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New Transit Observations for HAT-P-30 b, HAT-P-37 b, TrES-5 b, WASP-28 b, WASP-36 b and WASP-39 b

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Maciejewski G. , Dimitrov D. , Mancini L. , Southworth J. , Ciceri S. , D'Ago G. , Bruni I. , Raetz S. , Nowak G. , Ohlert J. , Puchalski D. , Saral G. , Derman E. , Petrucci R. , Jofre E. , Seeliger M. , Henning T.

Acta Astronomica

2016

tom Vol. 66, No. 1

55--74

We present new transit light curves for planets in six extrasolar planetary systems. They were acquired with 0.4-2.2 m telescopes located in west Asia, Europe, and South America. When combined with literature data, they allowed us to redetermine system parameters in a homogeneous way. Our results for individual systems are in agreement with values reported in previous studies. We refined transit ephemerides and reduced uncertainties of orbital periods by a factor between 2 and 7. No sign of any variations in transit times was detected for the planets studied.

OGLE-2017-BLG-1434Lb: Eighth q<1×10-4 Mass-Ratio Microlens Planet Confirms Turnover in Planet Mass-Ratio Function

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Udalski A. , Ryu Y.-H. , Sajadian S. , Gould A. , Mróz P. , Poleski R. , Szymański M. K. , Skowron J. , Soszyński I. , Kozłowski S. , Pietrukowicz P. , Ulaczyk K. , Pawlak M. , Rybicki K. , Iwanek P. , Albrow M. D. , Chung S. J. , Han C. , Hwang K.-H. , Jung Y. K. , Shin I.-G. , Shvartzvald Y. , Yee J. C. , Zang W. , Zhu W. , Cha S.-M. , Kim D.-J. , Kim H.-W. , Kim S.-L. , Lee C.-U. , Lee D.-J. , Lee Y. , Park B.-G. , Pogge R. W. , Bozza W. , Dominik M. , Helling C. , Hundertmark M. , Jørgensen U. G. , Longa-Peña P. , Lowry S. , Burgdorf M. , Campbell-White J. , Ciceri S. , Evans D. , Jaimes R. F. , Fujii Y. I. , Haikala L. K. , Henning T. , Hinse T. C. , Mancini L. , Peixinho N. , Rahvar S. , Rabus M. , Skottfelt J. , Snodgrass C. , Southworth J. , von Essen C.

Acta Astronomica

2018

tom Vol. 68, No. 1

1--42

We report the discovery of a cold Super-Earth planet (mp=4.4±0.5 M⊕) orbiting a low-mass (M=0.23±0.03 M⊙) M dwarf at projected separation a⊥=1.18±0.10 a.u., i.e., about 1.9 times the distance the snow line. The system is quite nearby for a microlensing planet, DL=0.86±0.09 kpc. Indeed, it was the large lens-source relative parallax πrel=1.0 mas (combined with the low mass M) that gave rise to the large, and thus well-measured, "microlens parallax" πE∝(πrel/M)1/2 that enabled these precise measurements. OGLE-2017-BLG-1434Lb is the eighth microlensing planet with planet-host mass ratio q<1×10-4. We apply a new planet-detection sensitivity method, which is a variant of "V/Vmax", to seven of these eight planets to derive the mass-ratio function in this regime. We find dN/d lnq ∝ qp, with p=1.05+0.78 -0.68, which confirms the "turnover" in the mass function found by Suzuki et al. relative to the power law of opposite sign n=-0.93±0.13 at higher mass ratios q≳2×10-4. We combine our result with that of Suzuki et al. to obtain p=0.73+0.42 -0.34.