The impact of the connectivity of the cosmic web on the physical properties of galaxies at its nodes

Kraljic, Katarina; Pichon, Christophe; Codis, Sandrine; Laigle, C.; Davé, Romeel; Dubois, Yohan; Hwang, Ho Seong; Pogosyan, D.; Arnouts, S.; Devriendt, Julien; Musso, Marcello; Peirani, Sébastien; Slyz, Adrianne; Treyer, Marie

doi:10.1093/mnras/stz3319

Cited by 61 publications

(51 citation statements)

References 90 publications

(108 reference statements)

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“…Large-scale models of the ΛCDM Universe predict a structure made of sheets and filaments of dark matter arranged in a cosmic web. The gas that we have characterized in this review -largely found within galaxy halos -is affected by the environment of those halos (Kraljic et al 2019). The ionized gas needed to resupply the neutral and molecular gas consumed by star formation (Figure 5) is ultimately drawn from the filaments within which galaxies are embedded.…”

Section: Pushing From the Global To The Localmentioning

confidence: 99%

The Cosmic Baryon and Metal Cycles

Péroux

Howk

2020

Annu. Rev. Astron. Astrophys.

266

200

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Characterizing the relationship between stars, gas, and metals in galaxies is a critical component of understanding the cosmic baryon cycle. We compile contemporary censuses of the baryons in collapsed structures and their chemical make-up and dust content. We show the following: ▪ The HI mass density of the Universe is well determined to redshifts z≈5 and shows minor evolution with time. New observations of molecular hydrogen reveal its evolution mirrors that of the global star-formation rate density, implying a universal cosmic molecular gas depletion timescale. The low-redshift decline of the star-formation history is thus driven by the lack of molecular gas supply due to a drop in net accretion rate related to the decreased growth of dark matter halos. ▪ The metal mass density in cold gas ( T≲104 K) contains virtually all the metals produced by stars for z≳2.5. At lower redshifts, the contributors to the total amount of metals are more diverse; at z < 1, most of the observed metals are bound in stars. Overall, there is little evidence for a “missing metals problem” in modern censuses. ▪ We characterize the dust content of neutral gas over cosmic time, finding the dust-to-gas and dust-to-metals ratios fall with decreasing metallicity. We calculate the cosmological dust mass density in the neutral gas up to z≈5. There is good agreement between multiple tracers of the dust content of the Universe. Expected final online publication date for the Annual Review of Astronomy and Astrophysics, Volume 58 is August 18, 2020. Please see http://www.annualreviews.org/page/journal/pubdates for revised estimates.

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Section: Pushing From the Global To The Localmentioning

confidence: 99%

The Cosmic Baryon and Metal Cycles

Péroux

Howk

2020

Annu. Rev. Astron. Astrophys.

266

200

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“…Connectivity can be predicted theoretically; Codis et al (2018) showed that on average, cluster connectivity depends on cluster mass and richness. Connectivity of poor groups is lower than that of rich groups (see also Darragh Ford et al 2019;Kraljic et al 2020;Gouin et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Multiscale cosmic web detachments, connectivity, and preprocessing in the supercluster SCl A2142 cocoon

Einasto

Deshev

Tenjes

et al. 2020

A&A

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Context. Superclusters of galaxies and their surrounding low-density regions (cocoons) represent dynamically evolving environments in which galaxies and their systems form and evolve. While evolutionary processes of galaxies in dense environments are extensively studied at present, galaxy evolution in low-density regions has received less attention. Aims. We study the properties, connectivity, and galaxy content of groups and filaments in the A2142 supercluster (SCl A2142) cocoon to understand the evolution of the supercluster with its surrounding structures and the galaxies within them. Methods. We calculated the luminosity-density field of SDSS galaxies and traced the SCl A2142 cocoon boundaries by the lowest luminosity-density regions that separate SCl A2142 from other superclusters. We determined galaxy filaments and groups in the cocoon and analysed the connectivity of groups, the high density core (HDC) of the supercluster, and the whole of the supercluster. We compared the distribution and properties of galaxies with different star-formation properties in the supercluster and in the cocoon. Results. The supercluster A2142 and the long filament that is connected to it forms the longest straight structure in the Universe detected so far, with a length of approximately 75 h −1 Mpc. The connectivity of the cluster A2142 and the whole supercluster is C = 6 − 7; poor groups exhibit C = 1 − 2. Long filaments around the supercluster's main body are detached from it at the turnaround region. Among various local and global environmental trends with regard to the properties of galaxies and groups, we find that galaxies with very old stellar populations lie in systems across a wide range of richness from the richest cluster to poorest groups and single galaxies. They lie even at local densities as low as D1 < 1 in the cocoon and up to D1 > 800 in the supercluster. Recently quenched galaxies lie in the cocoon mainly in one region and their properties are different in the cocoon and in the supercluster. The star-formation properties of single galaxies are similar across all environments. Conclusions. The collapsing main body of SCl A2142 with the detached long filaments near it are evidence of an important epoch in the supercluster evolution. There is a need for further studies to explore possible reasons behind the similarities between galaxies with very old stellar populations in extremely different environments, as well as mechanisms for galaxy quenching at very low densities. The presence of long, straight structures in the cosmic web may serve as a test for cosmological models.

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“…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%

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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The impact of the connectivity of the cosmic web on the physical properties of galaxies at its nodes

Cited by 61 publications

References 90 publications

The Cosmic Baryon and Metal Cycles

The Cosmic Baryon and Metal Cycles

Multiscale cosmic web detachments, connectivity, and preprocessing in the supercluster SCl A2142 cocoon

Characterising filaments in the SDSS volume from the galaxy distribution

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