| DOI | Resolve DOI: http://doi.org/10.1117/12.2055753 |
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| Author | Search for: Wang, Jason J.; Search for: Rajan, Abhijith; Search for: Graham, James R.; Search for: Savransky, Dmitry; Search for: Ingraham, Patrick J.; Search for: Ward-Duong, Kimberly; Search for: Patience, Jennifer; Search for: De Rosa, Robert J.; Search for: Bulger, Joanna; Search for: Sivaramakrishnan, Anand; Search for: Perrin, Marshall D.; Search for: Thomas, Sandrine J.; Search for: Sadakuni, Naru; Search for: Greenbaum, Alexandra Z.; Search for: Pueyo, Laurent; Search for: Marois, Christian1 ; Search for: Oppenheimer, Ben R.; Search for: Kalas, Paul; Search for: Cardwell, Andrew; Search for: Goodsell, Stephen; Search for: Hibon, Pascale; Search for: Rantakyrö, Fredrik T. |
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| Name affiliation | - National Research Council Canada. National Science Infrastructure
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| Type | Article |
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| Proceedings title | SPIE - International Society for Optical Engineering. Proceedings |
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| Conference | Ground-Based and Airborne Instrumentation for Astronomy V, 22 June 2014 through 26 June 2014 |
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| ISSN | 0277-786X |
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| ISBN | 9780819496157 |
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| Volume | 9147 |
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| Article number | 914755 |
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| Subject | Adaptive optics; Astronomy; Extrasolar planets; Infrared devices; Signal to noise ratio; Spectrophotometry; Stars; astrometry; Exo-planets; Gemini Planet Imager; GPI; High contrast imaging; Satellites |
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| Abstract | The Gemini Planet Imager (GPI) combines extreme adaptive optics, an integral field spectrograph, and a high performance coronagraph to directly image extrasolar planets in the near-infrared. Because the coronagraph blocks most of the light from the star, it prevents the properties of the host star from being measured directly. Instead, satellite spots, which are created by diffraction from a square grid in the pupil plane, can be used to locate the star and extract its spectrum. We describe the techniques implemented into the GPI Data Reduction Pipeline to measure the properties of the satellite spots and discuss the precision of the reconstructed astrometry and spectrophotometry of the occulted star. We find the astrometric precision of the satellite spots in an H-band datacube to be 0.05 pixels and is best when individual satellite spots have a signal to noise ratio (SNR) of > 20. In regards to satellite spot spectrophotometry, we find that the total flux from the satellite spots is stable to ∼7% and scales linearly with central star brightness and that the shape of the satellite spot spectrum varies on the 2% level. |
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| Publication date | 2014-07-24 |
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| Publisher | SPIE |
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| Language | English |
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| Peer reviewed | Yes |
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| NPARC number | 21275483 |
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| Export citation | Export as RIS |
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| Report a correction | Report a correction |
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Record identifier | 17e9a212-5008-472b-865a-1d3c73dcc2c8 | | Record created | 2015-07-14 |
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| Record modified | 2017-04-24 |
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