Open AccessThe FALCON concept: multi‐object adaptive optics and atmospheric tomography for integral field spectroscopy – principles and performance on an 8‐m telescope
Author(s) -
Assémat F.,
Gendron E.,
Hammer F.
Publication year - 2007
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2007.11422.x
Subject(s) - physics , adaptive optics , integral field spectrograph , telescope , galactic astronomy , spectrograph , observatory , galaxy , astronomy , angular resolution (graph drawing) , very large telescope , sky , field of view , cardinal point , spectral resolution , astrophysics , optics , milky way , mathematics , combinatorics , spectral line
Integral field spectrographs are major instruments with which to study the mechanisms involved in the formation and the evolution of early galaxies. When combined with multi‐object spectroscopy, those spectrographs can behave as machines used to derive physical parameters of galaxies during their formation process. Up to now, there has been only one available spectrograph with multiple integral field units, i.e. FLAMES/GIRAFFE on the European Southern Observatory (ESO) Very Large Telescope (VLT). However, current ground‐based instruments suffer from a degradation of their spatial resolution due to atmospheric turbulence. In this article we describe the performance of FALCON, an original concept of a new‐generation multi‐object integral field spectrograph with adaptive optics for the ESO VLT. The goal of FALCON is to combine high angular resolution (0.25 arcsec) and high spectral resolution ( R > 5000) in the J and H bands over a wide field of view (10 × 10 arcmin 2 ) in the VLT Nasmyth focal plane. However, instead of correcting the whole field, FALCON will use multi‐object adaptive optics (MOAO) to perform the adaptive optics correction locally on each scientific target. This requires us then to use atmospheric tomography in order to use suitable natural guide stars for wavefront sensing. We will show that merging MOAO and atmospheric tomography allows us to determine the internal kinematics of distant galaxies up to z ≈ 2 with a sky coverage of 50 per cent, even for objects observed near the Galactic pole. The application of such a concept to extremely large telescopes seems therefore to be a very promising way to study galaxy evolution from z = 1 to redshifts as high as z = 7.