{"id":1887,"date":"2022-01-17T13:21:28","date_gmt":"2022-01-17T12:21:28","guid":{"rendered":"https:\/\/pepsi.aip.de\/?p=1887"},"modified":"2022-01-17T13:21:28","modified_gmt":"2022-01-17T12:21:28","slug":"kelt-9-as-an-eclipsing-double-lined-spectroscopic-binary-a-unique-and-self-consistent-solution-to-the-system","status":"publish","type":"post","link":"https:\/\/pepsi.aip.de\/?p=1887","title":{"rendered":"KELT-9 as an Eclipsing Double-lined Spectroscopic Binary: A Unique and Self-consistent Solution to the System"},"content":{"rendered":"\n<p>Transiting hot Jupiters present a unique opportunity to measure absolute planetary masses due to the magnitude of their radial velocity signals and known orbital inclination. Measuring planet mass is critical to understanding atmospheric dynamics and escape under extreme stellar irradiation. Here we present the ultrahot Jupiter system KELT-9 as a double-lined spectroscopic binary. This allows us to directly and empirically constrain the mass of the star and its planetary companion without reference to any theoretical stellar evolutionary models or empirical stellar scaling relations. Using data from the PEPSI, HARPS-N, and TRES spectrographs across multiple epochs, we apply least-squares deconvolution to measure out-of-transit stellar radial velocities. With the PEPSI and HARPS-N data sets, we measure in-transit planet radial velocities using transmission spectroscopy. By fitting the circular orbital solution that captures these Keplerian motions, we recover a planetary dynamical mass of 2.17 \u00b1 0.56 M<sub>J<\/sub> and stellar dynamical mass of 2.11 \u00b1 0.78 M<sub>\u2299<\/sub>, both of which agree with the discovery paper. Furthermore, we argue that this system, as well as systems like it, are highly overconstrained, providing multiple independent avenues for empirically cross-validating model-independent solutions to the system parameters. We also discuss the implications of this revised mass for studies of atmospheric escape.<\/p>\n\n\n\n<div class=\"wp-block-image\"><figure class=\"aligncenter size-full\"><img loading=\"lazy\" decoding=\"async\" width=\"818\" height=\"782\" src=\"https:\/\/pepsi.aip.de\/wp-content\/uploads\/2022\/01\/KELT-9_2Dmap.png\" alt=\"\" class=\"wp-image-1886\" srcset=\"https:\/\/pepsi.aip.de\/wp-content\/uploads\/2022\/01\/KELT-9_2Dmap.png 818w, https:\/\/pepsi.aip.de\/wp-content\/uploads\/2022\/01\/KELT-9_2Dmap-300x287.png 300w, https:\/\/pepsi.aip.de\/wp-content\/uploads\/2022\/01\/KELT-9_2Dmap-768x734.png 768w\" sizes=\"auto, (max-width: 818px) 100vw, 818px\" \/><figcaption>A 2D map of transmission spectra over the course of KELT-9 b\u2019s\ntransit for the PEPSI 2018 data set; the blue track is formed by the planet\u2019s\natmospheric absorption, while the red track is the Doppler shadow from the\nRME. The top panel displays fully in-transit observations. The middle panel\nshows the best-fit model from MCMC sampling, with the Doppler shadow and\nCLV determined from numerical modeling of the planet\u2019s transit using SME\nstellar models, while the planet absorption track is a uniform Gaussian signal\nshifted in velocity according to the best-fit orbital motion of the planet,\nsystemic velocity, and best-fit dayside-to-nightside winds. The bottom panel\nshows the residuals (data\u2013model).<\/figcaption><\/figure><\/div>\n\n\n\n<p>Read more: <a href=\"https:\/\/ui.adsabs.harvard.edu\/abs\/2022AJ....163...40P\/abstract\">Pai Asnodkar et al. 2022, AJ, 163, 40P<\/a><\/p>\n\n\n","protected":false},"excerpt":{"rendered":"<p>Transiting hot Jupiters present a unique opportunity to measure absolute planetary masses due to the magnitude of their radial velocity signals and known orbital inclination. Measuring planet mass is critical to understanding atmospheric dynamics and escape under extreme stellar irradiation. Here we present the ultrahot Jupiter system KELT-9 as a double-lined spectroscopic binary. This allows &hellip; <a href=\"https:\/\/pepsi.aip.de\/?p=1887\" class=\"more-link\">Continue reading <span class=\"screen-reader-text\">KELT-9 as an Eclipsing Double-lined Spectroscopic Binary: A Unique and Self-consistent Solution to the System<\/span> <span class=\"meta-nav\">&rarr;<\/span><\/a><\/p>\n","protected":false},"author":5,"featured_media":0,"comment_status":"closed","ping_status":"","sticky":false,"template":"","format":"standard","meta":{"footnotes":""},"categories":[11],"tags":[],"class_list":["post-1887","post","type-post","status-publish","format-standard","hentry","category-publications"],"_links":{"self":[{"href":"https:\/\/pepsi.aip.de\/index.php?rest_route=\/wp\/v2\/posts\/1887","targetHints":{"allow":["GET"]}}],"collection":[{"href":"https:\/\/pepsi.aip.de\/index.php?rest_route=\/wp\/v2\/posts"}],"about":[{"href":"https:\/\/pepsi.aip.de\/index.php?rest_route=\/wp\/v2\/types\/post"}],"author":[{"embeddable":true,"href":"https:\/\/pepsi.aip.de\/index.php?rest_route=\/wp\/v2\/users\/5"}],"replies":[{"embeddable":true,"href":"https:\/\/pepsi.aip.de\/index.php?rest_route=%2Fwp%2Fv2%2Fcomments&post=1887"}],"version-history":[{"count":1,"href":"https:\/\/pepsi.aip.de\/index.php?rest_route=\/wp\/v2\/posts\/1887\/revisions"}],"predecessor-version":[{"id":1888,"href":"https:\/\/pepsi.aip.de\/index.php?rest_route=\/wp\/v2\/posts\/1887\/revisions\/1888"}],"wp:attachment":[{"href":"https:\/\/pepsi.aip.de\/index.php?rest_route=%2Fwp%2Fv2%2Fmedia&parent=1887"}],"wp:term":[{"taxonomy":"category","embeddable":true,"href":"https:\/\/pepsi.aip.de\/index.php?rest_route=%2Fwp%2Fv2%2Fcategories&post=1887"},{"taxonomy":"post_tag","embeddable":true,"href":"https:\/\/pepsi.aip.de\/index.php?rest_route=%2Fwp%2Fv2%2Ftags&post=1887"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}