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New infrared photometry of a sample of 39 stars in the open cluster NGC 752 is presented. These observations confirm the bimodality of the Main Sequence previously reported. We analyze the nature of this behaviour on the basis of the binary hypothesis.

Preliminary results on new CCD photometry inV andB bands of approximately 5000 stars in four overlapping fields in the globular cluster M3 are presented. The colour-magnitude diagram shows a very well-defined sequence with a small scatter, going fainter than previously published work on this cluster. The turn-off point found atV=19.1±0.2 mag and (B-V)=0.445±0.01, is slightly redder than those obtained in previous studies.

We present CCD photometry for stars in three fields centered on the old open cluster NGC 188 and in four fields on the intermediate-age cluster NGC 7789, which has been performed with the aim of investigating the HR diagram distribution of the cluster's Main-Sequence (MS) stars. A sufficiently well-defined sequence of subgiant, turn-off (TO), and MS stars have been detected, extending the observed lower MS down to aboutV=20 mag.

The Gran Telescopio Canarias (GTC) is, being assembled at the Observatorio del Roque de los Muchachos (ORM) in the island of La Palma. First light is expected for early 2005 with the first science observations late in 2005. The GTC, being a segmented primary mirror telescope, could be employed for testing several technological aspects relevant to the future generation of Extremely Large Telescopes (ELT). In the short term, the mass production of aespheric mirror segments can be examined in detail and improvements made along the way, or planned for the future. Indeed the GTC segments are now entering into a chain production scheme. Later on, different strategies for the control aspects of the primary mirror can be explored to optimize the optical performance of segmented telescopes. Moreover, the entire GTC active optics can offer a learning tool for testing various strategies and their application to ELTs.

Large-Scale observing facilities are scarce and costly. Even so, the perspective to enlarge or to increase the number of these facilities are quite real and several projects are undertaking their first steps in this direction. These costly facilities require the cooperation of highly qualified institutions, able to undertake the project from the scientific and technological point of view, as well as the vital collaboration and effective support of several countries, at the highest level, able to provide the necessary investment for their construction. Because of these technological implications and the financial magnitude of these projects, their impact goes well beyond the international astrophysical community. We propose to carry out a study on the socio-economic impact from the construction and operation of an Extremely Large Telescope of class 30 - 100 m. We plan to approach several aspects such as its impact in the promotion of the employment; social, educational and cultural integration of the population; the impulse of industries; its impact on the national and international policies on research; environmental issues; etc. We will also analyze the financial instruments available, and those special aids only accessible for some countries and regions to encourage their participation in projects of this magnitude.

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From a new infrared photometry of the globular cluster M10 its interstellar extinction and distance modulus are discussed. This is done by comparison with the well-studied clusters M3, M13, and M92. Final values ofE(B-V)=0.17±0.05 and (M v-V)=14.0±0.3 are proposed. The dependence on metallicity of these values is briefly discussed.

The results of photometric and spectroscopic observations of dwarf novae are presented. The data were obtained during an international program of multiwavelength observations, held in 1986 February at several observatories, of dwarf novae during the first and subsequent days of outburst. During the campaign numerous dwarf novae were monitored in order to catch them in outburst. Preliminary results and analysis of some objects are reported elsewhere. A total of 30 dwarf novae were observed in the northern and southern hemispheres. Among them 37% were caught in outburst, including 10% on the rise to outburst and 17% in decline. Photometric observations were carried out in the UBVRI system and colour indexes were calculated. Colour-colour diagrams and light curves of the particular stars were constructed. U - B, B - V and V - R, B - V diagrams are presented in Figs. 1 and 2 respectively. The data shown in Figs. 1 and 2 confirm many results obtained previously, and shows clustering of the objects, depending on their orbital periods, above the main sequence at minimum (Echevarria 1984; Echevarria, Costero & Michel 1993). This region is a very large one, reflecting differences in types of dwarf novae. SU UMa type stars and other short period systems are considerably bluer in both U - B and B - V colours. During an outburst cycle, the systems trace a loop on the colour-colour diagram, with the general pattern shown in the U - B, B - V diagram.

The first results of BVRI CCD photometry of the cluster IC 166, obtained at the new telescope IAC80 at the Observatorio del Teide (Tenerife, Spain) are presented. Using the Daophot crowded field photometric package, different color-magnitude diagrams were constructed and some cluster properties (reddening, distance and age) studied.

We present the results of a general programme aimed to study the effects of metallicity on the temperature scale of late main sequence stars (F0-K5). A sample of approximately 400 stars with published UBV(RI) and ubvy — β photometry has been collected from the literature. A three years campaign of observations (Alonso et al. 1994b) was carried out to obtain JHK photometry in order to apply the InfraRed Flux Method (IRFM) to derive effective temperatures. The effect of metallicity on Colour-Colour IR diagrams is discussed. The absolute flux calibration in the IR was revised in Alonso et al. (1994a). The effect of metallicity on the bolometric correction has been studied in Alonso et al. (1995) in order to derive bolometric fluxes. The temperatures have been derived by applying the IRFM using new Kurucz models. T eff = f(Colours, [Fe/H], log(g)) relations are obtained for dwarfs covering the ranges 4000K ≤ T eff ≤ 8000K, 3.5 ≤ logg ≤ 5.00, +0.5 ≤ [Fe/H] ≤ −3.00 which expands considerably the database of previous works. These relations are used to check atmosphere models through the analysis of UBV RIJHKubvy — β synthetic photometry in combination with the IRFM. The transformation from the theoretical HR diagram into an observational one is analyzed with the new relations. The influence of these points on the study of the evolution of the Galaxy is briefly discussed.

The results of photometric and spectroscopic observations of dwarf novae are presented. The data were obtained during an international program of multiwavelength observations, held in 1986 February at several observatories, of dwarf novae during the first and subsequent days of outburst. During the campaign numerous dwarf novae were monitored in order to catch them in outburst. Preliminary results and analysis of some objects are reported elsewhere. A total of 30 dwarf novae were observed in the northern and southern hemispheres. Among them 37% were caught in outburst, including 10% on the rise to outburst and 17% in decline. Photometric observations were carried out in the UBVRI system and colour indexes were calculated.

The sign of coefficient $a(3)$ in the general formula of Table 2 should be plus instead of minus. Thus, the formula should read: $$ \theta_{\rm eff}=a_{0} + a_{1} X + a_{2} X^{2} + a_{3} X {\rm [Fe/H]} + a_{4} {\rm [Fe/H]} + a_{5} {\rm [Fe/H]}^{2}. $$

The first results of BVRI CCD photometry of the cluster IC 166, obtained at the new telescope IAC80 at the Observatorio del Teide (Tenerife, Spain) are presented. Using the Daophot crowded field photometric package, different color-magnitude diagrams were constructed and some cluster properties (reddening, distance and age) studied.

We present a spectroscopic analysis for the gravity determination of τ Ceti on the basis of a new and high quality set of data. The iron lines are studied by using the Oxford oscillator strengths. The results are compared with those obtained with “solar” oscillator strengths. Non-LTE effects seem to be important in this star. The Fel at λ 526.955 nm line is used to apply the Blackwell and Willis (1977) method to determine the surface gravity. The derived log g is 4.70±0.1.

An observational test of the binary hypothesis for the origin of the blue straggler (BS) stars has been performed y searching for radial velocity variables among 27 BS in five galactic clusters. The significance of the BS phenomenon for the interpretation of evolutionary synthesis models and the spectra of elliptical galaxies is briefly discussed.

E-health is form of health created to improve the health status of patients through Internet and other related technologies. It is an expanding concept being applied in lots of countries because of its benefits. With it, telemedicine is evolving. Telemedicine uses IT‟s to improve patient‟s outcomes with services such as diagnosis, treatments, prevention disease and so on. The objective of this document is to compare different projects being realised in Spain, and in particular, in the Catalonia Region. To do so, it introduces e-health, telemedicine and other related terms. It also describes the actual situation in Spain regarding these subjects. It provides a description of different telemedicine projects dealt in Catalonia and Spain, as well as a detailed and structured description of the project PALANTE and its pilots, specially the Spanish ones. It defines a taxonomy model to classify all the projects and the Spanish pilots so that they can be compared to view the differences between them, and the tendency that the telemedicine sector is heading to. The different resulting ideas that have been extracted are: There are projects that full monitor the patients with oximeters, sensors, spirometers…. This full monitoring is closed related to a service that tries to prevent a relapse from patients, which causes a reduction on the readmission of them. Several projects offer patients a virtual platform or portal to manage their health. This one should include (some ones already do) a drug intake schedule and an educational service. The latest projects developed are trying to give access to electronic health records (EHR) to their patients. The projects are trying to use ICT‟s to get a synchronous link between patients and health professionals. Outgoing

CCD photometry for stars in three fields centered on the old open cluster NGC 188 is presented, with the aim of investigating the HR diagram distribution of cluster main-sequence stars. A sequence of subgiant, turnoff, and main-sequence stars has been detected, extending the observed lower main sequence down to about m(v) = 20 mag. It is found that the observed color-magnitude diagram appears well fitted by a theoretical isochrone for an age of about 6-billion yr, provided that Yale transformations from the theoretical into the observational plane are assumed. From the distribution of the stellar luminosities, it is found that the turnoff stars should have masses of about 1.3 solar mass. The cluster evolutionary scenario is discussed in connection with the reported luminosity of the clump of He-burning giants. 21 refs.

Desenvolupament d'un sistema assistit per visió per computador capaç d'identificar si en una biòpsia hi ha presència de càncer de mama o no. Development of a vision computer system that will able to identify whether cancer is present in a breast biopsy

The paper reports partially simultaneous observations of the 'rapid burster' (MXB 1730-335) at X-ray, infrared, and radio wavelengths, covering several hundred hours during 1979 and 1980. None of the authors of this report saw any infrared or radio bursts. On several occasions an absence of infrared bursting was observed during X-ray bursting. On one occasion an absence of X-ray bursting was observed during a radio burst (4.1 GHz) reported by Calla et al. (1979). To date, radio bursts (a total of at least a dozen) have been reported only by Calla et al. (1980). Considering these and other observations summarized here, the reported radio bursts are either unreal or do not bear a simple relation to the X-ray bursts from the 'rapid burster'. The status of the reported infrared bursts also remain ambiguous. Limits to the brightness of any persistent radio source at the position of MXB 1730-335, limits to persistent X-ray emission during an extended X-ray quiet phase, and a measurement of the infrared polarization in the direction of the X-ray source are also reported.

Se determinan empíricamente las relaciones temperatura efectiva-color-metalicidad para estrellas de Secuencia Principal con tipos espectrales comprendidos en el rango FO-K5. Para ello se obtuvo la fotometría en las bandas J,H y K para 360 estrellas, se estableció la calibración absoluta de la estrella Vega en las longitudes de onda efectivas de las bandas fotométricas consideradas, se determinaron los flujos cromáticos infrarrojos de las estrellas del programa y se estudió el efecto de la metalicidad sobre los flujos bolométricos de las estrellas enanas con tipos espectrales F, G y K. También se determina la temperaturas de unas 500 estrellas utilizando una red homogénea de modelos de atmósfera teóricos que incluyen nuevas opacidades asociadas a líneas metálicas débiles.