Catálogo de publicaciones - libros

We apply an evolutionary SED model of starbursts to submm galaxies, in order to predict the present-day colour, magnitude, and size of submm galaxies. The reproduced colour-magnitude and size-magnitude relation of present-day descendants of submm galaxies suggest that they are progenitor of elliptical galaxies on average, if the IMF of submm galaxies is slightly flatter than the Salpeter IMF.

A complete sample of roughly 1800 morphologically classified galaxies in the Sloan Digital Sky Survey (SDSS) is used in order to study the amount of light in bulges and disks, after a detailed two-dimensional bulge to disk decomposition is performed. We conclude that at low redshift (55 ± 2)% of the total light resides in the disk component, for a cosmological model with  = 0.3,  = 0.7 and  = 0.7.

The European Large Area ISO Survey [10, ELAIS] was the largest Open Time project carried out with the Infrared Space Observatory [3, ISO], mapping areas of about 12 deg at 15 and 90 m and smaller areas at 7 and 175 m with the ISOCAM [1] and ISOPHOT [8] cameras. Thanks to an extensive multi-wavelength coverage [11], the ELAIS fields have now arguably become the best studied sky areas of their size, and natural targets of on-going or planned large-area surveys with the most powerful ground and space-based facilities. Thus the need of reducing such data with the uttermost care and provide the community with an agreed-upon legacy from the ISO mission.

Early-type (E/SO) galaxies follow tight relations such as the Fundamental Plane, the Color-Magnitude Relation or the Mg– relation (Bender et al. 1992). However little is known about the relation between their morphological shapes and stellar populations (Conselice 2003), most likely because these two fields rely on methods that have grown up separately. Here we explore possible correlations between the Sérsic index , and relevant stellar population parameters.

A basic but crucial step toward our understanding of the evolution of the Universe and the objects within it is a complete accounting of the systems which produce the far-infrared background light. Once identified, the relationship between these populations and their role in the formation of galaxies must be determined. In this paper we focus on two equally interesting high-redshift populations: the submillimeter (submm) bright galaxies and the Extremely Red Objects (EROs).

We present a determination of the optical/UV AGN luminosity function and its evolution, based on a large sample of faint ( < 24) QSOs identified in the COMBO-17 survey. Using multi-band photometry in 17 filters within 350 nm < bs < 930 nm, we could simultaneously determine photometric redshifts with an accuracy of ≃ 0.03 and obtain spectral energy distributions. We select a sample covering the redshift range across 1.2 <  < 4.8. Even at ≃ 3, the sample reaches below luminosities corresponding to = –23, conventionally employed to distinguish between Seyfert galaxies and quasars.

We have imaged the Chandra Deep Field South (CDFS) among other fields for the COMBO-17 survey. We used the Wild Field Imager at the MPG/ESO-2.2-m telescope at La Silla, Chile, to observe 17 passbands from 350 to 930 nm (UBVRI plus 12 medium-bands). Such a photometric dataset allows quite reliable multi-colour classification and accurate photometric redshift estimation. The resulting object catalogue for the CDFS contains ~ 100 QSOs, ~ 1000 stars and ~ 10000 galaxies at  < 24. A further 50000 objects fainter than that are included in the catalogue, but have much less reliable redshifts. This catalogue was drawn from a deep R-band image with = 26.0 and 0.75 coadded PSF. It covers an area of 31.5 × 30 centered on  = 03 32 25 and  = –27° 48 50.

One approach to studying the epoch of galaxy formation is to infer formation redshifts from the ages of galaxies at known redshifts. When observed with optical instruments, galaxies lying at redshifts of z ~ 1 reveal their restframe UV spectra, which contain some features that show promise for breaking age-metallicity degeneracies inherent in techniques used for estimating galaxy ages. Early-type galaxies around the z ~ 1 epoch are of additional interest because they lie only a few Gyrs after the probable peak when galaxy mergers occurred. The spectra of young galaxies, such as these merger products, with ages of 1–5 Gyr are much more distinguishable than those of older galaxies, which results in more accurate age estimates.

We have studied in detail the properties of local active star-forming galaxies from the UCM survey, and in particular their star-formation histories. We have quantified the relative importance of the current episode of star formation in comparison to the underlying stellar populations. We have also determined the total stellar mass function and burst mass function for the UCM sample using a M/L calculated for each galaxy. Integrating this mass function we obtained a value for the stellar mass density of current star-forming galaxies in the local Universe.

Powerful radio sources mark the locations of massive galaxies. The -band ‘Hubble’ diagram shows that radio hosts form the bright envelope of near-infrared sources at every observed redshift [1]. Within the context of biased galaxy formation, massive galaxies mark the peaks in the overall density distribution [2,3]. We have exploited this correspondence to identify galaxy overdensities in the high-redshift Universe.