Publication Search Results

ID: 158251
Type: article
Authors: Abrams, Natasha S.; Bieryla, Allyson; Gomez, Sebastian; Huang, Jane; Lewis, John Arban; Garrison, Lehman H.; Carmichael, Theron
Abstract: We determined the rotational periods of 3122 Florence, 3830 Trelleborg, and (131077) 2000 YH105 with the Harvard Clay Telescope and KeplerCam at the Fred L. Whipple Observatory. We found the rotational periods to be 2.3580 ± 0.0015 h, 17.059 ± 0.017 h, and 1.813 ± 0.00003 h, respectively. Our measurement of 3122 Florence's period agrees with Warner (2016), who reported 2.3580 ± 0.0002 h.

ID: 158104
Type: article
Authors: Wibking, Benjamin D.; Weinberg, David H.; Salcedo, Andrés N.; Wu, Hao-Yi; Singh, Sukhdeep; Rodríguez-Torres, Sergio; Garrison, Lehman H.; Eisenstein, Daniel J.
Abstract: We describe our non-linear emulation (I.e. interpolation) framework that combines the halo occupation distribution (HOD) galaxy bias model with N-body simulations of non-linear structure formation, designed to accurately predict the projected clustering and galaxy-galaxy lensing signals from luminous red galaxies in the redshift range 0.16 _{p 8} = (σ₈/0.8228)(Ω_m/0.3107)^0.6 from mock measurements produced via subhalo abundance matching (SHAM)-based light-cones designed to approximately match the properties of the SDSS LOWZ galaxy sample. Applying our model to Baryon Oscillation Spectroscopic Survey (BOSS) Data Release 14 (DR14) LOWZ galaxy clustering and galaxy-shear cross-correlation measurements made with Sloan Digital Sky Survey (SDSS) Data Release 8 (DR8) imaging, we perform a prototype cosmological analysis marginalizing over wCDM cosmological parameters and galaxy HOD parameters. We obtain a 4.4 per cent measurement of S₈ = 0.847 ± 0.037, in 3.5σ tension with the Planck cosmological results of 1.00 ± 0.02. We discuss the possibility of underestimated systematic uncertainties or astrophysical effects that could explain this discrepancy.

ID: 154595
Type: article
Authors: Rodriguez, Joseph E.; Eastman, Jason D.; Zhou, George; Quinn, Samuel N.; Beatty, Thomas G.; Penev, Kaloyan; Johnson, Marshall C.; Cargile, Phillip A.; Latham, David W.; Bieryla, Allyson; Collins, Karen A.; Dressing, Courtney D.; Ciardi, David R.; Relles, Howard M.; Murawski, Gabriel; Nishiumi, Taku; Yonehara, Atsunori; Ishimaru, Ryo; Yoshida, Fumi; Gregorio, Joao; Lund, Michael B.; Stevens, Daniel J.; Stassun, Keivan G.; Gaudi, B. Scott; Colón, Knicole D.; Pepper, Joshua; Narita, Norio; Awiphan, Supachai; Chuanraksasat, Pongpichit; Benni, Paul; Zambelli, Roberto; Garrison, Lehman H.; Wilson, Maurice L.; Cornachione, Matthew A.; Wang, Sharon X.; Labadie-Bartz, Jonathan; Rodríguez, Romy; Siverd, Robert J.; Yao, Xinyu; Bayliss, Daniel; Berlind, Perry; Calkins, Michael L.; Christiansen, Jessie L.; Cohen, David H.; Conti, Dennis M.; Curtis, Ivan A.; DePoy, D. L.; Esquerdo, Gilbert A.; Evans, Phil; Feliz, Dax; Fulton, Benjamin J.; Holoien, Thomas W. -S; James, David J.; Jayasinghe, Tharindu; Jang-Condell, Hannah; Jensen, Eric L. N.; Johnson, John A.; Joner, Michael D.; Khakpash, Somayeh; Kielkopf, John F.; Kuhn, Rudolf B.; Manner, Mark; Marshall, Jennifer L.; McLeod, Kim K.; McCrady, Nate; Oberst, Thomas E.; Oelkers, Ryan J.; Penny, Matthew T.; Reed, Phillip A.; Sliski, David H.; Shappee, B. J.; Stephens, Denise C.; Stockdale, Chris; Tan, Thiam-Guan; Trueblood, Mark; Trueblood, Pat; Villanueva, Steven, Jr.; Wittenmyer, Robert A.; Wright, Jason T.
Abstract: 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 _eff = {6509}_-49⁺⁵⁰ K, a mass of M _* = {1.460}_-0.059^+0.055 M _☉, a radius of R _* = 1.506 ± 0.022 R _☉, and an age of {0.78}_-0.42^+0.61 Gyr. Its planetary companion (KELT-24 b) has a radius of R _P = 1.272 ± 0.021 R _J and a mass of M _P = {5.18}_-0.22^+0.21 M _J, and from Doppler tomographic observations, we find that the planet's orbit is well- aligned to its host star's projected spin axis (λ ={2.6}_-3.6^+5.1). 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.

ID: 153251
Type: article
Authors: Wibking, Benjamin D.; Salcedo, Andrés N.; Weinberg, David H.; Garrison, Lehman H.; Ferrer, Douglas; Tinker, Jeremy; Eisenstein, Daniel; Metchnik, Marc; Pinto, Philip