Miguel Sanchez PortalScientist (2007-2016)
Main Research Fields
I'm currently working as a scientist within the Herschel Project Scientist's Group. My main current research interests deal with:
a) The OSIRIS instrument at GTC. OSIRIS is the acronym for "Optical System for Imaging and low-Resolution Integrated Spectroscopy" and is an optical (365-1000 nm) instrument to perform broad and narrow-band imaging with tuneable filters in a large 8.6 x 8.6 armin FOV and multi-object low-resolution spectroscopy. Will be commissioned next year at a Nasmyth focus of the 10.4m GTC telescope at La Palma observatory. I have been involved in the instrument definition since the very beginning.
b) The OTELO survey: the Osiris Tuneable Emission Line Object survey is the OSIRIS key scientific project. This survey is designed to detect Halpha emitters at two windows located at z=0.24 and z=0.4 and it is aimed to be the deepest emission-line survey to date, reaching a flux of 1.0e-18 erg/s/cm^2. The tuneable filter scanning strategy will allow us to separate the Halpha and [NII] lines. Of course, we'll be able to detect other emission lines at different z, e.g. Lyman alpha up to z ~ 6.5. We intend to cover an area of 1 square degree, including "popular" blank fields like HDF-N, Groth, SXDS etc. Our scientific targets include: 1. Study of SFR evolution. 2. AGNs (this is my main topic of interest). 3. High-redshift QSOs. 4. Chemical evolution of the Universe up to z ~1.5. 5. Lyman-alpha emitters up to z~6.5 The survey is intended to provide a sample large enough to carry out the different scientific programs. We expect to detect more than 10,000 emission-line objects. OTELO is aimed to be a multi-wavelength study. For instance, we are currently studying the population of X-ray emitters based on public XMM-Newton and Chandra data. In the future we'll also exploit Herschel's capabilities in the FIR to produce extinction-corrected SFR estimates and to address the study of highly obscured AGNs. We are currently working on a broadband survey (carried out at the WHT 4.2m telescope at La Palma) to provide us with photometric redshifts and information on the morphology of the sample.