http://arxiv.org/abs/2202.07723
We present 12 new transit light curves and 16 new out-of-transit radial velocity measurements for the XO-3 system. By modelling our newly collected measurements together with archival photometric and Doppler velocimetric data, we confirmed the unusual configuration of the XO-3 system, which contains a massive planet ($M_P=11.92^{+0.59}{-0.63} M_J$) on a relatively eccentric ($e=0.2853^{+0.0027}{-0.0026}$) and short-period ($3.19152 \pm 0.00145\,$day) orbit around a massive star ($M_=1.219^{+0.090}{-0.095} M{\odot}$). Furthermore, we find no strong evidence for a temporal change of either $V\sin i_{}$ (and by extension, the stellar spin vector of XO-3), or the transit profile (and thus orbital angular momentum vector of XO-3b). We conclude that the discrepancy in previous Rossiter-McLaughlin measurements ($70.0^{\circ} \pm 15.0^{\circ}$ (Hebrard et al. 2008); $37.3^{\circ} \pm 3.7^{\circ}$ (Winn et al. 2009); $37.3^{\circ} \pm 3.0^{\circ}$ (Hirano et al. 2011)) may have stemmed from systematic noise sources.
K. Worku, S. Wang, J. Burt, et. al.
Thu, 17 Feb 22
25/60
Comments: Accepted for publication by The Astronomical Journal on January 18, 2022
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