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dc.contributor.authorBuzard, Cam
dc.contributor.authorFinnerty, Luke
dc.contributor.authorPiskorz, Danielle
dc.contributor.authorPelletier, Stefan
dc.contributor.authorBenneke, Björn
dc.contributor.authorBender, Chad F.
dc.contributor.authorLockwood, Alexandra C.
dc.contributor.authorWallack, Nicole L.
dc.contributor.authorWilkins, Olivia H.
dc.contributor.authorBlake, Geoffrey A.
dc.date.accessioned2020-07-13T18:30:29Z
dc.date.available2020-07-13T18:30:29Z
dc.date.issued2020-06-04
dc.identifier.citationCam Buzard et al 2020 AJ 160 1en_US
dc.identifier.issn0004-6256
dc.identifier.doi10.3847/1538-3881/ab8f9c
dc.identifier.urihttp://hdl.handle.net/10150/641835
dc.description.abstractWe report the 6.5 sigma detection of water from the hot Jupiter HD187123b with a Keplerian orbital velocity K-p of 53 +/- 13 km s(-1). This high-confidence detection is made using a multi-epoch, high-resolution, cross-correlation technique, and corresponds to a planetary mass of 1.4(-0.3)(1.05) M-J and an orbital inclination of 21 degrees +/- 5 degrees. The technique works by treating the planet/star system as a spectroscopic binary and obtaining high signal-to-noise, high-resolution observations at multiple points across the planet's orbit to constrain the system's binary dynamical motion. All together, seven epochs of Keck/NIRSPEC L-band observations were obtained, with five before the instrument upgrade and two after. Using high-resolution SCARLET planetary and PHOENIX stellar spectral models, we were able to drastically increase the confidence of the detection by running simulations that could reproduce, and thus remove, the nonrandom structured noise in the final likelihood space well. The ability to predict multi-epoch results will be extremely useful for furthering the technique. Here, we use these simulations to compare three different approaches to combining the cross correlations of high-resolution spectra and find that the Zucker log(L) approach is least affected by unwanted planet/star correlation for our HD187123 data set. Furthermore, we find that the same total signal-to-noise ratio (S/N) spread across an orbit in many, lower S/N epochs rather than fewer, higher S/N epochs could provide a more efficient detection. This work provides a necessary validation of multi-epoch simulations, which can be used to guide future observations and will be key to studying the atmospheres of farther separated, non-transiting exoplanets.en_US
dc.language.isoenen_US
dc.publisherIOP PUBLISHING LTDen_US
dc.rightsCopyright © 2020. The American Astronomical Society. All rights reserved.en_US
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/
dc.titleSimulating the Multi-epoch Direct Detection Technique to Isolate the Thermal Emission of the Non-transiting Hot Jupiter HD187123ben_US
dc.typeArticleen_US
dc.contributor.departmentUniv Arizona, Dept Astronen_US
dc.contributor.departmentUniv Arizona, Steward Observen_US
dc.identifier.journalASTRONOMICAL JOURNALen_US
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en_US
dc.eprint.versionFinal published versionen_US
dc.source.journaltitleThe Astronomical Journal
dc.source.volume160
dc.source.issue1
dc.source.beginpage1
refterms.dateFOA2020-07-13T18:30:31Z


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