Catálogo de publicaciones - libros

The UKIRT Infrared Deep Sky Survey (UKIDSS) is scheduled to commence in mid 2004, using the new Wide-Field Camera (WFCAM) to carry out a major series of long-term public surveys. Data will become public to the entire ESO community immediately. In this paper I briefly describe the camera and the UKIDSS survey plans, highlighting the Ultra-Deep Survey in particular which plans to reach depths of K=23, H=24 and J=25 over an unprecedented 0.8 deg region. This will map an enormous volume of the high-redshift Universe, providing the first detailed picture of large scale structure at ~ 3.

To collect informations is often boring and time consuming task. For this reason, we thought that a collection of information about the known surveys may be useful especially for planning future work. We collected information available in literature on completed, work in progress and planed surveys. The list of surveys may not be complete but we are willing to update it (and distribute it) upon request.

Insensitive to dust obscuration, radio wavelengths are ideal to study star-forming galaxies free of dust induced biases. Using data from the Phoenix Deep Survey, we have identified a sample of star-forming extremely red objects (EROs). Stacking of the radio images of the radio-undetected star-forming EROs revealed a significant radio detection. Using the expected median redshift, we estimate an average star-formation rate of 61 M yr for these galaxies.

We have analyzed the structure of bulges of early-to intermediate-type spirals, on nuclear and global scales, using NIR imaging together with ground-based NIR imaging. The goals are (a) to see whether results on bulge structure derived from ground-based, 1” FWHM seeing data remain valid when high-resolution data are used; (2) to compare nuclear properties of bulges to those of ellipticals; and (3) to provide bulge-disk scaling relations based on accurate profile decompositions employing the data. Details are presented in Balcells et al. (2003, 2004a, 2004b).

We analyze the distribution in color versus absolute magnitude of a low-redshift sample of galaxies from the Sloan Digital Sky Survey [4]. For each magnitude bin, the color function can be approximated as the sum of two normal Gaussians, a bimodal function. Thus, the distribution can be deconvolved into two dominant components that have associated color-magnitude relations, dispersion-magnitude relations and luminosity functions. This differs from the classical approach of using cuts in morphology or color to define classes and instead allows for a natural overlap. The observed distribution and the deconvolved red and blue distributions are shown in Fig. 1. We describe some of the results and points to note about the figure, below. For full details, see [1].

The central regions of superclusters, being the observative counterpart of the intersections of the large scale filaments, are the formation loci of rich galaxy clusters. In these environments, the fraction of merging is enhanced and the probability of a major merging (the collision of similar mass clusters) event is high. In these conditions it is possible to study not only such mergings but also the related astrophysical consequences, like the formation of radio halos and relics and the effect on the emission of the galaxy population. Here we present our recent results on the A3558 complex and the A3528 cluster in the Shapley Concentration and on the A2061-A2067 pair in the Corona Borealis supercluster.

Luminous Blue Compact Galaxies (BCGs) have low metallicities, high gas consumption rates and are frequently involved in mergers. These are properties characteristic of young galaxies in the hierarchical formation scenario. Local BCGs can therefore be used as a complement to high redshift studies provided that the evolution of BCGs can be understood in more detail and be applied to early galaxy formation. Although much is known about the central starburst, few studies discuss the relation between the starburst and the progenitor, or the “host galaxy” of the starburst. Here we report of an effort to derive information about the host from the colours of the faint halo.

We present a new method of constraining the star formation histories and hence the stellar M/L ratios by using the multicolor technique in COMBO-17 [7]. It estimates the stellar M/L ratio at the observed wavelength = 815 nm for each single galaxy on the basis of color information from 5 broadband and 12 medium band filters. The 815 nm mass estimations are in very good agreement to the masses derived from public , and data from the ESO Imaging survey [4] in a tiny area (5% of one of our fields). The stellar mass distribution in the range 0.1<<0.3 is compared to the result of Kauffmann et al. [5] for SDSS galaxies and shows a good agreement. Considering only galaxies with  > 3 × 10 M, we find that the integrated stellar mass density in galaxies increased by a factor of about 1.5 since redshift 1.0.

The cosmologically significant population of dusty galaxies detected at sub-mm and mm wavelengths by SCUBA and MAMBO have played a central part in many of the discussions at this workshop. Obtaining their redshifts is critical in understanding their role in galaxy formation and evolution, but this is a challenging task. Nevertheless, Chapman et al. [1] have made significant process by obtaining spectroscopic redshifts of the subset of sub-mm galaxies detected in deep radio images that have optical counterparts. This exploits the well-known Far-Infrared/Radio correlation, and allows the high resolution radio maps to be used as a surrogate for finding the correct optical counterpart for which spectroscopy can then be attempted.

Up-to-date theoretical SED of stellar populations at 2 Å FWHM resolution is obtained by coupling a new library of synthetic spectra from the ATLAS and NextGen atmosphere database with the Buzzoni population synthesis code. We briefly outline the current status of the project, aimed at settling a new theoretical framework of narrow-band spectrophotometric indices to study stellar populations of galaxies.