REVISITING THE MICROLENSING EVENT OGLE 2012-BLG-0026: A SOLAR MASS STAR WITH TWO COLD GIANT PLANETS
ABSTRACT Two cold gas giant planets orbiting a G-type main-sequence star in the galactic disk were previously discovered in the high-magnification microlensing event OGLE-2012-BLG-0026. Here, we present revised host star flux measurements and a refined model for the two-planet system using additiona...
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| Veröffentlicht in: | The Astrophysical journal 2016-06, Vol.824 (2), p.83-83 |
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| creator | Beaulieu, J.-P. Bennett, D. P. Batista, V. Fukui, A. Marquette, J.-B. Brillant, S. Cole, A. A. Rogers, L. A. Sumi, T. Abe, F. Bhattacharya, A. Koshimoto, N. Suzuki, D. Tristram, P. J. Han, C. Gould, A. Pogge, R. Yee, J. |
| description | ABSTRACT Two cold gas giant planets orbiting a G-type main-sequence star in the galactic disk were previously discovered in the high-magnification microlensing event OGLE-2012-BLG-0026. Here, we present revised host star flux measurements and a refined model for the two-planet system using additional light curve data. We performed high angular resolution adaptive optics imaging with the Keck and Subaru telescopes at two epochs while the source star was still amplified. We detected the lens flux, H = 16.39 0.08. The lens, a disk star, is brighter than predicted from the modeling in the original study. We revisited the light curve modeling using additional photometric data from the B&C telescope in New Zealand and CTIO 1.3 m H-band light curve. We then include the Keck and Subaru adaptive optic observation constraints. The system is composed of a ∼4-9 Gyr lens star of Mlens = 1.06 0.05 M at a distance of Dlens = 4.0 0.3 kpc, orbited by two giant planets of 0.145 0.008 MJup and 0.86 0.06 MJup, with projected separations of 4.0 0.5 au and 4.8 0.7 au, respectively. Because the lens is brighter than the source star by 16 8% in H, with no other blend within one arcsec, it will be possible to estimate its metallicity using subsequent IR spectroscopy with 8-10 m class telescopes. By adding a constraint on the metallicity it will be possible to refine the age of the system. |
| doi_str_mv | 10.3847/0004-637X/824/2/83 |
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P. ; Batista, V. ; Fukui, A. ; Marquette, J.-B. ; Brillant, S. ; Cole, A. A. ; Rogers, L. A. ; Sumi, T. ; Abe, F. ; Bhattacharya, A. ; Koshimoto, N. ; Suzuki, D. ; Tristram, P. J. ; Han, C. ; Gould, A. ; Pogge, R. ; Yee, J.</creator><creatorcontrib>Beaulieu, J.-P. ; Bennett, D. P. ; Batista, V. ; Fukui, A. ; Marquette, J.-B. ; Brillant, S. ; Cole, A. A. ; Rogers, L. A. ; Sumi, T. ; Abe, F. ; Bhattacharya, A. ; Koshimoto, N. ; Suzuki, D. ; Tristram, P. J. ; Han, C. ; Gould, A. ; Pogge, R. ; Yee, J.</creatorcontrib><description>ABSTRACT Two cold gas giant planets orbiting a G-type main-sequence star in the galactic disk were previously discovered in the high-magnification microlensing event OGLE-2012-BLG-0026. Here, we present revised host star flux measurements and a refined model for the two-planet system using additional light curve data. We performed high angular resolution adaptive optics imaging with the Keck and Subaru telescopes at two epochs while the source star was still amplified. We detected the lens flux, H = 16.39 0.08. The lens, a disk star, is brighter than predicted from the modeling in the original study. We revisited the light curve modeling using additional photometric data from the B&C telescope in New Zealand and CTIO 1.3 m H-band light curve. We then include the Keck and Subaru adaptive optic observation constraints. The system is composed of a ∼4-9 Gyr lens star of Mlens = 1.06 0.05 M at a distance of Dlens = 4.0 0.3 kpc, orbited by two giant planets of 0.145 0.008 MJup and 0.86 0.06 MJup, with projected separations of 4.0 0.5 au and 4.8 0.7 au, respectively. Because the lens is brighter than the source star by 16 8% in H, with no other blend within one arcsec, it will be possible to estimate its metallicity using subsequent IR spectroscopy with 8-10 m class telescopes. By adding a constraint on the metallicity it will be possible to refine the age of the system.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/0004-637X/824/2/83</identifier><language>eng</language><publisher>Goddard Space Flight Center: The American Astronomical Society</publisher><subject>Adaptive optics ; Astrophysics ; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ; DETECTION ; Flux ; GRAVITATIONAL LENSES ; gravitational lensing: micro ; INFRARED SPECTRA ; Lenses ; Light curve ; MAIN SEQUENCE STARS ; MASS ; METALLICITY ; Microlenses ; Modelling ; Physics ; PLANETS ; planets and satellites: detection ; planets and satellites: gaseous planets ; RESOLUTION ; SATELLITES ; SIMULATION ; Stars ; TELESCOPES ; VISIBLE RADIATION</subject><ispartof>The Astrophysical journal, 2016-06, Vol.824 (2), p.83-83</ispartof><rights>2016. The American Astronomical Society. All rights reserved.</rights><rights>Distributed under a Creative Commons Attribution 4.0 International License</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c508t-e460a6be07ed8ed291b0008505f311d3cb343a9e6631f1b9f723223f2496d2943</citedby><cites>FETCH-LOGICAL-c508t-e460a6be07ed8ed291b0008505f311d3cb343a9e6631f1b9f723223f2496d2943</cites><orcidid>0000-0002-5843-9433 ; 0000-0001-8043-8413 ; 0000-0002-4909-5763 ; 0000-0001-9481-7123 ; 0000-0003-0014-3354 ; 0000-0002-9782-0333 ; 0000-0003-1435-3053 ; 0000-0002-2641-9964 ; 0000-0003-0638-3455 ; 0000-0003-2302-9562 ; 0000-0003-0303-3855 ; 0000-0002-7901-7213</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.3847/0004-637X/824/2/83/pdf$$EPDF$$P50$$Giop$$H</linktopdf><link.rule.ids>230,314,776,780,881,27901,27902,38867,53842</link.rule.ids><linktorsrc>$$Uhttps://iopscience.iop.org/article/10.3847/0004-637X/824/2/83$$EView_record_in_IOP_Publishing$$FView_record_in_$$GIOP_Publishing</linktorsrc><backlink>$$Uhttps://hal.science/hal-02459069$$DView record in HAL$$Hfree_for_read</backlink><backlink>$$Uhttps://www.osti.gov/biblio/22666181$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>Beaulieu, J.-P.</creatorcontrib><creatorcontrib>Bennett, D. P.</creatorcontrib><creatorcontrib>Batista, V.</creatorcontrib><creatorcontrib>Fukui, A.</creatorcontrib><creatorcontrib>Marquette, J.-B.</creatorcontrib><creatorcontrib>Brillant, S.</creatorcontrib><creatorcontrib>Cole, A. A.</creatorcontrib><creatorcontrib>Rogers, L. A.</creatorcontrib><creatorcontrib>Sumi, T.</creatorcontrib><creatorcontrib>Abe, F.</creatorcontrib><creatorcontrib>Bhattacharya, A.</creatorcontrib><creatorcontrib>Koshimoto, N.</creatorcontrib><creatorcontrib>Suzuki, D.</creatorcontrib><creatorcontrib>Tristram, P. J.</creatorcontrib><creatorcontrib>Han, C.</creatorcontrib><creatorcontrib>Gould, A.</creatorcontrib><creatorcontrib>Pogge, R.</creatorcontrib><creatorcontrib>Yee, J.</creatorcontrib><title>REVISITING THE MICROLENSING EVENT OGLE 2012-BLG-0026: A SOLAR MASS STAR WITH TWO COLD GIANT PLANETS</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>ABSTRACT Two cold gas giant planets orbiting a G-type main-sequence star in the galactic disk were previously discovered in the high-magnification microlensing event OGLE-2012-BLG-0026. Here, we present revised host star flux measurements and a refined model for the two-planet system using additional light curve data. We performed high angular resolution adaptive optics imaging with the Keck and Subaru telescopes at two epochs while the source star was still amplified. We detected the lens flux, H = 16.39 0.08. The lens, a disk star, is brighter than predicted from the modeling in the original study. We revisited the light curve modeling using additional photometric data from the B&C telescope in New Zealand and CTIO 1.3 m H-band light curve. We then include the Keck and Subaru adaptive optic observation constraints. The system is composed of a ∼4-9 Gyr lens star of Mlens = 1.06 0.05 M at a distance of Dlens = 4.0 0.3 kpc, orbited by two giant planets of 0.145 0.008 MJup and 0.86 0.06 MJup, with projected separations of 4.0 0.5 au and 4.8 0.7 au, respectively. Because the lens is brighter than the source star by 16 8% in H, with no other blend within one arcsec, it will be possible to estimate its metallicity using subsequent IR spectroscopy with 8-10 m class telescopes. By adding a constraint on the metallicity it will be possible to refine the age of the system.</description><subject>Adaptive optics</subject><subject>Astrophysics</subject><subject>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</subject><subject>DETECTION</subject><subject>Flux</subject><subject>GRAVITATIONAL LENSES</subject><subject>gravitational lensing: micro</subject><subject>INFRARED SPECTRA</subject><subject>Lenses</subject><subject>Light curve</subject><subject>MAIN SEQUENCE STARS</subject><subject>MASS</subject><subject>METALLICITY</subject><subject>Microlenses</subject><subject>Modelling</subject><subject>Physics</subject><subject>PLANETS</subject><subject>planets and satellites: detection</subject><subject>planets and satellites: gaseous planets</subject><subject>RESOLUTION</subject><subject>SATELLITES</subject><subject>SIMULATION</subject><subject>Stars</subject><subject>TELESCOPES</subject><subject>VISIBLE RADIATION</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2016</creationdate><recordtype>article</recordtype><sourceid>CYI</sourceid><recordid>eNqNkU-P0zAQxS0EEqXwBRAHS3CAQ7b-kzg2t9DNppG8DWrCLjfLTR1tqm6SjVMkvj22suoJIU4ez_ze02geAO8xuqI8jFcIoTBgNP654iRckRWnL8ACR5QHIY3il2BxAV6DN9Ye_ZcIsQD1Lr3Ly7zKtxmsNim8zde7Qqbb0jfSu3RbwSKTKSQIk-CbzAKECPsKE1gWMtnB26QsYVm56j6vNrC6L-C6kNcwyxOn_C6TbVqVb8GrRp-seff8LsGPm7RabwJZZPk6kUEdIT4FJmRIs71BsTlwcyAC792aPEJRQzE-0HpPQ6qFYYziBu9FExNKCG1IKJijQ7oEH2ff3k6tsnU7mfqh7rvO1JMihDGGOXbUl5l60Cc1jO2jHn-rXrdqk0jle4iEkUBM_PLs55kdxv7pbOykHltbm9NJd6Y_W4W5oFzEnNH_QLkjGXPsEpAZrcfe2tE0lzUwUj5O5eNRPi3l4lREce__YRZ12mrVTaNVLhPmSBHH3vNqHrf9oI79eezcpf_t9-kvAj0cL4gaDg39AxqGqLA</recordid><startdate>20160620</startdate><enddate>20160620</enddate><creator>Beaulieu, J.-P.</creator><creator>Bennett, D. 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J.</creator><creator>Han, C.</creator><creator>Gould, A.</creator><creator>Pogge, R.</creator><creator>Yee, J.</creator><general>The American Astronomical Society</general><general>American Astronomical Society</general><scope>CYE</scope><scope>CYI</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>KL.</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>1XC</scope><scope>OTOTI</scope><orcidid>https://orcid.org/0000-0002-5843-9433</orcidid><orcidid>https://orcid.org/0000-0001-8043-8413</orcidid><orcidid>https://orcid.org/0000-0002-4909-5763</orcidid><orcidid>https://orcid.org/0000-0001-9481-7123</orcidid><orcidid>https://orcid.org/0000-0003-0014-3354</orcidid><orcidid>https://orcid.org/0000-0002-9782-0333</orcidid><orcidid>https://orcid.org/0000-0003-1435-3053</orcidid><orcidid>https://orcid.org/0000-0002-2641-9964</orcidid><orcidid>https://orcid.org/0000-0003-0638-3455</orcidid><orcidid>https://orcid.org/0000-0003-2302-9562</orcidid><orcidid>https://orcid.org/0000-0003-0303-3855</orcidid><orcidid>https://orcid.org/0000-0002-7901-7213</orcidid></search><sort><creationdate>20160620</creationdate><title>REVISITING THE MICROLENSING EVENT OGLE 2012-BLG-0026: A SOLAR MASS STAR WITH TWO COLD GIANT PLANETS</title><author>Beaulieu, J.-P. ; Bennett, D. 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P.</au><au>Batista, V.</au><au>Fukui, A.</au><au>Marquette, J.-B.</au><au>Brillant, S.</au><au>Cole, A. A.</au><au>Rogers, L. A.</au><au>Sumi, T.</au><au>Abe, F.</au><au>Bhattacharya, A.</au><au>Koshimoto, N.</au><au>Suzuki, D.</au><au>Tristram, P. J.</au><au>Han, C.</au><au>Gould, A.</au><au>Pogge, R.</au><au>Yee, J.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>REVISITING THE MICROLENSING EVENT OGLE 2012-BLG-0026: A SOLAR MASS STAR WITH TWO COLD GIANT PLANETS</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2016-06-20</date><risdate>2016</risdate><volume>824</volume><issue>2</issue><spage>83</spage><epage>83</epage><pages>83-83</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>ABSTRACT Two cold gas giant planets orbiting a G-type main-sequence star in the galactic disk were previously discovered in the high-magnification microlensing event OGLE-2012-BLG-0026. Here, we present revised host star flux measurements and a refined model for the two-planet system using additional light curve data. We performed high angular resolution adaptive optics imaging with the Keck and Subaru telescopes at two epochs while the source star was still amplified. We detected the lens flux, H = 16.39 0.08. The lens, a disk star, is brighter than predicted from the modeling in the original study. We revisited the light curve modeling using additional photometric data from the B&C telescope in New Zealand and CTIO 1.3 m H-band light curve. We then include the Keck and Subaru adaptive optic observation constraints. The system is composed of a ∼4-9 Gyr lens star of Mlens = 1.06 0.05 M at a distance of Dlens = 4.0 0.3 kpc, orbited by two giant planets of 0.145 0.008 MJup and 0.86 0.06 MJup, with projected separations of 4.0 0.5 au and 4.8 0.7 au, respectively. Because the lens is brighter than the source star by 16 8% in H, with no other blend within one arcsec, it will be possible to estimate its metallicity using subsequent IR spectroscopy with 8-10 m class telescopes. By adding a constraint on the metallicity it will be possible to refine the age of the system.</abstract><cop>Goddard Space Flight Center</cop><pub>The American Astronomical Society</pub><doi>10.3847/0004-637X/824/2/83</doi><tpages>6</tpages><orcidid>https://orcid.org/0000-0002-5843-9433</orcidid><orcidid>https://orcid.org/0000-0001-8043-8413</orcidid><orcidid>https://orcid.org/0000-0002-4909-5763</orcidid><orcidid>https://orcid.org/0000-0001-9481-7123</orcidid><orcidid>https://orcid.org/0000-0003-0014-3354</orcidid><orcidid>https://orcid.org/0000-0002-9782-0333</orcidid><orcidid>https://orcid.org/0000-0003-1435-3053</orcidid><orcidid>https://orcid.org/0000-0002-2641-9964</orcidid><orcidid>https://orcid.org/0000-0003-0638-3455</orcidid><orcidid>https://orcid.org/0000-0003-2302-9562</orcidid><orcidid>https://orcid.org/0000-0003-0303-3855</orcidid><orcidid>https://orcid.org/0000-0002-7901-7213</orcidid><oa>free_for_read</oa></addata></record> |
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| ispartof | The Astrophysical journal, 2016-06, Vol.824 (2), p.83-83 |
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| language | eng |
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| source | IOP Publishing Free Content |
| subjects | Adaptive optics Astrophysics ASTROPHYSICS, COSMOLOGY AND ASTRONOMY DETECTION Flux GRAVITATIONAL LENSES gravitational lensing: micro INFRARED SPECTRA Lenses Light curve MAIN SEQUENCE STARS MASS METALLICITY Microlenses Modelling Physics PLANETS planets and satellites: detection planets and satellites: gaseous planets RESOLUTION SATELLITES SIMULATION Stars TELESCOPES VISIBLE RADIATION |
| title | REVISITING THE MICROLENSING EVENT OGLE 2012-BLG-0026: A SOLAR MASS STAR WITH TWO COLD GIANT PLANETS |
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