Kepler K2 Campaign 9-II. First space-based discovery of an exoplanet using microlensing

被引：2

作者：

Specht, D. ^{[1
]}

Poleski, R. ^{[2
]}

Penny, M. T. ^{[3
]}

Kerins, E. ^{[1
]}

McDonald, I ^{[1
,4
]}

Lee, Chung-Uk ^{[5
,6
]}

Udalski, A. ^{[2
]}

Bond, I. A. ^{[7
]}

Shvartzvald, Y. ^{[8
]}

Zang, Weicheng ^{[9
,10
]}

Street, R. A. ^{[11
]}

Hogg, D. W. ^{[12
,13
]}

Gaudi, B. S. ^{[14
]}

Barclay, T. ^{[15
]}

Barentsen, G. ^{[16
]}

Howell, S. B. ^{[16
]}

Mullally, F. ^{[16
]}

Henderson, C. B. ^{[17
]}

Bryson, S. T. ^{[16
]}

Caldwell, D. A. ^{[16
]}

Haas, M. R. ^{[16
]}

Van Cleve, J. E. ^{[16
]}

Larson, K. ^{[18
]}

McCalmont, K. ^{[18
]}

Peterson, C. ^{[18
]}

Putnam, D. ^{[18
]}

Ross, S. ^{[18
]}

Packard, M. ^{[19
]}

Reedy, L. ^{[19
]}

Albrow, Michael D. ^{[20
]}

Chung, Sun-Ju ^{[5
,6
]}

Kil Jung, Youn ^{[5
]}

Gould, Andrew ^{[21
]}

Han, Cheongho ^{[22
]}

Hwang, Kyu-Ha

Ryu, Yoon-Hyun

Shin, In-Gu

Yang, Hongjing ^{[9
,10
]}

Yee, Jennifer C. ^{[23
]}

Cha, Sang-Mok ^{[5
]}

Kim, Dong-Jin ^{[5
]}

Kim, Seung-Lee ^{[5
,6
]}

Lee, Dong-Joo ^{[5
]}

Lee, Yongseok ^{[5
,24
]}

Park, Byeong-Gon ^{[5
,6
]}

Pogge, Richard W. ^{[14
]}

Szymanski, M. K. ^{[2
]}

Soszynski, I ^{[2
]}

Ulaczyk, K. ^{[2
,25
]}

Pietrukowicz, P. ^{[2
]}

机构：

[1] Univ Manchester, Jodrell Bank Ctr Astrophys, Dept Phys & Astron, Oxford Rd, Manchester M13 9PL, England

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

[3] Louisiana State Univ, 261-B Nicholson Hall,Tower Dr, Baton Rouge, LA 70803 USA

[4] Open Univ, Dept Phys Sci, Walton Hall, Milton Keynes MK7 6AA, England

[5] Korea Astron & Space Sci Inst, Daejon 34055, South Korea

[6] Korea Univ Sci & Technol, Korea UST, 217 Gajeong ro, Daejeon 34113, South Korea

[7] Massey Univ, Inst Nat & Math Sci, North Shore Mail Ctr, Private Bag 102904, Auckland 0745, New Zealand

[8] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel

[9] Tsinghua Univ, Dept Astron, Beijing 100084, Peoples R China

[10] CALTECH, Tsinghua Ctr Astrophys, 4800 Oak Grove Dr, Pasadena, CA USA

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

[12] NYU, Ctr Cosmol & Particle Phys, Dept Phys, 4 Washington Pl,Room 424, New York, NY USA

[13] NYU, Ctr Data Sci, 726 Broadway,7th Floor, New York, NY 10003 USA

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

[15] Univ Maryland Baltimore Cty, 1000 Hilltop Circle, Baltimore, MD 21250 USA

[16] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA

[17] CALTECH, IPAC, Mail Code 100-22,1200 Calif Blvd, Pasadena, CA 91125 USA

[18] Ball Aerosp & Technol, Boulder, CO 80301 USA

[19] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA

[20] Univ Canterbury, Dept Phys & Astron, Private Bag 4800, Daejeon 34113, South Korea

[21] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany

[22] Chungbuk Natl Univ, Dept Phys, Cheongju 28644, South Korea

[23] Ctr Astrophys Harvard & Smithsonian, Cambridge, MA 02138 USA

[24] Kyung Hee Univ, Sch Space Res, Yongin 17104, South Korea

[25] Univ Warwick, Dept Phys, Coventry CV4 7AL, England

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

[27] Chinese Acad Sci, Natl Astron Observ, A20 Datun Rd, Beijing 100012, Peoples R China

[28] CFHT Corp, 65-1238 Mamalahoa Hwy, Kamuela, HI 96743 USA

[29] Univ Toulouse, UPS OMP, IRAP, 14 Edouard Belin, F-31400 Toulouse, France

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

[31] NASA, Goddard Space Flight Ctr, Code 667, Greenbelt, MD 20771 USA

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

[33] Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, 7-3-1Hongo,Bunkyo Ku, Tokyo 1130033, Japan

[34] Inst Astrofis Canarias, Via Lactea S-N, E-38205 San Cristobal la Laguna, Tenerife, Spain

[35] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan

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

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

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

[39] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA

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

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2023年 / 520卷 / 04期

基金：

英国科学技术设施理事会;

关键词：

gravitational lensing; micro; -; methods; data analysis - telescopes - surveys - planets and satellites; detection; GRAVITATIONAL LENSING EXPERIMENT; LEGACY SCIENCE PROPOSAL; FREE-FLOATING PLANETS; MASS-RATIO FUNCTION; ESA EUCLID MISSION; STELLAR DIAMETERS; EVENTS; PREDICTIONS; PHOTOMETRY; SYSTEMS;

D O I：

10.1093/mnras/stad212

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present K2-2016-BLG-0005Lb, a densely sampled, planetary binary caustic-crossing microlensing event found from a blind search of data gathered from Campaign 9 of the Kepler K2 mission (K2C9). K2-2016-BLG-0005Lb is the first bound microlensing exoplanet discovered from space-based data. The event has caustic entry and exit points that are resolved in the K2C9 data, enabling the lens-source relative proper motion to be measured. We have fitted a binary microlens model to the Kepler data and to simultaneous observations from multiple ground-based surveys. Whilst the ground-based data only sparsely sample the binary caustic, they provide a clear detection of parallax that allows us to break completely the microlensing mass-position-velocity degeneracy and measure the planet's mass directly. We find a host mass of 0.58 +/- 0.04 M-? and a planetary mass of 1.1 +/- 0.1 M-J. The system lies at a distance of 5.2 +/- 0.2 kpc from Earth towards the Galactic bulge, more than twice the distance of the previous most distant planet found by Kepler. The sky-projected separation of the planet from its host is found to be 4.2 +/- 0.3 au which, for circular orbits, deprojects to a host separation a = 4.4(-0.4)(+1.9) au and orbital period P = 13(-2)(+9) yr. This makes K2-2016-BLG-0005Lb a close Jupiter analogue orbiting a low-mass host star. According to current planet formation models, this system is very close to the host mass threshold below which Jupiters are not expected to form. Upcoming space-based exoplanet microlensing surveys by NASA's Nancy Grace Roman Space Telescope and, possibly, ESA's Euclid mission, will provide demanding tests of current planet formation models.

引用

页码：6350 / 6366

页数：17

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