Galaxy And Mass Assembly (GAMA): The <i>M‐Z</i> relation for galaxy groups

Lara-López, M. A.; Hopkins, A. M.; Robotham, Aaron S. G.; Owers, Matt S.; Colless, Matthew; Brough, Sarah; Norberg, Peder; Steele, Oliver; Taylor, Edward N.; Thomas, Daniel

doi:10.1002/asna.201211882

Cited by 5 publications

(3 citation statements)

References 41 publications

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“…At small scales (a few tens of kpc), there is substantial evidence from observations and simulations for a decrement of metallicity and an enhancement of star-formation activity in galaxy close pairs, merging, and interacting systems compared to isolated, field galaxies, mostly attributed to the interaction-induced inflow of metal-poor gas from the periphery of interacting galaxies to the center, diluting their metal content, and increasing their gas fuel for star-formation (Mihos & Hernquist 1996;Kewley et al 2006;Michel-Dansac et al 2008;Ellison et al 2008;Sol Alonso et al 2010;Rupke et al 2010;Perez et al 2011;Scudder et al 2012b;Ellison et al 2013;Ly et al 2014). At intermediate group scales where galaxy interactions are more common compared to cluster and field environments (Perez et al 2009;Tonnesen & Cen 2012) (due to a combination of (1) a lower velocity dispersion of group galaxies relative to their cluster counterparts and (2) a higher number density of group galaxies compared to the field systems, which provide an ideal condition for interactions), there is also evidence for a deficit of metals in group galaxies compared to control samples in the field (Lara-López et al 2013b), possibly due to a higher fraction of interacting galaxies. At larger filamentary and cluster scales, the slight metal enhancement of galaxies relative to the field might be due to (1) the inflow of already enriched interafilamentary or interacluster gas into galaxies as observations and simulations have shown a more metal enriched IGM in cluster and filament environments compared to the field (Arnaud et al 1994;Aracil et al 2006;Stocke et al 2006Stocke et al , 2007Sato et al 2007;Davé et al 2011;Cen & Chisari 2011;Oppenheimer et al 2012), (2) the environmental strangulation (Larson et al 1980;Peng et al 2015) of low-metallicity diluting gas falling from the surrounding LSS cosmic web into galaxies, (3) the environmental ram pressure stripping (Gunn & Gott 1972;Abadi et al 1999) of the metal-poor diluting gas in the periphery of galaxies, and (4) trapping ...…”

Section: Discussionmentioning

confidence: 99%

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

Darvish

Mobasher

Sobral

et al. 2015

ApJ

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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∼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 (∼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 (∼0.1-0.15 dex), possibly owing to the inflow of the already-enriched intrafilamentary gas into filament galaxies. Moreover, we show that electron densities are significantly lower (a factor of ∼17) in filament starforming 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 intermediatedensity environments on the evolution of galaxies, which has been highly underestimated.

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Section: Discussionmentioning

confidence: 99%

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

Darvish

Mobasher

Sobral

et al. 2015

ApJ

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“…Peng & Maiolino (2014) find that metallicity correlates with environmental overdensity primarily for satellite galaxies, but much less so for central galaxies. While the tendency of galaxies in richer environments to have higher metallicities is generally agreed upon at z ≈ 0, the measured trends at higher redshifts span both positive and negative correlations (Magrini et al 2012;Kulas et al 2013;Lara-López et al 2013;Darvish et al 2015;Kacprzak et al 2015;Shimakawa et al 2015;Valentino et al 2015), and the verdict is still out.…”

Section: Introductionmentioning

confidence: 92%

How Environment Affects Galaxy Metallicity Through Stripping and Formation History: Lessons From the Illustris Simulation

Genel

2016

ApJ

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Recent studies have found higher galaxy metallicities in richer environments. It is not yet clear, however, whether metallicity-environment dependencies are merely an indirect consequence of environmentally dependent formation histories, or of environment related processes directly affecting metallicity. Here, we present a first detailed study of metallicity-environment correlations in a cosmological hydrodynamical simulation, in particular the Illustris simulation. Illustris galaxies display similar relations to those observed. Utilizing our knowledge of simulated formation histories, and leveraging the large simulation volume, we construct galaxy samples of satellites and centrals that are matched in formation histories. This allows us to find that ∼ 1/3 of the metallicity-environment correlation is due to different formation histories in different environments. This is a combined effect of satellites (in particular, in denser environments) having on average lower z = 0 star formation rates (SFRs), and of their older stellar ages, even at a given z = 0 SFR. Most of the difference, ∼ 2/3, however, is caused by the higher concentration of star-forming disks of satellite galaxies, as this biases their SFR-weighted metallicities toward their inner, more metal-rich parts. With a newly defined quantity, the 'radially averaged' metallicity, which captures the metallicity profile but is independent of the SFR profile, the metallicities of satellites and centrals become environmentally independent once they are matched in formation history. We find that circumgalactic metallicity (defined as rapidly inflowing gas around the virial radius), while sensitive to environment, has no measurable effect on the metallicity of the star-forming gas inside the galaxies.

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“…In the catalogue of visual morphologues (DMU VisualMorphologyv3 Kelvin et al 2014a, as used in, for example, Kelvin et al 2014b;Moffett et al 2016a;Lange et al 2016;Moffett et al 2016b;Alpaslan et al 2015), 0.81% of objects are not in the new catalogue. For the group catalogue (DMU G3Galv10 Robotham et al 2011, as used in for example Alpaslan et al 2012;Lara-López et al 2013;Alpaslan et al 2014;Robotham et al 2014;Davies et al 2015;Deeley et al 2017), this number is only 0.26%. For the SED-fitting catalogue using MagPhys (DMU Mag-Physv06 Driver et al 2016b, as used in, for example, Davies et al 2017;Mahajan et al 2018;Driver et al 2018) only 0.25% of objects are missing, and for the catalogue of Sérsic indices (DMU SersicCatSDSSv09 Kelvin et al 2012, as used in, for example, Kelvin et al 2014a;Deeley et al 2017;Bremer et al 2018) 0.87% of objects are missing.…”

Section: Impact On Existing Gama Studiesmentioning

confidence: 99%

Galaxy And Mass Assembly (GAMA): Assimilation of KiDS into the GAMA database

Bellstedt,

Driver,

Robotham

et al. 2020

Preprint

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The Galaxy And Mass Assembly Survey (GAMA) covers five fields with highly complete spectroscopic coverage (> 95 per cent) to intermediate depths (r < 19.8 or i < 19.0 mag), and collectively spans 250 square degrees of Equatorial or Southern sky. Four of the GAMA fields (G09, G12, G15 and G23) reside in the ESO VST KiDS and ESO VISTA VIKING survey footprints, which combined with our GALEX, WISE and Herschel data provide deep uniform imaging in the F U V N U V ugriZY JHK s W 1 W 2 W 3 W 4 P 100 P 160 S250 S350 S500 bands. Following the release of KiDS DR4, we describe the process by which we ingest the KiDS data into GAMA (replacing the SDSS data previously used for G09, G12 and G15), and redefine our core optical and near-IR catalogues to provide a complete and homogeneous dataset. The source extraction and analysis is based on the new ProFound image analysis package, providing matched-segment photometry across all bands. The data are classified into stars, galaxies, artefacts, and ambiguous objects, and objects are linked to the GAMA spectroscopic target catalogue. Additionally, a new technique is employed utilising ProFound to extract photometry in the unresolved MIR-FIR regime. The catalogues including the full FUV-FIR photometry are described and will be fully available as part of GAMA DR4. They are intended for both standalone science, selection for targeted follow-up with 4MOST, as well as an accompaniment to the upcoming and ongoing radio arrays now studying the GAMA 23 h field.

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Galaxy And Mass Assembly (GAMA): The M‐Z relation for galaxy groups

Cited by 5 publications

References 41 publications

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

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

How Environment Affects Galaxy Metallicity Through Stripping and Formation History: Lessons From the Illustris Simulation

Galaxy And Mass Assembly (GAMA): Assimilation of KiDS into the GAMA database

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