United States Records of Williamsonia Fletcheri (Odonata: Corduliidae)

Excerpt: Foley (1966) reported specimens of Williamsonia fletcheri Williamson from rand Traverse County, Michigan as the first record of the species from the lower peninsula and the second for the United States. However. two other records for the United States were overlooked and this was actually the fourt

KELT-23Ab: A Hot Jupiter Transiting a Near-solar Twin Close to the TESS and JWST Continuous Viewing Zones

We announce the discovery of KELT-23Ab, a hot Jupiter transiting the relatively bright (V = 10.3) star BD+66 911 (TYC 4187-996-1), and characterize the system using follow-up photometry and spectroscopy. A global fit to the system yields host-star properties of T-eff = 5900 +/- 49 K, M* = 0.945(-0.054)(+0.060) M-circle dot, R* = 0.995 +/- 0.015 R-circle dot, L* = 1.082(-0.048)(+0.051) L-circle dot, log g* = 4.418(-0.025)(+0.026). (cgs), and [Fe/H] = -0.105 +/- 0.077. KELT-23Ab is a hot Jupiter with a mass of M-p = 0.938(-0.042)(+0.045). M-J, radius of R-p = 1.322 0.025 R-J, and density of rho(p) = 0.504(0.035)(+0.038) g cm(-3). Intense insolation flux from the star has likely caused KELT-23Ab to become inflated. The time of inferior conjunction is T-0 = 2458149.40776 +/- 0.00091 BJD(TDB) and the orbital period is P = 2.255353(-0.000030)(+0.000031) ON days. There is strong evidence that KELT-23A is a member of a long-period binary star system with a less luminous companion, and due to tidal interactions, the planet is likely to spiral into its host within roughly a gigayear. This system has one of the highest positive ecliptic latitudes of all transiting planet hosts known to date, placing it near the Transiting Planet Survey Satellite and James Webb Space Telescope continuous viewing zones. Thus we expect it to be an excellent candidate for long-term monitoring and follow up with these facilities.Ohio State University; Vanderbilt University; Lehigh University; Harvard Future Faculty Leaders Postdoctoral fellowship; NSF CAREER Grant [AST-1056524]; National Science Foundation [DGE-1343012, 1559487]; Space Telescope Science Institute [HST-HF2-51402.001-A]; NASA [NAS 5-26555, 80NSSC18K1009, NNX17AB94G]; National Aeronautics and Space Administration; FAPESP [2017/23731-1]; Carol and Ray Neag Undergraduate Research Fund; KELT follow-up collaborationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at [email protected]

Special Censuses: Ruminating About Enumerating?

Information about how and why a city should conduct a special census

KELT-2Ab: A Hot Jupiter Transiting the Bright (V = 8.77) Primary Star of a Binary System

We report the discovery of KELT-2Ab, a hot Jupiter transiting the bright (V = 8.77) primary star of the HD 42176 binary system. The host is a slightly evolved late F-star likely in the very short-lived "blue-hook" stage of evolution, with T_(eff) = 6148 ± 48 K, log g = 4.030^(+0.015)_(–0.026) and [Fe/H] = 0.034 ± 0.78. The inferred stellar mass is M* = 1.314^(+0.063)_(–0.060) M☉ and the star has a relatively large radius of R* = 1.836^(+0.066)_(–0.046) R☉. The planet is a typical hot Jupiter with period 4.1137913 ± 0.00001 days and a mass of M_P = 1.524 ± 0.088 M J and radius of R_P = 1.290^(+0.064)_(–0.050) R_J. This is mildly inflated as compared to models of irradiated giant planets at the ~4 Gyr age of the system. KELT-2A is the third brightest star with a transiting planet identified by ground-based transit surveys, and the ninth brightest star overall with a transiting planet. KELT-2Ab's mass and radius are unique among the subset of planets with V < 9 host stars, and therefore increases the diversity of bright benchmark systems. We also measure the relative motion of KELT-2A and -2B over a baseline of 38 years, robustly demonstrating for the first time that the stars are bound. This allows us to infer that KELT-2B is an early K dwarf. We hypothesize that through the eccentric Kozai mechanism KELT-2B may have emplaced KELT-2Ab in its current orbit. This scenario is potentially testable with Rossiter-McLaughlin measurements, which should have an amplitude of ~44 m s^(–1)

Spin orbit alignment for KELT-7b and HAT-P-56b via Doppler tomography with TRES

We present Doppler tomographic analyses for the spectroscopic transits of KELT-7b and HAT-P-56b, two hot-Jupiters orbiting rapidly rotating F-dwarf host stars. These include analyses of archival TRES observations for KELT-7b, and a new TRES transit observation of HAT-P-56b. We report spin-orbit aligned geometries for KELT-7b (2.7 +/- 0.6 deg) and HAT-P-56b (8 +/- 2 deg). The host stars KELT-7 and HAT-P-56 are among some of the most rapidly rotating planet-hosting stars known. We examine the tidal re-alignment model for the evolution of the spin-orbit angle in the context of the spin rates of these stars. We find no evidence that the rotation rates of KELT-7 and HAT-P-56 have been modified by star-planet tidal interactions, suggesting that the spin-orbit angle of systems around these hot stars may represent their primordial configuration. In fact, KELT-7 and HAT-P-56 are two of three systems in super-synchronous, spin-orbit aligned states, where the rotation periods of the host stars are faster than the orbital periods of the planets.Comment: 9 pages, accepted for publication in MNRA