The TESS-Keck Survey. XVII. Precise Mass Measurements in a Young, High-multiplicity Transiting Planet System Using Radial Velocities and Transit Timing Variations

Copyright and License

© 2024. 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.

Acknowledgement

The primary TTV+RV analysis was carried out by C.B. with help from F.D. and P.R. Frequency analysis and additional figures were carried out with help from R.H. and J.L. J.A.M helped improve the atmospheric models used in our discussion section, and S.B. and R.A.R. helped contribute to cross-validation analysis. G.N. helped facilitate communication between the TKS and the HARPS-N collaborations. The TKS survey was designed and managed by the PIs N.M.B., I.C., C.D., B.F., A.W.H., D.H., H.I., S.R.K, E.A.P., A.R., and L.M.W. The TKS target pool was developed with help from T.M., M.L.H., J.L., C.B., A.W.M., J.A.M., and N.S. Final survey targets were developed by A.C., T.F., J.V.Z., J.A.M., C.B., and R.A.R. HIRES observations were acquired with help from C.L.B., D.T., A.W.M., M.M., A.C., J.A.M., C.B., S.G., S.B., F.D., J.V.Z, J.L., M.R., L.W., A.P., P.D., R.A.R., and A.B. HARPS-N day-to-day operations were executed with help from G.N., I.C., F.M., J.O., R.L., and E.P. Observations were obtained with help from J.K., R.B., G.M., M.O., and K.K.

The data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.

Additionally, the authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.

We wish to thank the anonymous referee for their diligent and detailed feedback. We feel that they have improved the paper significantly.

This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC;https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.

This paper includes data collected by the TESS mission. Funding for the TESS mission is provided by NASA's Science Mission Directorate. TESS data used during the analysis of this system are available on MAST (MAST Team 2021).

This work utilized the infrastructure for high-performance and high-throughput computing, research data storage and analysis, and scientific software tool integration built, operated, and updated by the Research Cyberinfrastructure Center (RCIC) at the University of California, Irvine (UCI). The RCIC provides cluster-based systems, application software, and scalable storage to directly support the UCI research community (http://rcic.uci.edu).

This work was partially supported by NASA grant No. 80NSSC22K0120 to support Guest Investigator programs for TESS Cycle 4.

This work was partially support by the Future Investigators in NASA Earth and Space Science and Technology (FINESST) program grant No. 80NSSC22K1754.

J.M.A.M. is supported by the National Science Foundation (NSF) Graduate Research Fellowship Program under grant No. DGE-1842400.

T.F. acknowledges support from the University of California President's Postdoctoral Fellowship Program.

G.N. gives thanks for research funding from the Ministry of Education and Science program the "Excellence Initiative—Research University" conducted at the Centre of Excellence in Astrophysics and Astrochemistry of the Nicolaus Copernicus University in Toruń, Poland.

R.L. acknowledges funding from University of La Laguna through the Margarita Salas Fellowship from the Spanish Ministry of Universities ref. UNI/551/2021-May 26, and under the EU Next Generation funds.

G.M. acknowledges funding from the Ariel Postdoctoral Fellowship program of the Swedish National Space Agency (SNSA).

M.R. thanks the Heising-Simons Foundation for their generous support.

L.M.W. acknowledges support from the NASA-Keck Key Strategic Mission Support program (grant No. 80NSSC19K1475) and the NASA Exoplanet Research Program (grant No. 80NSSC23K0269).

This work is partly supported by JSPS KAKENHI grant No. JP21K13955.

J.K. gratefully acknowledges the support of the Swedish National Space Agency (SNSA; DNR 2020-00104) and of the Swedish Research Council (VR: Etableringsbidrag 2017-04945).

Facilities

Gaia - , Keck:1 (HIRES) - , APF - , TNG (HARPS-N) - , TESS - , Exoplanet Archive -

Software References

ArviZ (Kumar et al. 2019), emcee (Foreman-Mackey et al. 2013), exoplanet (Foreman-Mackey et al. 2021a, 2021b), ipython (Pérez & Granger 2007), lightkurve (Lightkurve Collaboration et al. 2018), LMFit (Newville et al. 2014), matplotlib (Hunter 2007), numpy (Harris et al. 2020), pandas (McKinney 2010; pandas development team 2020), PyMC3 (Salvatier et al. 2016), RadVel (Fulton et al. 2018), SciPy (Virtanen et al. 2020), theano (Theano Development Team 2016), TTVFast (Deck et al. 2014)