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

OGLE-2017-BLG-1434Lb: Eighth q < 1 * 10^-4 Mass-Ratio Microlens Planet Confirms Turnover in Planet Mass-Ratio Function
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OGLE-2017-BLG-1434Lb：第八个 q < 1 * 10^-4 质量比微透镜行星确认行星质量比函数中的转换

DOI：
10.32023/0001-5237/68.1.1
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发表时间：
2018
期刊：
arXiv: Earth and Planetary Astrophysics
影响因子：
--
通讯作者：
C. V. Essen
C. V. Essen
中科院分区：
--
文献类型：
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作者：
A. Udalski;Y. Ryu;S. Sajadian;A. Gould;P. Mr'oz;R. Poleski;M. Szyma'nski;J. Skowron;I. Soszy'nski;S. Kozłowski;P. Pietrukowicz;K. Ulaczyk;M. Pawlak;K. Rybicki;P. Iwanek;M. Albrow;S. Chung;C. Han;K. Hwang;Y. Jung;I. Shin;Y. Shvartzvald;J. Yee;W. Zang;W. Zhu;S. Cha;D.;H.;S.;C.‐U. Lee;D.;Y. Lee;B.;R. Pogge;V. Bozza;M. Dominik;C. Helling;M. Hundertmark;U. Jørgensen;P. Longa;S. Lowry;M. Burgdorf;J. Campbell;S. Ciceri;D. Evans;R. Jaimes;Y. Fujii;L. Haikala;T. Henning;T. Hinse;L. Mancini;N. Peixinho;S.Rahvar;M. Rabus;J. Skottfelt;C. Snodgrass;J. Southworth;C. V. Essen

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我们报告发现了一颗低温的超级地球行星（m_p=4.4 +/- 0.5 M_Earth），绕着一颗低质量（M=0.23 +/- 0.03 M_Sun） M矮星运行，预计距离a_perp = 1.18 +/- 0.10 AU，即大约1.9倍的雪线。对于一个微透镜行星来说，这个系统非常接近，D_Lens = 0.86 +/- 0.09 kpc。事实上，正是大透镜-光源相对视差pi_rel=1.0 mas（结合低质量M）产生了大的、因此测量得很好的“微透镜视差”，使这些精确的测量成为可能。OGLE-2017-BLG-1434Lb是第八颗行星-宿主质量比q < 1 * 10^-4的微透镜行星。
We report the discovery of a cold Super-Earth planet (m_p=4.4 +/- 0.5 M_Earth) orbiting a low-mass (M=0.23 +/- 0.03 M_Sun) M dwarf at projected separation a_perp = 1.18 +/- 0.10 AU, i.e., about 1.9 times the snow line. The system is quite nearby for a microlensing planet, D_Lens = 0.86 +/- 0.09 kpc. Indeed, it was the large lens-source relative parallax pi_rel=1.0 mas (combined with the low mass M) that gave rise to the large, and thus well-measured, "microlens parallax" 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/V_max", to seven of these eight planets to derive the mass-ratio function in this regime. We find dN/d(ln q) ~ q^p, 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).