission from pulsar-pulsar wind nebula systems with the MAGIC telescope

The MAGIC collaboration has searched for high-energy gamma-ray emission of some of the most promising pulsar candidates above an energy threshold of 50 GeV, an energy not reachable up to now by other ground-based instruments. Neither pulsed nor steady gamma-ray emission has been observed at energies of 100 GeV from the classical radio pulsars PSR J0205+6449 and PSR J2229+6114 (and their nebulae 3C58 and Boomerang, respectively) and the millisecond pulsar PSR J0218+4232. Here, we present the flux upper limits for these sources and discuss their implications in the context of current model predictions.

Optical nebulosities associated with IRAS sources in dense cloud cores

I, H¿ and [SII] CCD images of the regions around 4 young IRAS sources embedded in the dense molecular cloud cores CB 6, CB 39, AFGL 5142, and L 1251 are presented. Reflection nebulosities are found in all 4 regions. Herbig-Haro objects are detected in AFGL 5142 and L 1251. In both cases, the HH objects are new discoveries.