A comparison of cosmological filaments catalogues

Rost, Agustín; Stasyszyn, Federico; Pereyra, Luis; Martínez, H.

doi:10.1093/mnras/staa320

Cited by 36 publications

(34 citation statements)

References 55 publications

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“…While a comparison of these catalogues is beyond the goal of this work (see e.g. Rost et al 2020) also because very different algorithms were employed, we still qualitatively compare our work with others from the literature. While the sky distribution of filaments appear to be visually similar (see e.g.…”

Section: Qualitative Comparison With the Literaturementioning

confidence: 99%

“…Surveys such as the Two-Degree Field Galaxy Redshift Survey (2dFGRS, Colless et al 2001), the Sloan Digital Sky Survey (SDSS, York et al 2000), the Galaxy And Mass Assembly survey (GAMA, Driver et al 2009), the Vimos Public Extragalactic Redshift Survey (VIPERS, Scodeggio et al 2018), or the COSMOS survey (Scoville et al 2007) have allowed us to obtain statistical samples of filaments and other LSS features. For example, Chen et al (2016) and Tempel et al (2014a) have produced filament catalogues in the SDSS (but see also the works by Aragón Calvo 2007;Sousbie et al 2011;Rost et al 2020;Shuntov et al 2020;Kraljic et al 2020, some of which also used the same algorithm as we used here). Other works such as Kraljic et al (2018) and Alpaslan et al (2014) detected filaments in GAMA, while Malavasi et al (2017) detected filaments in VIPERS.…”

Section: Introductionmentioning

confidence: 99%

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Characterising filaments in the SDSS volume from the galaxy distribution

Malavasi

Aghanim

Douspis

et al. 2020

A&A

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Detecting the large-scale structure of the Universe based on the galaxy distribution and characterising its components is of fundamental importance in astrophysics but is also a difficult task to achieve. Wide-area spectroscopic redshift surveys are required to accurately measure galaxy positions in space that also need to cover large areas of the sky. It is also difficult to create algorithms that can extract cosmic web structures (e.g. filaments). Moreover, these detections will be affected by systematic uncertainties that stem from the characteristics of the survey used (e.g. its completeness and coverage) and from the unique properties of the specific method adopted to detect the cosmic web (i.e. the assumptions it relies on and the free parameters it may employ). For these reasons, the creation of new catalogues of cosmic web features on wide sky areas is important, as this allows users to have at their disposal a well-understood sample of structures whose systematic uncertainties have been thoroughly investigated. In this paper we present the filament catalogues created using the discrete persistent structure extractor tool in the Sloan Digital Sky Survey (SDSS), and we fully characterise them in terms of their dependence on the choice of parameters pertaining to the algorithm, and with respect to several systematic issues that may arise in the skeleton as a result of the properties of the galaxy distribution (such as Finger-of-God redshift distortions and defects of the density field that are due to the boundaries of the survey).

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Section: Qualitative Comparison With the Literaturementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Characterising filaments in the SDSS volume from the galaxy distribution

Malavasi

Aghanim

Douspis

et al. 2020

A&A

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“…To add to the difficulty, different filament-finding algorithms are based on different implicit definitions of these objects. This leads to wide-ranging discrepancies in relation to the nature of identified objects found by the different filament finders (Libeskind et al 2018;Rost et al 2020), including DISPERSE (Sousbie 2011), Semita (Pereyra et al 2019), Nexus (Aragón-Calvo et al 2007;Cautun, van de Weygaert & Jones 2013), or Bisous (Tempel et al 2014). Despite these drawbacks, understanding the large-scale structures of the Universe, and how the galaxies they host evolve, remain key science challenges.…”

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confidence: 99%

the threehundred: the structure and properties of cosmic filaments in the outskirts of galaxy clusters

Rost

Kuchner

Welker

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Galaxy cluster outskirts are described by complex velocity fields induced by diffuse material collapsing towards filaments, gas, and galaxies falling into clusters, and gas shock processes triggered by substructures. A simple scenario that describes the large-scale tidal fields of the cosmic web is not able to fully account for this variety, nor for the differences between gas and collisionless dark matter. We have studied the filamentary structure in zoom-in resimulations centred on 324 clusters from the threehundred project, focusing on differences between dark and baryonic matter. This paper describes the properties of filaments around clusters out to five R200, based on the diffuse filament medium where haloes had been removed. For this, we stack the remaining particles of all simulated volumes to calculate the average profiles of dark matter and gas filaments. We find that filaments increase their thickness closer to nodes and detect signatures of gas turbulence at a distance of ${\sim}2 \rm {{{~h^{-1}\,{\rm Mpc}}}}$ from the cluster. These are absent in dark matter. Both gas and dark matter collapse towards filament spines at a rate of ${\sim}200 \,\rm {km ~ s^{-1}\, h^{-1}}$. We see that gas preferentially enters the cluster as part of filaments, and leaves the cluster centre outside filaments. We further see evidence for an accretion shock just outside the cluster. For dark matter, this preference is less obvious. We argue that this difference is related to the turbulent environment. This indicates that filaments act as highways to fuel the inner regions of clusters with gas and galaxies.

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“…Velocity flows in these exceptional regions in the Universe deserve a thorough discussion. In Rost et al (2020a) we do exactly that and investigate velocity flows of gas and dark matter around clusters in much greater detail, using the same simulations.…”

Section: The Velocity Field Of Filament Galaxiesmentioning

confidence: 99%

“…Filaments connected to clusters are only one aspect of a complex multiscale picture that encompasses thick filaments as well as thin tendrils on scales of a few Mpc up to 100 Mpc and more, as well as sheetlike membranes easily mistaken as filaments in projection. The last decade has seen a number of excellent methods to identify and classify features of the cosmic web (e.g., Aragón-Calvo et al 2007;Sousbie 2011;Cautun et al 2012;Courtois et al 2013;Tempel et al 2014;Falck & Neyrinck 2015), each designed to tackle specific problems to be applied to different kinds of data and thus disagreements are understandable and well documented (e.g., Libeskind et al 2017;Rost et al 2020b). Structure finding methods are successfully being applied to simulated and observed datasets alike, including photometric and spectroscopic surveys such as SDSS (Tempel et al 2013;Kuutma et al 2017;Chen et al 2016;Malavasi et al 2020), COS-MOS (Darvish et al 2017;Laigle et al 2017) and GAMA (Kraljic et al 2018;Welker et al 2019) amongst others (Malavasi et al 2016;Sarron et al 2019;Santiago-Bautista et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Cosmic filaments in galaxy cluster outskirts: quantifying finding filaments in redshift space

Kuchner

Aragón-Salamanca

Rost

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Inferring line-of-sight distances from redshifts in and around galaxy clusters is complicated by peculiar velocities, a phenomenon known as the ”Fingers of God” (FoG). This presents a significant challenge for finding filaments in large observational data sets as these artificial elongations can be wrongly identified as cosmic web filaments by extraction algorithms. Upcoming targeted wide-field spectroscopic surveys of galaxy clusters and their infall regions such as the WEAVE Wide-Field Cluster Survey motivate our investigation of the impact of FoG on finding filaments connected to clusters. Using zoom-in resimulations of 324 massive galaxy clusters and their outskirts from The ThreeHundred project, we test methods typically applied to large-scale spectroscopic data sets. This paper describes our investigation of whether a statistical compression of the FoG of cluster centres and galaxy groups can lead to correct filament extractions in the cluster outskirts. We find that within 5R200 (∼15 h−1Mpc) statistically correcting for FoG elongations of virialized regions does not achieve reliable filament networks compared to reference filament networks based on true positions. This is due to the complex flowing motions of galaxies towards filaments in addition to the cluster infall, which overwhelm the signal of the filaments relative to the volume we probe. While information from spectroscopic redshifts is still important to isolate the cluster regions, and thereby reduce background and foreground interlopers, we expect future spectroscopic surveys of galaxy cluster outskirts to rely on 2D positions of galaxies to extract cosmic filaments.

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A comparison of cosmological filaments catalogues

Cited by 36 publications

References 55 publications

Characterising filaments in the SDSS volume from the galaxy distribution

Characterising filaments in the SDSS volume from the galaxy distribution

the threehundred: the structure and properties of cosmic filaments in the outskirts of galaxy clusters

Cosmic filaments in galaxy cluster outskirts: quantifying finding filaments in redshift space

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