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Obliquity Constraints on the Planetary-mass Companion HD 106906 b
We constrain the angular momentum architecture of HD 106906, a 13 ± 2 Myr old system in the ScoCen complex composed of a compact central binary, a widely separated planetary-mass tertiary HD 106906 b, and a debris disk nested between the binary and tertiary orbital planes. We measure the orientation...
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| Published in: | The Astronomical journal 2021-11, Vol.162 (5), p.217 |
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| Main Authors: | , , , , |
| Format: | Article |
| Language: | English |
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| cites | cdi_FETCH-LOGICAL-c445t-6c3ffc25598264a8d2b9b058e69fa6f6dbebdea18c751f5dea1e62e62f8c0be03 |
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| container_issue | 5 |
| container_start_page | 217 |
| container_title | The Astronomical journal |
| container_volume | 162 |
| creator | Bryan, Marta L. Chiang, Eugene Morley, Caroline V. Mace, Gregory N. Bowler, Brendan P. |
| description | We constrain the angular momentum architecture of HD 106906, a 13 ± 2 Myr old system in the ScoCen complex composed of a compact central binary, a widely separated planetary-mass tertiary HD 106906 b, and a debris disk nested between the binary and tertiary orbital planes. We measure the orientations of three vectors: the companion spin axis, companion orbit normal, and disk normal. Using near-IR high-resolution spectra from Gemini/IGRINS, we obtain a projected rotational velocity of
v
sin
i
p
= 9.5 ± 0.2 km s
−1
for HD 106906 b. This measurement together with a published photometric rotation period implies the companion is viewed nearly pole-on, with a line-of-sight spin axis inclination of
i
p
= 14° ± 4° or 166° ± 4°. By contrast, the debris disk is known to be viewed nearly edge on. The likely misalignment of all three vectors suggests HD 106906 b formed by gravitational instability in a turbulent environment, either in a disk or cloud setting. |
| doi_str_mv | 10.3847/1538-3881/ac1bb1 |
| format | article |
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v
sin
i
p
= 9.5 ± 0.2 km s
−1
for HD 106906 b. This measurement together with a published photometric rotation period implies the companion is viewed nearly pole-on, with a line-of-sight spin axis inclination of
i
p
= 14° ± 4° or 166° ± 4°. By contrast, the debris disk is known to be viewed nearly edge on. The likely misalignment of all three vectors suggests HD 106906 b formed by gravitational instability in a turbulent environment, either in a disk or cloud setting.</description><identifier>ISSN: 0004-6256</identifier><identifier>EISSN: 1538-3881</identifier><identifier>DOI: 10.3847/1538-3881/ac1bb1</identifier><language>eng</language><publisher>Madison: The American Astronomical Society</publisher><subject>Angular momentum ; Astronomy ; Astrostatistics ; Exoplanet astronomy ; Exoplanet evolution ; Exoplanet formation ; Exoplanet systems ; Extrasolar planets ; Gravitational instability ; High resolution spectroscopy ; Misalignment ; Obliquity ; Rotation ; Rotational spectra ; Tertiary</subject><ispartof>The Astronomical journal, 2021-11, Vol.162 (5), p.217</ispartof><rights>2021. The American Astronomical Society. All rights reserved.</rights><rights>Copyright IOP Publishing Nov 2021</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c445t-6c3ffc25598264a8d2b9b058e69fa6f6dbebdea18c751f5dea1e62e62f8c0be03</citedby><cites>FETCH-LOGICAL-c445t-6c3ffc25598264a8d2b9b058e69fa6f6dbebdea18c751f5dea1e62e62f8c0be03</cites><orcidid>0000-0003-2649-2288 ; 0000-0002-6246-2310 ; 0000-0002-6076-5967 ; 0000-0002-4404-0456 ; 0000-0001-7875-6391</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,780,784,864,27924,27925</link.rule.ids></links><search><creatorcontrib>Bryan, Marta L.</creatorcontrib><creatorcontrib>Chiang, Eugene</creatorcontrib><creatorcontrib>Morley, Caroline V.</creatorcontrib><creatorcontrib>Mace, Gregory N.</creatorcontrib><creatorcontrib>Bowler, Brendan P.</creatorcontrib><title>Obliquity Constraints on the Planetary-mass Companion HD 106906 b</title><title>The Astronomical journal</title><addtitle>AJ</addtitle><addtitle>Astron. J</addtitle><description>We constrain the angular momentum architecture of HD 106906, a 13 ± 2 Myr old system in the ScoCen complex composed of a compact central binary, a widely separated planetary-mass tertiary HD 106906 b, and a debris disk nested between the binary and tertiary orbital planes. We measure the orientations of three vectors: the companion spin axis, companion orbit normal, and disk normal. Using near-IR high-resolution spectra from Gemini/IGRINS, we obtain a projected rotational velocity of
v
sin
i
p
= 9.5 ± 0.2 km s
−1
for HD 106906 b. This measurement together with a published photometric rotation period implies the companion is viewed nearly pole-on, with a line-of-sight spin axis inclination of
i
p
= 14° ± 4° or 166° ± 4°. By contrast, the debris disk is known to be viewed nearly edge on. The likely misalignment of all three vectors suggests HD 106906 b formed by gravitational instability in a turbulent environment, either in a disk or cloud setting.</description><subject>Angular momentum</subject><subject>Astronomy</subject><subject>Astrostatistics</subject><subject>Exoplanet astronomy</subject><subject>Exoplanet evolution</subject><subject>Exoplanet formation</subject><subject>Exoplanet systems</subject><subject>Extrasolar planets</subject><subject>Gravitational instability</subject><subject>High resolution spectroscopy</subject><subject>Misalignment</subject><subject>Obliquity</subject><subject>Rotation</subject><subject>Rotational spectra</subject><subject>Tertiary</subject><issn>0004-6256</issn><issn>1538-3881</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2021</creationdate><recordtype>article</recordtype><recordid>eNp9kEFLAzEQhYMoWKt3jwt6dO0k2WSzx1KrFQr1oOeQZBPc0u5uk_TQf2-WFb2IMDDDzDdvmIfQLYZHKopyhhkVORUCz5TBWuMzNPlpnaMJABQ5J4xfoqsQtgAYCygmaL7Ru-ZwbOIpW3RtiF41bQxZ12bx02ZvO9XaqPwp36sQErHvVduk4eopw8Ar4Jm-RhdO7YK9-c5T9PG8fF-s8vXm5XUxX-emKFjMuaHOGcJYJQgvlKiJrjQwYXnlFHe81lbXVmFhSoYdG0rLSQonDGgLdIruRt3ed4ejDVFuu6Nv00lJWIUpLynQRMFIGd-F4K2TvW_26QOJQQ5GycEVObgiR6PSysO40nT9r-Y_-P0fuNpKzIlkkuBS9rWjX98cdSo</recordid><startdate>20211101</startdate><enddate>20211101</enddate><creator>Bryan, Marta L.</creator><creator>Chiang, Eugene</creator><creator>Morley, Caroline V.</creator><creator>Mace, Gregory N.</creator><creator>Bowler, Brendan P.</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><orcidid>https://orcid.org/0000-0003-2649-2288</orcidid><orcidid>https://orcid.org/0000-0002-6246-2310</orcidid><orcidid>https://orcid.org/0000-0002-6076-5967</orcidid><orcidid>https://orcid.org/0000-0002-4404-0456</orcidid><orcidid>https://orcid.org/0000-0001-7875-6391</orcidid></search><sort><creationdate>20211101</creationdate><title>Obliquity Constraints on the Planetary-mass Companion HD 106906 b</title><author>Bryan, Marta L. ; Chiang, Eugene ; Morley, Caroline V. ; Mace, Gregory N. ; Bowler, Brendan P.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c445t-6c3ffc25598264a8d2b9b058e69fa6f6dbebdea18c751f5dea1e62e62f8c0be03</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2021</creationdate><topic>Angular momentum</topic><topic>Astronomy</topic><topic>Astrostatistics</topic><topic>Exoplanet astronomy</topic><topic>Exoplanet evolution</topic><topic>Exoplanet formation</topic><topic>Exoplanet systems</topic><topic>Extrasolar planets</topic><topic>Gravitational instability</topic><topic>High resolution spectroscopy</topic><topic>Misalignment</topic><topic>Obliquity</topic><topic>Rotation</topic><topic>Rotational spectra</topic><topic>Tertiary</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Bryan, Marta L.</creatorcontrib><creatorcontrib>Chiang, Eugene</creatorcontrib><creatorcontrib>Morley, Caroline V.</creatorcontrib><creatorcontrib>Mace, Gregory N.</creatorcontrib><creatorcontrib>Bowler, Brendan P.</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>The Astronomical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Bryan, Marta L.</au><au>Chiang, Eugene</au><au>Morley, Caroline V.</au><au>Mace, Gregory N.</au><au>Bowler, Brendan P.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Obliquity Constraints on the Planetary-mass Companion HD 106906 b</atitle><jtitle>The Astronomical journal</jtitle><stitle>AJ</stitle><addtitle>Astron. J</addtitle><date>2021-11-01</date><risdate>2021</risdate><volume>162</volume><issue>5</issue><spage>217</spage><pages>217-</pages><issn>0004-6256</issn><eissn>1538-3881</eissn><abstract>We constrain the angular momentum architecture of HD 106906, a 13 ± 2 Myr old system in the ScoCen complex composed of a compact central binary, a widely separated planetary-mass tertiary HD 106906 b, and a debris disk nested between the binary and tertiary orbital planes. We measure the orientations of three vectors: the companion spin axis, companion orbit normal, and disk normal. Using near-IR high-resolution spectra from Gemini/IGRINS, we obtain a projected rotational velocity of
v
sin
i
p
= 9.5 ± 0.2 km s
−1
for HD 106906 b. This measurement together with a published photometric rotation period implies the companion is viewed nearly pole-on, with a line-of-sight spin axis inclination of
i
p
= 14° ± 4° or 166° ± 4°. By contrast, the debris disk is known to be viewed nearly edge on. The likely misalignment of all three vectors suggests HD 106906 b formed by gravitational instability in a turbulent environment, either in a disk or cloud setting.</abstract><cop>Madison</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-3881/ac1bb1</doi><tpages>10</tpages><orcidid>https://orcid.org/0000-0003-2649-2288</orcidid><orcidid>https://orcid.org/0000-0002-6246-2310</orcidid><orcidid>https://orcid.org/0000-0002-6076-5967</orcidid><orcidid>https://orcid.org/0000-0002-4404-0456</orcidid><orcidid>https://orcid.org/0000-0001-7875-6391</orcidid><oa>free_for_read</oa></addata></record> |
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| ispartof | The Astronomical journal, 2021-11, Vol.162 (5), p.217 |
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| language | eng |
| recordid | cdi_iop_journals_10_3847_1538_3881_ac1bb1 |
| source | Directory of Open Access Journals |
| subjects | Angular momentum Astronomy Astrostatistics Exoplanet astronomy Exoplanet evolution Exoplanet formation Exoplanet systems Extrasolar planets Gravitational instability High resolution spectroscopy Misalignment Obliquity Rotation Rotational spectra Tertiary |
| title | Obliquity Constraints on the Planetary-mass Companion HD 106906 b |
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