Galaxy And Mass Assembly (GAMA): estimating galaxy group masses via caustic analysis

Alpaslan, Mehmet; Robotham, Aaron S. G.; Driver, Simon P.; Norberg, Peder; Peacock, J. A.; Baldry, I. K.; Bland-Hawthorn, Joss; Brough, Sarah; Hopkins, A. M.; Kelvin, Lee S.; Liske, J.; Loveday, Jon; Merson, A.; Nichol, R. C.; Pimbblet, Kevin A.

doi:10.1111/j.1365-2966.2012.21020.x

Cited by 25 publications

(24 citation statements)

References 32 publications

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“…Our isolated galaxies are therefore considered to be isolated down to GAMA's detection limit of mr = 19.8 mag. The accuracy of these group and pair classifications has been indepently verified (Alpaslan et al 2012), and benefits from GAMA's high target density and spectroscopic completeness, ensuring that our isolation criteria for our sample is very robust. By excluding such paired and grouped galaxies, one can study the stellar mass growth of spiral galaxies whose stellar populations and star formation rates are not affected by processes that typically affect star formation in groups and pairs (e.g Ellison et al 2008;Robotham et al 2013;Davies et al 2015).…”

Section: Spiral Galaxy Selectionmentioning

confidence: 83%

Galaxy And Mass Assembly (GAMA): stellar mass growth of spiral galaxies in the cosmic web

Alpaslan

Grootes

Marcum

et al. 2016

Mon. Not. R. Astron. Soc.

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We look for correlated changes in stellar mass and star formation rate along filaments in the cosmic web by examining the stellar masses and UV-derived star formation rates (SFR) of 1,799 ungrouped and unpaired spiral galaxies that reside in filaments. We devise multiple distance metrics to characterise the complex geometry of filaments, and find that galaxies closer to the cylindrical centre of a filament have higher stellar masses than their counterparts near the periphery of filaments, on the edges of voids. In addition, these peripheral spiral galaxies have higher specific star formation rates (SSFR) at a given mass. Complementing our sample of filament spiral galaxies with spiral galaxies in tendrils and voids, we find that the average SFR of these objects in different large scale environments are similar to each other with the primary discriminant in SFR being stellar mass, in line with previous works. However, the distributions of SFRs are found to vary with large-scale environment. Our results thus suggest a model in which in addition to stellar mass as the primary discriminant, the large-scale environment is imprinted in the SFR as a second order effect. Furthermore, our detailed results for filament galaxies suggest a model in which gas accretion from voids onto filaments is primarily in an orthogonal direction. Overall, we find our results to be in line with theoretical expectations of the thermodynamic properties of the intergalactic medium in different large-scale environments.

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Section: Spiral Galaxy Selectionmentioning

confidence: 83%

Galaxy And Mass Assembly (GAMA): stellar mass growth of spiral galaxies in the cosmic web

Alpaslan

Grootes

Marcum

et al. 2016

Mon. Not. R. Astron. Soc.

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“…The application of the caustic technique (e.g., Alpaslan et al 2012;Serra & Diaferio 2013) is shown in panels (c & g) of Figure 8 for two rescale parameters, q = 25 (cyan lines) and q = 35 (pink lines). Although this technique is quite successful when applied to the cluster outskirts, it misses some of the true members located within the core, which are the most important galaxies affecting the dynamics of the clusters.…”

Section: A Comparison Of Membershipmentioning

confidence: 99%

GalWeight: A New and Effective Weighting Technique for Determining Galaxy Cluster and Group Membership

Abdullah

Wilson

Klypin

2018

ApJ

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We introduce GalWeight, a new technique for assigning galaxy cluster membership. This technique is specifically designed to simultaneously maximize the number of bona fide cluster members while minimizing the number of contaminating interlopers. The GalWeight technique can be applied to both massive galaxy clusters and poor galaxy groups. Moreover, it is effective in identifying members in both the virial and infall regions with high efficiency. We apply the GalWeight technique to MDPL2 & Bolshoi N-body simulations, and find that it is > 98% accurate in correctly assigning cluster membership. We show that GalWeight compares very favorably against four well-known existing cluster membership techniques (shifting gapper, den Hartog, caustic, SIM). We also apply the GalWeight technique to a sample of twelve Abell clusters (including the Coma cluster) using observations from the Sloan Digital Sky Survey. We end by discussing GalWeight's potential for other astrophysical applications.

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“…Cluver et al (2014) obtained mid-infrared photometry for GAMA galaxies from reprocessed WISE data. Finally, the environment of GAMA galaxies was characterized by Brough et al (2013) using galaxy number surface density, while presented the GAMA Galaxy Group Catalogue (G 3 C; see also Alpaslan et al 2012). The above have been used, inter alia, to derive the broad-band (Loveday et al 2012(Loveday et al , 2015 and Hα (Gunawardhana et al 2013) luminosity and stellar mass (Baldry et al 2012;Gunawardhana et al 2015) functions, to consider the luminosity and stellar mass functions split by Hubble type (Kelvin et al 2014a,b) and in different environments (McNaught-Roberts et al 2014;Eardley et al 2015), to determine the effect of mergers on the stellar mass function , to study variations and dependences of the galaxy initial mass function (Gunawardhana et al 2011) and of the star formation rate (SFR; Wijesinghe et al 2012), and to investigate satellite galaxies (Prescott et al 2011;Schneider et al 2013), the effect of the local environment on L galaxies (Robotham et al 2013), the relations between stellar mass, metallicity and (specific) SFR (Foster et al 2012;Bauer et al 2013;Lara-López et al 2013), and the cosmic spectral energy distribution (SED; Driver et al 2012).…”

Section: Introductionmentioning

confidence: 99%

Galaxy And Mass Assembly (GAMA): end of survey report and data release 2

Liske¹,

Baldry²,

Driver³

et al. 2015

Mon. Not. R. Astron. Soc.

539

516

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Galaxy And Mass Assembly (GAMA): estimating galaxy group masses via caustic analysis

Cited by 25 publications

References 32 publications

Galaxy And Mass Assembly (GAMA): stellar mass growth of spiral galaxies in the cosmic web

Galaxy And Mass Assembly (GAMA): stellar mass growth of spiral galaxies in the cosmic web

GalWeight: A New and Effective Weighting Technique for Determining Galaxy Cluster and Group Membership

Galaxy And Mass Assembly (GAMA): end of survey report and data release 2

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