Nulling at short wavelengths: theoretical performance constraints and a demonstration of faint companion detection inside the diffraction limit with a rotating-baseline interferometer
| العنوان: | Nulling at short wavelengths: theoretical performance constraints and a demonstration of faint companion detection inside the diffraction limit with a rotating-baseline interferometer |
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| المؤلفون: | Eugene Serabyn, Sara F. Martin, J Kühn, B. Mennesson, Kurt Liewer |
| المصدر: | Monthly Notices of the Royal Astronomical Society. 489:1291-1303 |
| بيانات النشر: | Oxford University Press (OUP), 2019. |
| سنة النشر: | 2019 |
| مصطلحات موضوعية: | Wavefront, Physics, Beam diameter, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Phase (waves), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, 010309 optics, Azimuth, Telescope, Interferometry, Optics, Space and Planetary Science, law, 0103 physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Adaptive optics, business, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Nuller |
| الوصف: | The Palomar Fiber Nuller (PFN) is a rotating-baseline nulling interferometer that enables high-accuracy near-infrared (NIR) nulling observations with full azimuth coverage. To achieve NIR null-depth accuracies of several x 10-4, the PFN uses a common-mode optical system to provide a high degree of symmetry, single-mode-fiber beam combination to reduce sensitivity to pointing and wavefront errors, extreme adaptive optics to stabilize the fiber coupling and the cross-aperture fringe phase, rapid signal calibration and camera readout to minimize temporal effects, and a statistical null-depth fluctuation analysis to relax the phase stabilization requirement. Here we describe the PFN final design and performance, and provide a demonstration of faint-companion detection by means of nulling-baseline rotation, as originally envisioned for space-based nulling interferometry. Specifically, the Ks-band null-depth rotation curve measured on the spectroscopic binary eta Peg reflects both a secondary star 1.08 +/- 0.06 x 10-2 as bright as the primary, and a null-depth contribution of 4.8 +/- 1.6 x 10-4 due to the size of the primary star. With a 30 mas separation at the time, eta Peg B was well inside both the telescope diffraction-limited beam diameter (88 mas) and typical coronagraphic inner working angles. Finally, we discuss potential improvements that can enable a number of small-angle nulling observations on larger telescopes. 26 pages, 4 figures, accepted for publication in MNRAS |
| تدمد: | 1365-2966 0035-8711 |
| URL الوصول: | https://explore.openaire.eu/search/publication?articleId=doi_dedup___::c652bb535114921029518dbc966a72b5 https://doi.org/10.1093/mnras/stz2163 |
| حقوق: | OPEN |
| رقم الأكسشن: | edsair.doi.dedup.....c652bb535114921029518dbc966a72b5 |
| قاعدة البيانات: | OpenAIRE |
| تدمد: | 13652966 00358711 |
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