Predicting Interstellar Object Chemodynamics with Gaia
The interstellar object (ISO) population of the Milky Way is a product of its stars. However, what is in fact a complex structure in the solar neighborhood has traditionally in ISO studies been described as smoothly distributed. Using a debiased stellar population derived from the Gaia Data Release...
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IOP Publishing
2025-01-01
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| Series: | The Astronomical Journal |
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| Online Access: | https://doi.org/10.3847/1538-3881/ad9eb3 |
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| author | Matthew J. Hopkins Michele T. Bannister Chris Lintott |
| author_facet | Matthew J. Hopkins Michele T. Bannister Chris Lintott |
| author_sort | Matthew J. Hopkins |
| collection | DOAJ |
| description | The interstellar object (ISO) population of the Milky Way is a product of its stars. However, what is in fact a complex structure in the solar neighborhood has traditionally in ISO studies been described as smoothly distributed. Using a debiased stellar population derived from the Gaia Data Release 3 stellar sample, we predict that the velocity distribution of ISOs is far more textured than a smooth Gaussian. The moving groups caused by Galactic resonances dominate the distribution. 1I/‘Oumuamua and 2I/Borisov have entirely normal places within these distributions; 1I is within the noncoeval moving group that includes the Matariki (Pleiades) cluster, and 2I within the Coma Berenices moving group. We show that for the composition of planetesimals formed beyond the ice line, these velocity structures also have a chemodynamic component. This variation will be visible on the sky. We predict that this richly textured distribution will be differentiable from smooth Gaussians in samples that are within the expected discovery capacity of the Vera C. Rubin Observatory. Solar neighborhood ISOs will be of all ages and come from a dynamic mix of many different populations of stars, reflecting their origins from all around the Galactic disk. |
| format | Article |
| id | doaj-art-d9325ee381804a78b9db9e0de49b70ec |
| institution | Kabale University |
| issn | 1538-3881 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astronomical Journal |
| spelling | doaj-art-d9325ee381804a78b9db9e0de49b70ec2025-01-17T17:30:15ZengIOP PublishingThe Astronomical Journal1538-38812025-01-0116927810.3847/1538-3881/ad9eb3Predicting Interstellar Object Chemodynamics with GaiaMatthew J. Hopkins0https://orcid.org/0000-0001-6314-873XMichele T. Bannister1https://orcid.org/0000-0003-3257-4490Chris Lintott2https://orcid.org/0000-0001-5578-359XDepartment of Physics, University of Oxford , Denys Wilkinson Building, Keble Road, Oxford, OX1 3RH, UK ; matthew.hopkins@physics.ox.ac.uk; School of Physical and Chemical Sciences–Te Kura Matū, University of Canterbury , Private Bag 4800, Christchurch 8140, New ZealandSchool of Physical and Chemical Sciences–Te Kura Matū, University of Canterbury , Private Bag 4800, Christchurch 8140, New ZealandDepartment of Physics, University of Oxford , Denys Wilkinson Building, Keble Road, Oxford, OX1 3RH, UK ; matthew.hopkins@physics.ox.ac.ukThe interstellar object (ISO) population of the Milky Way is a product of its stars. However, what is in fact a complex structure in the solar neighborhood has traditionally in ISO studies been described as smoothly distributed. Using a debiased stellar population derived from the Gaia Data Release 3 stellar sample, we predict that the velocity distribution of ISOs is far more textured than a smooth Gaussian. The moving groups caused by Galactic resonances dominate the distribution. 1I/‘Oumuamua and 2I/Borisov have entirely normal places within these distributions; 1I is within the noncoeval moving group that includes the Matariki (Pleiades) cluster, and 2I within the Coma Berenices moving group. We show that for the composition of planetesimals formed beyond the ice line, these velocity structures also have a chemodynamic component. This variation will be visible on the sky. We predict that this richly textured distribution will be differentiable from smooth Gaussians in samples that are within the expected discovery capacity of the Vera C. Rubin Observatory. Solar neighborhood ISOs will be of all ages and come from a dynamic mix of many different populations of stars, reflecting their origins from all around the Galactic disk.https://doi.org/10.3847/1538-3881/ad9eb3Interstellar objectsMilky Way GalaxyGalaxy dynamics |
| spellingShingle | Matthew J. Hopkins Michele T. Bannister Chris Lintott Predicting Interstellar Object Chemodynamics with Gaia The Astronomical Journal Interstellar objects Milky Way Galaxy Galaxy dynamics |
| title | Predicting Interstellar Object Chemodynamics with Gaia |
| title_full | Predicting Interstellar Object Chemodynamics with Gaia |
| title_fullStr | Predicting Interstellar Object Chemodynamics with Gaia |
| title_full_unstemmed | Predicting Interstellar Object Chemodynamics with Gaia |
| title_short | Predicting Interstellar Object Chemodynamics with Gaia |
| title_sort | predicting interstellar object chemodynamics with gaia |
| topic | Interstellar objects Milky Way Galaxy Galaxy dynamics |
| url | https://doi.org/10.3847/1538-3881/ad9eb3 |
| work_keys_str_mv | AT matthewjhopkins predictinginterstellarobjectchemodynamicswithgaia AT micheletbannister predictinginterstellarobjectchemodynamicswithgaia AT chrislintott predictinginterstellarobjectchemodynamicswithgaia |