OGLE-2016-BLG-0156: Microlensing Event With Pronounced Microlens-Parallax Effects Yielding Precise Lens Mass Measurement. (arXiv:1901.06457v1 [astro-ph.SR])

OGLE-2016-BLG-0156: Microlensing Event With Pronounced Microlens-Parallax Effects Yielding Precise Lens Mass Measurement. (arXiv:1901.06457v1 [astro-ph.SR])
<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:+Han_C/0/1/0/all/0/1">Cheongho Han</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:+Udalski_A/0/1/0/all/0/1">Andrzej Udalski</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:+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:+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:+Yee_J/0/1/0/all/0/1">Jennifer C. Yee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jee_M/0/1/0/all/0/1">M. James Jee</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:+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:+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:+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>, <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:+Itow_Y/0/1/0/all/0/1">Yoshitaka Itow</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kawasaki_K/0/1/0/all/0/1">Kohei Kawasaki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kondo_I/0/1/0/all/0/1">Iona Kondo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koshimoto_N/0/1/0/all/0/1">Naoki Koshimoto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_M/0/1/0/all/0/1">Man Cheung Alex Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matsubara_Y/0/1/0/all/0/1">Yutaka Matsubara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Muraki_Y/0/1/0/all/0/1">Yasushi Muraki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miyazaki_S/0/1/0/all/0/1">Shota Miyazaki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nagakane_M/0/1/0/all/0/1">Masayuki~Nagakane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ranc_C/0/1/0/all/0/1">Cl&#xe9;ment Ranc</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rattenbury_N/0/1/0/all/0/1">Nicholas J. Rattenbury</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Suematsu_H/0/1/0/all/0/1">Haruno Suematsu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sullivan_D/0/1/0/all/0/1">Denis J. Sullivan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sumi_T/0/1/0/all/0/1">Takahiro Sumi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Suzuki_D/0/1/0/all/0/1">Daisuke Suzuki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tristram_P/0/1/0/all/0/1">Paul J. Tristram</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yonehara_A/0/1/0/all/0/1">Atsunori Yonehara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mroz_P/0/1/0/all/0/1">Przemek Mr&#xf3;z</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:+Skowron_J/0/1/0/all/0/1">Jan Skowron</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Szymanski_M/0/1/0/all/0/1">Micha&#x142; K. Szyma&#x144;ski</a>, et al. (5 additional authors not shown)

We analyze the gravitational binary-lensing event OGLE-2016-BLG-0156, for
which the lensing light curve displays pronounced deviations induced by
microlens-parallax effects. The light curve exhibits 3 distinctive
widely-separated peaks and we find that the multiple-peak feature provides a
very tight constraint on the microlens-parallax effect, enabling us to
precisely measure the microlens parallax $pi_{rm E}$. All the peaks are
densely and continuously covered from high-cadence survey observations using
globally located telescopes and the analysis of the peaks leads to the precise
measurement of the angular Einstein radius $theta_{rm E}$. From the
combination of the measured $pi_{rm E}$ and $theta_{rm E}$, we determine
the physical parameters of the lens. It is found that the lens is a binary
composed of two M dwarfs with masses $M_1=0.18pm 0.01 M_odot$ and
$M_2=0.16pm 0.01 M_odot$ located at a distance $D_{rm L}= 1.35pm 0.09
{rm kpc}$. According to the estimated lens mass and distance, the flux from
the lens comprises an important fraction, $sim 25%$, of the blended flux. The
bright nature of the lens combined with the high relative lens-source motion,
$mu=6.94pm 0.50 {rm mas} {rm yr}^{-1}$, suggests that the lens can be
directly observed from future high-resolution follow-up observations.

We analyze the gravitational binary-lensing event OGLE-2016-BLG-0156, for
which the lensing light curve displays pronounced deviations induced by
microlens-parallax effects. The light curve exhibits 3 distinctive
widely-separated peaks and we find that the multiple-peak feature provides a
very tight constraint on the microlens-parallax effect, enabling us to
precisely measure the microlens parallax $pi_{rm E}$. All the peaks are
densely and continuously covered from high-cadence survey observations using
globally located telescopes and the analysis of the peaks leads to the precise
measurement of the angular Einstein radius $theta_{rm E}$. From the
combination of the measured $pi_{rm E}$ and $theta_{rm E}$, we determine
the physical parameters of the lens. It is found that the lens is a binary
composed of two M dwarfs with masses $M_1=0.18pm 0.01 M_odot$ and
$M_2=0.16pm 0.01 M_odot$ located at a distance $D_{rm L}= 1.35pm 0.09
{rm kpc}$. According to the estimated lens mass and distance, the flux from
the lens comprises an important fraction, $sim 25%$, of the blended flux. The
bright nature of the lens combined with the high relative lens-source motion,
$mu=6.94pm 0.50 {rm mas} {rm yr}^{-1}$, suggests that the lens can be
directly observed from future high-resolution follow-up observations.

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