On the Structure of the Sagittarius Spiral Arm in the Inner Milky Way
We report measurements of trigonometric parallax and proper motion for two 6.7 GHz methanol and two 22 GHz water masers located in the far portion of the Sagittarius spiral arm as part of the BeSSeL Survey. Distances for these sources are estimated from parallax measurements combined with three-dime...
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| Veröffentlicht in: | The Astronomical journal 2024-06, Vol.167 (6), p.267 |
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| container_title | The Astronomical journal |
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| creator | Bian, S. B. Wu, Y. W. Xu, Y. Reid, M. J. Li, J. J. Zhang, B. Menten, K. M. Moscadelli, L. Brunthaler, A. |
| description | We report measurements of trigonometric parallax and proper motion for two 6.7 GHz methanol and two 22 GHz water masers located in the far portion of the Sagittarius spiral arm as part of the BeSSeL Survey. Distances for these sources are estimated from parallax measurements combined with three-dimensional kinematic distances. The distances of G033.64−00.22, G035.57−00.03, G041.15−00.20, and G043.89−00.78 are 9.9 ± 0.5, 10.2 ± 0.6, 7.6 ± 0.5, and 7.5 ± 0.3 kpc, respectively. Based on these measurements, we suggest that the Sagittarius arm segment beyond about 8 kpc from the Sun in the first Galactic quadrant should be adjusted radially outward relative to previous models. This supports the suggestion of Xu et al. that the Sagittarius and Perseus spiral arms might merge in the first quadrant before spiraling inward to the far end of the Galactic bar. |
| doi_str_mv | 10.3847/1538-3881/ad4030 |
| format | Article |
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B. ; Wu, Y. W. ; Xu, Y. ; Reid, M. J. ; Li, J. J. ; Zhang, B. ; Menten, K. M. ; Moscadelli, L. ; Brunthaler, A.</creator><creatorcontrib>Bian, S. B. ; Wu, Y. W. ; Xu, Y. ; Reid, M. J. ; Li, J. J. ; Zhang, B. ; Menten, K. M. ; Moscadelli, L. ; Brunthaler, A.</creatorcontrib><description>We report measurements of trigonometric parallax and proper motion for two 6.7 GHz methanol and two 22 GHz water masers located in the far portion of the Sagittarius spiral arm as part of the BeSSeL Survey. Distances for these sources are estimated from parallax measurements combined with three-dimensional kinematic distances. The distances of G033.64−00.22, G035.57−00.03, G041.15−00.20, and G043.89−00.78 are 9.9 ± 0.5, 10.2 ± 0.6, 7.6 ± 0.5, and 7.5 ± 0.3 kpc, respectively. Based on these measurements, we suggest that the Sagittarius arm segment beyond about 8 kpc from the Sun in the first Galactic quadrant should be adjusted radially outward relative to previous models. This supports the suggestion of Xu et al. that the Sagittarius and Perseus spiral arms might merge in the first quadrant before spiraling inward to the far end of the Galactic bar.</description><identifier>ISSN: 0004-6256</identifier><identifier>EISSN: 1538-3881</identifier><identifier>DOI: 10.3847/1538-3881/ad4030</identifier><language>eng</language><publisher>Madison: The American Astronomical Society</publisher><subject>Astronomical models ; Galactic structure ; Interstellar masers ; Kinematics ; Masers ; Milky Way ; Milky Way Galaxy ; Parallax ; Quadrants ; Star forming regions ; Trigonometric parallax</subject><ispartof>The Astronomical journal, 2024-06, Vol.167 (6), p.267</ispartof><rights>2024. The Author(s). Published by the American Astronomical Society.</rights><rights>2024. The Author(s). Published by the American Astronomical Society. This work is published under http://creativecommons.org/licenses/by/4.0/ (the “License”). 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| subjects | Astronomical models Galactic structure Interstellar masers Kinematics Masers Milky Way Milky Way Galaxy Parallax Quadrants Star forming regions Trigonometric parallax |
| title | On the Structure of the Sagittarius Spiral Arm in the Inner Milky Way |
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