Galaxy evolution in the metric of the cosmic web

Kraljic, Katarina; Arnouts, S.; Pichon, Christophe; Laigle, C.; Torre, S. de la; Vibert, D.; Cadiou, Corentin; Dubois, Yohan; Treyer, Marie; Schimd, C.; Codis, Sandrine; Lapparent, V. de; Devriendt, Julien; Hwang, Ho Seong; Borgne, D. Le; Malavasi, Nicola; Milliard, B.; Musso, Marcello; Pogosyan, D.; Alpaslan, Mehmet; Bland-Hawthorn, Joss; Wright, Angus H.

doi:10.1093/mnras/stx2638

Cited by 183 publications

(192 citation statements)

References 127 publications

(173 reference statements)

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“…Inside the filaments, the fractions of non-active galaxies and LINERs increase, indicating a possible post-activity phase. A similar result for the star-forming galaxies has been observed by Kraljic et al (2018), for the GAMA spectroscopic survey.…”

Section: Discussionsupporting

confidence: 87%

“…These results are in good agreement with the results presented by Chen et al (2017) for MGS sample from DR7 (Abazajian et al, 2009). Our results are also compatible with those presented by Alpaslan et al (2016) and Kraljic et al (2018), for the GAMA spectroscopic survey, who find similar trends for the filaments found at redshifts z < 0.09 and 0.03 ≤ z ≤ 0.25, respectively.…”

Section: Stellar Mass Profilesupporting

confidence: 94%

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Identification of filamentary structures in the environment of superclusters of galaxies in the Local Universe

Santiago-Bautista

Caretta

Bravo-Alfaro

et al. 2020

A&A

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Context. The characterization of the internal structure of the superclusters of galaxies (walls, filaments and knots where the clusters are located) is paramount for understanding the formation of the Large Scale Structure and for outlining the environment where galaxies evolved in the last gigayears. Aims. (i) To detect the compact regions of high relative density (clusters and rich groups of galaxies); (ii) to map the elongated structures of low relative density (filaments, bridges and tendrils of galaxies); (iii) to characterize the galaxy populations on filaments and study the environmental effects they are subject to. Methods. We employed optical galaxies with spectroscopic redshifts from the SDSS-DR13 inside rectangular boxes encompassing the volumes of a sample of 46 superclusters of galaxies, up to z = 0.15. A virial approximation was applied to correct the positions of the galaxies in the redshift space for the "finger of God" projection effect. Our methodology implements different classical pattern recognition and machine learning techniques (Voronoi tessellation, hierarchical clustering, graph-network theory, minimum spanning trees, among others), pipelined in the Galaxy Systems-Finding algorithm and the Galaxy Filaments-Finding algorithm. Results. We detected in total 2 705 galaxy systems (clusters and groups, of which 159 are new) and 144 galaxy filaments in the 46 superclusters of galaxies. The filaments we detected have a density contrast above 3, with a mean value around 10, a radius of about 2.5 h −1 70 Mpc and lengths between 9 and 130 h −1 70 Mpc. Correlations between the galaxy properties (mass, morphology and activity) and the environment in which they reside (systems, filaments and the dispersed component) suggest that galaxies closer to the skeleton of the filaments are more massive by up to 25% compared to those in the dispersed component; 70% of the galaxies in the filament region present early type morphologies and the fractions of active galaxies (both AGN and SF) seem to decrease as galaxies approach the filament. Conclusions. Our results support the idea that galaxies in filaments are subject to environmental effects leading them to be more massive (probably due to larger rates of both merging and gas accretion), less active both in star formation and nuclear activity, and prone to the density-morphology relation. These results suggest that preprocessing in large scale filaments could have significant effects on galaxy evolution.

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Section: Discussionsupporting

confidence: 87%

Section: Stellar Mass Profilesupporting

confidence: 94%

Identification of filamentary structures in the environment of superclusters of galaxies in the Local Universe

Santiago-Bautista

Caretta

Bravo-Alfaro

et al. 2020

A&A

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“…Galaxies are significantly ∼ 10% more massive, and ∼ 10% less star-forming. This trend is expected since the excess of passive galaxies near the filaments spines was already shown in several studies (e.g., Malavasi et al 2017;Laigle et al 2018;Kraljic et al 2018;Sarron et al 2019). This implies a different ratio of passive over active galaxies with increasing distance to the filaments' spine, producing these gradients.…”

Section: Average Propertiessupporting

confidence: 70%

Filament profiles from WISExSCOS galaxies as probes of the impact of environmental effects

Bonjean

Aghanim

Douspis

et al. 2020

A&A

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The role played by the large-scale structures in the galaxy evolution is not quite well understood yet. In this study, we investigate properties of galaxy in the range 0.1 < z < 0.3 from a value-added version of the WISExSCOS catalogue around cosmic filaments detected with DisPerSE. We have fitted a profile of galaxy over-density around cosmic filaments and found a typical radius of r m = 7.5 ± 0.2 Mpc. We have measured an excess of passive galaxies near the filament's spine, higher than the excess of transitioning and active galaxies. We have also detected SFR and M gradients pointing towards the filament's spine. We have investigated this result and found an M gradient for each type of galaxies: active, transitioning, and passive, and a positive SFR gradient for passive galaxies. We also link the galaxy properties and the gas content in the Cosmic Web. To do so, we have investigated the quiescent fraction f Q profile of galaxies around the cosmic filaments. Based on recent studies about the effect of the gas and of the Cosmic Web on galaxy properties, we have modelled f Q with a β model of gas pressure. The slope obtained here, β = 0.54 ± 0.18, is compatible with the scenario of projected isothermal gas in hydrostatic equilibrium (β = 2/3), and with the profiles of gas fitted in SZ.

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“…This is a natural consequence of the biased distribution: passive galaxies are preferentially in the high-density regions of the CW compared to star-forming galaxies. This segregation effect was recently quantified with respect to filaments in spectroscopic (Malavasi et al 2017;Kraljic et al 2018) and photometric (Laigle et al 2018) surveys. At least at low redshifts, passive galaxies are statistically closer to filaments than active ones at similar stellar mass.…”

Section: Galaxy Typementioning

confidence: 98%

“…The vast majority of galaxies thus lie within the remaining 10% composed of the dense regions distributed in a geometric pattern of walls, filaments, and nodes. The most massive galaxies live preferentially in the nodes (highest density regions), but segregation also occurs in filamentary regions where more massive or passive galaxies are closer to the center of the filaments (Malavasi et al 2017;Kraljic et al 2018).…”

Section: Introductionmentioning

confidence: 99%

PhotoWeb redshift: boosting photometric redshift accuracy with large spectroscopic surveys

Shuntov

Pasquet

Arnouts

et al. 2020

A&A

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Improving distance measurements in large imaging surveys is a major challenge to better reveal the distribution of galaxies on a large scale and to link galaxy properties with their environments. As recently shown, photometric redshifts can be efficiently combined with the cosmic web extracted from overlapping spectroscopic surveys to improve their accuracy. In this paper we apply a similar method using a new generation of photometric redshifts based on a convolution neural network (CNN). The CNN is trained on the SDSS images with the main galaxy sample (SDSS-MGS, r ≤ 17.8) and the GAMA spectroscopic redshifts up to r ∼ 19.8. The mapping of the cosmic web is obtained with 680,000 spectroscopic redshifts from the MGS and BOSS surveys. The redshift probability distribution functions (PDF), which are well calibrated (unbiased and narrow, ≤ 120 Mpc), intercept a few cosmic web structures along the line of sight. Combining these PDFs with the density field distribution provides new photometric redshifts, z web , whose accuracy is improved by a factor of two (i.e., σ ∼ 0.004(1 + z)) for galaxies with r ≤ 17.8. For half of them, the distance accuracy is better than 10 cMpc. The narrower the original PDF, the larger the boost in accuracy. No gain is observed for original PDFs wider than 0.03. The final z web PDFs also appear well calibrated. The method performs slightly better for passive galaxies than star-forming ones, and for galaxies in massive groups since these populations better trace the underlying large-scale structure. Reducing the spectroscopic sampling by a factor of 8 still improves the photometric redshift accuracy by 25%. Finally, extending the method to galaxies fainter than the MGS limit still improves the redshift estimates for 70% of the galaxies, with a gain in accuracy of 20% at low z where the resolution of the cosmic web is the highest. As two competing factors contribute to the performance of the method, the photometric redshift accuracy and the resolution of the cosmic web, the benefit of combining cosmological imaging surveys with spectroscopic surveys at higher redshift remains to be evaluated.

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Galaxy evolution in the metric of the cosmic web

Cited by 183 publications

References 127 publications

Identification of filamentary structures in the environment of superclusters of galaxies in the Local Universe

Identification of filamentary structures in the environment of superclusters of galaxies in the Local Universe

Filament profiles from WISExSCOS galaxies as probes of the impact of environmental effects

PhotoWeb redshift: boosting photometric redshift accuracy with large spectroscopic surveys

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