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2. ULTIMATE-Subaru: GLAO preliminary design overview

Author

Yosuke Minowa, Yoshito Ono, Yoko Tanaka, Hiroshige Yoshida, Koki Terao, Yusei Koyama, Sadman Ali, Ichi Tanaka, Takashi Hattori, Hirofumi Okita, Yutaka Hayano, Shin Oya, Kentaro Motohara, Kenshi Yanagisawa, Michitoshi Yoshida, Masayuki Akiyama, Tadayuki Kodama, Hajime Ogane, Masahiro Konishi, Noelia Martínez Rey, Nicholas Herrald, Céline d'Orgeville, François Rigaut, Israel Vaughn, David Chandler, Dionne Haynes, Warrick Schofield, Shiang-Yu Wang, Chi-Yi Chou, and Masahiko Kimura

Published
2022

6. MAVIS: imager and spectrograph

Author

Simon . Ellis, Anthony Horton, Christian Schwab, Timothy Chin, Robert Content, Nuwanthika Fernando, Nuria Lorente, Richard McDermid, Mahesh Mohanan, Helen McGregor, Jacob Pember, David Robertson, Scott Smedley, Will Saunders, Lew Waller, Ross Zhelem, Jessica Zheng, Johan Kosmalski, Giovanni Cresci, Trevor Mendel, Andrea Bianco, David Brodrick, Jennifer Burgess, Dionne Haynes, Davide Greggio, François Rigaut, and Alessio Zanutta

Published
2022

7. The MAVIS Image Simulator: predicting the astrometric performance of MAVIS

Author

Giuseppe Bono, Dionne Haynes, Mojtaba Taheri, Daniele Vassallo, Giuliana Fiorentino, Jesse Cranney, Stephanie Monty, Guido Agapito, Cedric Plantet, Richard M. McDermid, Christian Schwab, J. Trevor Mendel, Davide Greggio, and Francois Rigaut

Subjects
Photometry (optics), Point spread function, Computer science, Globular cluster, High spatial resolution, Astrometry, High order, Residual, Simulation
Abstract

"We present initial results from the Multi-conjugate Adaptive-optics Visible Imager-Spectrograph Image Simulator (MAVISIM) to explore the astrometric capabilities of the next generation instrument MAVIS. A core scientific and operational requirement of MAVIS will be to achieve highly accurate differential astrometry, with accuracies on the order that of the extremely large telescopes. To better understand the impact of known and anticipated astrometric error terms, we have created an initial astrometric budget which we present here to motivate the creation of MAVISIM. In this first version of MAVISIM we include three major astrometric error sources; point spread function (PSF) field variability due to high order aberrations, PSF degradation and field variability due to tip-tilt residual error, and field distortions due to non-common path aberrations in the AO module. An overview of MAVISIM is provided along with initial results from a study using MAVISIM to simulate an image of a Milky Way-like globular cluster. Astrometric accuracies are extracted using PSF-fitting photometry with encouraging results that suggest MAVIS will deliver accuracies of 150µas down to faint magnitudes."

Published
2020

8. First demonstration of OH suppression in a high efficiency near-infrared spectrograph

Author

Dionne Haynes, Sylvain Veilleux, Lisa J. Kewley, Markus Roth, Seong-sik Min, Kalaga Madhav, Ross Zhelem, Domenico Giannone, Joss Bland-Hawthorn, Christopher H. Betters, Rob Sharp, W. Couch, Aashia Rahman, Simon Ellis, R Haynes, Naveen Pai, Scott Case, E. Hernandez, Lee R. Spitler, Sergio G. Leon-Saval, Anthony Horton, Richard M. McDermid, and Jon Lawrence

Subjects
Physics, Brightness, business.industry, media_common.quotation_subject, Near-infrared spectroscopy, FOS: Physical sciences, Astronomy and Astrophysics, Rotational–vibrational spectroscopy, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 010309 optics, Atmosphere, Optics, Space and Planetary Science, Sky, 0103 physical sciences, Photonics, Astrophysics - Instrumentation and Methods for Astrophysics, Spectroscopy, business, 010303 astronomy & astrophysics, Spectrograph, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, media_common
Abstract

Ground-based near-infrared astronomy is severely hampered by the forest of atmospheric emission lines resulting from the rovibrational decay of OH molecules in the upper atmosphere. The extreme brightness of these lines, as well as their spatial and temporal variability, makes accurate sky subtraction difficult. Selectively filtering these lines with OH suppression instruments has been a long standing goal for near-infrared spectroscopy. We have shown previously the efficacy of fibre Bragg gratings combined with photonic lanterns for achieving OH suppression. Here we report on PRAXIS, a unique near-infrared spectrograph that is optimised for OH suppression with fibre Bragg gratings. We show for the first time that OH suppression (of any kind) is possible with high overall throughput (18 per cent end-to-end), and provide examples of the relative benefits of OH suppression., Comment: Accepted for publication in MNRAS

Published
2020
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9. 4MOST

Author

Roelof S. de Jong, Olga Bellido-Tirado, Cristina Chiappini, Éric Depagne, Roger Haynes, Diana Johl, Olivier Schnurr, Axel Schwope, Jakob Walcher, Frank Dionies, Dionne Haynes, Andreas Kelz, Francisco S. Kitaura, Georg Lamer, Ivan Minchev, Volker Müller, Sebastián E. Nuza, Jean-Christophe Olaya, Tilmann Piffl, Emil Popow, Matthias Steinmetz, Ugur Ural, Mary Williams, Roland Winkler, Lutz Wisotzki, Wolfgang R. Ansorge, Manda Banerji, Eduardo Gonzalez Solares, Mike Irwin, Robert C. Kennicutt, Dave King, Richard G. McMahon, Sergey Koposov, Ian R. Parry, David Sun, Nicholas A. Walton, Gert Finger, Olaf Iwert, Mirko Krumpe, Jean-Louis Lizon, Mainieri Vincenzo, Jean-Philippe Amans, Piercarlo Bonifacio, Mathieu Cohen, Patrick Francois, Pascal Jagourel, Shan B. Mignot, Frédéric Royer, Paola Sartoretti, Ralf Bender, Frank Grupp, Hans-Joachim Hess, Florian Lang-Bardl, Bernard Muschielok, Hans Böhringer, Thomas Boller, Angela Bongiorno, Marcella Brusa, Tom Dwelly, Andrea Merloni, Kirpal Nandra, Mara Salvato, Johannes H. Pragt, Ramón Navarro, Gerrit Gerlofsma, Ronald Roelfsema, Gavin B. Dalton, Kevin F. Middleton, Ian A. Tosh, Corrado Boeche, Elisabetta Caffau, Norbert Christlieb, Eva K. Grebel, Camilla Hansen, Andreas Koch, Hans-G. Ludwig, Andreas Quirrenbach, Luca Sbordone, Walter Seifert, Guido Thimm, Trifon Trifonov, Amina Helmi, Scott C. Trager, Sofia Feltzing, Andreas Korn, Wilfried Boland, Astronomy, and Kapteyn Astronomical Institute

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Nongalactic Astrophysics (astro-ph.CO), Data products, Computer science, FOS: Physical sciences, Public survey, Object (computer science), Astrophysics - Astrophysics of Galaxies, law.invention, Square degree, Telescope, Conceptual design, law, Astrophysics of Galaxies (astro-ph.GA), Metre, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics, Remote sensing
Abstract

The 4MOST consortium is currently halfway through a Conceptual Design study for ESO with the aim to develop a wide-field (>3 square degree, goal >5 square degree), high-multiplex (>1500 fibres, goal 3000 fibres) spectroscopic survey facility for an ESO 4m-class telescope (VISTA). 4MOST will run permanently on the telescope to perform a 5 year public survey yielding more than 20 million spectra at resolution R~5000 (��=390-1000 nm) and more than 2 million spectra at R~20,000 (395-456.5 nm & 587-673 nm). The 4MOST design is especially intended to complement three key all-sky, space-based observatories of prime European interest: Gaia, eROSITA and Euclid. Initial design and performance estimates for the wide-field corrector concepts are presented. We consider two fibre positioner concepts, a well-known Phi-Theta system and a new R-Theta concept with a large patrol area. The spectrographs are fixed configuration two-arm spectrographs, with dedicated spectrographs for the high- and low-resolution. A full facility simulator is being developed to guide trade-off decisions regarding the optimal field-of-view, number of fibres needed, and the relative fraction of high-to-low resolution fibres. Mock catalogues with template spectra from seven Design Reference Surveys are simulated to verify the science requirements of 4MOST. The 4MOST consortium aims to deliver the full 4MOST facility by the end of 2018 and start delivering high-level data products for both consortium and ESO community targets a year later with yearly increments., To appear in the proceedings of the SPIE Astronomical Instrumentation + Telescopes conference, Amsterdam, 2012. 15 pages, 16 figures

Published
2012

11. Toward a conceptual design for MAVIS

Author

Francois Rigaut, David Brodrick, Guido Agapito, Valentina Viotto, Cedric Plantet, Bernardo Salasnich, Mcdermid, Richard M., Giovanni Cresci, Simon Ellis, Matteo Aliverti, Simone Antoniucci, Andrea Balestra, Andrea Baruffolo, Maria Bergomi, Marco Bonaglia, Giuseppe Bono, Lorenzo Busoni, Elena Carolo, Simonetta Chinellato, Gayandhi De Silva, Simone Esposito, Daniela Fantinel, Jacopo Farinato, Thierry Fusco, Dionne Haynes, Anthony Horton, Gaston Gausachs, James Gilbert, Damien Gratadour, Davide Greggio, Marco Gullieuszik, Pierre Haguenauer, Visa Korkiakoski, Demetrio Magrin, Laura Magrini, Luca Marafatto, Helen McGregor, Trevor Mendel, Stephanie Monty, Benoit Neichel, Fernando Pedichini, Enrico Pinna, Elisa Portaluri, Kalyan Radhakrishnan, Roberto Ragazzoni, David Robertson, Christian Schwab, Rob Sharp, Marco Stangalini, Stefan Stroebele, Elliott Thorn, Annino Vaccarella, Daniele Vassallo, Sudharshan Venkatesan, Lew Waller, Stacy Warner, Frederic Zamkotsian, and Hao Zhang

12. Fiber-based three-dimensional multi-mode interference device as efficient power divider and vector curvature sensor.

Author

Ziyang Zhang, Julia Fiebrandt, Dionne Haynes, Kai Sun, Kalaga Madhav, Andreas Stoll, Kirill Makan, Vadim Makan, and Martin Roth

Subjects
MULTIMODE-mode optical fibers, OPTICAL interference, MULTIPLEXING equipment, PHOTODETECTORS, WAVELENGTH measurement
Abstract

Three-dimensional multi-mode interference devices are demonstrated using a single-mode fiber (SMF) center-spliced to a section of polygon-shaped core multimode fiber (MMF). This simple structure can effectively generate well-localized self-focusing spots that match to the layout of a chosen multi-core fiber (MCF) as a launcher device. An optimized hexagon-core MMF can provide efficient coupling from a SMF to a 7-core MCF with an insertion loss of 0.6 dB and a power imbalance of 0.5 dB, while a square-core MMF can form a self-imaging pattern with symmetrically distributed 2 × 2, 3 × 3 or 4 × 4 spots. These spots can be directly received by a two-dimensional detector array. The device can work as a vector curvature sensor by comparing the relative power among the spots with a resolution of ∼0.1° over a 1.8 mm-long MMF. [ABSTRACT FROM AUTHOR]

Published
2018
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