SPECTROSCOPIC STUDY OF STAR-FORMING GALAXIES IN FILAMENTS AND THE FIELD AT<i>z</i>∼ 0.5: EVIDENCE FOR ENVIRONMENTAL DEPENDENCE OF ELECTRON DENSITY

Darvish, Behnam; Mobasher, Bahram; Sobral, David; Hemmati, Shoubaneh; Nayyeri, Hooshang; Shivaei, Irene

doi:10.1088/0004-637x/814/2/84

Cited by 61 publications

(116 citation statements)

References 224 publications

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“…The effects of the environment on the metal content of latetype galaxies has been debated for a long time (Shields et al 1991;Vílchez 1995;Skillman et al 1996;Pilyugin et al 2002;Mouhcine et al 2007;Ellison et al 2009;Hughes et al 2013;Peng & Maiolino 2014;Pustilnik et al 2013;Nicholls et al 2014;Darvish et al 2015;Kacprzak et al 2015;Kreckel et al 2015;Shimakawa et al 2015;Valentino et al 2015, among many others).…”

Section: Discussionmentioning

confidence: 99%

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On the influence of the environment on galactic chemical abundances

Pilyugin¹,

Grebel²,

Zinchenko³

et al. 2016

Mon. Not. R. Astron. Soc.

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We examine the influence of the environment on the chemical abundances of late-type galaxies with masses of 10 9.1 M ⊙ -10 11 M ⊙ using data from the Sloan Digital Sky Survey (SDSS). We find that the environmental influence on galactic chemical abundances is strongest for galaxies with masses of 10 9.1 M ⊙ to 10 9.6 M ⊙ . The galaxies in the densest environments may exceed the average oxygen abundances by about ∼ 0.05 dex (the median value of the overabundances for 101 galaxies in the densest environments) and show higher abundances in nitrogen by about ∼ 0.1. The abundance excess decreases with increasing galaxy mass and with decreasing environmental density. Since only a small fraction of late-type galaxies is located in high-density environments these galaxies do not have a significant influence on the general X/H -M relation. The metallicity -mass relations for isolated galaxies and for galaxies with neighbours are very similar. The mean shift of non-isolated galaxies around the metallicity -mass relation traced by the isolated galaxies is less than ∼ 0.01 dex for oxygen and less than ∼ 0.02 dex for nitrogen. The scatter in the galactic chemical abundances is large for any number of neighbour galaxies (at any environmental density), i.e., galaxies with both enhanced and reduced abundances can be found at any environmental density. This suggests that environmental effects do not play a key role in evolution of late-type galaxies as was also concluded in some of the previous studies.

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Section: Discussionmentioning

confidence: 99%

“…Darvish et al (2015) studied the properties of a sample of 28 starforming galaxies in a large filamentary structure at z ∼ 0.53 (using Keck spectroscopic data) and compared them with a control sample of 30 field galaxies. They found that, on average, star-forming galaxies in filaments are more metal-enriched (∼ 0.1 -0.15 dex).…”

Section: Discussionmentioning

confidence: 99%

On the influence of the environment on galactic chemical abundances

Pilyugin¹,

Grebel²,

Zinchenko³

et al. 2016

Mon. Not. R. Astron. Soc.

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“…For example, the "galactic conformity"-the observation that satellites are more likely to be quenched around quiescent centrals than star-forming (SF) ones-has been found on both small and larger megaparsec scales (Weinmann et al 2006;Kauffmann et al 2013;Hartley et al 2015;Hearin et al 2015;Berti et al 2017;Hatfield & Jarvis 2016;Kawinwanichakij et al 2016), suggesting the role of the large-scale gravitational tidal field on galaxy properties. Moreover, several observations have found that the star formation activity and other galaxy properties depend on the large-scale cosmic web (Fadda et al 2008;Porter et al 2008;Biviano et al 2011;Darvish et al 2014;Ricciardelli et al 2014;Chen et al 2016b;Darvish et al 2015a;Guo et al 2015;Alpaslan et al 2016;Pandey & Sarkar 2016), whereas others have seen no or at best a weak dependence between the properties of galaxies and the global cosmic web environments (Alpaslan et al 2015;Eardley et al 2015;Filho et al 2015;Penny et al 2015;Alonso et al 2016;Beygu et al 2016;Brouwer et al 2016;Vulcani et al 2016a).…”

Section: For Reviews)mentioning

confidence: 99%

“…In pilot studies to target the cosmic web, Darvish et al (2014Darvish et al ( , 2015a used the 2D version of the MMF algorithm and applied it to potential large-scale structures in the COSMOS at z∼0.83 and 0.53. The z ∼ 0.83 structure clearly showed a filament linking several clusters and groups and was traced by the distribution of Hα emitters (Sobral et al 2011;Darvish et al 2014).…”

Section: For Reviews)mentioning

confidence: 99%

Cosmic Web of Galaxies in the COSMOS Field: Public Catalog and Different Quenching for Centrals and Satellites

Darvish

Mobasher

Martin

et al. 2017

ApJ

Self Cite

103

170

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We use a mass complete (log(  M M )  9.6) sample of galaxies with accurate photometric redshifts in the COSMOS field to construct the density field and the cosmic web to z=1.2. The comic web extraction relies on the density field Hessian matrix and breaks the density field into clusters, filaments, and the field. We provide the density field and cosmic web measures to the community. We show that at z0.8, the median star formation rate (SFR) in the cosmic web gradually declines from the field to clusters and this decline is especially sharp for satellites (∼1 dex versus ∼0.5 dex for centrals). However, at z0.8, the trend flattens out for the overall galaxy population and satellites. For star-forming (SF) galaxies only, the median SFR is constant at z0.5 but declines by ∼0.3-0.4 dex from the field to clusters for satellites and centrals at z0.5. We argue that for satellites, the main role of the cosmic web environment is to control their SF fraction, whereas for centrals, it is mainly to control their overall SFR at z0.5 and to set their fraction at z0.5. We suggest that most satellites experience a rapid quenching mechanism as they fall from the field into clusters through filaments, whereas centrals mostly undergo a slow environmental quenching at z0.5 and a fast mechanism at higher redshifts. Our preliminary results highlight the importance of the large-scale cosmic web on galaxy evolution.

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“…From a theoretical point of view, Aragon-Calvo et al (2016) showed that the star formation quenching in galaxies can be explained as the influence of filamentary environment, due to the non-linear interaction of the cosmic web. Meanwhile, a variety of case studies of particular filamentary structures have reported an increased fraction of star-forming galaxies (Fadda et al 2008;Tran et al 2009;Biviano et al 2011;Darvish et al 2014), and higher metallicities and lower electron densities (Darvish et al 2015) in filaments with respect to field environments. Unfortunately, most of these studies encompass a relatively small number of galaxies and limited volumes, making them sensitive to the cosmic variance.…”

Section: Introductionmentioning

confidence: 99%

From voids to filaments: environmental transformations of galaxies in the SDSS

Kuutma

Tamm

Tempel

2017

A&A

101

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Aims. We investigate the impact of filament and void environments on galaxies, looking for residual effects beyond the known relations with environment density. Methods. We quantified the host environment of galaxies as the distance to the spine of the nearest filament, and compared various galaxy properties within 12 bins of this distance. We considered galaxies up to 10 h −1 Mpc from filaments, i.e. deep inside voids. The filaments were defined by a point process (the Bisous model) from the Sloan Digital Sky Survey data release 10. In order to remove the dependence of galaxy properties on the environment density and redshift, we applied weighting to normalise the corresponding distributions of galaxy populations in each bin. Results. After the normalisation with respect to environment density and redshift, several residual dependencies of galaxy properties still remain. Most notable is the trend of morphology transformations, resulting in a higher elliptical-to-spiral ratio while moving from voids towards filament spines, bringing along a corresponding increase in the g − i colour index and a decrease in star formation rate. After separating elliptical and spiral subsamples, some of the colour index and star formation rate evolution still remains. The mentioned trends are characteristic only for galaxies brighter than about M r = −20 mag. Unlike some other recent studies, we do not witness an increase in the galaxy stellar mass while approaching filaments. The detected transformations can be explained by an increase in the galaxy-galaxy merger rate and/or the cut-off of extragalactic gas supplies (starvation) near and inside filaments. Conclusions. Unlike voids, large-scale galaxy filaments are not a mere density enhancement, but have their own specific impact on the constituent galaxies, reducing the star formation rate and raising the chances of elliptical morphology also at a fixed environment density level.

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SPECTROSCOPIC STUDY OF STAR-FORMING GALAXIES IN FILAMENTS AND THE FIELD ATz∼ 0.5: EVIDENCE FOR ENVIRONMENTAL DEPENDENCE OF ELECTRON DENSITY

Cited by 61 publications

References 224 publications

On the influence of the environment on galactic chemical abundances

On the influence of the environment on galactic chemical abundances

Cosmic Web of Galaxies in the COSMOS Field: Public Catalog and Different Quenching for Centrals and Satellites

From voids to filaments: environmental transformations of galaxies in the SDSS

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