Exploring the stellar streams and satellites around the giant low surface brightness galaxy Malin 1
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| Main Authors: | , , , , , , , , , |
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| Format: | Preprint |
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2025
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| _version_ | 1866915154197741568 |
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| author | Bustos-Espinoza, Roy O. E. Blaña, Matias Galaz, Gaspar Mora, Marcelo Junais Das, Mousumi Barway, Sudhanshu Kumar, Ankit Johnston, Evelyn J. Puzia, Thomas |
| author_facet | Bustos-Espinoza, Roy O. E. Blaña, Matias Galaz, Gaspar Mora, Marcelo Junais Das, Mousumi Barway, Sudhanshu Kumar, Ankit Johnston, Evelyn J. Puzia, Thomas |
| contents | Context. Giant Low Surface Brightness galaxies, such as Malin 1, host extended stellar and gaseous disks exceeding 100 kpc in radius. Their formation and evolution remain debated, with interactions with satellite galaxies and accretion streams proposed as key contributors. Malin 1 has multiple satellites, including Malin 1A, Malin 1B, and the newly reported Malin 1C, along with eM1 at 350 kpc. Additionally, it exhibits two giant stellar streams, the largest extending 200 kpc, likely linked to past interactions.
Aims. We investigate the orbital dynamics of Malin 1's satellites and their relationship with the observed stellar streams, testing their consistency with different formation scenarios.
Methods. We constructed gravitational potentials using optical and H I rotation curve data, using stellar, gaseous, and dark matter components. We explored a wide parameter space to see if the candidate progenitors of the stellar streams could have originated from past interactions, testing both NFW and isothermal halo profiles.
Results. Among ten explored scenarios, seven produced bound orbital solutions. The isothermal halo model, with a virial mass of 3.8 x 10^12 solar masses and a virial radius of approximately 323 kpc, favors bound satellite orbits more than the NFW model (1.7 x 10^12 solar masses). We find that eM1 probably had a pericenter passage 1.3 Gyr ago, Malin 1A around 1.4 Gyr ago, and Malin 1B's leading arm may be experiencing one now. Malin 1C displays both leading and trailing arms. Furthermore, we identify three unbound orbital solutions that could link eM1, Malin 1A, or Malin 1B to the streams.
Conclusions. The alignment of satellites and streams supports the idea that past interactions contributed to Malin 1's morphology, enriched its gas reservoir, and influenced the development of its extended disk, providing insights into the evolution of gLSBGs. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2502_11041 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Exploring the stellar streams and satellites around the giant low surface brightness galaxy Malin 1 Bustos-Espinoza, Roy O. E. Blaña, Matias Galaz, Gaspar Mora, Marcelo Junais Das, Mousumi Barway, Sudhanshu Kumar, Ankit Johnston, Evelyn J. Puzia, Thomas Astrophysics of Galaxies Context. Giant Low Surface Brightness galaxies, such as Malin 1, host extended stellar and gaseous disks exceeding 100 kpc in radius. Their formation and evolution remain debated, with interactions with satellite galaxies and accretion streams proposed as key contributors. Malin 1 has multiple satellites, including Malin 1A, Malin 1B, and the newly reported Malin 1C, along with eM1 at 350 kpc. Additionally, it exhibits two giant stellar streams, the largest extending 200 kpc, likely linked to past interactions. Aims. We investigate the orbital dynamics of Malin 1's satellites and their relationship with the observed stellar streams, testing their consistency with different formation scenarios. Methods. We constructed gravitational potentials using optical and H I rotation curve data, using stellar, gaseous, and dark matter components. We explored a wide parameter space to see if the candidate progenitors of the stellar streams could have originated from past interactions, testing both NFW and isothermal halo profiles. Results. Among ten explored scenarios, seven produced bound orbital solutions. The isothermal halo model, with a virial mass of 3.8 x 10^12 solar masses and a virial radius of approximately 323 kpc, favors bound satellite orbits more than the NFW model (1.7 x 10^12 solar masses). We find that eM1 probably had a pericenter passage 1.3 Gyr ago, Malin 1A around 1.4 Gyr ago, and Malin 1B's leading arm may be experiencing one now. Malin 1C displays both leading and trailing arms. Furthermore, we identify three unbound orbital solutions that could link eM1, Malin 1A, or Malin 1B to the streams. Conclusions. The alignment of satellites and streams supports the idea that past interactions contributed to Malin 1's morphology, enriched its gas reservoir, and influenced the development of its extended disk, providing insights into the evolution of gLSBGs. |
| title | Exploring the stellar streams and satellites around the giant low surface brightness galaxy Malin 1 |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2502.11041 |