Spectroscopic Cosmological Surveys in the Far-IR

Abstract

We show the feasibility of spectroscopic cosmological surveys with the SAFARI instrument onboard of SPICA. The work is done through simulations that make use of both empirical methods, i.e. the use of observed luminosity functions and theoretical models for galaxy formation and evolution. The relations assumed between the line emission to trace AGN and star formation activity have been derived from the observations of local samples of galaxies. The results converge to indicate the use of blind spectroscopy with the SAFARI FTS at various resolutions to study galaxy evolution from the local to the distant (z∼3) Universe.Specifically, two different and independent galaxy evolution models predict about 7-10 sources to be spectroscopically detected in more than one line in a 2'× 2' SA-FARI field of view, down to the expected flux limits of SAFARI, with about 20% of sources to be detected at z>2. SPICA-SAFARI will be therefore excellent at detecting high-z sources and at assessing in a direct way their nature (e.g whether mainly AGN or Star Formation powered) thanks to blind spectroscopy.

Impact of particles on thePlanckHFI detectors: Ground-based measurements and physical interpretation

“…In this section we discuss in particular how our results can be used to improve the design of new arrays of millimeter detectors for future space missions such as SPICA-SAFARI (Goicoechea et al 2011;Spinoglio et al 2011), PIXIE (Kogut et al 2011), andCORE (CORE Team 2011).…”

The candidate Seyfert 1-like objects found from ULIRGs in the Sloan Digital Sky Survey, 2dF Galaxy Redshift Survey and 6dF Galaxy Survey

“…It should be pointed out that the criteria either in the FIR or in the NIR mentioned above can be used to identify can- didate Seyfert 1-like sources, just because, compared with other sources, Seyfert 1 sources have a flatter spectral continuum (thus blue colors) in the FIR and steeper spectral continuum (thus red colors) in the NIR (e.g. Desai et al 2007;Spinoglio et al 2009). It is noted from the results above that the criterion using the IRAS two-color diagram is more efficient than that using the 2MASS two-color diagram, because 11 sources in Table 2 are candidate Seyfert 1-like sources which is about 30% of the sources, while 14 sources in Table 3 are candidate Seyfert 1-like sources which is only about 7% of the sources.…”