NEID Rossiter-McLaughlin Measurement of TOI-1268b: A Young Warm Saturn Aligned with Its Cool Host Star

Creators: Dong, Jiayin; Huang, Chelsea X.; Zhou, George; Dawson, Rebekah I.; Stefánsson, Gumundur K.; Bender, Chad F.; Blake, Cullen H.; Ford, Eric B.; Halverson, Samuel; Kanodia, Shubham; Mahadevan, Suvrath; McElwain, Michael W.; Ninan, Joe P.; Robertson, Paul; Roy, Arpita; Schwab, Christian; Stevens, Daniel J.; Terrien, Ryan C.; Vanderburg, Andrew; Kraus, Adam L.; Douglas, Stephanie; Newton, Elisabeth; Rampalli, Rayna; Krolikowski, Daniel M.; Collins, Karen A.; Rodriguez, Joseph E.; Feliz, Dax L.; Srdoc, Gregor; Ziegler, Carl; Barkaoui, Khalid; Pozuelos, Francisco J.; Jehin, Emmanuel; Michaël, C.; Benkhaldoun, Zouhair; Lewin, Pablo; Forés-Toribio, Raquel; Muñoz, Jose A.; McLeod, Kim K.; Powers Özyurt, Fiona; Horta, Ferran Grau; Murgas, Felipe; Latham, David W.; Quinn, Samuel N.; Bieryla, Allyson; Howell, Steve B.; Gnilka, Crystal L.; Ciardi, David R.; Lund, Michael B.; Dressing, Courtney D.; Giacalone, Steven; Savel, Arjun B.; Strakhov, Ivan A.; Belinski, Alexander A.; Ricker, George R.; Seager, S.; Winn, Joshua N.; Jenkins, Jon M.; Torres, Guillermo; Paegert, Martin

Abstract

Close-in gas giants present a surprising range of stellar obliquity, the angle between a planet's orbital axis and its host star's spin axis. It is unclear whether the obliquities reflect the planets' dynamical history (e.g., aligned for in situ formation or disk migration versus misaligned for high-eccentricity tidal migration) or whether other mechanisms (e.g., primordial misalignment or planet–star interactions) are more important in sculpting the obliquity distribution. Here we present the stellar obliquity measurement of TOI-1268 (TIC-142394656, V_(mag) ∼ 10.9), a young K-type dwarf hosting an 8.2 day period, Saturn-sized planet. TOI-1268's lithium abundance and rotation period suggest the system age between the ages of the Pleiades cluster (∼120 Myr) and the Prasepe cluster (∼670 Myr). Using the newly commissioned NEID spectrograph, we constrain the stellar obliquity of TOI-1268 via the Rossiter–McLaughlin effect from both radial velocity and Doppler tomography signals. The 3σ upper bounds of the projected stellar obliquity ∣λ∣ from both models are below 60°. The large host star separation (a/R ⋆ ∼ 17), combined with the system's young age, makes it unlikely that the planet has realigned its host star. The stellar obliquity measurement of TOI-1268 probes the architecture of a young gas giant beyond the reach of tidal realignment (a/R ⋆ ≳ 10) and reveals an aligned or slightly misaligned system.

Additional Information

© 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2021 December 10; revised 2022 January 19; accepted 2022 January 20; published 2022 February 16. Computations for this research were performed on the Pennsylvania State University's Institute for Computational & Data Sciences Advanced CyberInfrastructure (ICS-ACI). This content is solely the responsibility of the authors and does not necessarily represent the views of the Institute for CyberScience. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University and the Eberly College of Science. We gratefully acknowledge support by NASA XRP 80NSSC18K0355 and NASA TESS GO 80NSSC18K1695. These results are based on observations obtained with NEID on the WIYN 3.5 m Telescope at Kitt Peak National Observatory. WIYN is a joint facility of the University of Wisconsin–Madison, Indiana University, NSF's NOIRLab, the Pennsylvania State University, Purdue University, University of California, Irvine, and the University of Missouri. The authors are honored to be permitted to conduct astronomical research on Iolkam Du'ag (Kitt Peak), a mountain with particular significance to the Tohono O'odham. This work makes use of observations from the LCOGT network. This work was performed for the Jet Propulsion Laboratory, California Institute of Technology, sponsored by the United States Government under the Prime Contract 80NM0018D0004 between Caltech and NASA. The research leading to these results has received funding from the ARC grant for Concerted Research Actions, financed by the Wallonia-Brussels Federation. TRAPPIST is funded by the Belgian Fund for Scientific Research (Fond National de la Recherche Scientifique, FNRS) under the grant PDR T.0120.21, with the participation of the Swiss National Science Foundation (SNF). TRAPPIST-North is a project funded by the University of Liege (Belgium), in collaboration with Cadi Ayyad University of Marrakech (Morocco). M.G. and E.J. are F.R.S.-FNRS Senior Research Associates. C.D.D. acknowledges support from the NASA Exoplanet Research Program (XRP) under award 80NSSC20K0250. A.A.B. and I.A.S. acknowledge the support of Ministry of Science and Higher Education of the Russian Federation under the grant 075-15-2020-780 (N13.1902.21.0039). We acknowledge the use of public TESS data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. This research made use of exoplanet (Foreman-Mackey et al. 2019, 2021) and its dependencies (Astropy Collaboration et al. 2013; Kipping 2013; Salvatier et al. 2016; Theano Development Team 2016; Foreman-Mackey et al. 2017; Foreman-Mackey 2018; Astropy Collaboration et al. 2018; Foreman-Mackey et al. 2019; Luger et al. 2019; Agol et al. 2020). Some/all of the data presented in this Letter were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute. The specific observations analyzed can be accessed via doi:10.17909/t9-nmc8-f686. Facilities: TESS - , Gaia - , LCOGT - , TRAPPIST-North - , PHARON - , `Alopeke - , ShARCS - , KELT - , TRES - , NEID - , Exoplanet Archive - Software: ArviZ (Kumar et al. 2019), astroARIADNE, AstroImageJ (Collins et al. 2017), astropy (Astropy Collaboration et al. 2013, 2018), BAFFLES (Stanford-Moore et al. 2020), celerite2 (Foreman-Mackey et al. 2017; Foreman-Mackey 2018), Comove (Tofflemire et al. 2021), EXOFASTv2 (Eastman et al. 2013, 2019), exoplanet (Foreman-Mackey et al. 2021), Jupyter (Kluyver et al. 2016), Matplotlib (Hunter 2007; Droettboom et al. 2016), NumPy (van der Walt et al. 2011; Harris et al. 2020), pandas (McKinney 2010), PyMC (Salvatier et al. 2016), SciPy (Virtanen et al. 2020), starry (Luger et al. 2019), Tapir (Jensen 2013), VARTOOLS (Hartman & Bakos 2016).

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