MOA-2020-BLG-208Lb: Cool Sub-Saturn-mass Planet within Predicted Desert
We analyze the MOA-2020-BLG-208 gravitational microlensing event and present the discovery and characterization of a new planet, MOA-2020-BLG-208Lb, with an estimated sub-Saturn mass. With a mass ratio $q={3.17}_{-0.26}^{+0.28}\times {10}^{-4}$ , the planet lies near the peak of the mass-ratio funct...
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| Autor*in: |
Greg Olmschenk [verfasserIn] David P. Bennett [verfasserIn] Ian A. Bond [verfasserIn] Weicheng Zang [verfasserIn] Youn Kil Jung [verfasserIn] Jennifer C. Yee [verfasserIn] Etienne Bachelet [verfasserIn] Leading authors [verfasserIn] Fumio Abe [verfasserIn] Richard K. Barry [verfasserIn] Aparna Bhattacharya [verfasserIn] Hirosane Fujii [verfasserIn] Akihiko Fukui [verfasserIn] Yuki Hirao [verfasserIn] Stela Ishitani Silva [verfasserIn] Yoshitaka Itow [verfasserIn] Rintaro Kirikawa [verfasserIn] Iona Kondo [verfasserIn] Naoki Koshimoto [verfasserIn] Yutaka Matsubara [verfasserIn] Sho Matsumoto [verfasserIn] Shota Miyazaki [verfasserIn] Brandon Munford [verfasserIn] Yasushi Muraki [verfasserIn] Arisa Okamura [verfasserIn] Clément Ranc [verfasserIn] Nicholas J. Rattenbury [verfasserIn] Yuki Satoh [verfasserIn] Takahiro Sumi [verfasserIn] Daisuke Suzuki [verfasserIn] Taiga Toda [verfasserIn] Paul J. Tristram [verfasserIn] Aikaterini Vandorou [verfasserIn] Hibiki Yama [verfasserIn] The MOA Collaboration [verfasserIn] Michael D. Albrow [verfasserIn] Sang-Mok Cha [verfasserIn] Sun-Ju Chung [verfasserIn] Andrew Gould [verfasserIn] Cheongho Han [verfasserIn] Kyu-Ha Hwang [verfasserIn] Dong-Jin Kim [verfasserIn] Hyoun-Woo Kim [verfasserIn] Seung-Lee Kim [verfasserIn] Chung-Uk Lee [verfasserIn] Dong-Joo Lee [verfasserIn] Yongseok Lee [verfasserIn] Byeong-Gon Park [verfasserIn] Richard W. Pogge [verfasserIn] Yoon-Hyun Ryu [verfasserIn] In-Gu Shin [verfasserIn] Yossi Shvartzvald [verfasserIn] The KMTNet Collaboration [verfasserIn] Grant Christie [verfasserIn] Tony Cooper [verfasserIn] John Drummond [verfasserIn] Jonathan Green [verfasserIn] Steve Hennerley [verfasserIn] Jennie McCormick [verfasserIn] L. A. G. Monard [verfasserIn] Tim Natusch [verfasserIn] Ian Porritt [verfasserIn] Thiam-Guan Tan [verfasserIn] The MicroFUN Collaboration [verfasserIn] Shude Mao [verfasserIn] Dan Maoz [verfasserIn] Matthew T. Penny [verfasserIn] Wei Zhu [verfasserIn] The MAP Follow-Up Collaboration [verfasserIn] V. Bozza [verfasserIn] Arnaud Cassan [verfasserIn] Martin Dominik [verfasserIn] Markus Hundertmark [verfasserIn] R. Figuera Jaimes [verfasserIn] K. Kruszyńska [verfasserIn] K. A. Rybicki [verfasserIn] R. A. Street [verfasserIn] Y. Tsapras [verfasserIn] Joachim Wambsganss [verfasserIn] Ł. Wyrzykowski [verfasserIn] P. Zieliński [verfasserIn] The OMEGA Collaboration [verfasserIn] Gioia Rau [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2023 |
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| Schlagwörter: |
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| Übergeordnetes Werk: |
In: The Astronomical Journal - IOP Publishing, 2022, 165(2023), 4, p 175 |
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| Übergeordnetes Werk: |
volume:165 ; year:2023 ; number:4, p 175 |
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| DOI / URN: |
10.3847/1538-3881/acbcc8 |
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| Katalog-ID: |
DOAJ089160592 |
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| 100 | 0 | |a Greg Olmschenk |e verfasserin |4 aut | |
| 245 | 1 | 0 | |a MOA-2020-BLG-208Lb: Cool Sub-Saturn-mass Planet within Predicted Desert |
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| 520 | |a We analyze the MOA-2020-BLG-208 gravitational microlensing event and present the discovery and characterization of a new planet, MOA-2020-BLG-208Lb, with an estimated sub-Saturn mass. With a mass ratio $q={3.17}_{-0.26}^{+0.28}\times {10}^{-4}$ , the planet lies near the peak of the mass-ratio function derived by the MOA collaboration and near the edge of expected sample sensitivity. For these estimates we provide results using two mass-law priors: one assuming that all stars have an equal planet-hosting probability, and the other assuming that planets are more likely to orbit around more massive stars. In the first scenario, we estimate that the lens system is likely to be a planet of mass ${m}_{\mathrm{planet}}={46}_{-24}^{+42}\,{M}_{\oplus }$ and a host star of mass ${M}_{\mathrm{host}}={0.43}_{-0.23}^{+0.39}\,{M}_{\odot }$ , located at a distance ${D}_{L}={7.49}_{-1.13}^{+0.99}\,\mathrm{kpc}$ . For the second scenario, we estimate ${m}_{\mathrm{planet}}={69}_{-34}^{+37}\,{M}_{\oplus }$ , ${M}_{\mathrm{host}}={0.66}_{-0.32}^{+0.35}\,{M}_{\odot }$ , and ${D}_{L}={7.81}_{-0.93}^{+0.93}\,\mathrm{kpc}$ . The planet has a projected separation as a fraction of the Einstein ring radius $s={1.3807}_{-0.0018}^{+0.0018}$ . As a cool sub-Saturn-mass planet, this planet adds to a growing collection of evidence for revised planetary formation models. | ||
| 650 | 4 | |a Gravitational microlensing | |
| 650 | 4 | |a Gravitational microlensing exoplanet detection | |
| 650 | 4 | |a Binary lens microlensing | |
| 653 | 0 | |a Astronomy | |
| 700 | 0 | |a David P. Bennett |e verfasserin |4 aut | |
| 700 | 0 | |a Ian A. Bond |e verfasserin |4 aut | |
| 700 | 0 | |a Weicheng Zang |e verfasserin |4 aut | |
| 700 | 0 | |a Youn Kil Jung |e verfasserin |4 aut | |
| 700 | 0 | |a Jennifer C. Yee |e verfasserin |4 aut | |
| 700 | 0 | |a Etienne Bachelet |e verfasserin |4 aut | |
| 700 | 0 | |a Leading authors |e verfasserin |4 aut | |
| 700 | 0 | |a Fumio Abe |e verfasserin |4 aut | |
| 700 | 0 | |a Richard K. Barry |e verfasserin |4 aut | |
| 700 | 0 | |a Aparna Bhattacharya |e verfasserin |4 aut | |
| 700 | 0 | |a Hirosane Fujii |e verfasserin |4 aut | |
| 700 | 0 | |a Akihiko Fukui |e verfasserin |4 aut | |
| 700 | 0 | |a Yuki Hirao |e verfasserin |4 aut | |
| 700 | 0 | |a Stela Ishitani Silva |e verfasserin |4 aut | |
| 700 | 0 | |a Yoshitaka Itow |e verfasserin |4 aut | |
| 700 | 0 | |a Rintaro Kirikawa |e verfasserin |4 aut | |
| 700 | 0 | |a Iona Kondo |e verfasserin |4 aut | |
| 700 | 0 | |a Naoki Koshimoto |e verfasserin |4 aut | |
| 700 | 0 | |a Yutaka Matsubara |e verfasserin |4 aut | |
| 700 | 0 | |a Sho Matsumoto |e verfasserin |4 aut | |
| 700 | 0 | |a Shota Miyazaki |e verfasserin |4 aut | |
| 700 | 0 | |a Brandon Munford |e verfasserin |4 aut | |
| 700 | 0 | |a Yasushi Muraki |e verfasserin |4 aut | |
| 700 | 0 | |a Arisa Okamura |e verfasserin |4 aut | |
| 700 | 0 | |a Clément Ranc |e verfasserin |4 aut | |
| 700 | 0 | |a Nicholas J. Rattenbury |e verfasserin |4 aut | |
| 700 | 0 | |a Yuki Satoh |e verfasserin |4 aut | |
| 700 | 0 | |a Takahiro Sumi |e verfasserin |4 aut | |
| 700 | 0 | |a Daisuke Suzuki |e verfasserin |4 aut | |
| 700 | 0 | |a Taiga Toda |e verfasserin |4 aut | |
| 700 | 0 | |a Paul J. Tristram |e verfasserin |4 aut | |
| 700 | 0 | |a Aikaterini Vandorou |e verfasserin |4 aut | |
| 700 | 0 | |a Hibiki Yama |e verfasserin |4 aut | |
| 700 | 0 | |a The MOA Collaboration |e verfasserin |4 aut | |
| 700 | 0 | |a Michael D. Albrow |e verfasserin |4 aut | |
| 700 | 0 | |a Sang-Mok Cha |e verfasserin |4 aut | |
| 700 | 0 | |a Sun-Ju Chung |e verfasserin |4 aut | |
| 700 | 0 | |a Andrew Gould |e verfasserin |4 aut | |
| 700 | 0 | |a Cheongho Han |e verfasserin |4 aut | |
| 700 | 0 | |a Kyu-Ha Hwang |e verfasserin |4 aut | |
| 700 | 0 | |a Dong-Jin Kim |e verfasserin |4 aut | |
| 700 | 0 | |a Hyoun-Woo Kim |e verfasserin |4 aut | |
| 700 | 0 | |a Seung-Lee Kim |e verfasserin |4 aut | |
| 700 | 0 | |a Chung-Uk Lee |e verfasserin |4 aut | |
| 700 | 0 | |a Dong-Joo Lee |e verfasserin |4 aut | |
| 700 | 0 | |a Yongseok Lee |e verfasserin |4 aut | |
| 700 | 0 | |a Byeong-Gon Park |e verfasserin |4 aut | |
| 700 | 0 | |a Richard W. Pogge |e verfasserin |4 aut | |
| 700 | 0 | |a Yoon-Hyun Ryu |e verfasserin |4 aut | |
| 700 | 0 | |a In-Gu Shin |e verfasserin |4 aut | |
| 700 | 0 | |a Yossi Shvartzvald |e verfasserin |4 aut | |
| 700 | 0 | |a The KMTNet Collaboration |e verfasserin |4 aut | |
| 700 | 0 | |a Grant Christie |e verfasserin |4 aut | |
| 700 | 0 | |a Tony Cooper |e verfasserin |4 aut | |
| 700 | 0 | |a John Drummond |e verfasserin |4 aut | |
| 700 | 0 | |a Jonathan Green |e verfasserin |4 aut | |
| 700 | 0 | |a Steve Hennerley |e verfasserin |4 aut | |
| 700 | 0 | |a Jennie McCormick |e verfasserin |4 aut | |
| 700 | 0 | |a L. A. G. Monard |e verfasserin |4 aut | |
| 700 | 0 | |a Tim Natusch |e verfasserin |4 aut | |
| 700 | 0 | |a Ian Porritt |e verfasserin |4 aut | |
| 700 | 0 | |a Thiam-Guan Tan |e verfasserin |4 aut | |
| 700 | 0 | |a The MicroFUN Collaboration |e verfasserin |4 aut | |
| 700 | 0 | |a Shude Mao |e verfasserin |4 aut | |
| 700 | 0 | |a Dan Maoz |e verfasserin |4 aut | |
| 700 | 0 | |a Matthew T. Penny |e verfasserin |4 aut | |
| 700 | 0 | |a Wei Zhu |e verfasserin |4 aut | |
| 700 | 0 | |a The MAP Follow-Up Collaboration |e verfasserin |4 aut | |
| 700 | 0 | |a V. Bozza |e verfasserin |4 aut | |
| 700 | 0 | |a Arnaud Cassan |e verfasserin |4 aut | |
| 700 | 0 | |a Martin Dominik |e verfasserin |4 aut | |
| 700 | 0 | |a Markus Hundertmark |e verfasserin |4 aut | |
| 700 | 0 | |a R. Figuera Jaimes |e verfasserin |4 aut | |
| 700 | 0 | |a K. Kruszyńska |e verfasserin |4 aut | |
| 700 | 0 | |a K. A. Rybicki |e verfasserin |4 aut | |
| 700 | 0 | |a R. A. Street |e verfasserin |4 aut | |
| 700 | 0 | |a Y. Tsapras |e verfasserin |4 aut | |
| 700 | 0 | |a Joachim Wambsganss |e verfasserin |4 aut | |
| 700 | 0 | |a Ł. Wyrzykowski |e verfasserin |4 aut | |
| 700 | 0 | |a P. Zieliński |e verfasserin |4 aut | |
| 700 | 0 | |a The OMEGA Collaboration |e verfasserin |4 aut | |
| 700 | 0 | |a Gioia Rau |e verfasserin |4 aut | |
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10.3847/1538-3881/acbcc8 doi (DE-627)DOAJ089160592 (DE-599)DOAJ7071297452874f4699f42ea1eb0bd198 DE-627 ger DE-627 rakwb eng QB1-991 Greg Olmschenk verfasserin aut MOA-2020-BLG-208Lb: Cool Sub-Saturn-mass Planet within Predicted Desert 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We analyze the MOA-2020-BLG-208 gravitational microlensing event and present the discovery and characterization of a new planet, MOA-2020-BLG-208Lb, with an estimated sub-Saturn mass. With a mass ratio $q={3.17}_{-0.26}^{+0.28}\times {10}^{-4}$ , the planet lies near the peak of the mass-ratio function derived by the MOA collaboration and near the edge of expected sample sensitivity. For these estimates we provide results using two mass-law priors: one assuming that all stars have an equal planet-hosting probability, and the other assuming that planets are more likely to orbit around more massive stars. In the first scenario, we estimate that the lens system is likely to be a planet of mass ${m}_{\mathrm{planet}}={46}_{-24}^{+42}\,{M}_{\oplus }$ and a host star of mass ${M}_{\mathrm{host}}={0.43}_{-0.23}^{+0.39}\,{M}_{\odot }$ , located at a distance ${D}_{L}={7.49}_{-1.13}^{+0.99}\,\mathrm{kpc}$ . For the second scenario, we estimate ${m}_{\mathrm{planet}}={69}_{-34}^{+37}\,{M}_{\oplus }$ , ${M}_{\mathrm{host}}={0.66}_{-0.32}^{+0.35}\,{M}_{\odot }$ , and ${D}_{L}={7.81}_{-0.93}^{+0.93}\,\mathrm{kpc}$ . The planet has a projected separation as a fraction of the Einstein ring radius $s={1.3807}_{-0.0018}^{+0.0018}$ . As a cool sub-Saturn-mass planet, this planet adds to a growing collection of evidence for revised planetary formation models. Gravitational microlensing Gravitational microlensing exoplanet detection Binary lens microlensing Astronomy David P. Bennett verfasserin aut Ian A. Bond verfasserin aut Weicheng Zang verfasserin aut Youn Kil Jung verfasserin aut Jennifer C. Yee verfasserin aut Etienne Bachelet verfasserin aut Leading authors verfasserin aut Fumio Abe verfasserin aut Richard K. Barry verfasserin aut Aparna Bhattacharya verfasserin aut Hirosane Fujii verfasserin aut Akihiko Fukui verfasserin aut Yuki Hirao verfasserin aut Stela Ishitani Silva verfasserin aut Yoshitaka Itow verfasserin aut Rintaro Kirikawa verfasserin aut Iona Kondo verfasserin aut Naoki Koshimoto verfasserin aut Yutaka Matsubara verfasserin aut Sho Matsumoto verfasserin aut Shota Miyazaki verfasserin aut Brandon Munford verfasserin aut Yasushi Muraki verfasserin aut Arisa Okamura verfasserin aut Clément Ranc verfasserin aut Nicholas J. Rattenbury verfasserin aut Yuki Satoh verfasserin aut Takahiro Sumi verfasserin aut Daisuke Suzuki verfasserin aut Taiga Toda verfasserin aut Paul J. Tristram verfasserin aut Aikaterini Vandorou verfasserin aut Hibiki Yama verfasserin aut The MOA Collaboration verfasserin aut Michael D. Albrow verfasserin aut Sang-Mok Cha verfasserin aut Sun-Ju Chung verfasserin aut Andrew Gould verfasserin aut Cheongho Han verfasserin aut Kyu-Ha Hwang verfasserin aut Dong-Jin Kim verfasserin aut Hyoun-Woo Kim verfasserin aut Seung-Lee Kim verfasserin aut Chung-Uk Lee verfasserin aut Dong-Joo Lee verfasserin aut Yongseok Lee verfasserin aut Byeong-Gon Park verfasserin aut Richard W. Pogge verfasserin aut Yoon-Hyun Ryu verfasserin aut In-Gu Shin verfasserin aut Yossi Shvartzvald verfasserin aut The KMTNet Collaboration verfasserin aut Grant Christie verfasserin aut Tony Cooper verfasserin aut John Drummond verfasserin aut Jonathan Green verfasserin aut Steve Hennerley verfasserin aut Jennie McCormick verfasserin aut L. A. G. Monard verfasserin aut Tim Natusch verfasserin aut Ian Porritt verfasserin aut Thiam-Guan Tan verfasserin aut The MicroFUN Collaboration verfasserin aut Shude Mao verfasserin aut Dan Maoz verfasserin aut Matthew T. Penny verfasserin aut Wei Zhu verfasserin aut The MAP Follow-Up Collaboration verfasserin aut V. Bozza verfasserin aut Arnaud Cassan verfasserin aut Martin Dominik verfasserin aut Markus Hundertmark verfasserin aut R. Figuera Jaimes verfasserin aut K. Kruszyńska verfasserin aut K. A. Rybicki verfasserin aut R. A. Street verfasserin aut Y. Tsapras verfasserin aut Joachim Wambsganss verfasserin aut Ł. Wyrzykowski verfasserin aut P. Zieliński verfasserin aut The OMEGA Collaboration verfasserin aut Gioia Rau verfasserin aut In The Astronomical Journal IOP Publishing, 2022 165(2023), 4, p 175 (DE-627)312175647 (DE-600)2003104-X 15383881 nnns volume:165 year:2023 number:4, p 175 https://doi.org/10.3847/1538-3881/acbcc8 kostenfrei https://doaj.org/article/7071297452874f4699f42ea1eb0bd198 kostenfrei https://doi.org/10.3847/1538-3881/acbcc8 kostenfrei https://doaj.org/toc/1538-3881 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2006 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2110 GBV_ILN_2129 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 165 2023 4, p 175 |
| spelling |
10.3847/1538-3881/acbcc8 doi (DE-627)DOAJ089160592 (DE-599)DOAJ7071297452874f4699f42ea1eb0bd198 DE-627 ger DE-627 rakwb eng QB1-991 Greg Olmschenk verfasserin aut MOA-2020-BLG-208Lb: Cool Sub-Saturn-mass Planet within Predicted Desert 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We analyze the MOA-2020-BLG-208 gravitational microlensing event and present the discovery and characterization of a new planet, MOA-2020-BLG-208Lb, with an estimated sub-Saturn mass. With a mass ratio $q={3.17}_{-0.26}^{+0.28}\times {10}^{-4}$ , the planet lies near the peak of the mass-ratio function derived by the MOA collaboration and near the edge of expected sample sensitivity. For these estimates we provide results using two mass-law priors: one assuming that all stars have an equal planet-hosting probability, and the other assuming that planets are more likely to orbit around more massive stars. In the first scenario, we estimate that the lens system is likely to be a planet of mass ${m}_{\mathrm{planet}}={46}_{-24}^{+42}\,{M}_{\oplus }$ and a host star of mass ${M}_{\mathrm{host}}={0.43}_{-0.23}^{+0.39}\,{M}_{\odot }$ , located at a distance ${D}_{L}={7.49}_{-1.13}^{+0.99}\,\mathrm{kpc}$ . For the second scenario, we estimate ${m}_{\mathrm{planet}}={69}_{-34}^{+37}\,{M}_{\oplus }$ , ${M}_{\mathrm{host}}={0.66}_{-0.32}^{+0.35}\,{M}_{\odot }$ , and ${D}_{L}={7.81}_{-0.93}^{+0.93}\,\mathrm{kpc}$ . The planet has a projected separation as a fraction of the Einstein ring radius $s={1.3807}_{-0.0018}^{+0.0018}$ . As a cool sub-Saturn-mass planet, this planet adds to a growing collection of evidence for revised planetary formation models. Gravitational microlensing Gravitational microlensing exoplanet detection Binary lens microlensing Astronomy David P. Bennett verfasserin aut Ian A. Bond verfasserin aut Weicheng Zang verfasserin aut Youn Kil Jung verfasserin aut Jennifer C. Yee verfasserin aut Etienne Bachelet verfasserin aut Leading authors verfasserin aut Fumio Abe verfasserin aut Richard K. Barry verfasserin aut Aparna Bhattacharya verfasserin aut Hirosane Fujii verfasserin aut Akihiko Fukui verfasserin aut Yuki Hirao verfasserin aut Stela Ishitani Silva verfasserin aut Yoshitaka Itow verfasserin aut Rintaro Kirikawa verfasserin aut Iona Kondo verfasserin aut Naoki Koshimoto verfasserin aut Yutaka Matsubara verfasserin aut Sho Matsumoto verfasserin aut Shota Miyazaki verfasserin aut Brandon Munford verfasserin aut Yasushi Muraki verfasserin aut Arisa Okamura verfasserin aut Clément Ranc verfasserin aut Nicholas J. Rattenbury verfasserin aut Yuki Satoh verfasserin aut Takahiro Sumi verfasserin aut Daisuke Suzuki verfasserin aut Taiga Toda verfasserin aut Paul J. Tristram verfasserin aut Aikaterini Vandorou verfasserin aut Hibiki Yama verfasserin aut The MOA Collaboration verfasserin aut Michael D. Albrow verfasserin aut Sang-Mok Cha verfasserin aut Sun-Ju Chung verfasserin aut Andrew Gould verfasserin aut Cheongho Han verfasserin aut Kyu-Ha Hwang verfasserin aut Dong-Jin Kim verfasserin aut Hyoun-Woo Kim verfasserin aut Seung-Lee Kim verfasserin aut Chung-Uk Lee verfasserin aut Dong-Joo Lee verfasserin aut Yongseok Lee verfasserin aut Byeong-Gon Park verfasserin aut Richard W. Pogge verfasserin aut Yoon-Hyun Ryu verfasserin aut In-Gu Shin verfasserin aut Yossi Shvartzvald verfasserin aut The KMTNet Collaboration verfasserin aut Grant Christie verfasserin aut Tony Cooper verfasserin aut John Drummond verfasserin aut Jonathan Green verfasserin aut Steve Hennerley verfasserin aut Jennie McCormick verfasserin aut L. A. G. Monard verfasserin aut Tim Natusch verfasserin aut Ian Porritt verfasserin aut Thiam-Guan Tan verfasserin aut The MicroFUN Collaboration verfasserin aut Shude Mao verfasserin aut Dan Maoz verfasserin aut Matthew T. Penny verfasserin aut Wei Zhu verfasserin aut The MAP Follow-Up Collaboration verfasserin aut V. Bozza verfasserin aut Arnaud Cassan verfasserin aut Martin Dominik verfasserin aut Markus Hundertmark verfasserin aut R. Figuera Jaimes verfasserin aut K. Kruszyńska verfasserin aut K. A. Rybicki verfasserin aut R. A. Street verfasserin aut Y. Tsapras verfasserin aut Joachim Wambsganss verfasserin aut Ł. Wyrzykowski verfasserin aut P. Zieliński verfasserin aut The OMEGA Collaboration verfasserin aut Gioia Rau verfasserin aut In The Astronomical Journal IOP Publishing, 2022 165(2023), 4, p 175 (DE-627)312175647 (DE-600)2003104-X 15383881 nnns volume:165 year:2023 number:4, p 175 https://doi.org/10.3847/1538-3881/acbcc8 kostenfrei https://doaj.org/article/7071297452874f4699f42ea1eb0bd198 kostenfrei https://doi.org/10.3847/1538-3881/acbcc8 kostenfrei https://doaj.org/toc/1538-3881 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2006 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2110 GBV_ILN_2129 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 165 2023 4, p 175 |
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10.3847/1538-3881/acbcc8 doi (DE-627)DOAJ089160592 (DE-599)DOAJ7071297452874f4699f42ea1eb0bd198 DE-627 ger DE-627 rakwb eng QB1-991 Greg Olmschenk verfasserin aut MOA-2020-BLG-208Lb: Cool Sub-Saturn-mass Planet within Predicted Desert 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We analyze the MOA-2020-BLG-208 gravitational microlensing event and present the discovery and characterization of a new planet, MOA-2020-BLG-208Lb, with an estimated sub-Saturn mass. With a mass ratio $q={3.17}_{-0.26}^{+0.28}\times {10}^{-4}$ , the planet lies near the peak of the mass-ratio function derived by the MOA collaboration and near the edge of expected sample sensitivity. For these estimates we provide results using two mass-law priors: one assuming that all stars have an equal planet-hosting probability, and the other assuming that planets are more likely to orbit around more massive stars. In the first scenario, we estimate that the lens system is likely to be a planet of mass ${m}_{\mathrm{planet}}={46}_{-24}^{+42}\,{M}_{\oplus }$ and a host star of mass ${M}_{\mathrm{host}}={0.43}_{-0.23}^{+0.39}\,{M}_{\odot }$ , located at a distance ${D}_{L}={7.49}_{-1.13}^{+0.99}\,\mathrm{kpc}$ . For the second scenario, we estimate ${m}_{\mathrm{planet}}={69}_{-34}^{+37}\,{M}_{\oplus }$ , ${M}_{\mathrm{host}}={0.66}_{-0.32}^{+0.35}\,{M}_{\odot }$ , and ${D}_{L}={7.81}_{-0.93}^{+0.93}\,\mathrm{kpc}$ . The planet has a projected separation as a fraction of the Einstein ring radius $s={1.3807}_{-0.0018}^{+0.0018}$ . As a cool sub-Saturn-mass planet, this planet adds to a growing collection of evidence for revised planetary formation models. Gravitational microlensing Gravitational microlensing exoplanet detection Binary lens microlensing Astronomy David P. Bennett verfasserin aut Ian A. Bond verfasserin aut Weicheng Zang verfasserin aut Youn Kil Jung verfasserin aut Jennifer C. Yee verfasserin aut Etienne Bachelet verfasserin aut Leading authors verfasserin aut Fumio Abe verfasserin aut Richard K. Barry verfasserin aut Aparna Bhattacharya verfasserin aut Hirosane Fujii verfasserin aut Akihiko Fukui verfasserin aut Yuki Hirao verfasserin aut Stela Ishitani Silva verfasserin aut Yoshitaka Itow verfasserin aut Rintaro Kirikawa verfasserin aut Iona Kondo verfasserin aut Naoki Koshimoto verfasserin aut Yutaka Matsubara verfasserin aut Sho Matsumoto verfasserin aut Shota Miyazaki verfasserin aut Brandon Munford verfasserin aut Yasushi Muraki verfasserin aut Arisa Okamura verfasserin aut Clément Ranc verfasserin aut Nicholas J. Rattenbury verfasserin aut Yuki Satoh verfasserin aut Takahiro Sumi verfasserin aut Daisuke Suzuki verfasserin aut Taiga Toda verfasserin aut Paul J. Tristram verfasserin aut Aikaterini Vandorou verfasserin aut Hibiki Yama verfasserin aut The MOA Collaboration verfasserin aut Michael D. Albrow verfasserin aut Sang-Mok Cha verfasserin aut Sun-Ju Chung verfasserin aut Andrew Gould verfasserin aut Cheongho Han verfasserin aut Kyu-Ha Hwang verfasserin aut Dong-Jin Kim verfasserin aut Hyoun-Woo Kim verfasserin aut Seung-Lee Kim verfasserin aut Chung-Uk Lee verfasserin aut Dong-Joo Lee verfasserin aut Yongseok Lee verfasserin aut Byeong-Gon Park verfasserin aut Richard W. Pogge verfasserin aut Yoon-Hyun Ryu verfasserin aut In-Gu Shin verfasserin aut Yossi Shvartzvald verfasserin aut The KMTNet Collaboration verfasserin aut Grant Christie verfasserin aut Tony Cooper verfasserin aut John Drummond verfasserin aut Jonathan Green verfasserin aut Steve Hennerley verfasserin aut Jennie McCormick verfasserin aut L. A. G. Monard verfasserin aut Tim Natusch verfasserin aut Ian Porritt verfasserin aut Thiam-Guan Tan verfasserin aut The MicroFUN Collaboration verfasserin aut Shude Mao verfasserin aut Dan Maoz verfasserin aut Matthew T. Penny verfasserin aut Wei Zhu verfasserin aut The MAP Follow-Up Collaboration verfasserin aut V. Bozza verfasserin aut Arnaud Cassan verfasserin aut Martin Dominik verfasserin aut Markus Hundertmark verfasserin aut R. Figuera Jaimes verfasserin aut K. Kruszyńska verfasserin aut K. A. Rybicki verfasserin aut R. A. Street verfasserin aut Y. Tsapras verfasserin aut Joachim Wambsganss verfasserin aut Ł. Wyrzykowski verfasserin aut P. Zieliński verfasserin aut The OMEGA Collaboration verfasserin aut Gioia Rau verfasserin aut In The Astronomical Journal IOP Publishing, 2022 165(2023), 4, p 175 (DE-627)312175647 (DE-600)2003104-X 15383881 nnns volume:165 year:2023 number:4, p 175 https://doi.org/10.3847/1538-3881/acbcc8 kostenfrei https://doaj.org/article/7071297452874f4699f42ea1eb0bd198 kostenfrei https://doi.org/10.3847/1538-3881/acbcc8 kostenfrei https://doaj.org/toc/1538-3881 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2006 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2110 GBV_ILN_2129 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 165 2023 4, p 175 |
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10.3847/1538-3881/acbcc8 doi (DE-627)DOAJ089160592 (DE-599)DOAJ7071297452874f4699f42ea1eb0bd198 DE-627 ger DE-627 rakwb eng QB1-991 Greg Olmschenk verfasserin aut MOA-2020-BLG-208Lb: Cool Sub-Saturn-mass Planet within Predicted Desert 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We analyze the MOA-2020-BLG-208 gravitational microlensing event and present the discovery and characterization of a new planet, MOA-2020-BLG-208Lb, with an estimated sub-Saturn mass. With a mass ratio $q={3.17}_{-0.26}^{+0.28}\times {10}^{-4}$ , the planet lies near the peak of the mass-ratio function derived by the MOA collaboration and near the edge of expected sample sensitivity. For these estimates we provide results using two mass-law priors: one assuming that all stars have an equal planet-hosting probability, and the other assuming that planets are more likely to orbit around more massive stars. In the first scenario, we estimate that the lens system is likely to be a planet of mass ${m}_{\mathrm{planet}}={46}_{-24}^{+42}\,{M}_{\oplus }$ and a host star of mass ${M}_{\mathrm{host}}={0.43}_{-0.23}^{+0.39}\,{M}_{\odot }$ , located at a distance ${D}_{L}={7.49}_{-1.13}^{+0.99}\,\mathrm{kpc}$ . For the second scenario, we estimate ${m}_{\mathrm{planet}}={69}_{-34}^{+37}\,{M}_{\oplus }$ , ${M}_{\mathrm{host}}={0.66}_{-0.32}^{+0.35}\,{M}_{\odot }$ , and ${D}_{L}={7.81}_{-0.93}^{+0.93}\,\mathrm{kpc}$ . The planet has a projected separation as a fraction of the Einstein ring radius $s={1.3807}_{-0.0018}^{+0.0018}$ . As a cool sub-Saturn-mass planet, this planet adds to a growing collection of evidence for revised planetary formation models. Gravitational microlensing Gravitational microlensing exoplanet detection Binary lens microlensing Astronomy David P. Bennett verfasserin aut Ian A. Bond verfasserin aut Weicheng Zang verfasserin aut Youn Kil Jung verfasserin aut Jennifer C. Yee verfasserin aut Etienne Bachelet verfasserin aut Leading authors verfasserin aut Fumio Abe verfasserin aut Richard K. Barry verfasserin aut Aparna Bhattacharya verfasserin aut Hirosane Fujii verfasserin aut Akihiko Fukui verfasserin aut Yuki Hirao verfasserin aut Stela Ishitani Silva verfasserin aut Yoshitaka Itow verfasserin aut Rintaro Kirikawa verfasserin aut Iona Kondo verfasserin aut Naoki Koshimoto verfasserin aut Yutaka Matsubara verfasserin aut Sho Matsumoto verfasserin aut Shota Miyazaki verfasserin aut Brandon Munford verfasserin aut Yasushi Muraki verfasserin aut Arisa Okamura verfasserin aut Clément Ranc verfasserin aut Nicholas J. Rattenbury verfasserin aut Yuki Satoh verfasserin aut Takahiro Sumi verfasserin aut Daisuke Suzuki verfasserin aut Taiga Toda verfasserin aut Paul J. Tristram verfasserin aut Aikaterini Vandorou verfasserin aut Hibiki Yama verfasserin aut The MOA Collaboration verfasserin aut Michael D. Albrow verfasserin aut Sang-Mok Cha verfasserin aut Sun-Ju Chung verfasserin aut Andrew Gould verfasserin aut Cheongho Han verfasserin aut Kyu-Ha Hwang verfasserin aut Dong-Jin Kim verfasserin aut Hyoun-Woo Kim verfasserin aut Seung-Lee Kim verfasserin aut Chung-Uk Lee verfasserin aut Dong-Joo Lee verfasserin aut Yongseok Lee verfasserin aut Byeong-Gon Park verfasserin aut Richard W. Pogge verfasserin aut Yoon-Hyun Ryu verfasserin aut In-Gu Shin verfasserin aut Yossi Shvartzvald verfasserin aut The KMTNet Collaboration verfasserin aut Grant Christie verfasserin aut Tony Cooper verfasserin aut John Drummond verfasserin aut Jonathan Green verfasserin aut Steve Hennerley verfasserin aut Jennie McCormick verfasserin aut L. A. G. Monard verfasserin aut Tim Natusch verfasserin aut Ian Porritt verfasserin aut Thiam-Guan Tan verfasserin aut The MicroFUN Collaboration verfasserin aut Shude Mao verfasserin aut Dan Maoz verfasserin aut Matthew T. Penny verfasserin aut Wei Zhu verfasserin aut The MAP Follow-Up Collaboration verfasserin aut V. Bozza verfasserin aut Arnaud Cassan verfasserin aut Martin Dominik verfasserin aut Markus Hundertmark verfasserin aut R. Figuera Jaimes verfasserin aut K. Kruszyńska verfasserin aut K. A. Rybicki verfasserin aut R. A. Street verfasserin aut Y. Tsapras verfasserin aut Joachim Wambsganss verfasserin aut Ł. Wyrzykowski verfasserin aut P. Zieliński verfasserin aut The OMEGA Collaboration verfasserin aut Gioia Rau verfasserin aut In The Astronomical Journal IOP Publishing, 2022 165(2023), 4, p 175 (DE-627)312175647 (DE-600)2003104-X 15383881 nnns volume:165 year:2023 number:4, p 175 https://doi.org/10.3847/1538-3881/acbcc8 kostenfrei https://doaj.org/article/7071297452874f4699f42ea1eb0bd198 kostenfrei https://doi.org/10.3847/1538-3881/acbcc8 kostenfrei https://doaj.org/toc/1538-3881 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2006 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2110 GBV_ILN_2129 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 165 2023 4, p 175 |
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10.3847/1538-3881/acbcc8 doi (DE-627)DOAJ089160592 (DE-599)DOAJ7071297452874f4699f42ea1eb0bd198 DE-627 ger DE-627 rakwb eng QB1-991 Greg Olmschenk verfasserin aut MOA-2020-BLG-208Lb: Cool Sub-Saturn-mass Planet within Predicted Desert 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We analyze the MOA-2020-BLG-208 gravitational microlensing event and present the discovery and characterization of a new planet, MOA-2020-BLG-208Lb, with an estimated sub-Saturn mass. With a mass ratio $q={3.17}_{-0.26}^{+0.28}\times {10}^{-4}$ , the planet lies near the peak of the mass-ratio function derived by the MOA collaboration and near the edge of expected sample sensitivity. For these estimates we provide results using two mass-law priors: one assuming that all stars have an equal planet-hosting probability, and the other assuming that planets are more likely to orbit around more massive stars. In the first scenario, we estimate that the lens system is likely to be a planet of mass ${m}_{\mathrm{planet}}={46}_{-24}^{+42}\,{M}_{\oplus }$ and a host star of mass ${M}_{\mathrm{host}}={0.43}_{-0.23}^{+0.39}\,{M}_{\odot }$ , located at a distance ${D}_{L}={7.49}_{-1.13}^{+0.99}\,\mathrm{kpc}$ . For the second scenario, we estimate ${m}_{\mathrm{planet}}={69}_{-34}^{+37}\,{M}_{\oplus }$ , ${M}_{\mathrm{host}}={0.66}_{-0.32}^{+0.35}\,{M}_{\odot }$ , and ${D}_{L}={7.81}_{-0.93}^{+0.93}\,\mathrm{kpc}$ . The planet has a projected separation as a fraction of the Einstein ring radius $s={1.3807}_{-0.0018}^{+0.0018}$ . As a cool sub-Saturn-mass planet, this planet adds to a growing collection of evidence for revised planetary formation models. Gravitational microlensing Gravitational microlensing exoplanet detection Binary lens microlensing Astronomy David P. Bennett verfasserin aut Ian A. Bond verfasserin aut Weicheng Zang verfasserin aut Youn Kil Jung verfasserin aut Jennifer C. Yee verfasserin aut Etienne Bachelet verfasserin aut Leading authors verfasserin aut Fumio Abe verfasserin aut Richard K. Barry verfasserin aut Aparna Bhattacharya verfasserin aut Hirosane Fujii verfasserin aut Akihiko Fukui verfasserin aut Yuki Hirao verfasserin aut Stela Ishitani Silva verfasserin aut Yoshitaka Itow verfasserin aut Rintaro Kirikawa verfasserin aut Iona Kondo verfasserin aut Naoki Koshimoto verfasserin aut Yutaka Matsubara verfasserin aut Sho Matsumoto verfasserin aut Shota Miyazaki verfasserin aut Brandon Munford verfasserin aut Yasushi Muraki verfasserin aut Arisa Okamura verfasserin aut Clément Ranc verfasserin aut Nicholas J. Rattenbury verfasserin aut Yuki Satoh verfasserin aut Takahiro Sumi verfasserin aut Daisuke Suzuki verfasserin aut Taiga Toda verfasserin aut Paul J. Tristram verfasserin aut Aikaterini Vandorou verfasserin aut Hibiki Yama verfasserin aut The MOA Collaboration verfasserin aut Michael D. Albrow verfasserin aut Sang-Mok Cha verfasserin aut Sun-Ju Chung verfasserin aut Andrew Gould verfasserin aut Cheongho Han verfasserin aut Kyu-Ha Hwang verfasserin aut Dong-Jin Kim verfasserin aut Hyoun-Woo Kim verfasserin aut Seung-Lee Kim verfasserin aut Chung-Uk Lee verfasserin aut Dong-Joo Lee verfasserin aut Yongseok Lee verfasserin aut Byeong-Gon Park verfasserin aut Richard W. Pogge verfasserin aut Yoon-Hyun Ryu verfasserin aut In-Gu Shin verfasserin aut Yossi Shvartzvald verfasserin aut The KMTNet Collaboration verfasserin aut Grant Christie verfasserin aut Tony Cooper verfasserin aut John Drummond verfasserin aut Jonathan Green verfasserin aut Steve Hennerley verfasserin aut Jennie McCormick verfasserin aut L. A. G. Monard verfasserin aut Tim Natusch verfasserin aut Ian Porritt verfasserin aut Thiam-Guan Tan verfasserin aut The MicroFUN Collaboration verfasserin aut Shude Mao verfasserin aut Dan Maoz verfasserin aut Matthew T. Penny verfasserin aut Wei Zhu verfasserin aut The MAP Follow-Up Collaboration verfasserin aut V. Bozza verfasserin aut Arnaud Cassan verfasserin aut Martin Dominik verfasserin aut Markus Hundertmark verfasserin aut R. Figuera Jaimes verfasserin aut K. Kruszyńska verfasserin aut K. A. Rybicki verfasserin aut R. A. Street verfasserin aut Y. Tsapras verfasserin aut Joachim Wambsganss verfasserin aut Ł. Wyrzykowski verfasserin aut P. Zieliński verfasserin aut The OMEGA Collaboration verfasserin aut Gioia Rau verfasserin aut In The Astronomical Journal IOP Publishing, 2022 165(2023), 4, p 175 (DE-627)312175647 (DE-600)2003104-X 15383881 nnns volume:165 year:2023 number:4, p 175 https://doi.org/10.3847/1538-3881/acbcc8 kostenfrei https://doaj.org/article/7071297452874f4699f42ea1eb0bd198 kostenfrei https://doi.org/10.3847/1538-3881/acbcc8 kostenfrei https://doaj.org/toc/1538-3881 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2006 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2110 GBV_ILN_2129 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 165 2023 4, p 175 |
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The Astronomical Journal |
| authorswithroles_txt_mv |
Greg Olmschenk @@aut@@ David P. Bennett @@aut@@ Ian A. Bond @@aut@@ Weicheng Zang @@aut@@ Youn Kil Jung @@aut@@ Jennifer C. Yee @@aut@@ Etienne Bachelet @@aut@@ Leading authors @@aut@@ Fumio Abe @@aut@@ Richard K. Barry @@aut@@ Aparna Bhattacharya @@aut@@ Hirosane Fujii @@aut@@ Akihiko Fukui @@aut@@ Yuki Hirao @@aut@@ Stela Ishitani Silva @@aut@@ Yoshitaka Itow @@aut@@ Rintaro Kirikawa @@aut@@ Iona Kondo @@aut@@ Naoki Koshimoto @@aut@@ Yutaka Matsubara @@aut@@ Sho Matsumoto @@aut@@ Shota Miyazaki @@aut@@ Brandon Munford @@aut@@ Yasushi Muraki @@aut@@ Arisa Okamura @@aut@@ Clément Ranc @@aut@@ Nicholas J. Rattenbury @@aut@@ Yuki Satoh @@aut@@ Takahiro Sumi @@aut@@ Daisuke Suzuki @@aut@@ Taiga Toda @@aut@@ Paul J. Tristram @@aut@@ Aikaterini Vandorou @@aut@@ Hibiki Yama @@aut@@ The MOA Collaboration @@aut@@ Michael D. Albrow @@aut@@ Sang-Mok Cha @@aut@@ Sun-Ju Chung @@aut@@ Andrew Gould @@aut@@ Cheongho Han @@aut@@ Kyu-Ha Hwang @@aut@@ Dong-Jin Kim @@aut@@ Hyoun-Woo Kim @@aut@@ Seung-Lee Kim @@aut@@ Chung-Uk Lee @@aut@@ Dong-Joo Lee @@aut@@ Yongseok Lee @@aut@@ Byeong-Gon Park @@aut@@ Richard W. Pogge @@aut@@ Yoon-Hyun Ryu @@aut@@ In-Gu Shin @@aut@@ Yossi Shvartzvald @@aut@@ The KMTNet Collaboration @@aut@@ Grant Christie @@aut@@ Tony Cooper @@aut@@ John Drummond @@aut@@ Jonathan Green @@aut@@ Steve Hennerley @@aut@@ Jennie McCormick @@aut@@ L. A. G. Monard @@aut@@ Tim Natusch @@aut@@ Ian Porritt @@aut@@ Thiam-Guan Tan @@aut@@ The MicroFUN Collaboration @@aut@@ Shude Mao @@aut@@ Dan Maoz @@aut@@ Matthew T. Penny @@aut@@ Wei Zhu @@aut@@ The MAP Follow-Up Collaboration @@aut@@ V. Bozza @@aut@@ Arnaud Cassan @@aut@@ Martin Dominik @@aut@@ Markus Hundertmark @@aut@@ R. Figuera Jaimes @@aut@@ K. Kruszyńska @@aut@@ K. A. Rybicki @@aut@@ R. A. Street @@aut@@ Y. Tsapras @@aut@@ Joachim Wambsganss @@aut@@ Ł. Wyrzykowski @@aut@@ P. Zieliński @@aut@@ The OMEGA Collaboration @@aut@@ Gioia Rau @@aut@@ |
| publishDateDaySort_date |
2023-01-01T00:00:00Z |
| hierarchy_top_id |
312175647 |
| id |
DOAJ089160592 |
| language_de |
englisch |
| fullrecord |
<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000naa a22002652 4500</leader><controlfield tag="001">DOAJ089160592</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20230505015850.0</controlfield><controlfield tag="007">cr uuu---uuuuu</controlfield><controlfield tag="008">230505s2023 xx |||||o 00| ||eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.3847/1538-3881/acbcc8</subfield><subfield code="2">doi</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)DOAJ089160592</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-599)DOAJ7071297452874f4699f42ea1eb0bd198</subfield></datafield><datafield tag="040" ind1=" " ind2=" "><subfield code="a">DE-627</subfield><subfield code="b">ger</subfield><subfield code="c">DE-627</subfield><subfield code="e">rakwb</subfield></datafield><datafield tag="041" ind1=" " ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="050" ind1=" " ind2="0"><subfield code="a">QB1-991</subfield></datafield><datafield tag="100" ind1="0" ind2=" "><subfield code="a">Greg Olmschenk</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">MOA-2020-BLG-208Lb: Cool Sub-Saturn-mass Planet within Predicted Desert</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2023</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">Text</subfield><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">Computermedien</subfield><subfield code="b">c</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Online-Ressource</subfield><subfield code="b">cr</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">We analyze the MOA-2020-BLG-208 gravitational microlensing event and present the discovery and characterization of a new planet, MOA-2020-BLG-208Lb, with an estimated sub-Saturn mass. With a mass ratio $q={3.17}_{-0.26}^{+0.28}\times {10}^{-4}$ , the planet lies near the peak of the mass-ratio function derived by the MOA collaboration and near the edge of expected sample sensitivity. For these estimates we provide results using two mass-law priors: one assuming that all stars have an equal planet-hosting probability, and the other assuming that planets are more likely to orbit around more massive stars. In the first scenario, we estimate that the lens system is likely to be a planet of mass ${m}_{\mathrm{planet}}={46}_{-24}^{+42}\,{M}_{\oplus }$ and a host star of mass ${M}_{\mathrm{host}}={0.43}_{-0.23}^{+0.39}\,{M}_{\odot }$ , located at a distance ${D}_{L}={7.49}_{-1.13}^{+0.99}\,\mathrm{kpc}$ . For the second scenario, we estimate ${m}_{\mathrm{planet}}={69}_{-34}^{+37}\,{M}_{\oplus }$ , ${M}_{\mathrm{host}}={0.66}_{-0.32}^{+0.35}\,{M}_{\odot }$ , and ${D}_{L}={7.81}_{-0.93}^{+0.93}\,\mathrm{kpc}$ . The planet has a projected separation as a fraction of the Einstein ring radius $s={1.3807}_{-0.0018}^{+0.0018}$ . As a cool sub-Saturn-mass planet, this planet adds to a growing collection of evidence for revised planetary formation models.</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Gravitational microlensing</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Gravitational microlensing exoplanet detection</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Binary lens microlensing</subfield></datafield><datafield tag="653" ind1=" " ind2="0"><subfield code="a">Astronomy</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">David P. Bennett</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Ian A. Bond</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Weicheng Zang</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Youn Kil Jung</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Jennifer C. 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Rattenbury</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Yuki Satoh</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Takahiro Sumi</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Daisuke Suzuki</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Taiga Toda</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Paul J. Tristram</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Aikaterini Vandorou</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Hibiki Yama</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">The MOA Collaboration</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Michael D. Albrow</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Sang-Mok Cha</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Sun-Ju Chung</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Andrew Gould</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Cheongho Han</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Kyu-Ha Hwang</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Dong-Jin Kim</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Hyoun-Woo Kim</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Seung-Lee Kim</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Chung-Uk Lee</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Dong-Joo Lee</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Yongseok Lee</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Byeong-Gon Park</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Richard W. 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Greg Olmschenk David P. Bennett Ian A. Bond Weicheng Zang Youn Kil Jung Jennifer C. Yee Etienne Bachelet Leading authors Fumio Abe Richard K. Barry Aparna Bhattacharya Hirosane Fujii Akihiko Fukui Yuki Hirao Stela Ishitani Silva Yoshitaka Itow Rintaro Kirikawa Iona Kondo Naoki Koshimoto Yutaka Matsubara Sho Matsumoto Shota Miyazaki Brandon Munford Yasushi Muraki Arisa Okamura Clément Ranc Nicholas J. Rattenbury Yuki Satoh Takahiro Sumi Daisuke Suzuki Taiga Toda Paul J. Tristram Aikaterini Vandorou Hibiki Yama The MOA Collaboration Michael D. Albrow Sang-Mok Cha Sun-Ju Chung Andrew Gould Cheongho Han Kyu-Ha Hwang Dong-Jin Kim Hyoun-Woo Kim Seung-Lee Kim Chung-Uk Lee Dong-Joo Lee Yongseok Lee Byeong-Gon Park Richard W. Pogge Yoon-Hyun Ryu In-Gu Shin Yossi Shvartzvald The KMTNet Collaboration Grant Christie Tony Cooper John Drummond Jonathan Green Steve Hennerley Jennie McCormick L. A. G. Monard Tim Natusch Ian Porritt Thiam-Guan Tan The MicroFUN Collaboration Shude Mao Dan Maoz Matthew T. Penny Wei Zhu The MAP Follow-Up Collaboration V. Bozza Arnaud Cassan Martin Dominik Markus Hundertmark R. Figuera Jaimes K. Kruszyńska K. A. Rybicki R. A. Street Y. Tsapras Joachim Wambsganss Ł. Wyrzykowski P. Zieliński The OMEGA Collaboration Gioia Rau |
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moa-2020-blg-208lb: cool sub-saturn-mass planet within predicted desert |
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MOA-2020-BLG-208Lb: Cool Sub-Saturn-mass Planet within Predicted Desert |
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We analyze the MOA-2020-BLG-208 gravitational microlensing event and present the discovery and characterization of a new planet, MOA-2020-BLG-208Lb, with an estimated sub-Saturn mass. With a mass ratio $q={3.17}_{-0.26}^{+0.28}\times {10}^{-4}$ , the planet lies near the peak of the mass-ratio function derived by the MOA collaboration and near the edge of expected sample sensitivity. For these estimates we provide results using two mass-law priors: one assuming that all stars have an equal planet-hosting probability, and the other assuming that planets are more likely to orbit around more massive stars. In the first scenario, we estimate that the lens system is likely to be a planet of mass ${m}_{\mathrm{planet}}={46}_{-24}^{+42}\,{M}_{\oplus }$ and a host star of mass ${M}_{\mathrm{host}}={0.43}_{-0.23}^{+0.39}\,{M}_{\odot }$ , located at a distance ${D}_{L}={7.49}_{-1.13}^{+0.99}\,\mathrm{kpc}$ . For the second scenario, we estimate ${m}_{\mathrm{planet}}={69}_{-34}^{+37}\,{M}_{\oplus }$ , ${M}_{\mathrm{host}}={0.66}_{-0.32}^{+0.35}\,{M}_{\odot }$ , and ${D}_{L}={7.81}_{-0.93}^{+0.93}\,\mathrm{kpc}$ . The planet has a projected separation as a fraction of the Einstein ring radius $s={1.3807}_{-0.0018}^{+0.0018}$ . As a cool sub-Saturn-mass planet, this planet adds to a growing collection of evidence for revised planetary formation models. |
| abstractGer |
We analyze the MOA-2020-BLG-208 gravitational microlensing event and present the discovery and characterization of a new planet, MOA-2020-BLG-208Lb, with an estimated sub-Saturn mass. With a mass ratio $q={3.17}_{-0.26}^{+0.28}\times {10}^{-4}$ , the planet lies near the peak of the mass-ratio function derived by the MOA collaboration and near the edge of expected sample sensitivity. For these estimates we provide results using two mass-law priors: one assuming that all stars have an equal planet-hosting probability, and the other assuming that planets are more likely to orbit around more massive stars. In the first scenario, we estimate that the lens system is likely to be a planet of mass ${m}_{\mathrm{planet}}={46}_{-24}^{+42}\,{M}_{\oplus }$ and a host star of mass ${M}_{\mathrm{host}}={0.43}_{-0.23}^{+0.39}\,{M}_{\odot }$ , located at a distance ${D}_{L}={7.49}_{-1.13}^{+0.99}\,\mathrm{kpc}$ . For the second scenario, we estimate ${m}_{\mathrm{planet}}={69}_{-34}^{+37}\,{M}_{\oplus }$ , ${M}_{\mathrm{host}}={0.66}_{-0.32}^{+0.35}\,{M}_{\odot }$ , and ${D}_{L}={7.81}_{-0.93}^{+0.93}\,\mathrm{kpc}$ . The planet has a projected separation as a fraction of the Einstein ring radius $s={1.3807}_{-0.0018}^{+0.0018}$ . As a cool sub-Saturn-mass planet, this planet adds to a growing collection of evidence for revised planetary formation models. |
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We analyze the MOA-2020-BLG-208 gravitational microlensing event and present the discovery and characterization of a new planet, MOA-2020-BLG-208Lb, with an estimated sub-Saturn mass. With a mass ratio $q={3.17}_{-0.26}^{+0.28}\times {10}^{-4}$ , the planet lies near the peak of the mass-ratio function derived by the MOA collaboration and near the edge of expected sample sensitivity. For these estimates we provide results using two mass-law priors: one assuming that all stars have an equal planet-hosting probability, and the other assuming that planets are more likely to orbit around more massive stars. In the first scenario, we estimate that the lens system is likely to be a planet of mass ${m}_{\mathrm{planet}}={46}_{-24}^{+42}\,{M}_{\oplus }$ and a host star of mass ${M}_{\mathrm{host}}={0.43}_{-0.23}^{+0.39}\,{M}_{\odot }$ , located at a distance ${D}_{L}={7.49}_{-1.13}^{+0.99}\,\mathrm{kpc}$ . For the second scenario, we estimate ${m}_{\mathrm{planet}}={69}_{-34}^{+37}\,{M}_{\oplus }$ , ${M}_{\mathrm{host}}={0.66}_{-0.32}^{+0.35}\,{M}_{\odot }$ , and ${D}_{L}={7.81}_{-0.93}^{+0.93}\,\mathrm{kpc}$ . The planet has a projected separation as a fraction of the Einstein ring radius $s={1.3807}_{-0.0018}^{+0.0018}$ . As a cool sub-Saturn-mass planet, this planet adds to a growing collection of evidence for revised planetary formation models. |
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