MATISSE, the VLTI mid-infrared imaging spectro-interferometer
Creators: name: Lopez, B.
name: Lagarde, S.
name: Petrov, R. G.
name: Jaffe, W.
name: Antonelli, P.
name: Allouche, F.
name: Berio, P.
name: Matter, A.
name: Meilland, A.
name: Millour, F.
name: Robbe-Dubois, S.
name: Henning, Th.
name: Weigelt, G.
name: Glindemann, A.
name: Agocs, T.
name: Bailet, Ch.
name: Beckmann, U.
name: Bettonvil, F.
name: van Boekel, R.
name: Bourget, P.
name: Bresson, Y.
name: Bristow, P.
name: Cruzalèbes, P.
name: Eldswijk, E.
name: Caujolle, Y. Fanteï
name: Herrera, J. C. González
name: Graser, U.
name: Guajardo, P.
name: Heininger, M.
name: Hofmann, K. -H.
name: Kroes, G.
name: Laun, W.
name: Lehmitz, M.
name: Leinert, C.
name: Meisenheimer, K.
name: Morel, S.
name: Neumann, U.
name: Paladini, C.
name: Percheron, I.
name: Riquelme, M.
name: Schoeller, M.
name: Stee, Ph.
name: Venema, L.
name: Woillez, J.
name: Zins, G.
name: Ábrahám, P.
name: Abadie, S.
name: Abuter, R.
name: Accardo, M.
name: Adler, T.
name: Alonso, J.
name: Augereau, J. -C.
name: Böhm, A.
name: Bazin, G.
name: Beltran, J.
name: Bensberg, A.
name: Boland, W.
name: Brast, R.
name: Burtscher, L.
name: Castillo, R.
name: Chelli, A.
name: Cid, C.
name: Clausse, J. -M.
name: Connot, C.
name: Conzelmann, R. D.
name: Danchi, W. -C.
name: Delbo, M.
name: Drevon, J.
name: Dominik, C.
name: van Duin, A.
name: Ebert, M.
name: Eisenhauer, F.
name: Flament, S.
name: Frahm, R.
name: Rosas, V. Gámez
name: Gabasch, A.
name: Gallenne, A.
name: Garces, E.
name: Girard, P.
name: Glazenborg, A.
name: Gonté, F. Y. J.
name: Guitton, F.
name: de Haan, M.
name: Hanenburg, H.
name: Haubois, X.
name: Hocdé, V.
name: Hogerheijde, M.
name: ter Horst, R.
name: Hron, J.
name: Hummel, C. A.
name: Hubin, N.
name: Huerta, R.
name: Idserda, J.
name: Isbell, J. W.
name: Ives, D.
name: Jakob, G.
name: Jaskó, A.
name: Jochum, L.
name: Klarmann, L.
name: Klein, R.
name: Kragt, J.
name: Kuindersma, S.
name: Kokoulina, E.
name: Labadie, L.
name: Lacour, S.
name: Leftley, J.
name: Poole, R. Le
name: Lizon, J. -L.
name: Lopez, M.
name: Mérand, A.
name: Marcotto, A.
name: Mauclert, N.
name: Maurer, T.
name: Mehrgan, L. H.
name: Meisner, J.
name: Meixner, K.
name: Mellein, M.
name: Menut, J. L.
name: Mohr, L.
name: Mosoni, L.
name: Navarro, R.
name: Nussbaum, E.
name: Pallanca, L.
name: Pantin, E.
name: Pasquini, L.
name: Duc, T. Phan
name: Pott, J. -U.
name: Pozna, E.
name: Richichi, A.
name: Ridinger, A.
name: Rigal, F.
name: Rivinius, Th.
name: Roelfsema, R.
name: Rohloff, R. -R.
name: Rousseau, S.
name: Salabert, D.
name: Schertl, D.
name: Schuhler, N.
name: Schuil, M.
name: Shabun, K.
name: Soulain, A.
name: Stephan, C.
name: Toledo, P.
name: Tristram, K.
name: Tromp, N.
name: Vakili, F.
name: Varga, J.
name: Vinther, J.
name: Waters, L. B. F. M.
name: Wittkowski, M.
name: Wolf, S.
name: Wrhel, F.
name: Yoffe, G.
Publisher: name: arXiv
Year: 2021
Subjects: subject: Instrumentation and Methods for Astrophysics (astro-ph.IM)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: Context:Optical interferometry is at a key development stage. ESO's VLTI has established a stable, robust infrastructure for long-baseline interferometry for general astronomical observers. The present second-generation instruments offer a wide wavelength coverage and improved performance. Their sensitivity and measurement accuracy lead to data and images of high reliability. Aims:We have developed MATISSE, the Multi AperTure mid-Infrared SpectroScopic Experiment, to access high resolution imaging in a wide spectral domain and explore topics such: stellar activity and mass loss; planet formation and evolution in the gas and dust disks around young stars; accretion processes around super massive black holes in AGN. Methods:The instrument is a spectro-interferometric imager covering three atmospheric bands (L,M,N) from 2.8 to 13.0 mu, combining four optical beams from the VLTI's telscopes. Its concept, related observing procedure, data reduction and calibration approach are the product of 30 years of instrumental research. The instrument utilizes a multi-axial beam combination that delivers spectrally dispersed fringes. The signal provides the following quantities at several spectral resolutions: photometric flux, coherent fluxes, visibilities, closure phases, wavelength differential visibilities and phases, and aperture-synthesis imaging. Results:We provide an overview of the physical principle of the instrument and its functionalities, the characteristics of the delivered signal, a description of the observing modes and of their performance limits. An ensemble of data and reconstructed images are illustrating the first acquired key observations. Conclusion:The instrument has been in operation at Cerro Paranal, ESO, Chile since 2018, and has been open for science use by the international community since April 2019. The first scientific results are being published now.
description: 24 pages, 26 figures, submitted to Astronomy &amp; Astrophysics