Improving and Assessing Planet Sensitivity of the GPI Exoplanet Survey with a Forward Model Matched Filter

• Main Authors: Ruffio, Jean-Baptiste, Macintosh, Bruce, Wang, Jason J., Pueyo, Laurent, Nielsen, Eric L., Rosa, Robert J. De, Czekala, Ian, Marley, Mark S., Arriaga, Pauline, Bailey, Vanessa P., Barman, Travis, Bulger, Joanna, Chilcote, Jeffrey, Cotten, Tara, Doyon, Rene, Duchene, Gaspard, Fitzgerald, Michael P., Follette, Katherine B., Gerard, Benjamin L., Goodsell, Stephen J., Graham, James R., Greenbaum, Alexandra Z., Hibon, Pascale, Hung, Li-Wei, Ingraham, Patrick, Kalas, Paul, Konopacky, Quinn, Larkin, James E., Maire, Jerome, Marchis, Franck, Marois, Christian, Metchev, Stanimir, Millar-Blanchaer, Maxwell A., Morzinski, Katie M., Oppenheimer, Rebecca, Palmer, David, Patience, Jennifer, Perrin, Marshall, Poyneer, Lisa, Rajan, Abhijith, Rameau, Julien, Rantakyro, Fredrik T., Savransky, Dmitry, Schneider, Adam C., Sivaramakrishnan, Anand, Song, Inseok, Soummer, Remi, Thomas, Sandrine, Wallace, J. Kent, Ward-Duong, Kimberly, Wiktorowicz, Sloane, Wolff, Schuyler
• Other Authors: Univ Arizona, Lunar & Planetary Lab
• Language: en
• Published: IOP PUBLISHING LTD 2017
• Subjects: instrumentation: adaptive optics; methods: statistical; planetary systems; surveys; techniques: high angular resolution; techniques: image processing
• Online Access: http://hdl.handle.net/10150/624437; http://arizona.openrepository.com/arizona/handle/10150/624437

We present a new matched-filter algorithm for direct detection of point sources in the immediate vicinity of bright stars. The stellar point-spread function (PSF) is first subtracted using a Karhunen-Love image processing (KLIP) algorithm with angular and spectral differential imaging (ADI and SDI). The KLIP-induced distortion of the astrophysical signal is included in the matched-filter template by computing a forward model of the PSF at every position in the image. To optimize the performance of the algorithm, we conduct extensive planet injection and recovery tests and tune the exoplanet spectra template and KLIP reduction aggressiveness to maximize the signalto- noise ratio (S/N) of the recovered planets. We show that only two spectral templates are necessary to recover any young Jovian exoplanets with minimal S/N loss. We also developed a complete pipeline for the automated detection of point-source candidates, the calculation of receiver operating characteristics (ROC), contrast curves based on. false positives, and completeness contours. We process in a uniform manner more than 330 data sets from the Gemini Planet Imager Exoplanet Survey and assess GPI typical sensitivity as a function of the star and the hypothetical companion spectral type. This work allows for the first time a comparison of different detection algorithms at a survey scale accounting for both planet completeness and false-positive rate. We show that the new forward model matched filter allows the detection of 50% fainter objects than a conventional cross-correlation technique with a Gaussian PSF template for the same false-positive rate.