Abstract: For several years we have collected photometric and spectroscopic information, in a wide range of wavelengths, for a large, isolated, and massive star formation complex in the outer border of NGC 6946. Despite the considerable observational effort, the nature and origin of this object still remain elusive. In this talk we'll show the pieces of the puzzle and ask to the kind public for its best collaboration.

Enmarcado en el proyecto del estudio de la estructura de la galaxia subyacente de las compactas azules (BCDs) a partir de su modelado 2D, se presenta una comparación entre ajustes en una y dos dimensiones a las posibles estructuras de algunas de las galaxias de la muestra.

Previous attempts to model the emission line intensity ratios in the DIG of spiral galaxies have failed to explain some of the observed trends. Moreover, the physical basics underlying the models are not understood. This leads to distinguish classical HII regions from the more diffuse gas in the DIG. We present 1D photoionization models that, with a correct geometrical interpretation of the observations, account for all the observed trends and naturally explains the underlying physics in the behaviour of the emission line ratios.

The LMC4 region of the Large Magellanic Cloud hosts the unique system of 5 possible stellar arcs, of which two have the small age range of their stars and clusters and are the perfect segments of circles, thus being surely the real physical structures, whose coherent formation was triggered by some event(s). It is demonstrated that neither central pressure sources (SNe/O-stars), nor the cloud infall might be such events. The arc-shaped working surfaces of some jets from radio galaxies nuclei are most similar morphologically to the LMC stellar arcs. These arcs were probably triggered by some jets, the origin of which is discussed.

We present the multiphase chemical evolution model applied to dwarf galaxies using new low and intermediate mass stars yields. These yields are based on a careful modelling of the TP-AGB phase, that affects mainly the production of Nitrogen and Carbon

We present a study of the stellar population in Low Luminosity Active Galactic Nuclei (LLAGN). Our goal is to search for spectroscopic signatures of young and intermediate age stars, and to investigate their relationship with the ionization mechanism in LLAGN. The method used is based on the stellar population synthesis of the optical continuum of the innermost (20-100 pc) regions in these galaxies. For this purpose, we have collected high spatial resolution optical (2900-5700 A) STIS spectra of 28 nearby LLAGN, plus UV-optical SED of a few LLAGNs that are available in the Hubble Space Telescope archive, in addition to 51 ground-based optical spectra of LLAGNs. Our main findings are: (1) No features due to Wolf-Rayet stars were convincingly detected in the STIS spectra. (2) Young stars contribute very little to the optical continuum in the ground-based aperture. However, the fraction of light provided by these stars is higher than 10% in most of the weak-[OI] ([OI]/Halpha $\leq$ 0.25) LLAGN STIS spectra. (3) Intermediate age stars contribute significantly to the optical continuum of these nuclei. This population is more frequent in objects with weak than with strong [OI]. Weak-[OI] LLAGN that have young stars stand out for their intermediate age population. (4) Most of the strong-[OI] LLAGN have predominantly old stellar population. Few of these objects also show a feature-less continuum that contributes significantly to the optical continuum. These results suggest that young and intermediate age stars do not play a significant role in the ionization of LLAGN with strong [OI]. However, the ionization in weak-[OI] LLAGN with young and/or intermediate age population could be due to stellar processes. A comparison of the properties of these objects with Seyfert 2 galaxies that harbor a nuclear starburst, suggests that weak-[OI] LLAGN are the lower luminosity counterparts of the Seyfert 2 composite nuclei.

The environment of clusters provides an ideal laboratory for testing the effects of galaxy density, galaxy interactions and interaction with the intracluster medium on the properties of galaxies. In this respect the analysis of quantitative morphology of cluster galaxies and the study of the diffuse intracluster light can provide useful evolutionary constrains. I will present the results of the quantitative morphology of bright and dwarf galaxies in Coma cluster and the analysis of the intracluster light in Virgo cluster. The results will be discussed in terms of the galaxy evolutionary scenarios for galaxy clusters.

A preliminary work on the study of the starburst knots in a sample of 9 BCDs will be presented. I report the starburst knots catalogues for all the sample of galaxies in both, narrow band photometry in the Balmer emission line Halpha and broad band photometry in the Jonhson filters U, B, V, R and I. Fluxes, luminosities, sizes, SFRs, magnitudes, etc. for each starbursting region are included in the catalogues. Color distributions of the total knots of each galaxy will be compared with other types of dwarf galaxies from the literature.

I will present the last results obtained by our group about the origin of the multiwavelength emission coming from the central 10 pc of NGC 1068. While the standard paradigm attributes this emission to light originated in the active nucleus, and reflected towards our line of sight, I will discuss an alternative model based on an intense starburst episode taking place around the active nucleus. This starburst could be responsible for most of the optical to soft X-rays emission, while the reflected nuclear light would be responsible for the hard X-rays. The nuclear source would also be responsible for most of the mid to far infrared emission detected in this galaxy.

We present a photometric catalog of young stellar clusters in the nuclear starburst of M82 observed with the Hubble Space Telescope WFPC2 in Halpha (F656N) and continuum images. We found 194 super star clusters candidates. The strong extinction in the starburst divide it in five different parts and we present a catalog for each part. We also list all brilliant knots in Halpha and continuum with it position and radius. For the super star clusters candidates we measure it positions, radius and fluxes, and we derive luminosities, masses, equivalent widths, etc.

The purpose of this work is to analyze if variations in the IMF due to its stochastic nature may have important effects on the final chemical abundances measured in the ISM. We show that, efectively, a high dispersion around the expected averaged abundance is possible if the stars form in clusters as small as 10³ or 10⁴ M_☉. This dispersion depends on the stellar cluster mass, decreasing below the error bar when the cluster is 10⁵ M_☉

A catalogue of Young SSCs in the central region of M82 is presented in this meeting by V. Melo. In this talk I describe the new model we have developed to understand the M82 SGW features, which takes into account the presence and distribution of the census SSCs. A comparison with starburts with no SGW is also made.

Among "empirical" methods for estimating oxygen abundances in H II regions, the ratio [O III]/[N II] first introduced by Alloin et al. in 1979 is reappraised with modern data and shown to have certain advantages over the others, notably at high red-shift.

We explore a few examples of the degeneracy of the solutions found when fitting a multiple population to an observed spectrum of a MSFR. We will discuss about the properties of a minimum population basis, and present results if we get some in the ensuing time till the meeting.

We have obtained the V-band luminosity function (LF) of galaxies in the Hercules cluster (Abell 2151). Best fit Schechter parameters have been derived for three different fields across the cluster and for the overall surveyed area. Comparisons between these parameters and analysis of the LFs are also presented.

With the advent of extra large databases from groundbase and space telescopes that immediately become public (and many more to come in the near future) in order to analyse the data the astronomer has, per force, to make use of the most efficient existing computer algorithms and to develop new ones in close collaboration with computer scientists. I will recount the experience we are acquiring in that sense with our colleagues of the Computer Science department at INAOE, and some results we have already obtained in studying the stellar population of young massive clusters in the nuclei of normal and active galaxies.