Women artists of the international avant-garde: the case of "Abstraction-Création" (1931-1936)

Women’s contribution to abstract art in the interwar period is a subject that, to date, has received very little attention. In this article we deal with the untold story of the participation of women artists in Abstraction-Création, the foremost international group dedicated to abstract art in the 1930s. Founded in Paris in 1931, the group took on the work of two previous collectives to become a platform for the dissemination and promotion of abstract art and consisted of around a hundred members. Twelve of these were women, whose writings and works were published in the group’s annual magazine, abstraction creátion art non figuratif (1932-1936), and who participated in a number of the group’s exhibitions. Compared to what had occurred in previous groups, the participation of women, although reduced in number, was comparable to that of the male artists and being members of the group had a generally positive impact on the women’s careers. However, all this came at the expense of relinquishing any gender specificity in their work and the public presentation of it, and demonstrates that the normalization of women’s contributions to the avant-garde could only be brought about alongside a questioning of the more dogmatic views of modernity.

Los nuevos territorios de la gráfica: imagen, proceso y distribución

La gráfica se encuentra en un proceso de simbiosis con la cultura visual en el que la tecnología de la imagen, la descentralización de la matriz y la adaptación del formato expositivo se funden con el resto de las actividades artísticas. El análisis de las comunidades formadas alrededor de esta práctica configura un puzzle, aparentemente bien encajado, que se divide entre el formalismo y el conceptualismo y entre la idea y el proceso. Las bienales y trienales, a la vanguardia del discurso, cuestionan cualquier concepto que se haya podido asentar con solidez: ante la decadencia del proceso artesanal el mensaje se profundiza nutriéndose de la invectiva provocada por las contradicciones sociales, territoriales y medioambientales para convertirse en un reflejo de la sociedad contemporánea. Comprender la gráfica actual pasa por un ejercicio de aperturismo y un proceso de adaptación al cambio técnico e iconográfico de los sectores implicados. El grabado es ahora un territorio en el que la integración de todas las artes permite cruzar sus fronteras con fluidez.

El patrimonio a través de la educación artística en la etapa de primaria

El área de educación artística en el currículum de primaria ha estado ligada a la enseñanza del patrimonio en las tres últimas décadas y, seguida del área de Ciencias Sociales en sus diferentes denominaciones, ha sido la materia que más se ha ocupado del la enseñanza de nuestro legado cultural, desde la LOGSE, pasando por la LOE hasta la actual LOMCE. Sin embargo, con la última reforma educativa ha sufrido una pérdida de presencia que la sitúa como una materia prescindible, en tanto un alumno puede transitar por toda la etapa de Primaria sin recibir una sola hora de educación artística. En efecto, las CCAA y los centros, en el ejercicio de sus competencias (Artículo 3) pueden decidir no ofertarla o, aun ofertándola, puede no ser elegida de entre otras asignaturas específicas como Segunda Lengua Extranjera, Religión o Valores Sociales y Cívicos.Por todo ello, proponemos un análisis del contenido de las tres grandes leyes generales de educación de las tres últimas décadas -LOGSE, LOE y LOMCE- examinando la presencia del patrimonio en la educación artística, para detectar los enfoques y concepciones subyacentes en los diferentes desarrollos curriculares. Todo ello nos situará ante un escenario, el presente, en el que podremos demandar la recuperación de contenidos o competencias perdidas, pero también promover el máximo aprovechamiento de las que sí se han incluido en el currículum vigente. Por todo ello, proponemos un análisis del contenido de las tres grandes leyes generales de educación de las tres últimas décadas -LOGSE, LOE y LOMCE- examinando la presencia del patrimonio en la educación artística, para detectar los enfoques y concepciones subyacentes en los diferentes desarrollos curriculares. Todo ello nos situará ante un escenario, el presente, en el que podremos demandar la recuperación de contenidos o competencias perdidas, pero también promover el máximo aprovechamiento de las que sí se han incluido en el currículum vigente.

Artistic proposals of visual arts of Ecuador since the second half of the twentieth century to the present

This article is the result of a research that analyzes the most important artistic proposals of Visual Arts in Ecuador, since the second half of the twentieth century to the present. Through literature review and data collection held in the city of Guayaquil, we could determine their influence and impact on the circuit of contemporary art. The instruments used for data collection were depth interviews that were done to experts in the field. Like surveys of attendees at different artistic events (exhibitions, permanent exhibitions, seminars), allowed to establish the social interests of those proposals. The methodology was mixed approach, quantitative and qualitative data were used.

Incorporating Higher Moments into Value at Risk Forecasting

Value-at-risk (VaR) forecasting generally relies on a parametric density function of portfolio returns that ignores higher moments or assumes them constant. In this paper, we propose a simple approach to forecasting of a portfolio VaR. We employ the Gram-Charlier expansion (GCE) augmenting the standard normal distribution with the first four moments, which are allowed to vary over time. In an extensive empirical study, we compare the GCE approach to other models of VaR forecasting and conclude that it provides accurate and robust estimates of the realized VaR. In spite of its simplicity, on our dataset GCE outperforms other estimates that are generated by both constant and time-varying higher-moments models.

Efficient Evaluation of Multidimensional Time-Varying Density Forecasts

We propose two simple evaluation methods for time varying density forecasts of continuous higher dimensional random variables. Both methods are based on the probability integral transformation for unidimensional forecasts. The first method tests multinormal densities and relies on the rotation of the coordinate system. The advantage of the second method is not only its applicability to any continuous distribution but also the evaluation of the forecast accuracy in specific regions of its domain as defined by the user’s interest. We show that the latter property is particularly useful for evaluating a multidimensional generalization of the Value at Risk. In simulations and in an empirical study, we examine the performance of both tests.

Dynamic Density Forecasts for Multivariate Asset Returns

We propose a simple and flexible framework for forecasting the joint density of asset returns. The multinormal distribution is augmented with a polynomial in (time-varying) non-central co-moments of assets. We estimate the coefficients of the polynomial via the Method of Moments for a carefully selected set of co-moments. In an extensive empirical study, we compare the proposed model with a range of other models widely used in the literature. Employing a recently proposed as well as standard techniques to evaluate multivariate forecasts, we conclude that the augmented joint density provides highly accurate forecasts of the “negative tail” of the joint distribution.

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%.

Theory of pixel lensing towards M31 - I. The density contribution and mass of MACHOs

POINT-AGAPE is an Angle-French collaboration which is employing the Isaac Newton Telescope (INT) to conduct a pixel-lensing survey towards M31. Pixel lensing is a technique which permits the detection of microlensing against unresolved stellar fields. The survey aims to constrain the stellar population in M31, and also the distribution and nature of massive compact halo objects (MACHOs) in both M31 and the Galaxy.