While earlier work has emphasized Kant's philosophy of religion as thinly
disguised morality, this timely and original reappraisal of Kant's philosophy of
religion incorporates recent scholarship. In ...this volume, Chris L. Firestone,
Stephen R. Palmquist, and the other contributors make a strong case for more
specific focus on religious topics in the Kantian corpus. Main themes include the
relationship between Kant's philosophy of religion and his philosophy as a whole,
the contemporary relevance of specific issues arising out of Kant's philosophical
theology, and the relationship of Kant's philosophy to Christian theology. As a
whole, this book capitalizes on contemporary movements in Kant studies by looking at
Kant not as an anti-metaphysician, but as a genuine seeker of spirituality in the
human experience.
We present the discovery of KELT-24 b, a massive hot Jupiter orbiting a bright (V=8.3 mag, K=7.2 mag) young F-star with a period of 5.6 days. The host star, KELT-24 (HD 93148), has a \(T_{\rm eff}\) ...=\(6509^{+50}_{-49}\) K, a mass of \(M_{*}\) = \(1.460^{+0.055}_{-0.059}\) \(M_{\odot}\), radius of \(R_{*}\) = \(1.506\pm0.022\) \(R_{\odot}\), and an age of \(0.78^{+0.61}_{-0.42}\) Gyr. Its planetary companion (KELT-24 b) has a radius of \(R_{\rm P}\) = \(1.272\pm0.021\) \(R_{\rm J}\), a mass of \(M_{\rm P}\) = \(5.18^{+0.21}_{-0.22}\) \(M_{\rm J}\), and from Doppler tomographic observations, we find that the planet's orbit is well-aligned to its host star's projected spin axis (\(\lambda\) = \(2.6^{+5.1}_{-3.6}\)). The young age estimated for KELT-24 suggests that it only recently started to evolve from the zero-age main sequence. KELT-24 is the brightest star known to host a transiting giant planet with a period between 5 and 10 days. Although the circularization timescale is much longer than the age of the system, we do not detect a large eccentricity or significant misalignment that is expected from dynamical migration. The brightness of its host star and its moderate surface gravity make KELT-24b an intriguing target for detailed atmospheric characterization through spectroscopic emission measurements since it would bridge the current literature results that have primarily focused on lower mass hot Jupiters and a few brown dwarfs.
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