The spiral structure of the Milky Way
The morphology and kinematics of the spiral structure of the Milky Way are long-standing problems in astrophysics. In this review we firstly summarize various methods with different tracers used to solve this puzzle. The astrometry of Galactic sources is gradually alleviating this difficult situatio...
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| Veröffentlicht in: | Research in astronomy and astrophysics 2018-12, Vol.18 (12), p.146 |
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| creator | Xu, Ye Hou, Li-Gang Wu, Yuan-Wei |
| description | The morphology and kinematics of the spiral structure of the Milky Way are long-standing problems in astrophysics. In this review we firstly summarize various methods with different tracers used to solve this puzzle. The astrometry of Galactic sources is gradually alleviating this difficult situation caused mainly by large distance uncertainties, as we can currently obtain accurate parallaxes (a few μas) and proper motions (≈1 km s−1) by using Very Long Baseline Interferometry (VLBI). On the other hand, the Gaia mission is providing the largest, uniform sample of parallaxes for O-type stars in the entire Milky Way. Based upon the VLBI maser and Gaia O-star parallax measurements, nearby spiral structures of the Perseus, Local, Sagittarius and Scutum Arms are determined in unprecedented detail. Meanwhile, we estimate fundamental Galactic parameters of the distance to the Galactic center, R0, to be 8.35 ± 0.18 kpc, and circular rotation speed at the Sun, Θ0, to be 240±10 km s−1. We found kinematic differences between O stars and interstellar masers: the O stars, on average, rotate faster, >8 km s−1 than maser-traced high-mass star forming regions. |
| doi_str_mv | 10.1088/1674-4527/18/12/146 |
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Astron. Astrophys</addtitle><description>The morphology and kinematics of the spiral structure of the Milky Way are long-standing problems in astrophysics. In this review we firstly summarize various methods with different tracers used to solve this puzzle. The astrometry of Galactic sources is gradually alleviating this difficult situation caused mainly by large distance uncertainties, as we can currently obtain accurate parallaxes (a few μas) and proper motions (≈1 km s−1) by using Very Long Baseline Interferometry (VLBI). On the other hand, the Gaia mission is providing the largest, uniform sample of parallaxes for O-type stars in the entire Milky Way. Based upon the VLBI maser and Gaia O-star parallax measurements, nearby spiral structures of the Perseus, Local, Sagittarius and Scutum Arms are determined in unprecedented detail. Meanwhile, we estimate fundamental Galactic parameters of the distance to the Galactic center, R0, to be 8.35 ± 0.18 kpc, and circular rotation speed at the Sun, Θ0, to be 240±10 km s−1. We found kinematic differences between O stars and interstellar masers: the O stars, on average, rotate faster, >8 km s−1 than maser-traced high-mass star forming regions.</description><subject>Astrometry</subject><subject>Astrophysics</subject><subject>Gaia Mission</subject><subject>Galaxy: kinematics and dynamics</subject><subject>Galaxy: structure</subject><subject>Interferometry</subject><subject>Interstellar masers</subject><subject>Kinematics</subject><subject>masers</subject><subject>Massive stars</subject><subject>Milky Way</subject><subject>Morphology</subject><subject>O stars</subject><subject>Parallax</subject><subject>Parameter estimation</subject><subject>Star formation</subject><subject>stars: formation</subject><subject>techniques: high angular resolution</subject><subject>Tracers</subject><subject>Very long base interferometry</subject><issn>1674-4527</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2018</creationdate><recordtype>article</recordtype><recordid>eNp9kEtPwzAQhH0AiVL4BVwioR5DvHb8yBFVQJGKuBRxtBw_REogwU4O-fe4CqIXxGk1q29mtYPQFeAbwFIWwEWZl4yIApIgBZT8BC1-t2foPMY9xpwxThZotXtzWeyboNssDmE0wxhc1vlsSPunpn2fslc9XaBTr9voLn_mEr3c3-3Wm3z7_PC4vt3mhpZiyCkQVlfUCFobTKUvtdfAa4ZrLq2gzkLFgArJOMcSpPcGrLdEOAbWkZrSJbqec_vQfY0uDmrfjeEznVSEMsGqSogyUXSmTOhiDM6rPjQfOkwKsDp0oA7fqsO3CpIgKnWQXKvZ1XT9MTZofWRUb33iij-4_5K_AS_BaYc</recordid><startdate>201812</startdate><enddate>201812</enddate><creator>Xu, Ye</creator><creator>Hou, Li-Gang</creator><creator>Wu, Yuan-Wei</creator><general>National Astronomical Observatories, CAS and IOP Publishing Ltd</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></search><sort><creationdate>201812</creationdate><title>The spiral structure of the Milky Way</title><author>Xu, Ye ; Hou, Li-Gang ; Wu, Yuan-Wei</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c347t-3125b93c73bc038f4afa16b50b68d73ed19513785660818ffc1dfd27e51de2b33</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2018</creationdate><topic>Astrometry</topic><topic>Astrophysics</topic><topic>Gaia Mission</topic><topic>Galaxy: kinematics and dynamics</topic><topic>Galaxy: structure</topic><topic>Interferometry</topic><topic>Interstellar masers</topic><topic>Kinematics</topic><topic>masers</topic><topic>Massive stars</topic><topic>Milky Way</topic><topic>Morphology</topic><topic>O stars</topic><topic>Parallax</topic><topic>Parameter estimation</topic><topic>Star formation</topic><topic>stars: formation</topic><topic>techniques: high angular resolution</topic><topic>Tracers</topic><topic>Very long base interferometry</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Xu, Ye</creatorcontrib><creatorcontrib>Hou, Li-Gang</creatorcontrib><creatorcontrib>Wu, Yuan-Wei</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>Research in astronomy and astrophysics</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Xu, Ye</au><au>Hou, Li-Gang</au><au>Wu, Yuan-Wei</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The spiral structure of the Milky Way</atitle><jtitle>Research in astronomy and astrophysics</jtitle><addtitle>Res. Astron. Astrophys</addtitle><date>2018-12</date><risdate>2018</risdate><volume>18</volume><issue>12</issue><spage>146</spage><pages>146-</pages><issn>1674-4527</issn><abstract>The morphology and kinematics of the spiral structure of the Milky Way are long-standing problems in astrophysics. In this review we firstly summarize various methods with different tracers used to solve this puzzle. The astrometry of Galactic sources is gradually alleviating this difficult situation caused mainly by large distance uncertainties, as we can currently obtain accurate parallaxes (a few μas) and proper motions (≈1 km s−1) by using Very Long Baseline Interferometry (VLBI). On the other hand, the Gaia mission is providing the largest, uniform sample of parallaxes for O-type stars in the entire Milky Way. Based upon the VLBI maser and Gaia O-star parallax measurements, nearby spiral structures of the Perseus, Local, Sagittarius and Scutum Arms are determined in unprecedented detail. Meanwhile, we estimate fundamental Galactic parameters of the distance to the Galactic center, R0, to be 8.35 ± 0.18 kpc, and circular rotation speed at the Sun, Θ0, to be 240±10 km s−1. We found kinematic differences between O stars and interstellar masers: the O stars, on average, rotate faster, >8 km s−1 than maser-traced high-mass star forming regions.</abstract><cop>Beijing</cop><pub>National Astronomical Observatories, CAS and IOP Publishing Ltd</pub><doi>10.1088/1674-4527/18/12/146</doi><tpages>20</tpages></addata></record> |
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| ispartof | Research in astronomy and astrophysics, 2018-12, Vol.18 (12), p.146 |
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| language | eng |
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| source | IOP Publishing Journals; Alma/SFX Local Collection |
| subjects | Astrometry Astrophysics Gaia Mission Galaxy: kinematics and dynamics Galaxy: structure Interferometry Interstellar masers Kinematics masers Massive stars Milky Way Morphology O stars Parallax Parameter estimation Star formation stars: formation techniques: high angular resolution Tracers Very long base interferometry |
| title | The spiral structure of the Milky Way |
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