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Enhancing Stellar Spectroscopy with Extreme Adaptive Optics and Photonics

Jovanovic, N. and Schwab, C. and Cvetojevic, N. and Guyon, O. and Martinache, F. (2016) Enhancing Stellar Spectroscopy with Extreme Adaptive Optics and Photonics. Publications of the Astronomical Society of the Pacific, 128 (970). Art. No. 121001. ISSN 0004-6280. http://resolver.caltech.edu/CaltechAUTHORS:20190415-143514279

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Abstract

Extreme adaptive optics (AO) systems are now in operation across the globe. These systems, capable of high order wavefront correction, deliver Strehl ratios of ~90% in the near-infrared. Originally intended for the direct imaging of exoplanets, these systems are often equipped with advanced coronagraphs that suppress the on-axis-star, interferometers to calibrate wavefront errors, and low order wavefront sensors to stabilize any tip/tilt residuals to a degree never seen before. Such systems are well positioned to facilitate the detailed spectroscopic characterization of faint substellar companions at small angular separations from the host star. Additionally, the increased light concentration of the point-spread function and the unprecedented stability create opportunities in other fields of astronomy as well, including spectroscopy. With such Strehl ratios, efficient injection into single-mode fibers (SMFs) or photonic lanterns becomes possible. With diffraction-limited components feeding the instrument, calibrating a spectrograph's line profile becomes considerably easier, as modal noise or imperfect scrambling of the fiber output are no longer an issue. It also opens up the possibility of exploiting photonic technologies for their advanced functionalities, inherent replicability, and small, lightweight footprint to design and build future instrumentation. In this work, we outline how extreme AO systems will enable advanced photonic and diffraction-limited technologies to be exploited in spectrograph design and the impact it will have on spectroscopy. We illustrate that the precision of an instrument based on these technologies, with light injected from an efficient SMF feed would be entirely limited by the spectral content and stellar noise alone on cool stars and would be capable of achieving a radial velocity precision of several m/s; the level required for detecting an exo-Earth in the habitable zone of a nearby M-dwarf.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1088/1538-3873/128/970/121001DOIArticle
https://arxiv.org/abs/1609.06388arXivDiscussion Paper
ORCID:
AuthorORCID
Guyon, O.0000-0002-1097-9908
Martinache, F.0000-0003-1180-4138
Additional Information:© 2016 The Astronomical Society of the Pacific. Original content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2016 May 25; accepted 2016 September 2; published 2016 November 8. This research was supported by the Australian Research Council Centre of Excellence for Ultrahigh bandwidth Devices for Optical Systems (project number CE110001018). The authors acknowledge support from the JSPS (Grant-in-Aid for Research #23340051 & #26220704). We would like to thank Yulia Gurevich for help with the manuscript.
Funders:
Funding AgencyGrant Number
Australian Research CouncilCE110001018
Japan Society for the Promotion of Science (JSPS)23340051
Japan Society for the Promotion of Science (JSPS)26220704
Subject Keywords:instrumentation: adaptive optics – instrumentation: high angular resolution – instrumentation: spectrographs
Record Number:CaltechAUTHORS:20190415-143514279
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20190415-143514279
Official Citation:N. Jovanovic et al 2016 PASP 128 121001
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:94715
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:16 Apr 2019 23:41
Last Modified:16 Apr 2019 23:41

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