Home > Research > Publications & Outputs > Spectroscopic study of star-forming galaxies in...

Associated organisational unit

Electronic data

  • 1510.05009

    Accepted author manuscript, 1.39 MB, PDF document

    Available under license: CC BY: Creative Commons Attribution 4.0 International License

Links

Text available via DOI:

View graph of relations

Spectroscopic study of star-forming galaxies in filaments and the field at $z\sim$0.5: evidence for environmental dependence of electron density

Research output: Contribution to journalJournal articlepeer-review

Published

Standard

Spectroscopic study of star-forming galaxies in filaments and the field at $z\sim$0.5 : evidence for environmental dependence of electron density. / Darvish, Behnam; Mobasher, Bahram; Sobral, David; Hemmati, Shoubaneh; Nayyeri, Hooshang; Shivaei, Irene.

In: The Astrophysical Journal, Vol. 814, No. 2, 84, 01.12.2015.

Research output: Contribution to journalJournal articlepeer-review

Harvard

APA

Vancouver

Author

Darvish, Behnam ; Mobasher, Bahram ; Sobral, David ; Hemmati, Shoubaneh ; Nayyeri, Hooshang ; Shivaei, Irene. / Spectroscopic study of star-forming galaxies in filaments and the field at $z\sim$0.5 : evidence for environmental dependence of electron density. In: The Astrophysical Journal. 2015 ; Vol. 814, No. 2.

Bibtex

@article{2b6c68a27caf4e8e99cf0c64e8254cea,
title = "Spectroscopic study of star-forming galaxies in filaments and the field at $z\sim$0.5: evidence for environmental dependence of electron density",
abstract = "We study the physical properties of a spectroscopic sample of 28 star-forming galaxies in a large filamentary structure in the COSMOS field at $z\sim$0.53, with spectroscopic data taken with the Keck/DEIMOS spectrograph, and compare them with a control sample of 30 field galaxies. We spectroscopically confirm the presence of a large galaxy filament ($\sim$ 8 Mpc), along which five confirmed X-ray groups exist. We show that within the uncertainties, the ionization parameter, equivalent width (EW), EW versus specific star-formation rate (sSFR) relation, EW versus stellar mass relation, line-of-sight velocity dispersion, dynamical mass, and stellar-to-dynamical mass ratio are similar for filament and field star-forming galaxies. However, we show that on average, filament star-forming galaxies are more metal-enriched ($\sim$ 0.1$-$0.15 dex), possibly due to the inflow of the already enriched intrafilamentary gas into filament galaxies. Moreover, we show that electron densities are significantly lower (a factor of $\sim$17) in filament star-forming systems compared to those in the field, possibly because of a longer star-formation timescale for filament star-forming galaxies. Our results highlight the potential pre-processing role of galaxy filaments and intermediate-density environments on the evolution of galaxies, which has been highly underestimated.",
keywords = "galaxies: abundances, galaxies: evolution, galaxies: fundamental parameters, galaxies: starburst, large-scale structure of universe, MASS-METALLICITY RELATION, DIGITAL SKY SURVEY, EMISSION-LINE GALAXIES, TULLY-FISHER RELATION, LARGE-SCALE STRUCTURE, NEAR-INFRARED SPECTROSCOPY, HOT INTERGALACTIC MEDIUM, RAY LUMINOUS CLUSTERS, VIRGO SPIRAL GALAXIES, II EMITTING GALAXIES",
author = "Behnam Darvish and Bahram Mobasher and David Sobral and Shoubaneh Hemmati and Hooshang Nayyeri and Irene Shivaei",
note = "main figs. 1,7,8,9,10 and 13. ",
year = "2015",
month = dec,
day = "1",
doi = "10.1088/0004-637X/814/2/84",
language = "English",
volume = "814",
journal = "The Astrophysical Journal",
issn = "0004-637X",
publisher = "Institute of Physics Publishing",
number = "2",

}

RIS

TY - JOUR

T1 - Spectroscopic study of star-forming galaxies in filaments and the field at $z\sim$0.5

T2 - evidence for environmental dependence of electron density

AU - Darvish, Behnam

AU - Mobasher, Bahram

AU - Sobral, David

AU - Hemmati, Shoubaneh

AU - Nayyeri, Hooshang

AU - Shivaei, Irene

N1 - main figs. 1,7,8,9,10 and 13.

PY - 2015/12/1

Y1 - 2015/12/1

N2 - We study the physical properties of a spectroscopic sample of 28 star-forming galaxies in a large filamentary structure in the COSMOS field at $z\sim$0.53, with spectroscopic data taken with the Keck/DEIMOS spectrograph, and compare them with a control sample of 30 field galaxies. We spectroscopically confirm the presence of a large galaxy filament ($\sim$ 8 Mpc), along which five confirmed X-ray groups exist. We show that within the uncertainties, the ionization parameter, equivalent width (EW), EW versus specific star-formation rate (sSFR) relation, EW versus stellar mass relation, line-of-sight velocity dispersion, dynamical mass, and stellar-to-dynamical mass ratio are similar for filament and field star-forming galaxies. However, we show that on average, filament star-forming galaxies are more metal-enriched ($\sim$ 0.1$-$0.15 dex), possibly due to the inflow of the already enriched intrafilamentary gas into filament galaxies. Moreover, we show that electron densities are significantly lower (a factor of $\sim$17) in filament star-forming systems compared to those in the field, possibly because of a longer star-formation timescale for filament star-forming galaxies. Our results highlight the potential pre-processing role of galaxy filaments and intermediate-density environments on the evolution of galaxies, which has been highly underestimated.

AB - We study the physical properties of a spectroscopic sample of 28 star-forming galaxies in a large filamentary structure in the COSMOS field at $z\sim$0.53, with spectroscopic data taken with the Keck/DEIMOS spectrograph, and compare them with a control sample of 30 field galaxies. We spectroscopically confirm the presence of a large galaxy filament ($\sim$ 8 Mpc), along which five confirmed X-ray groups exist. We show that within the uncertainties, the ionization parameter, equivalent width (EW), EW versus specific star-formation rate (sSFR) relation, EW versus stellar mass relation, line-of-sight velocity dispersion, dynamical mass, and stellar-to-dynamical mass ratio are similar for filament and field star-forming galaxies. However, we show that on average, filament star-forming galaxies are more metal-enriched ($\sim$ 0.1$-$0.15 dex), possibly due to the inflow of the already enriched intrafilamentary gas into filament galaxies. Moreover, we show that electron densities are significantly lower (a factor of $\sim$17) in filament star-forming systems compared to those in the field, possibly because of a longer star-formation timescale for filament star-forming galaxies. Our results highlight the potential pre-processing role of galaxy filaments and intermediate-density environments on the evolution of galaxies, which has been highly underestimated.

KW - galaxies: abundances

KW - galaxies: evolution

KW - galaxies: fundamental parameters

KW - galaxies: starburst

KW - large-scale structure of universe

KW - MASS-METALLICITY RELATION

KW - DIGITAL SKY SURVEY

KW - EMISSION-LINE GALAXIES

KW - TULLY-FISHER RELATION

KW - LARGE-SCALE STRUCTURE

KW - NEAR-INFRARED SPECTROSCOPY

KW - HOT INTERGALACTIC MEDIUM

KW - RAY LUMINOUS CLUSTERS

KW - VIRGO SPIRAL GALAXIES

KW - II EMITTING GALAXIES

U2 - 10.1088/0004-637X/814/2/84

DO - 10.1088/0004-637X/814/2/84

M3 - Journal article

VL - 814

JO - The Astrophysical Journal

JF - The Astrophysical Journal

SN - 0004-637X

IS - 2

M1 - 84

ER -