We propose the design and construction of TARSIS, a new wide-FoV, blue-optimized, intermediate-resolution Integral Field Spectrograph (IFS). This will be a unique instrument that is able to explore large areas of the sky in blind spectroscopy reaching relatively unexplored wavelengths as blue as 320 nm and until 810 nm.
TARSIS Institutions: Universidad Complutense de Madrid, Instituto de Astrofísica de Andalucía (CSIC), Instituto Nacional de Astrofísica, Óptica y Electrónica (INAOE, Mexico), Universidad de Granada, Universidad de Sevilla, Universidad de Almería, Centro de Astrobiología (INTA-CSIC), Fractal SLNE.
The requirements for the TARSIS instrument are drawn from scientific top-level requirements. In order to achieve them, the TARSIS instrument relies on the replication of 3 high-efficiency, all-refractive, VPH-based, blue-optimized (320-520nm) spectrographs and 1 red-optimized one (510-810nm) based on that developed for MEGARA at GTC. Thus, TARSIS is composed by its focal-plane optics and 4 wavelength-optimized spectrographs & CCDs.
CATARSIS will carry out a magnitude limited (mAB<22.0) spectroscopic survey over an area of 1.7 deg2 with a spectral resolution ranging from R~1000 and a wavelength coverage from 320-810 nm. The fields are chosen to target clusters of galaxies at z~0.15-0.23 up to the infall region and the filaments joining them. We aim at collecting galaxy spectra with high-enough S/N to undertake a detailed analysis of their star formation histories, stellar and nebular abundances, cluster dynamics, etc. The redshift has been chosen so the rest-frame spectra (~278-700 nm) includes the NUV region, essential for detailed analysis of stellar populations, as well as Hα and [NII], needed to cover our science goals. More information on the CATARSIS webpage.
Science Team: The project Science Team includes scientists from all TARSIS Consortium institutions and from other Spanish and foreign research institutions and Universities, mainly members of the CATARSIS Survey team but also part of the “Galactic & Local-Group”, “Solar system” and “ToO” Advisory Groups (AGs). Our science team at-large is composed by Á. Álvarez-Candal (U. Alicante), Y. Ascasibar (UAM), N. Cardiel (UCM), A. Carramiñana (INAOE), E. Carrasco (INAOE), A. Castillo-Morales (UCM), R. Duffard (IAA), A. Ferré Mateu (UB), L. Galbany (UGR), J. Gallego (UCM), M. García (CAB), M. L. García Vargas (Fractal), A. Gil de Paz (UCM), M. A. Gómez-Flechoso (UCM), J. Gorgas (UCM), M. Guerrero (IAA), A. Herrero (IAC), J. Iglesias (IAA), A. Labiano (CAB), A. de Lorenzo-Cáceres (UCM), C. Kehrig (IAA), J. Maíz-Apellániz (CAB), M. Mas (CAB), D. Mayya (INAOE), J. Mendez Abreu (IAC), A. Montaña (INAOE), R. Mújica (INAOE), E. de Oña Wihelmi (ICE), J. Oñorbe (US), S. Pascual (UCM), P. G. Pérez-González (CAB), E. Pérez-Montero (IAA), J. Piqueras (CAB), M. Relaño (UGR), S. Roca-Fàbrega (UCM), D. Rosa (INAOE), S. Sánchez (UNAM), P. Sánchez-Blázquez (UCM), D. Sobral (Lancaster University), E. Terlevich (INAOE), R. Terlevich (INAOE), A. Vazdekis (IAC), J. M. Vílchez (IAA), E. Villaver (CAB), J. Zamorano (UCM), A. Zurita (UGR).
Instrument Team (roles): M. García Vargas (Project Manager), A. Pérez (System Engineer), E. Carrasco (Spectrographs optics leader), R. Izazaga (Optics lab manager), E. Sánchez (Optical Designer), M. Maldonado (Mechanical Engineer), J. Iglesias (Instrument Control System & Outreach and communication), J. Oñorbe (on-site UV tests), N. Cardiel (Scientific Software lead), A. Sánchez (Purchase manager). The ambitious goals of the Scientific Software work-package (WP) are distributed among the following sub-WP leaders: A. Labiano (Simulator), S. Pascual (Data Processing), A. Castillo (Post-Processing), C. Kehrig (Quality Control), V. González (HPC), J. Piqueras (Storage), M. Relaño (CATARSIS tools).