Biología y pesquería de tiburones de las Islas Lobos, Perú

Pemite conocer los resultados del estudio realizado entre el 18 de setiembre y el 02 de octubre de 1995 al oeste de las islas Lobos de Tierra y Lobos de Afuera. El informe indica que sí es posible el desarrollo de la pesquería comercial de tiburones y sugiere la necesidad de elaborar estudios de mercadeo y comercialización para la utilización de este recurso. Asimismo, aporta mayor información del recurso tiburón con la finalidad de tener mayor conocimiento de su biología y pesquería, permitiendo así su mejor administración mediante la intervención de organismos que desarrollen Programas Regionales y Mundiales de manejo y conservación del recurso.

Composición funcional del grupo Polychaeta en la bahía de Paita y la plataforma adyacente (5°S), Perú. Febrero 2003 a octubre 2008.

El objetivo fue determinar la variación batimétrica y temporal de la composición funcional por gremios tróficos del grupo Poliquetos. Se colectaron muestras de macrobentos e información oceanográfica en tres estaciones ubicadas en la bahía (BH, 35 m), plataforma interna (PI, 65 m) y plataforma externa (PE, 117 m), de febrero 2003 a octubre 2008. Los resultados indicaron que la variabilidad estacional está sujeta a cambios de mayor escala, como el incremento de la producción primaria en primavera y verano, posibilitando un aumento de los depositívoros superficiales (SDF) en la BH durante primavera, por efecto de la acumulación de materia orgánica fitoplanctónica que llega al fondo. Asimismo, la disminución de los depositívoros superficiales (SDF) y el aumento de los suspensívoros (SF) en verano, en la BH y PI, se pueden explicar debido al incremento de la descarga de partículas terrígenas de origen vegetal, que afectan físicamente al sustrato. En tanto, los consumidores de interfaz (IF) que dominaron en verano/otoño en la PE, donde la influencia continental es menor, pueden haber sido favorecidos por la mayor calidad de flujo acumulado de fitodetritus en los sedimentos y a un menor contenido de OD, lo cual disminuyó quizás la presión por predación y competencia.

Identificación de estructuras y relaciones espaciales en los componentes del sistema de la corriente de Humboldt: una comparación de métodos estadísticos

Para lograr la sostenibilidad de los recursos marinos es necesario comprender las relaciones que existen entre los diferentes procesos que ocurren dentro de los ecosistemas (procesos físicos o procesos biológicos). La mayoría de los datos que provienen de la ecología tienen una fuerte autocorrelación, la cual hace imposible aplicar métodos estadísticos tradicionales que requieren el supuesto de independencia de las observaciones. En este trabajo hemos aplicado y comparado 4 metodologías que nos permiten trabajar con datos autocorrelacionados; estas metodologías son: la correlación con ajuste del tamaño de muestra, los m´todos geoestadísticos, los PCNM (análisis de coordenadas principales) y los métodos wavelets. Dichas metodologías fueron aplicadas para estudiar las estructuras presentes en la profundidad de la zona mínima de oxígeno (ZMO), el zooplancton y los peces del Sistema de la Corriente de Humboldt. Como resultado se pudo observar las ventajas que ofrecen los métodos PCNM para estudiar las estructuras para cada variable y las interacciones entre la ZMO y el zooplancton, el zooplancton y peces y entre la ZMO y peces. También se observó que los cuatro métodos dieron como resultado la presencia de tres estructuras presentes en cada una de las tres variables. Siendo estas estructuras desde los 500 m hasta los 30 km, desde los 30 km hasta los 60 o 70km y finalmente desde los 70 km hasta los 130 km. Estas estructuras corresponden a dos escalas espaciales que son: la sub-meso escala (100s m a kms) y la mesoescala (10s km a 100s km). Finalmente se observó que existe una relación positiva entre la ZMO y el zooplancton, también se observó relaciones positivas entre el zooplancton y peces.

Identificação de estruturas de processos multi-escala em ecossistemas marinhos utilizando ondaletas

Ecossistemas marinhos de upwelling são muito heterogêneos e apresentam uma intensa atividade de mesoescala de dimensão de dezenas de quilômetros e submesoescala que variam de centenas de metros até quilômetros dos processos físicos. A importância das estruturas dos processos físicos está na estruturação que eles exercem sob a biomassa de zooplâncton. O presente trabalho está relacionado a um estudo realizado a cabo no Norte do Sistema da Corrente de Humboldt (Peru). Utilizou-se duas variáveis, a profundidade do limite superior da zona de mínimo oxigênio (ZMO) e a biomassa de zooplâncton. É desenvolvida uma metodologia de análise baseada no uso de ondaletas para a identi cação das estruturas dos processos físicos em suas diferentes escalas. O método foi aplicado aos dados de ZMO. Estudos de simula ção mostraram que o método tem a capacidade de identi car as estruturas de interesse, tendo erro de estimação nas bordas do espectro da potência de ondaleta. A tipologia das estruturas identi cadas mostraram que existe três tipos de estruturas, estruturas maiores de mesoescala, duas estruturas pequenas de submesoescala com profundidades diferentes. Outro resultado importante foi que dentro das estruturas pequenas e mais profundas existe maior biomassa de zooplâncton, principalmente nas estruturas de downwelling.

Tortugas marinas durante el 2010 en Pisco, Perú

Durante el 2010, se capturó 55 ejemplares de tortuga verde Chelonia mydas en La Aguada (13°51’S y 76°15’W) al sureste de la bahía de Paracas; el número promedio de tortugas capturadas por kilómetro de red tendida fue 3,08±2,5; el tamaño promedio de la LCC fue 60,3±10,5cm; el 78% de los ejemplares presentaron el patrón 5c, 4d, 4i y 11d, 11i, para los escudos centrales, costales y marginales, respectivamente. La TSM donde se capturaron varió entre 15,2 y 20,9 °C, la mayor ocurrencia de tortugas se registró de 18,5 a 20 °C. Los epibiontes más representativos fueron Platylepas hexastylos (56,8%), Conchoderma virgatum (26,9%) y Chelonibia testudinaria (13,3%); la ocurrencia de los ítems alimenticios: Clorophyta (78%), Rhodophyta (30%), Cnidaria (43%), Crustacea (43%), Polichaeta (17%), Mollusca (17%), arena (26%) y plástico (17%); el 72% de las tortugas presentaron cobertura algal, de las cuales el 65% fue el alga verde Enteromorpha sp.

UBVRI photoelectric photometry of nearby stars. II.

A second set of UBVRI photometry results for nearby stars of Gliese's (1969) catalog and its supplements, including in this case some multiple systems, are presented. Most of the observations were carried out between July 1984 and December 1985 at Calar Alto with the 1.23-m Centro Astronomico Hispano-Aleman telescope and the 1.52-m Observatorio Astronomico Nacional telescope. The number of observations of program and standard stars for the six runs and the final results for 60 stars are presented.

Electromagnetic radiation initiated by hadronic jets from microquasars in the ISM

Microquasars are potential candidates to produce a non-negligible fraction of the observed galactic cosmic rays. The protons accelerated at the jet termination shock interact with the interstellar medium and may produce detectable fluxes of extended emission at different energy bands: high-energy and very high-energy gamma-rays produced by neutral pion-decay, synchrotron and bremsstrahlung emission in a wide energy range generated by the secondary electrons produced by charged pion-decay. We discuss the association between this scenario and some of the unidentified EGRET sources in the galactic plane.

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.

One-sided jet at milliarcsecond scales in LSI+61·303

We present Very Long Baseline Interferometry (VLBI) observations of the high mass X-ray binary LSI+61303, carried out with the European VLBI Network (EVN). Over the 11 hour observing run, performed 10 days after a radio outburst, the radio source showed a constant flux density, which allowed sensitive imaging of the emission distribution. The structure in the map shows a clear extension to the southeast. Comparing our data with previous VLBI observations we interpret the extension as a collimated radio jet as found in several other X-ray binaries. Assuming that the structure is the result of an expansion that started at the onset of the outburst, we derive an apparent expansion velocity of 0.003 c, which, in the context of Doppler boosting, corresponds to an intrinsic velocity of at least 0.4 c for an ejection close to the line of sight. From the apparent velocity in all available epochs we are able to establish variations in the ejection angle which imply a precessing accretion disk. Finally we point out that LSI+61303, like SS433 and Cygnus X-1, shows evidence for an emission region almost orthogonal to the relativistic jet.

The extraordinarily bright optical afterglow of GRB 991208 and its host galaxy

Observations of the extraordinarily bright optical afterglow (OA) of GRB 991208 started 2.1 d after the event. The flux decay constant of the OA in the R-band is -2.30 +/- 0.07 up to 5 d, which is very likely due to the jet effect, and after that it is followed by a much steeper decay with constant -3.2 +/- 0.2, the fastest one ever seen in a GRB OA. A negative detection in several all-sky films taken simultaneously to the event implies either a previous additional break prior to 2 d after the occurrence of the GRB (as expected from the jet effect). The existence of a second break might indicate a steepening in the electron spectrum or the superposition of two events. Once the afterglow emission vanished, contribution of a bright underlying SN is found, but the light curve is not sufficiently well sampled to rule out a dust echo explanation. Our determination of z = 0.706 indicates that GRB 991208 is at 3.7 Gpc, implying an isotropic energy release of 1.15 x 10E53 erg which may be relaxed by beaming by a factor > 100. Precise astrometry indicates that the GRB coincides within 0.2' with the host galaxy, thus given support to a massive star origin. The absolute magnitude is M_B = -18.2, well below the knee of the galaxy luminosity function and we derive a star-forming rate of 11.5 +/- 7.1 Mo/yr. The quasi-simultaneous broad-band photometric spectral energy distribution of the afterglow is determined 3.5 day after the burst (Dec 12.0) implying a cooling frequency below the optical band, i.e. supporting a jet model with p = -2.30 as the index of the power-law electron distribution.

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.