Spectroscopic Mass and Host-star Metallicity Measurements for Newly Discovered Microlensing Planet OGLE-2018-BLG-0740Lb. (arXiv:1905.00155v1 [astro-ph.EP])

Spectroscopic Mass and Host-star Metallicity Measurements for Newly Discovered Microlensing Planet OGLE-2018-BLG-0740Lb. (arXiv:1905.00155v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Han_C/0/1/0/all/0/1">Cheongho Han</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yee_J/0/1/0/all/0/1">Jennifer C. Yee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Udalski_A/0/1/0/all/0/1">Andrzej Udalski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bond_I/0/1/0/all/0/1">Ian A. Bond</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bozza_V/0/1/0/all/0/1">Valerio Bozza</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cassan_A/0/1/0/all/0/1">Arnaud Cassan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hirao_Y/0/1/0/all/0/1">Yuki Hirao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dong_S/0/1/0/all/0/1">Subo Dong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kollmeier_J/0/1/0/all/0/1">Juna A. Kollmeier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morrell_N/0/1/0/all/0/1">Nidia Morrell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boutsia_K/0/1/0/all/0/1">Konstantina Boutsia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Albrow_M/0/1/0/all/0/1">Michael D. Albrow</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chung_S/0/1/0/all/0/1">Sun-Ju Chung</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gould_A/0/1/0/all/0/1">Andrew Gould</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hwang_K/0/1/0/all/0/1">Kyu-Ha Hwang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_C/0/1/0/all/0/1">Chung-Uk Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ryu_Y/0/1/0/all/0/1">Yoon-Hyun Ryu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shin_I/0/1/0/all/0/1">In-Gu Shin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shvartzvald_Y/0/1/0/all/0/1">Yossi Shvartzvald</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jung_Y/0/1/0/all/0/1">Youn Kil Jung</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_D/0/1/0/all/0/1">Doeon Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_W/0/1/0/all/0/1">Woong-Tae Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cha_S/0/1/0/all/0/1">Sang-Mok Cha</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_D/0/1/0/all/0/1">Dong-Jin Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_H/0/1/0/all/0/1">Hyoun-Woo Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hong_K/0/1/0/all/0/1">Kyeongsoo Hong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_S/0/1/0/all/0/1">Seung-Lee Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_D/0/1/0/all/0/1">Dong-Joo Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_Y/0/1/0/all/0/1">Yongseok Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Park_B/0/1/0/all/0/1">Byeong-Gon Park</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pogge_R/0/1/0/all/0/1">Richard W. Pogge</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zang_W/0/1/0/all/0/1">Weicheng Zang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mroz_P/0/1/0/all/0/1">Przemek Mróz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Szymanski_M/0/1/0/all/0/1">Michał K. Szymański</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Skowron_J/0/1/0/all/0/1">Jan Skowron</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Poleski_R/0/1/0/all/0/1">Radek Poleski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Soszynski_I/0/1/0/all/0/1">Igor Soszyński</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pietrukowicz_P/0/1/0/all/0/1">Paweł Pietrukowicz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kozlowski_S/0/1/0/all/0/1">Szymon Kozłowski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ulaczyk_K/0/1/0/all/0/1">Krzysztof Ulaczyk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rybicki_K/0/1/0/all/0/1">Krzysztof A. Rybicki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Iwanek_P/0/1/0/all/0/1">Patryk Iwanek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wrona_M/0/1/0/all/0/1">Marcin Wrona</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abe_F/0/1/0/all/0/1">Fumio Abe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barry_R/0/1/0/all/0/1">Richard Barry</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bennett_D/0/1/0/all/0/1">David P. Bennett</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bhattacharya_A/0/1/0/all/0/1">Aparna Bhattacharya</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Donachie_M/0/1/0/all/0/1">Martin Donachie</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fukui_A/0/1/0/all/0/1">Akihiko Fukui</a>, et al. (17 additional authors not shown)

We report the discovery of the microlensing planet OGLE-2018-BLG-0740Lb. The
planet is detected with a very strong signal of $Deltachi^2sim 4630$, but
the interpretation of the signal suffers from two types of degeneracies. One
type is caused by the previously known close/wide degeneracy, and the other is
caused by an ambiguity between two solutions, in which one solution requires to
incorporate finite-source effects, while the other solution is consistent with
a point-source interpretation. Although difficult to be firmly resolved based
on only the photometric data, the degeneracy is resolved in strong favor of the
point-source solution with the additional external information obtained from
astrometric and spectroscopic observations. The small astrometric offset
between the source and baseline object supports that the blend is the lens and
this interpretation is further secured by the consistency of the spectroscopic
distance estimate of the blend with the lensing parameters of the point-source
solution. The estimated mass of the host is $1.0pm 0.1~M_odot$ and the mass
of the planet is $4.5pm 0.6~M_{rm J}$ (close solution) or $4.8pm 0.6~M_{rm
J}$ (wide solution) and the lens is located at a distance of $3.2pm 0.5$~kpc.
The bright nature of the lens, with $Isim 17.1$ ($Vsim 18.2$), combined with
its dominance of the observed flux suggest that radial-velocity (RV) follow-up
observations of the lens can be done using high-resolution spectrometers
mounted on large telescopes, e.g., VLT/ESPRESSO, and this can potentially not
only measure the period and eccentricity of the planet but also probe for
close-in planets. We estimate that the expected RV amplitude would be $sim
60sin i ~{rm m~s}^{-1}$.

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