Estimating the Masses of Supercluster-scale Filaments from Redshift Dispersions
We present a strategy for estimating the mass per unit length along supercluster-scale filaments that are oriented across the sky, based on mock redshift surveys of 264 filaments from the Millennium simulation. In our fiducial scenario, we place each simulated filament at a distance of 300 Mpc, perp...
Saved in:
| Main Authors: | , , , |
|---|---|
| Format: | Article |
| Language: | English |
| Published: |
IOP Publishing
2024-01-01
|
| Series: | The Astrophysical Journal |
| Subjects: | |
| Online Access: | https://doi.org/10.3847/1538-4357/ad8ba8 |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1846149875758006272 |
|---|---|
| author | Mary Crone Odekon Trevor W. Viscardi Jake Rabinowitz Brandon Young |
| author_facet | Mary Crone Odekon Trevor W. Viscardi Jake Rabinowitz Brandon Young |
| author_sort | Mary Crone Odekon |
| collection | DOAJ |
| description | We present a strategy for estimating the mass per unit length along supercluster-scale filaments that are oriented across the sky, based on mock redshift surveys of 264 filaments from the Millennium simulation. In our fiducial scenario, we place each simulated filament at a distance of 300 Mpc, perpendicular to the line of sight, and calculate the redshift dispersion using galaxies with magnitudes r < 19.5. Some regions are dynamically complicated in ways that interfere with finding a simple relationship between dispersion σ and linear mass density μ . However, by examining individual overlapping segments along the filaments, we find a relationship that allows us to successfully predict $\mathrm{log}\mu $ from $\mathrm{log}\sigma $ with a scatter of about ±0.20 dex, for ∼70% of the regions along filaments. This relationship is robust to changes in the distance to the filament if the physical segment length and the absolute magnitude for galaxy selection are held constant. The relationship between redshift dispersion and mass is similar to that obtained for a simple analytical model where filaments are dynamically relaxed, and we examine the possibility that the galaxies are indeed relaxed within the gravitational potential of the filament. We find that this is not the case; galaxy dynamics are strongly affected by infall to the filament and by orbits within groups and clusters. |
| format | Article |
| id | doaj-art-4188445ccd324bae920146b11bc865c2 |
| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj-art-4188445ccd324bae920146b11bc865c22024-11-29T09:53:55ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-0197712810.3847/1538-4357/ad8ba8Estimating the Masses of Supercluster-scale Filaments from Redshift DispersionsMary Crone Odekon0https://orcid.org/0000-0003-0162-1012Trevor W. Viscardi1https://orcid.org/0000-0001-9064-1132Jake Rabinowitz2https://orcid.org/0000-0003-0109-9308Brandon Young3https://orcid.org/0009-0001-9736-5596Department of Physics, Skidmore College , Saratoga Springs, NY 12866, USA ; mcrone@skidmore.edu, twviscardi@gmail.com, byoung@alumni.skidmore.eduDepartment of Physics, Skidmore College , Saratoga Springs, NY 12866, USA ; mcrone@skidmore.edu, twviscardi@gmail.com, byoung@alumni.skidmore.eduDepartment of Physics, Columbia University , USA ; jar2334@columbia.eduDepartment of Physics, Skidmore College , Saratoga Springs, NY 12866, USA ; mcrone@skidmore.edu, twviscardi@gmail.com, byoung@alumni.skidmore.eduWe present a strategy for estimating the mass per unit length along supercluster-scale filaments that are oriented across the sky, based on mock redshift surveys of 264 filaments from the Millennium simulation. In our fiducial scenario, we place each simulated filament at a distance of 300 Mpc, perpendicular to the line of sight, and calculate the redshift dispersion using galaxies with magnitudes r < 19.5. Some regions are dynamically complicated in ways that interfere with finding a simple relationship between dispersion σ and linear mass density μ . However, by examining individual overlapping segments along the filaments, we find a relationship that allows us to successfully predict $\mathrm{log}\mu $ from $\mathrm{log}\sigma $ with a scatter of about ±0.20 dex, for ∼70% of the regions along filaments. This relationship is robust to changes in the distance to the filament if the physical segment length and the absolute magnitude for galaxy selection are held constant. The relationship between redshift dispersion and mass is similar to that obtained for a simple analytical model where filaments are dynamically relaxed, and we examine the possibility that the galaxies are indeed relaxed within the gravitational potential of the filament. We find that this is not the case; galaxy dynamics are strongly affected by infall to the filament and by orbits within groups and clusters.https://doi.org/10.3847/1538-4357/ad8ba8Large-scale structure of the universeDark matter distributionRedshift surveysGalaxies |
| spellingShingle | Mary Crone Odekon Trevor W. Viscardi Jake Rabinowitz Brandon Young Estimating the Masses of Supercluster-scale Filaments from Redshift Dispersions The Astrophysical Journal Large-scale structure of the universe Dark matter distribution Redshift surveys Galaxies |
| title | Estimating the Masses of Supercluster-scale Filaments from Redshift Dispersions |
| title_full | Estimating the Masses of Supercluster-scale Filaments from Redshift Dispersions |
| title_fullStr | Estimating the Masses of Supercluster-scale Filaments from Redshift Dispersions |
| title_full_unstemmed | Estimating the Masses of Supercluster-scale Filaments from Redshift Dispersions |
| title_short | Estimating the Masses of Supercluster-scale Filaments from Redshift Dispersions |
| title_sort | estimating the masses of supercluster scale filaments from redshift dispersions |
| topic | Large-scale structure of the universe Dark matter distribution Redshift surveys Galaxies |
| url | https://doi.org/10.3847/1538-4357/ad8ba8 |
| work_keys_str_mv | AT marycroneodekon estimatingthemassesofsuperclusterscalefilamentsfromredshiftdispersions AT trevorwviscardi estimatingthemassesofsuperclusterscalefilamentsfromredshiftdispersions AT jakerabinowitz estimatingthemassesofsuperclusterscalefilamentsfromredshiftdispersions AT brandonyoung estimatingthemassesofsuperclusterscalefilamentsfromredshiftdispersions |