In this work we analyze the physical properties of a sample of 56
spectroscopically selected star-forming (SF) Ly$\alpha$ emitting
galaxies at 2.0$\lesssim$z$\lesssim$3.5 using both a spectral energy
distribution (SED) fitting procedure from rest-frame UV to mid-IR and
direct 160$\mu$m observations taken with the Photodetector Array Camera
& Spectrometer (PACS) instrument onboard \emph{Herschel Space
Observatory}. We define LAEs as those Ly$\alpha$ emitting galaxies whose
rest-frame Ly$\alpha$ equivalent widths (Ly$\alpha$ EW$_{rest-frame}$)
are above 20\AA, the typical threshold in…
In this work we focus on the evolution of the SFR, metallicity of the
gas, and morphology of galaxies at low redshift in search of signs of
evolution. We analyzed the evolution of the SFR, metallicity, and
morphology, through the mass-metallicity, luminosity-metallicity, SFR-stellar mass, and SFR-metallicity relationships of star-forming
galaxies from SDSS-DR5 (Sloan Digital Sky Survey-Data Release 5), using
redshift intervals in bins of 0.1 from ˜ 0 to 0.4We used data
processed with the STARLIGHT spectral synthesis code, correcting the
fluxes for dust extinction, and estimating…
The OTELO project is the extragalactic survey currently under way using
the tunable filters of theinstrument OSIRIS at the GTC. OTELO is
providing the deepest emission line object survey of the universe up to
a redshift 7. In this contribution, the first images will be shown
together with some preliminary results.
Despite their brightness at maximum, classical novae are very faint at
minimum light implying little or no follow up at all during quiescence.
In fact, about 3/4 of the 204 novae that erupted before 1980 still lack
spectroscopic observations or even an unambiguous identification of the
post-nova. We embarked on a project aimed at deriving the physical
properties of old novae decades after the explosion thus placing
post-novae in the framework of CV-evolution and being able to compare
the characteristics of the eruption with the characteristics of the
remnant. We present an overview of this project as well as preliminary
results.
