The Carlina-type diluted telescope
Stellar fringes on Deneb
1 Aix Marseille Université, CNRS, OHP (Observatoire de Haute Provence), Institut Pythéas UMS 3470, 04870 Saint-Michel-l’Observatoire, France
2 Laboratoire d’Astrophysique de Marseille, Pôle de l’Étoile Site de Château-Gombert, 38 rue Frédéric Joliot-Curie, 13388 Marseille Cedex 13, France
3 Université Nice-Sophia Antipolis, Observatoire de la Côte d’Azur, CNRS UMR 6525, BP 4229, 06304 Nice Cedex, France
4 University of Namur (UNamur), research Center for Physics of Radiation and Matter (PMR-LARN), 61 rue de Bruxelles, 5000 Namur, Belgium
5 Lund Observatory, Box 43, 221 00 Lund, Sweden
6 Instituto de Astronomía – UNAM, Km 103 Carretera Tijuana Ensenada, 422860 Ensenada, B. C., Mexico
Received: 17 July 2014
Accepted: 6 October 2014
Context. The performance of interferometers has been much increased over the past ten years. But the number of observable objects is still limited by the low sensitivity and imaging capability of the current facilities. Studies have been conducted with the aim to propose a new generation of interferometers.
Aims. The Carlina concept studied at the Haute-Provence Observatory consists of an optical interferometer configured as a diluted version of the Arecibo radio telescope: above the diluted primary mirror made of fixed co-spherical segments, a helium balloon or cables that are suspended between two mountains and/or pylons carry a gondola containing the focal optics. This concept does not require delay lines.
Methods. Since 2003, we have been building a technical demonstrator of this diluted telescope. The main goals of this project were to find opto-mechanical solutions to stabilize the optics attached to cables at several tens of meters above the ground, and to characterize this diluted telescope under real conditions. In 2012, we obtained metrology fringes, and co-spherized the primary mirrors within one micron accuracy. In 2013, we tested the whole optical train: servo loop, metrology, and the focal gondola.
Results. We obtained stellar fringes on Deneb in September 2013. We here present the characteristics of these observations: quality of the guiding, signal-to-noise ratio reached, and possible improvements for a future system.
Conclusions. By detecting fringes on Deneb, we confirm that the entire system conceptually has worked correctly. It also proves that when the primary mirrors are aligned using the metrology system, we can directly record fringes in the focal gondola, even in blind operation. It is an important step that demonstrates the feasibility of building a diluted telescope using cables strained between cliffs or pylons. Carlina, like the Multiple Mirror Telescope (MMT) or Large Binocular Telescope (LBT), could be one of the first members of a new class of telescopes named large diluted telescopes. Its optical architecture has many advantages for future projects: Planet Formation Imager (PFI), post-ELTs, interferometer in space.
Key words: instrumentation: high angular resolution / instrumentation: interferometers / telescopes
© ESO, 2015