OGLE-2015-BLG-1649Lb: A Gas Giant Planet around a Low-mass Dwarf

被引：3

作者：

Nagakane, M. ^{[1
]}

Lee, Chien-Hsiu ^{[2
]}

Koshimoto, N. ^{[3
,4
]}

Suzuki, D. ^{[5
]}

Udalski, A. ^{[6
]}

Beaulieu, J. P. ^{[7
]}

Sumi, T. ^{[1
]}

Bennett, D. P. ^{[8
,9
]}

Bond, I. A. ^{[10
]}

Rattenbury, N. ^{[11
]}

Bachelet, E. ^{[12
]}

Dominik, M. ^{[13
]}

Abe, F. ^{[14
]}

Barry, R. K. ^{[8
]}

Bhattacharya, A. ^{[8
,9
]}

Donachie, M. ^{[11
]}

Fujii, H. ^{[14
]}

Fukui, A. ^{[3
,15
]}

Hirao, Y. ^{[1
]}

Itow, Y. ^{[14
]}

Kamei, Y. ^{[14
]}

Kondo, I ^{[1
]}

Li, M. C. A. ^{[11
]}

Matsubara, Y. ^{[14
]}

Matsuo, T. ^{[1
]}

Miyazaki, S. ^{[1
]}

Muraki, Y. ^{[14
]}

Ranc, C. ^{[8
]}

Shibai, H. ^{[1
]}

Suematsu, H. ^{[1
]}

Sullivan, D. J. ^{[16
]}

Tristram, P. J. ^{[17
]}

Yamakawa, T. ^{[14
]}

Yonehara, A. ^{[18
]}

Mroz, P. ^{[6
]}

Poleski, R. ^{[6
,19
]}

Skowron, J. ^{[6
]}

Szymanski, M. K. ^{[6
]}

Soszynski, I ^{[6
]}

Pietrukowicz, P. ^{[6
]}

Kozlowski, S. ^{[6
]}

Ulaczyk, K. ^{[6
,20
]}

Bramich, D. M. ^{[21
,22
,23
]}

Cassan, A. ^{[24
]}

Figuera Jaimes, R. ^{[25
]}

Horne, K. ^{[26
]}

Hundertmark, M. ^{[27
]}

Mao, S. ^{[28
,29
,30
]}

Menzies, J. ^{[31
]}

Schmidt, R. ^{[27
]}

机构：

[1] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, 1-1 Machikaneyama, Toyonaka, Osaka 5600043, Japan

[2] 650 N Aohoku Pl, Hilo, HI 96720 USA

[3] Univ Tokyo, Grad Sch Sci, Dept Astron, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan

[4] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan

[5] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan

[6] Univ Warsaw, Astron Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland

[7] UPMC Univ Paris 06, CNRS, Inst Astrophys Paris, UMR 7095,Sorbonne Univ, F-75014 Paris, France

[8] NASA, Lab Exoplanets & Stellar Astrophys, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[9] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[10] Massey Univ, North Shore Mail Ctr, Inst Informat & Math Sci, Private Bag 102-904, Auckland, New Zealand

[11] Univ Auckland, Dept Phys, Private Bag 92019, Auckland, New Zealand

[12] Las Cumbres Observ Global Telescope Network, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA

[13] Univ St Andrews, Ctr Exoplanet Sci, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland

[14] Nagoya Univ, Inst Space Earth Environm Res, Nagoya, Aichi 4648601, Japan

[15] Inst Astrofis Canarias, Via Lactea S-N, E-38205 Tenerife, Spain

[16] Victoria Univ, Sch Chem & Phys Sci, Wellington, New Zealand

[17] Univ Canterbury, Mt John Observ, POB 56, Lake Tekapo 8770, New Zealand

[18] Kyoto Sangyo Univ, Fac Sci, Dept Phys, Kyoto 6038555, Japan

[19] Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA

[20] Univ Warwick, Dept Phys, Gibbet Hill Rd, Coventry CV4 7AL, W Midlands, England

[21] New York Univ Abu Dhabi, Ctr Space Sci, NYUAD Inst, POB 129188, Abu Dhabi, U Arab Emirates

[22] New York Univ Abu Dhabi, Div Sci, POB 129188, Abu Dhabi, U Arab Emirates

[23] New York Univ Abu Dhabi, Div Engn, POB 129188, Abu Dhabi, U Arab Emirates

[24] Sorbonne Univ, CNRS, Inst Astrophys Paris, UMR 7095, 98 Bis Bd Arago, F-75014 Paris, France

[25] Univ San Sebastian, Fac Ingn & Tecnol, Gen Lagos 1163, Valdivia 5110693, Chile

[26] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland

[27] Heidelberg Univ, Zentrum Astron, Astron Rechen Inst, Monchhofstr 12-14, D-69120 Heidelberg, Germany

[28] Tsinghua Univ, Phys Dept, Beijing 100084, Peoples R China

[29] Tsinghua Univ, Tsinghua Ctr Astrophys, Beijing 100084, Peoples R China

[30] Chinese Acad Sci, Natl Astron Observ, 20A Datun Rd, Beijing 100012, Peoples R China

[31] South African Astron Observ, POB 9, ZA-7935 Observatory, South Africa

[32] Open Univ, Dept Phys Sci, Planetary & Space Sci, Milton Keynes MK7 6AA, Bucks, England

[33] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland

[34] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool CH41 1LD, Merseyside, England

[35] Int Space Sci Inst, Haller Str 6, CH-3012 Bern, Switzerland

[36] Univ Copenhagen, Niels Bohr Inst, Oster Voldgade 5, DK-1350 Copenhagen, Denmark

[37] Univ Copenhagen, Ctr Star & Planet Format, Oster Voldgade 5, DK-1350 Copenhagen, Denmark

[38] Univ Salerno, Dipartimento Fis ER Caianiello, Via Giovanni Paolo II 132, I-84084 Fisciano, Italy

[39] Ist Nazl Fis Nucl, Sez Napoli, Naples, Italy

[40] Univ Antofagasta, Ctr Astronom CITEVA, Avda U Antofagasta 02800, Antofagasta, Chile

[41] Univ Coimbra, Geophys & Astron Observ, CITEUC Ctr Earth & Space Res, R Observ S-N, P-3040004 Coimbra, Portugal

[42] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England

[43] Niels Bohr Inst, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark

[44] Univ Hamburg, Fac Math Informat & Nat Sci, Dept Earth Sci, Meteorol Inst, Bundesstr 55, D-20146 Hamburg, Germany

[45] Pontificia Univ Catolica Chile, Fac Fis, Ctr Astroingn, Av Vicuna Mackenna 4860, Santiago 7820436, Chile

[46] Chungnam Natl Univ, Dept Astron & Space Sci, Daejeon 34134, South Korea

[47] Las Cumbres Observ Global Telescope, 6740 Cortona Dr,Suite 102, Goleta, CA 93111 USA

[48] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA

[49] Sharif Univ Technol, Dept Phys, POB 11155-9161, Tehran, Iran

来源：

ASTRONOMICAL JOURNAL | 2019年 / 158卷 / 05期

关键词：

GALACTIC BULGE; CAMERA; STARS; MODEL; HOST;

D O I：

10.3847/1538-3881/ab4881

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report the discovery of an exoplanet from the analysis of the gravitational microlensing event OGLE-2015-BLG-1649 that challenges the core accretion model of planet formation and appears to support the disk instability model. The planet/host-star mass ratio is q = 7.2 x 10(3) and the projected separation normalized to the angular Einstein radius is s = 0.9. We conducted high-resolution follow-up observations using the Infrared Camera and Spectrograph (IRCS) camera on the Subaru telescope and are able to place an upper limit on the lens flux. From these measurements we are able to exclude all host stars greater than or equal in mass to a G-type dwarf. We conducted a Bayesian analysis with these new flux constraints included as priors resulting in estimates of the masses of the host star and planet. These are M-L respectively. The distance to the system is The estimated relative lens-source proper motion, is fairly high and thus the lens can be better constrained if additional follow-up observations are conducted several years after the event.

引用

页数：9

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