TY - JOUR
T1 - Tracking Advanced Planetary Systems (TAPAS) with HARPS-N
T2 - IV. TYC 3667-1280-1: The most massive red giant star hosting a warm Jupiter
AU - Niedzielski, A.
AU - Villaver, E.
AU - Nowak, G.
AU - Adamów, M.
AU - Maciejewski, G.
AU - Kowalik, K.
AU - Wolszczan, A.
AU - Deka-Szymankiewicz, B.
AU - Adamczyk, M.
N1 - Funding Information:
We thank the HET and IAC resident astronomers and telescope operators for their support. M.A. acknowledges the Mobility+III fellowship from the Polish Ministry of Science and Higher Education. M.A., A.N., B.D., and MiA were supported by the Polish National Science Centre grant No. UMO-2012/07/B/ST9/04415. E.V. acknowledges support from the Spanish Ministerio de Econom?a y Competitividad under grant AYA2014-55840P. K.K. was funded in part by the Gordon and Betty Moore Foundation's Data-Driven Discovery Initiative through Grant GBMF4561. This research was supported in part by PL-Grid Infrastructure. The HET is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximilians-Universit?t M?nchen, and Georg-August-Universit?t G?ttingen. The HET is named in honor of its principal benefactors, William P. Hobby and Robert E. Eberly. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. This work made use of NumPy (Walt et al. 2011), Matplotlib (Hunter 2007), Pandas (McKinney 2010) and yt (Turk et al. 2011).
Publisher Copyright:
© ESO, 2016.
PY - 2016/5/1
Y1 - 2016/5/1
N2 - Context. We present the latest result of the TAPAS project that is devoted to intense monitoring of planetary candidates that are identified within the PennState-Toruń planet search. Aims. We aim to detect planetary systems around evolved stars to be able to build sound statistics on the frequency and intrinsic nature of these systems, and to deliver in-depth studies of selected planetary systems with evidence of star-planet interaction processes. Methods. The paper is based on precise radial velocity measurements: 13 epochs collected over 1920 days with the Hobby-Eberly Telescope and its High-Resolution Spectrograph, and 22 epochs of ultra-precise HARPS-N data collected over 961 days. Results. We present a warm-Jupiter (Teq = 1350 K, m2 sin i = 5.4 ± 0.4 MJ) companion with an orbital period of 26.468 days in a circular (e = 0.036) orbit around a giant evolved (log g = 3.11 ± 0.09, R = 6.26 ± 0.86 R⊙) star with M∗ = 1.87 ± 0.17 M⊙. This is the most massive and oldest star found to be hosting a close-in giant planet. Its proximity to its host (a = 0.21 au) means that the planet has a 13.9 ± 2.0% probability of transits; this calls for photometric follow-up study. Conclusions. This massive warm Jupiter with a near circular orbit around an evolved massive star can help set constraints on general migration mechanisms for warm Jupiters and, given its high equilibrium temperature, can help test energy deposition models in hot Jupiters.
AB - Context. We present the latest result of the TAPAS project that is devoted to intense monitoring of planetary candidates that are identified within the PennState-Toruń planet search. Aims. We aim to detect planetary systems around evolved stars to be able to build sound statistics on the frequency and intrinsic nature of these systems, and to deliver in-depth studies of selected planetary systems with evidence of star-planet interaction processes. Methods. The paper is based on precise radial velocity measurements: 13 epochs collected over 1920 days with the Hobby-Eberly Telescope and its High-Resolution Spectrograph, and 22 epochs of ultra-precise HARPS-N data collected over 961 days. Results. We present a warm-Jupiter (Teq = 1350 K, m2 sin i = 5.4 ± 0.4 MJ) companion with an orbital period of 26.468 days in a circular (e = 0.036) orbit around a giant evolved (log g = 3.11 ± 0.09, R = 6.26 ± 0.86 R⊙) star with M∗ = 1.87 ± 0.17 M⊙. This is the most massive and oldest star found to be hosting a close-in giant planet. Its proximity to its host (a = 0.21 au) means that the planet has a 13.9 ± 2.0% probability of transits; this calls for photometric follow-up study. Conclusions. This massive warm Jupiter with a near circular orbit around an evolved massive star can help set constraints on general migration mechanisms for warm Jupiters and, given its high equilibrium temperature, can help test energy deposition models in hot Jupiters.
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U2 - 10.1051/0004-6361/201628417
DO - 10.1051/0004-6361/201628417
M3 - Article
AN - SCOPUS:84964282779
VL - 589
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
SN - 0004-6361
M1 - L1
ER -