Local star-forming galaxies
To study in detail nearby galaxies, i.e. those belonging to the local Universe, is a mandatory first step necessary to understand the results obtained when we observe galaxies at great distances. Our group works to make some light in different topics which are listed bellow. Please, follow the links to complete the information.
Integral Field Spectroscopy in LCBGs
Our group in collaboration with Florida University is involved in the study of a representative sample of Luminous Compact Blue Galaxies (LCBGs) within 100 Mpc selected from the DR4 of the SDSS and the UCM surveys. This project is based on the integral field spectroscopy provided by the instrument PPAK at 3.5m CAHA and is part of a major multiwavelength study which goes from FUV (GALEX) to cm (VLA). Optical PPAK observations provide us with spatially resolved maps of kinematics, extinction, SFR, and metallicity which allow us to study the star formation history, galactic mass, and the role of SN feedback in these starbursts.
Analysis of SINGS data
Our team belongs to the GALEX-SINGS collaboration, obtaining multiband radial profiles for these galaxies with the aim of studying the radial profile of the stellar population and of the dust. SINGS survey is a legacy project of the infrared space observatory Spitzer. Its goal is to study, with spatial resolution, the physical processes connecting star formation to the ISM properties of galaxies, and a vital foundation of data, diagnostic tools, and astrophysical inputs for understanding the distant universe, ultraluminous galaxies, and the formation and evolution of galaxies.
Blue Compact Galaxies
We discovered a huge horseshoe of molecular gas (CO) around the center of the the Blue Compact Galaxy Mrk86. That gas has been swept out from the galaxy's central regions during the evolution of a massive starburst. This process started about 30 million years ago when the first of a series of supernovae in the starburst exploded. This result complemented with previous observations in visible and near-infrared confirm the scenario of a ring of clusters of newly formed stars coinciding with the position of the horseshoe of gas.
Stellar populations and star formation
The main properties of the stellar populations of the UCM survey galaxies has been studied. The recent star-forming bursts that took place in these UCM galaxies are embedded in a evolved stellar population which dominates the total stellar mass of these galaxies.
This was a survey which the aim of finding and analysing emission line galaxies ELGs at low redshift. The UCM survey was carried out using an low dispersion objective-prism with the Schmidt telescope at the german-spanish observatory of Calar Alto. The star-forming galaxies were selected by the presence of Hα emission line in the low resolution spectra registered in the objective-prism 5.5x5.5 square degrees photographic plates (plates 24 cm wide, i.e. plate scale is 86 arcsec/mm).
Densidad de tasa de formación estelar a z=0
Hemos determinado de la densidad de Tasa de Formación Estelar (SFRd) a partir de la luminosidad Hα usando la muestra de galaxias de la Exploración UCM. Obtuvimos una SFRd de 0.013±0.001 Masas solares por año por Mpc³ integrando la función de luminosidad de la figura.
Este trabajo, publicado en 'The Current Star Formation Rate of the Local Universe' 1995, Astrophysical Journal Letters 455, L1 es una referencia en esta línea de investigación. más información
The CAHA-XUV project (Exploring the outer edges of spiral galaxies) aims in characterizing the multi-wavelength properties of the extended UV (XUV) disks recently found by the GALEX satellite in ~10% of late-type nearby galaxies. During the next three years we will be obtaining deep optical and near-infrared imaging and multi-object spectroscopy of a total of 46 northern XUV disks selected from the GALEX Atlas of Nearby Galaxies (Gil de Paz et al. 2007, Ap.J.Suppl.173:185-255,astro-ph/0606440).
The goal of CLUES is to calibrate the [CII]158μm line as a mesure of the Star Formation Rate (SFR) by comparing with other tracers (Hα, UV, IR continuum) and to do it against variations in the properties of the ISM; all with spatial resolution. We will be applying to a Herschel Open Time Key Program aimed to calibrate the fine-structure [CII]158μm line. This line will be routinely observed at low redshift with Herschel and at high redshift with ALMA.