Gemini planet imager observational calibrations V: astrometry and distortion

From National Research Council Canada

DOI	Resolve DOI: https://doi.org/10.1117/12.2056646
Author	Search for: Konopacky, Quinn M.; Search for: Thomas, Sandrine J.; Search for: MacIntosh, Bruce A.; Search for: Dillon, Daren; Search for: Sadakuni, Naru; Search for: Maire, Jérôme; Search for: Fitzgerald, Michael; Search for: Hinkley, Sasha; Search for: Kalas, Paul; Search for: Esposito, Thomas; Search for: Marois, Christian¹; Search for: Ingraham, Patrick J.; Search for: Marchis, Franck; Search for: Perrin, Marshall D.; Search for: Graham, James R.; Search for: Wang, Jason J.; Search for: De Rosa, Robert J.; Search for: Morzinski, Katie; Search for: Pueyo, Laurent; Search for: Chilcote, Jeffrey K.; Search for: Larkin, James E.; Search for: Fabrycky, Daniel; Search for: Goodsell, Stephen J.; Search for: Oppenheimer, B. R.; Search for: Patience, Jenny; Search for: Saddlemyer, Leslie¹; Search for: Sivaramakrishnan, Anand
Name affiliation	National Research Council of Canada. National Science Infrastructure
Format	Text, Article
Proceedings title	Ground-Based and Airborne Instrumentation for Astronomy V
Series title	Proceedings of SPIE; no. 9147
Conference	Ground-Based and Airborne Instrumentation for Astronomy V, June 22-26, 2014
ISSN	0277-786X 1996-756X
ISBN	9780819496157
Article number	914784
Subject	Adaptive optics; Astronomy; Calibration; Distortion (waves); Monte Carlo methods; Spectrographs; astrometry; Gemini Planet Imager; GPI; High contrast imaging; Integral Field Spectroscopy; Pixels
Abstract	We present the results of both laboratory and on sky astrometric characterization of the Gemini Planet Imager (GPI). This characterization includes measurement of the pixel scale∗ of the integral field spectrograph (IFS), the position of the detector with respect to north, and optical distortion. Two of these three quantities (pixel scale and distortion) were measured in the laboratory using two transparent grids of spots, one with a square pattern and the other with a random pattern. The pixel scale in the laboratory was also estimate using small movements of the artificial star unit (ASU) in the GPI adaptive optics system. On sky, the pixel scale and the north angle are determined using a number of known binary or multiple systems and Solar System objects, a subsample of which had concurrent measurements at Keck Observatory. Our current estimate of the GPI pixel scale is 14.14 ± 0.01 millarcseconds/pixel, and the north angle is -1.00 ± 0.03°. Distortion is shown to be small, with an average positional residual of 0.26 pixels over the field of view, and is corrected using a 5th order polynomial. We also present results from Monte Carlo simulations of the GPI Exoplanet Survey (GPIES) assuming GPI achieves ∼1 milliarcsecond relative astrometric precision. We find that with this precision, we will be able to constrain the eccentricities of all detected planets, and possibly determine the underlying eccentricity distribution of widely separated Jovians.
Publication date	2014-07-28
Publisher	SPIE
Language	English
Peer reviewed	Yes
NPARC number	21275511
Export citation	Export as RIS
Report a correction	Report a correction
Record identifier	c634324c-d26b-45f0-a5d2-b506accea13d
Record created	2015-07-14
Record modified	2020-04-22

Report a problem on this page

Date modified:: 2021-03-04