The anomaly in the candidate microlensing event PA-99-N2

The light curve of PA-99-N2, one of the recently announced microlensing candidates toward M31, shows small deviations from the standard Paczynski form. We explore a number of possible explanations, including correlations with the seeing, the parallax effect, and a binary lens. We find that the observations are consistent with an unresolved red giant branch or asymptotic giant branch star in M31 being microlensed by a binary lens. We find that the best-fit binary lens mass ratio is similar to1.2x10(-2), which is one of the most extreme values found for a binary lens so far. If both the source and lens lie in the M31 disk, then the standard M31 model predicts the probable mass range of the system to be 0.02-3.6 M-circle dot (95% confidence limit). In this scenario, the mass of the secondary component is therefore likely to be below the hydrogen-burning limit. On the other hand, if a compact halo object in M31 is lensing a disk or spheroid source, then the total lens mass is likely to lie between 0.09 and 32 M-circle dot, which is consistent with the primary being a stellar remnant and the secondary being a low-mass star or brown dwarf. The optical depth (or, alternatively, the differential rate) along the line of sight toward the event indicates that a halo lens is more likely than a stellar lens, provided that dark compact objects comprise no less than 15% (or 5%) of halos.

Theory of pixel lensing toward M31. II. The velocity anisotropy and flattening of the MACHO distribution

The POINT-AGAPE collaboration is currently searching for massive compact halo objects (MACHOs) toward the Andromeda galaxy (M31). The survey aims to exploit the high inclination of the M31 disk, which causes an asymmetry in the spatial distribution of M31 MACHOs. Here, we investigate the effects of halo velocity anisotropy and flattening on the asymmetry signal using simple halo models. For a spherically symmetric and isotropic halo, we find that the underlying pixel lensing rate in far-disk M31 MACHOs is more than 5 times the rate of near-disk events. We find that the asymmetry is further increased by about 30% if the MACHOs occupy radial orbits rather than tangential orbits, but it is substantially reduced if the MACHOs lie in a flattened halo. However, even for halos with a minor- to major-axis ratio of q = 0.3, the number of M31 MACHOs in the far side outnumber those in the near side by a factor of similar to2. There is also a distance asymmetry, in that the events on the far side are typically farther from the major axis. We show that, if this positional information is exploited in addition to number counts, then the number of candidate events required to confirm asymmetry for a range of flattened and anisotropic halo models is achievable, even with significant contamination by variable stars and foreground microlensing events. For pixel lensing surveys that probe a representative portion of the M31 disk, a sample of around 50 candidates is likely to be sufficient to detect asymmetry within spherical halos, even if half the sample is contaminated, or to detect asymmetry in halos as flat as q = 0.3, provided less than a third of the sample comprises contaminants. We also argue that, provided its mass-to-light ratio is less than 100, the recently observed stellar stream around M31 is not problematic for the detection of asymmetry.

The POINT-AGAPE survey: 4 high signal-to-noise microlensing candidates detected towards M 31

We have carried out a survey of the Andromeda galaxy for unresolved microlensing (pixel lensing). We present a subset of four short timescale, high signal-to-noise microlensing candidates found by imposing severe selection criteria: the source flux variation exceeds the flux of an R = 21 magnitude star and the full width at half maximum timescale is less than 25 days. Remarkably, in three out of four cases, we have been able to measure or strongly constrain the Einstein crossing time of the event. One event, which lies projected on the M 31 bulge, is almost certainly due to a stellar lens in the bulge of M 31. The other three candidates can be explained either by stars in M 31 and M 32 or by MACHOs.

A candidate M31/M32 intergalactic microlensing event

We report the discovery of a microlensing candidate projected 2'54

A short-timescale candidate microlensing event in the point-agape pixel lensing survey of M31

We report the discovery of a short-duration microlensing candidate in the northern field of the POINT-AGAPE pixel lensing survey toward M31. Almost certainly, the source star has been identified on Hubble Space Telescope archival images, allowing us to infer an Einstein crossing time of t(E) = 10.4 days, a maximum magnification of A(max) similar to 18, and a lens-source proper motion mu (rel) > 0.3 mu as day(-1). The event has a projected separation of 8' from the center of M31, beyond the bulk of the stellar lens population. There are three plausible identifications/locations for the lensing object: a massive compact halo object (MACHO) in either M31 or the Milky Way, or a star in the M31 disk. The most probable mass is 0.06 M-. for an M31 MACHO, 0.02 M-. for a Milky Way MACHO, and 0.2 M-. for an M31 stellar lens. While the stellar interpretation is possible, the MACHO interpretation is the most probable for halo fractions above 20%.

Geometría de la red de arrastre de fondo utilizada en la prospección de recursos pelágico costeros y demersales costeros E/E Huamanga 9611-12

Describe las actividades de rastreo del E/E Huamanga, que efectuó del 01 al 18 de diciembre de 1996, entre Puerto Pizarro y Callao. Se demuestra la longitud del cable principal de arrastre y la profundidad que se determinó en una proporción de 3:1. Así mismo, la correspondencia entre los parámetros de abertura vertical y horizontal de la boca de red en función a la velocidad de arrastre, la misma que fue inversa y directamente proporcional teniendo un alto grado de correlación.

Determinación de la edad y crecimiento de la Sardina Sardinops sagax sagax (J)

Determinación de la sardina Sardinops sagax sagax (J.), del área del Callao, mediante métodos de lecturas y mediciones de las marcas de los anillos de crecimiento de 243 otolitos. Los métodos empleados se adjuntan a la especie estudiada con facilidad y los resultados se consideran satisfactorios. En el cálculo de los parámetros de crecimiento se aplica la ecuación de Von Bertalanffy, con cuyas expresiones se calcularon las tallas y pesos teóricos por edades. Al relacionar la edad con las tallas de captura, para los niños 1973 y 1974, se determinó la predominancia del grupo de edad 4 años en 1973; posteriormente, en 1974 se experimentaron cambios en la estructura poblacional presentándose una predominancia del grupo de edad 2 conjuntamente con el de 3 años de edad. La edad relacionada al peso deja ver que existe una correspondencia entre ambos, muy similar en machos y hembras hasta la edad de 3 años; esto hace suponer la igualdad de condiciones nutricionales. A partir de esa edad, las hembras incrementan su peso en menor proporción, lo que debe depender del mayor desgastes en los desoves, muy notorio en individuos mayores. La tasa máxima de crecimiento es alcanzada a los 4 años en los machos y a los 3 años en las hembras, con un promedio de 1.90 y 1.17, respectivamente. La distribución por edades guarda relación con los grupos de tallas correspondientes a las capturas, a pesar de que la cantidad de observaciones no cubre el rango de distribución real por tallas.

Relación histórica y moral de la portentosa imágen de N. Sr. Jesucristo crucificado aparecido en una de las cuevas de S. Miguel de Chalma, hoy real convento y santuario de este nombre, de religiosos ermitaños de N.G.P. y doctor S. Agustin, en esta Nueva España, y en esta provincia del santísimo nombre de Jesús de México : con los compendios de las vidas de los dos venerables religiosos legos y primeros anacoretas de este santo desierto, F. Bartolomé de Jesús María, y F. Juande San Josef

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Cartas de Cicerón con breves argumentos y notas

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Pitman's commercial correspondance and comercial english

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Cartas éruditas y críticas del P. Andrés Marcos Burriel de la compañia de Jesús

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Thesuarus hispano-latinus utriusque linque verbis, et pharasibus abundans olim a p. Bartholomaeo Bravo e societate Jesu inventus: postea ap. Petro de Salas ex endem societate.

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Cartas dirigidas por el doctor Basilio Arrillaga al doctor D. José M. Luis Mora, citándolo ante el tribunal de la sana crítica, de la religión católica y de la verdadera política, a responder por los fundamentos y resultados de sus opiniones.

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Dos antiguas relaciones de la Florida

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Carta del General José María Tornel a sus amigos, sobre un artículo inserto en el Cosmopolita del día 17 de agosto del presente año por José María Tornel.

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