The Next Generation Virgo Cluster Survey (NGVS). III. A Catalog of Surface Brightness Fluctuation Distances and the Three-Dimensional Distribution of Galaxies in the Virgo Cluster
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| Format: | Preprint |
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2024
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| author | Cantiello, Michele Blakeslee, John P. Côté, Patrick Raimondo, Gabriella Cuillandre, Jean-Charles Durrell, Patrick R. Gwyn, Stephen Hazra, Nandini Peng, Eric W. Roediger, Joel C. Sánchez-Janssen, Rúben Kurzner, Max |
| author_facet | Cantiello, Michele Blakeslee, John P. Côté, Patrick Raimondo, Gabriella Cuillandre, Jean-Charles Durrell, Patrick R. Gwyn, Stephen Hazra, Nandini Peng, Eric W. Roediger, Joel C. Sánchez-Janssen, Rúben Kurzner, Max |
| contents | The surface brightness fluctuation (SBF) method is a robust and efficient way of measuring distances to galaxies containing evolved stellar populations. Although many recent applications of the method have used space-based imaging, SBF remains a powerful technique for ground-based telescopes. Deep, wide-field imaging surveys with subarsecond seeing enable SBF measurements for numerous nearby galaxies. Using a preliminary calibration, Cantiello et al. (2018) presented SBF distances for 89 bright, mainly early-type galaxies observed in the Next Generation Virgo Cluster Survey (NGVS). Here, we present a refined calibration and SBF distances for 278 galaxies extending several magnitudes fainter than in previous work. The derived distances have uncertainties of 5-12\% depending on the properties of the individual galaxies, and our sample is more than three times larger than any previous SBF study of this region. Virgo has a famously complex structure with numerous subclusters, clouds and groups; we associate individual galaxies with the various substructures and map their three-dimensional spatial distribution. Curiously, subcluster A, centered around M87, appears to have two peaks in distance: the main peak at $\sim$16.5 Mpc and a smaller one at $\sim$19.4 Mpc. Subclusters B and C have distances of $\sim$15.8 Mpc. The W and W' groups form a filament-like structure, extending more than 15~Mpc behind the cluster with a commensurate velocity increase of $\sim$1000 \kms\ along its length. These measurements are a valuable resource for future studies of the relationship between galaxy properties and local environment within a dynamic and evolving region. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2403_16235 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The Next Generation Virgo Cluster Survey (NGVS). III. A Catalog of Surface Brightness Fluctuation Distances and the Three-Dimensional Distribution of Galaxies in the Virgo Cluster Cantiello, Michele Blakeslee, John P. Côté, Patrick Raimondo, Gabriella Cuillandre, Jean-Charles Durrell, Patrick R. Gwyn, Stephen Hazra, Nandini Peng, Eric W. Roediger, Joel C. Sánchez-Janssen, Rúben Kurzner, Max Astrophysics of Galaxies The surface brightness fluctuation (SBF) method is a robust and efficient way of measuring distances to galaxies containing evolved stellar populations. Although many recent applications of the method have used space-based imaging, SBF remains a powerful technique for ground-based telescopes. Deep, wide-field imaging surveys with subarsecond seeing enable SBF measurements for numerous nearby galaxies. Using a preliminary calibration, Cantiello et al. (2018) presented SBF distances for 89 bright, mainly early-type galaxies observed in the Next Generation Virgo Cluster Survey (NGVS). Here, we present a refined calibration and SBF distances for 278 galaxies extending several magnitudes fainter than in previous work. The derived distances have uncertainties of 5-12\% depending on the properties of the individual galaxies, and our sample is more than three times larger than any previous SBF study of this region. Virgo has a famously complex structure with numerous subclusters, clouds and groups; we associate individual galaxies with the various substructures and map their three-dimensional spatial distribution. Curiously, subcluster A, centered around M87, appears to have two peaks in distance: the main peak at $\sim$16.5 Mpc and a smaller one at $\sim$19.4 Mpc. Subclusters B and C have distances of $\sim$15.8 Mpc. The W and W' groups form a filament-like structure, extending more than 15~Mpc behind the cluster with a commensurate velocity increase of $\sim$1000 \kms\ along its length. These measurements are a valuable resource for future studies of the relationship between galaxy properties and local environment within a dynamic and evolving region. |
| title | The Next Generation Virgo Cluster Survey (NGVS). III. A Catalog of Surface Brightness Fluctuation Distances and the Three-Dimensional Distribution of Galaxies in the Virgo Cluster |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2403.16235 |