The effect of cosmic web filaments on galaxy properties in the RESOLVE and ECO surveys

Hoosain, Munira; Blyth, Sarah-L; Skelton, Rosalind E; Kannappan, Sheila J; Stark, David V; Eckert, Kathleen D; Hutchens, Zackary L; Carr, Derrick S; Kraljic, Katarina

doi:10.1093/mnras/stae174

Cited by 5 publications

(1 citation statement)

References 75 publications

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“…The green valley is assigned as the region between where the red Gaussian is 10× the blue Gaussian and vice versa. While tangent functions provide smoother divisions, we used line segments to create the u − r divisions for ECO galaxies for consistency with Moffett et al (2015) and Hoosain et al (2024). As in these studies, our line segments extend horizontally both below the lowest-mass bin and above the highest-mass bin.…”

Section: Sf and Color Assignmentsmentioning

confidence: 99%

Identification and Quenching of Nugget Galaxies in the RESOLVE Survey at z = 0

Carr,

Kannappan,

Norris

et al. 2024

ApJ

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We present a complete census of candidate nuggets, i.e., dense galaxies likely formed by compaction with intense gas influx, within the volume-limited redshift z ∼ 0 REsolved Spectroscopy Of a Local VolumE (RESOLVE) survey. These nuggets span all evolutionary stages and 3 orders of magnitude in stellar mass (M * ∼ 108 to 1011 M ⊙) from the dwarf to the giant regime. We develop selection criteria for our z ∼ 0 nugget candidates based on structure and introduce the use of environmental criteria to eliminate nugget-like objects with suspected non-compaction origins. The resulting z ∼ 0 nuggets follow expectations with respect to structure (i.e., density, size), population frequency, and likely origins. We show that the properties of our nugget census are consistent with permanent quenching above the gas-richness threshold scale (halo mass M halo ∼ 1011.4 M ⊙), cyclic temporary quenching below the threshold scale, and feedback from active galactic nuclei (AGN) assisting in permanent quenching. As predicted in simulations, most nuggets quench within a halo mass range of M halo ∼ 1011.45 to 1011.9 M ⊙. We find ∼0.29 dex scatter around the star-forming main sequence for candidate blue nuggets below the threshold scale, which is consistent with temporary quenching as seen in simulations. A transitional population of green nuggets appears above the threshold scale. AGN also become more common in nuggets above this scale, and we see a likely AGN excess in nuggets versus comparably selected non-nuggets. Our results provide the first observational confirmation of the mass-dependent, AGN-mediated shift from cyclic quenching to halo quenching in nuggets.

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Section: Sf and Color Assignmentsmentioning

confidence: 99%

Identification and Quenching of Nugget Galaxies in the RESOLVE Survey at z = 0

Carr,

Kannappan,

Norris

et al. 2024

ApJ

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Large-scale structure around the Fornax-Eridanus complex

Raj,

Awad,

Peletier

et al. 2024

A&A

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Our objectives are to map the filamentary network around the Fornax-Eridanus complex and probe the influence of the local environment on galaxy morphology. We employed the novel machine-learning tool, named, 1-Dimensional, Recovery, Extraction, and Analysis of Manifolds (1-DREAM) to detect and model filaments around the Fornax cluster. We then used the morphology-density relation of galaxies to examine the variation in the galaxies' morphology with respect to their distance from the central axis of the detected filaments. We detected 27 filaments that vary in length and galaxy-number density around the Fornax-Eridanus complex. We find that 81<!PCT!> of galaxies in our catalogue belong to filaments and 19<!PCT!> of galaxies are located outside filaments. The filaments around the Fornax-Eridanus complex showcase a variety of environments:\ some filaments encompass groups and clusters, while others are only inhabited by galaxies in pristine filamentary environments. In this context, we reveal a well-known structure, namely:\ the Fornax Wall, which passes through the Dorado group, Fornax cluster, and Eridanus supergroup. With regard to the morphology of galaxies, we find that early-type galaxies (ETGs) populate high-density filaments and high-density regions of the Fornax Wall. Furthermore, the fraction of the ETG-population decreases as the distance to the central axis of the filament increases. The fraction of late-type galaxies (LTGs; 8<!PCT!>) is lower than that of ETGs (12<!PCT!>) at 0.5 Mpc/$h$ from the filament spine. Of the total galaxy population in filaments around the Fornax-Eridanus complex, sim 7<!PCT!> are ETGs and sim 24<!PCT!> are LTGs located in pristine environments of filaments, while sim 27<!PCT!> are ETGs and sim 42<!PCT!> are LTGs in groups and clusters within filaments. Among the galaxies in the filamentary network around the Fornax-Eridanus complex, 44<!PCT!> of them belong to the Fornax Wall. This study reveals the cosmic web around the Fornax cluster, which exhibits a variety of filamentary environments. With this, our research asserts that filamentary environments are heterogeneous in nature. When investigating the role of the environment on galaxy morphology, it is essential to consider both the local number-density and a galaxy's proximity to the filament spine (i.e. the filament core). Within this framework, we ascribe the observed morphological segregation in the Fornax Wall to the pre-processing of galaxies among groups embedded in it.

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Virgo Filaments

Zakharova,

Vulcani,

De Lucia

et al. 2024

A&A

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Galaxy evolution depends on the environment in which galaxies are located. The various physical processes (ram-pressure stripping, tidal interactions, etc.) that are able to affect the gas content in galaxies have different efficiencies in different environments. In this work, we examine the gas (atomic HI and molecular H2 ) content of local galaxies inside and outside clusters, groups, and filaments as well as in isolation using a combination of observational and simulated data. We exploited a catalogue of galaxies in the Virgo cluster (including the surrounding filaments and groups) and compared the data against the predictions of the Galaxy Evolution and Assembly (GAEA) semi-analytic model, which has explicit prescriptions for partitioning the cold gas content in its atomic and molecular phases. We extracted from the model both a mock catalogue that mimics the observational biases and one not tailored to observations in order to study the impact of observational limits on the results and predict trends in regimes not covered by the current observations. The observations and simulated data show that galaxies within filaments exhibit intermediate cold gas content between galaxies in clusters and in isolation. The amount of HI is typically more sensitive to the environment than H2 and low-mass galaxies ($ M star M sun < 10$) are typically more affected than their massive ($ M star M sun > 10$) counterparts. Considering only model data, we identified two distinct populations among filament galaxies present in similar proportions: those simultaneously lying in groups and isolated galaxies. The former has properties more similar to cluster and group galaxies, and the latter is more similar to those of field galaxies. We therefore did not detect the strong effects of filaments themselves on the gas content of galaxies, and we ascribe the results to the presence of groups in filaments.

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The effect of cosmic web filaments on galaxy properties in the RESOLVE and ECO surveys

Cited by 5 publications

References 75 publications

Identification and Quenching of Nugget Galaxies in the RESOLVE Survey at z = 0

Identification and Quenching of Nugget Galaxies in the RESOLVE Survey at z = 0

Large-scale structure around the Fornax-Eridanus complex

Virgo Filaments

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