Filaments in observed and mock galaxy catalogues

Stoica, Radu; Martínez, V. J.; Saar, E.

doi:10.1051/0004-6361/200912823

Cited by 63 publications

(73 citation statements)

References 44 publications

(60 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This algorithm provides a quantitative classification which agrees with the visual impression of the cosmic web and is based on a robust and well-defined mathematical scheme. A detailed description of the Bisous model is given in Stoica et al (2007Stoica et al ( , 2010 and Tempel et al (2014b); for convenience, a brief description is given below. The marked point process we propose for filament detection is different from the ones already used in cosmology.…”

Section: Bisous Model: Extracting Filaments From Galaxy Distributionmentioning

confidence: 99%

Galaxy filaments as pearl necklaces

Tempel

Kipper

Saar

et al. 2014

A&A

Self Cite

View full text Add to dashboard Cite

Context. Galaxies in the Universe form chains (filaments) that connect groups and clusters of galaxies. The filamentary network includes nearly half of the galaxies and is visually the most striking feature in cosmological maps. Aims. We study the distribution of galaxies along the filamentary network, trying to find specific patterns and regularities. Methods. Galaxy filaments are defined by the Bisous model, a marked point process with interactions. We use the two-point correlation function and the Rayleigh Z-squared statistic to study how galaxies and galaxy groups are distributed along the filaments. Results. We show that galaxies and groups are not uniformly distributed along filaments, but tend to form a regular pattern. The characteristic length of the pattern is around 7 h −1 Mpc. A slightly smaller characteristic length 4 h −1 Mpc can also be found, using the Z-squared statistic. Conclusions. We find that galaxy filaments in the Universe are like pearl necklaces, where the pearls are galaxy groups distributed more or less regularly along the filaments. We propose that this well-defined characteristic scale could be used to test various cosmological models and to probe environmental effects on the formation and evolution of galaxies.Key words. methods: numerical -methods: observational -large-scale structure of Universe IntroductionMany cosmological probes have been developed and used to estimate the parameters of the cosmological models describing our Universe. Most of them rely on some aspects of the large-scale structure. The most common probe used to quantify galaxy clustering is the two-point correlation function which was first used decades ago (Davis & Geller 1976;Groth & Peebles 1977;Davis et al. 1988;Hamilton 1988;White et al. 1988;Boerner et al. 1989;Einasto 1991) It is well known that galaxy filaments are visually the most dominant structures in the galaxy distribution, being part of the so-called cosmic network (Jõeveer et al. 1978;Bond et al. 1996). Presumably, nearly half (∼40%) of the galaxies (or mass in simulations) are located in filaments. This number is based on morphological or dynamical classification of the cosmic web (e.g. Jasche et al. 2010;Tempel et al. 2014b;Cautun et al. 2014). Properties of the three-point correlation function also indicate that galaxies tend to populate filamentary structures (Guo et al. 2014a) and, indeed, filaments have been found between galaxy clusters (e.g. Dietrich et al. 2012). Tempel et al. (2014a) show Appendices are available in electronic form at

show abstract

Section: Bisous Model: Extracting Filaments From Galaxy Distributionmentioning

confidence: 99%

Galaxy filaments as pearl necklaces

Tempel

Kipper

Saar

et al. 2014

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…Stoica et al 2010;Bond et al 2010;Aragón-Calvo et al 2010). Many of the algorithms make use of the fact that filaments are the bridges that connect systems of galaxies (Pimbblet et al 2004;Pimbblet 2005;Colberg et al 2005;González & Padilla 2010;Smith et al 2012;Zhang et al 2013;Alpaslan et al 2014).…”

Section: Introductionmentioning

confidence: 99%

Galaxies infalling into groups: filaments versus isotropic infall

Martínez

Muriel

Coenda

2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We perform a comparative analysis of the properties of galaxies infalling into groups classifying them accordingly to whether they are: falling along filamentary structures; or they are falling isotropically. For this purpose, we identify filamentary structures connecting massive groups of galaxies in the SDSS. We perform a comparative analysis of some properties of galaxies in filaments, in the isotropic infall region, in the field, and in groups. We study the luminosity functions (LF) and the dependence of the specific star formation rate (SSFR) on stellar mass, galaxy type, and projected distance to the groups that define the filaments. We find that the LF of galaxies in filaments and in the isotropic infalling region are basically indistinguishable between them, with the possible exception of late-type galaxies. On the other hard, regardless of galaxy type, their LFs are clearly different from that of field or group galaxies. Both of them have characteristic absolute magnitudes and faint end slopes in between the field and group values. More significant differences between galaxies in filaments and in the isotropic infall region are observed when we analyse the SSFR. We find that galaxies in filaments have a systematically higher fraction of galaxies with low SSFR as a function of both, stellar mass and distance to the groups, indicating a stronger quenching of the star formation in the filaments compared to both, the isotropic infalling region, and the field. Our results suggest that some physical mechanisms that determine the differences observed between field galaxies and galaxies in systems, affect galaxies even when they are not yet within the systems.

show abstract

“…COSMIC WEB CLASSIFICATION SCHEME With the rich and complex of the cosmic web, there are numerous methods by which one can classify the elements of the cosmic web. These range from techniques utilizing minimal-spanning trees (Barrow et al 1985;Alpaslan et al 2014), the Candy model (Stoica et al 2005(Stoica et al , 2010, Morse theory-based 'skeleton' methods (Colombi et al 2000;Novikov et al 2006;Sousbie et al 2009;Sousbie 2011), tessellation methods (González & Padilla 2010), multi-scale morphological methods (Aragón-Calvo 6 http://tinyurl.com/lya-tomography-sim-data et al 2007Cautun et al 2013), ridge-finding (Chen et al 2015), and others; (see Cautun et al 2014, for a comprehensive summary).…”

Section: Simulationsmentioning

confidence: 99%

REVEALING THE z ∼ 2.5 COSMIC WEB WITH 3D Lyα FOREST TOMOGRAPHY: A DEFORMATION TENSOR APPROACH

Lee

White

2016

ApJ

View full text Add to dashboard Cite

Studies of cosmological objects should take into account their positions within the cosmic web of largescale structure. Unfortunately, the cosmic web has only been extensively mapped at low-redshifts (z < 1), using galaxy redshifts as tracers of the underlying density field. At z > 1, the required galaxy densities are inaccessible for the foreseeable future, but 3D reconstructions of Lyα forest absorption in closely-separated background QSOs and star-forming galaxies already offer a detailed window into z ∼ 2 − 3 large-scale structure. We quantify the utility of such maps for studying the cosmic web by using realistic z = 2.5 Lyα forest simulations matched to observational properties of upcoming surveys. A deformation tensor-based analysis is used to classify voids, sheets, filaments and nodes in the flux, which is compared to those determined from the underlying dark matter field. We find an extremely good correspondence, with 70% of the volume in the flux maps correctly classified relative to the dark matter web, and 99% classified to within 1 eigenvalue. This compares favorably to the performance of galaxy-based classifiers with even the highest galaxy densities from low-redshift surveys. We find that narrow survey geometries can degrade the cosmic web recovery unless the survey is 60 h −1 Mpc or 1 deg on the sky. We also examine halo abundances as a function of the cosmic web, and find a clear dependence as a function of flux overdensity, but little explicit dependence on the cosmic web. These methods will provide a new window on cosmological environments of galaxies at this very special time in galaxy formation, "high noon", and on overall properties of cosmological structures at this epoch.

show abstract

Filaments in observed and mock galaxy catalogues

Cited by 63 publications

References 44 publications

Galaxy filaments as pearl necklaces

Galaxy filaments as pearl necklaces

Galaxies infalling into groups: filaments versus isotropic infall

REVEALING THE z ∼ 2.5 COSMIC WEB WITH 3D Lyα FOREST TOMOGRAPHY: A DEFORMATION TENSOR APPROACH

Contact Info

Product

Resources

About