OGLE-2018-BLG-0799Lb: a q ∼2.7 × 10-3planet with Spitzer parallax

Weicheng Zang; Yossi Shvartzvald; Andrzej Udalski; Jennifer C. Yee; Chung Uk Lee; Takahiro Sumi; Xiangyu Zhang; Hongjing Yang; Shude Mao; Sebastiano Calchi Novati; Andrew Gould; Wei Zhu; Charles A. Beichman; Geoffery Bryden; Sean Carey; B. Scott Gaudi; Calen B. Henderson; Przemek Mróz; Jan Skowron; Radoslaw Poleski; Michał K. Szymański; Igor Soszyński; Paweł Pietrukowicz; Szymon Kozłowski; Krzysztof Ulaczyk; Krzysztof A. Rybicki; Patryk Iwanek; Marcin Wrona; Michael D. Albrow; Sun Ju Chung; Cheongho Han; Kyu Ha Hwang; Youn Kil Jung; Yoon Hyun Ryu; In Gu Shin; Sang Mok Cha; Dong Jin Kim; Hyoun Woo Kim; Seung Lee Kim; Dong Joo Lee; Yongseok Lee; Byeong Gon Park; Richard W. Pogge; Ian A. Bond; Fumio Abe; Richard Barry; David P. Bennett; Aparna Bhattacharya; Martin Donachie; Hirosane Fujii; Akihiko Fukui; Yuki Hirao; Yoshitaka Itow; Rintaro Kirikawa; Iona Kondo; Naoki Koshimoto; Man Cheung Alex Li; Yutaka Matsubara; Yasushi Muraki; Shota Miyazaki; Clément Ranc; Nicholas J. Rattenbury; Yuki Satoh; Hikaru Shoji; Daisuke Suzuki; Yuzuru Tanaka; Paul J. Tristram; Tsubasa Yamawaki; Atsunori Yonehara; Etienne Bachelet; Markus P.G. Hundertmark; R. Figuera Jaimes; Dan Maoz; Matthew T. Penny; Rachel A. Street; Yiannis Tsapras

doi:10.1093/mnras/stac1631

OGLE-2018-BLG-0799Lb: a q ∼2.7 × 10^-3planet with Spitzer parallax

Weicheng Zang^*, Yossi Shvartzvald, Andrzej Udalski, Jennifer C. Yee, Chung Uk Lee, Takahiro Sumi, Xiangyu Zhang, Hongjing Yang, Shude Mao, Sebastiano Calchi Novati, Andrew Gould, Wei Zhu, Charles A. Beichman, Geoffery Bryden, Sean Carey, B. Scott Gaudi, Calen B. Henderson, Przemek Mróz, Jan Skowron, Radoslaw PoleskiMichał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Michael D. Albrow, Sun Ju Chung, Cheongho Han, Kyu Ha Hwang, Youn Kil Jung, Yoon Hyun Ryu, In Gu Shin, Sang Mok Cha, Dong Jin Kim, Hyoun Woo Kim, Seung Lee Kim, Dong Joo Lee, Yongseok Lee, Byeong Gon Park, Richard W. Pogge, Ian A. Bond, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Martin Donachie, Hirosane Fujii, Akihiko Fukui, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Man Cheung Alex Li, Yutaka Matsubara, Yasushi Muraki, Shota Miyazaki, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Hikaru Shoji, Daisuke Suzuki, Yuzuru Tanaka, Paul J. Tristram, Tsubasa Yamawaki, Atsunori Yonehara, Etienne Bachelet, Markus P.G. Hundertmark, R. Figuera Jaimes, Dan Maoz, Matthew T. Penny, Rachel A. Street, Yiannis Tsapras

^*Corresponding author for this work

School of Physics and Astronomy

Research output: Contribution to journal › Article › peer-review

5 Scopus citations

Abstract

We report the discovery and analysis of a planet in the microlensing event OGLE-2018-BLG-0799. The planetary signal was observed by several ground-based telescopes, and the planet-host mass ratio is q = (2.65 ± 0.16) × 10-3. The ground-based observations yield a constraint on the angular Einstein radius θE, and the microlensing parallax vector πE, is strongly constrained by the Spitzer data. However, the 2019 Spitzer baseline data reveal systematics in the Spitzer photometry, so there is ambiguity in the magnitude of the parallax. In our preferred interpretation, a full Bayesian analysis using a Galactic model indicates that the planetary system is composed of an Mplanet = 0 . 26 + 0 . 22-0 . 11 MJ planet orbiting an Mhost = 0 . 093 +0.082-0.038 M ⊙, at a distance of DL = 3 . 71 + 3 . 24-1 . 70 kpc. An alternate interpretation of the data shifts the localization of the minima along the arc-shaped microlens parallax constraints. This, in turn, yields a more massive host with median mass of 0.13 M⊙ at a distance of 6.3 kpc. This analysis demonstrates the robustness of the osculating circles formalism, but shows that further investigation is needed to assess how systematics affect the specific localization of the microlens parallax vector and, consequently, the inferred physical parameters.

Original language	English
Pages (from-to)	5952-5968
Number of pages	17
Journal	Monthly Notices of the Royal Astronomical Society
Volume	514
Issue number	4
DOIs	https://doi.org/10.1093/mnras/stac1631
State	Published - 1 Aug 2022

Funding

Funders	Funder number
National Aeronautics and Space Administration
Ministry of Finance
SAAO
CTIO
Seventh Framework Programme
Chinese Academy of Sciences
Korea Astronomy and Space Science Institute
National Astronomical Observatories, Chinese Academy of Sciences
Japan Society for the Promotion of Science	20J20633
Narodowe Centrum Nauki	MAESTRO 2014/14/A/ST9/00121
Jet Propulsion Laboratory	1571564
European Research Council	321035
National Research Foundation of Korea	2017R1A4A1015178, 2019R1A2C2085965
California Institute of Technology	1500811, AST-1516842
National Natural Science Foundation of China	12133005
Deutsche Forschungsgemeinschaft	WA 1047/11-1
Scleroderma Society of Ontario	JP17H02871, JSPS24253004, JSPS15H00781, JSPS23340064, JSPS26247023, JP16H06287

Keywords

gravitational lensing: micro
planets and satellites: detection

Access to Document

10.1093/mnras/stac1631

Cite this

Zang, W., Shvartzvald, Y., Udalski, A., Yee, J. C., Lee, C. U., Sumi, T., Zhang, X., Yang, H., Mao, S., Novati, S. C., Gould, A., Zhu, W., Beichman, C. A., Bryden, G., Carey, S., Gaudi, B. S., Henderson, C. B., Mróz, P., Skowron, J., ... Tsapras, Y. (2022). OGLE-2018-BLG-0799Lb: a q ∼2.7 × 10^-3planet with Spitzer parallax. Monthly Notices of the Royal Astronomical Society, 514(4), 5952-5968. https://doi.org/10.1093/mnras/stac1631

@article{c49901a1196e4b8eb0c1a04bd33c1bbe,

title = "OGLE-2018-BLG-0799Lb: a q ∼2.7 × 10-3planet with Spitzer parallax",

abstract = "We report the discovery and analysis of a planet in the microlensing event OGLE-2018-BLG-0799. The planetary signal was observed by several ground-based telescopes, and the planet-host mass ratio is q = (2.65 ± 0.16) × 10-3. The ground-based observations yield a constraint on the angular Einstein radius θE, and the microlensing parallax vector πE, is strongly constrained by the Spitzer data. However, the 2019 Spitzer baseline data reveal systematics in the Spitzer photometry, so there is ambiguity in the magnitude of the parallax. In our preferred interpretation, a full Bayesian analysis using a Galactic model indicates that the planetary system is composed of an Mplanet = 0 . 26 + 0 . 22-0 . 11 MJ planet orbiting an Mhost = 0 . 093 +0.082-0.038 M ⊙, at a distance of DL = 3 . 71 + 3 . 24-1 . 70 kpc. An alternate interpretation of the data shifts the localization of the minima along the arc-shaped microlens parallax constraints. This, in turn, yields a more massive host with median mass of 0.13 M⊙ at a distance of 6.3 kpc. This analysis demonstrates the robustness of the osculating circles formalism, but shows that further investigation is needed to assess how systematics affect the specific localization of the microlens parallax vector and, consequently, the inferred physical parameters.",

keywords = "gravitational lensing: micro, planets and satellites: detection",

author = "Weicheng Zang and Yossi Shvartzvald and Andrzej Udalski and Yee, {Jennifer C.} and Lee, {Chung Uk} and Takahiro Sumi and Xiangyu Zhang and Hongjing Yang and Shude Mao and Novati, {Sebastiano Calchi} and Andrew Gould and Wei Zhu and Beichman, {Charles A.} and Geoffery Bryden and Sean Carey and Gaudi, {B. Scott} and Henderson, {Calen B.} and Przemek Mr{\'o}z and Jan Skowron and Radoslaw Poleski and Szyma{\'n}ski, {Micha{\l} K.} and Igor Soszy{\'n}ski and Pawe{\l} Pietrukowicz and Szymon Koz{\l}owski and Krzysztof Ulaczyk and Rybicki, {Krzysztof A.} and Patryk Iwanek and Marcin Wrona and Albrow, {Michael D.} and Chung, {Sun Ju} and Cheongho Han and Hwang, {Kyu Ha} and Jung, {Youn Kil} and Ryu, {Yoon Hyun} and Shin, {In Gu} and Cha, {Sang Mok} and Kim, {Dong Jin} and Kim, {Hyoun Woo} and Kim, {Seung Lee} and Lee, {Dong Joo} and Yongseok Lee and Park, {Byeong Gon} and Pogge, {Richard W.} and Bond, {Ian A.} and Fumio Abe and Richard Barry and Bennett, {David P.} and Aparna Bhattacharya and Martin Donachie and Hirosane Fujii and Akihiko Fukui and Yuki Hirao and Yoshitaka Itow and Rintaro Kirikawa and Iona Kondo and Naoki Koshimoto and Li, {Man Cheung Alex} and Yutaka Matsubara and Yasushi Muraki and Shota Miyazaki and Cl{\'e}ment Ranc and Rattenbury, {Nicholas J.} and Yuki Satoh and Hikaru Shoji and Daisuke Suzuki and Yuzuru Tanaka and Tristram, {Paul J.} and Tsubasa Yamawaki and Atsunori Yonehara and Etienne Bachelet and Hundertmark, {Markus P.G.} and Jaimes, {R. Figuera} and Dan Maoz and Penny, {Matthew T.} and Street, {Rachel A.} and Yiannis Tsapras",

note = "Publisher Copyright: {\textcopyright} 2022 The Author(s).",

year = "2022",

month = aug,

day = "1",

doi = "10.1093/mnras/stac1631",

language = "אנגלית",

volume = "514",

pages = "5952--5968",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

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Zang, W, Shvartzvald, Y, Udalski, A, Yee, JC, Lee, CU, Sumi, T, Zhang, X, Yang, H, Mao, S, Novati, SC, Gould, A, Zhu, W, Beichman, CA, Bryden, G, Carey, S, Gaudi, BS, Henderson, CB, Mróz, P, Skowron, J, Poleski, R, Szymański, MK, Soszyński, I, Pietrukowicz, P, Kozłowski, S, Ulaczyk, K, Rybicki, KA, Iwanek, P, Wrona, M, Albrow, MD, Chung, SJ, Han, C, Hwang, KH, Jung, YK, Ryu, YH, Shin, IG, Cha, SM, Kim, DJ, Kim, HW, Kim, SL, Lee, DJ, Lee, Y, Park, BG, Pogge, RW, Bond, IA, Abe, F, Barry, R, Bennett, DP, Bhattacharya, A, Donachie, M, Fujii, H, Fukui, A, Hirao, Y, Itow, Y, Kirikawa, R, Kondo, I, Koshimoto, N, Li, MCA, Matsubara, Y, Muraki, Y, Miyazaki, S, Ranc, C, Rattenbury, NJ, Satoh, Y, Shoji, H, Suzuki, D, Tanaka, Y, Tristram, PJ, Yamawaki, T, Yonehara, A, Bachelet, E, Hundertmark, MPG, Jaimes, RF, Maoz, D, Penny, MT, Street, RA & Tsapras, Y 2022, 'OGLE-2018-BLG-0799Lb: a q ∼2.7 × 10^-3planet with Spitzer parallax', Monthly Notices of the Royal Astronomical Society, vol. 514, no. 4, pp. 5952-5968. https://doi.org/10.1093/mnras/stac1631

TY - JOUR

T1 - OGLE-2018-BLG-0799Lb

T2 - a q ∼2.7 × 10-3planet with Spitzer parallax

AU - Zang, Weicheng

AU - Shvartzvald, Yossi

AU - Udalski, Andrzej

AU - Yee, Jennifer C.

AU - Lee, Chung Uk

AU - Sumi, Takahiro

AU - Zhang, Xiangyu

AU - Yang, Hongjing

AU - Mao, Shude

AU - Novati, Sebastiano Calchi

AU - Gould, Andrew

AU - Zhu, Wei

AU - Beichman, Charles A.

AU - Bryden, Geoffery

AU - Carey, Sean

AU - Gaudi, B. Scott

AU - Henderson, Calen B.

AU - Mróz, Przemek

AU - Skowron, Jan

AU - Poleski, Radoslaw

AU - Szymański, Michał K.

AU - Soszyński, Igor

AU - Pietrukowicz, Paweł

AU - Kozłowski, Szymon

AU - Ulaczyk, Krzysztof

AU - Rybicki, Krzysztof A.

AU - Iwanek, Patryk

AU - Wrona, Marcin

AU - Albrow, Michael D.

AU - Chung, Sun Ju

AU - Han, Cheongho

AU - Hwang, Kyu Ha

AU - Jung, Youn Kil

AU - Ryu, Yoon Hyun

AU - Shin, In Gu

AU - Cha, Sang Mok

AU - Kim, Dong Jin

AU - Kim, Hyoun Woo

AU - Kim, Seung Lee

AU - Lee, Dong Joo

AU - Lee, Yongseok

AU - Park, Byeong Gon

AU - Pogge, Richard W.

AU - Bond, Ian A.

AU - Abe, Fumio

AU - Barry, Richard

AU - Bennett, David P.

AU - Bhattacharya, Aparna

AU - Donachie, Martin

AU - Fujii, Hirosane

AU - Fukui, Akihiko

AU - Hirao, Yuki

AU - Itow, Yoshitaka

AU - Kirikawa, Rintaro

AU - Kondo, Iona

AU - Koshimoto, Naoki

AU - Li, Man Cheung Alex

AU - Matsubara, Yutaka

AU - Muraki, Yasushi

AU - Miyazaki, Shota

AU - Ranc, Clément

AU - Rattenbury, Nicholas J.

AU - Satoh, Yuki

AU - Shoji, Hikaru

AU - Suzuki, Daisuke

AU - Tanaka, Yuzuru

AU - Tristram, Paul J.

AU - Yamawaki, Tsubasa

AU - Yonehara, Atsunori

AU - Bachelet, Etienne

AU - Hundertmark, Markus P.G.

AU - Jaimes, R. Figuera

AU - Maoz, Dan

AU - Penny, Matthew T.

AU - Street, Rachel A.

AU - Tsapras, Yiannis

PY - 2022/8/1

Y1 - 2022/8/1

N2 - We report the discovery and analysis of a planet in the microlensing event OGLE-2018-BLG-0799. The planetary signal was observed by several ground-based telescopes, and the planet-host mass ratio is q = (2.65 ± 0.16) × 10-3. The ground-based observations yield a constraint on the angular Einstein radius θE, and the microlensing parallax vector πE, is strongly constrained by the Spitzer data. However, the 2019 Spitzer baseline data reveal systematics in the Spitzer photometry, so there is ambiguity in the magnitude of the parallax. In our preferred interpretation, a full Bayesian analysis using a Galactic model indicates that the planetary system is composed of an Mplanet = 0 . 26 + 0 . 22-0 . 11 MJ planet orbiting an Mhost = 0 . 093 +0.082-0.038 M ⊙, at a distance of DL = 3 . 71 + 3 . 24-1 . 70 kpc. An alternate interpretation of the data shifts the localization of the minima along the arc-shaped microlens parallax constraints. This, in turn, yields a more massive host with median mass of 0.13 M⊙ at a distance of 6.3 kpc. This analysis demonstrates the robustness of the osculating circles formalism, but shows that further investigation is needed to assess how systematics affect the specific localization of the microlens parallax vector and, consequently, the inferred physical parameters.

AB - We report the discovery and analysis of a planet in the microlensing event OGLE-2018-BLG-0799. The planetary signal was observed by several ground-based telescopes, and the planet-host mass ratio is q = (2.65 ± 0.16) × 10-3. The ground-based observations yield a constraint on the angular Einstein radius θE, and the microlensing parallax vector πE, is strongly constrained by the Spitzer data. However, the 2019 Spitzer baseline data reveal systematics in the Spitzer photometry, so there is ambiguity in the magnitude of the parallax. In our preferred interpretation, a full Bayesian analysis using a Galactic model indicates that the planetary system is composed of an Mplanet = 0 . 26 + 0 . 22-0 . 11 MJ planet orbiting an Mhost = 0 . 093 +0.082-0.038 M ⊙, at a distance of DL = 3 . 71 + 3 . 24-1 . 70 kpc. An alternate interpretation of the data shifts the localization of the minima along the arc-shaped microlens parallax constraints. This, in turn, yields a more massive host with median mass of 0.13 M⊙ at a distance of 6.3 kpc. This analysis demonstrates the robustness of the osculating circles formalism, but shows that further investigation is needed to assess how systematics affect the specific localization of the microlens parallax vector and, consequently, the inferred physical parameters.

KW - gravitational lensing: micro

KW - planets and satellites: detection

UR - http://www.scopus.com/inward/record.url?scp=85135141255&partnerID=8YFLogxK

U2 - 10.1093/mnras/stac1631

DO - 10.1093/mnras/stac1631

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AN - SCOPUS:85135141255

SN - 0035-8711

VL - 514

SP - 5952

EP - 5968

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 4

ER -