Galaxy And Mass Assembly (GAMA): the signatures of galaxy interactions as viewed from small-scale galaxy clustering

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dc.contributor.authorGunawardhan, M. L. P.
dc.contributor.authorNorberg, P.
dc.contributor.authorZehavi, I.
dc.contributor.authorFarrow, D. J.
dc.contributor.authorLoveday, J.
dc.contributor.authorHopkins, A. M.
dc.contributor.authorDavie, L. J. M.
dc.contributor.authorWang, L.
dc.contributor.authorAlpaslan, M.
dc.contributor.authorBland-Hawthorn, J.
dc.contributor.authorBrough, S.
dc.contributor.authorHolwerda, B. W.
dc.contributor.authorOwers, M. S.
dc.contributor.authorWrigh, A. H.
dc.date.accessioned2022-05-24T14:48:09Z
dc.date.available2022-05-24T14:48:09Z
dc.date.issued2018
dc.description.abstractStatistical studies of galaxy-galaxy interactions often utilize net change in physical properties of progenitors as a function of the separation between their nuclei to trace both the strength and the observable time-scale of their interaction. In this study, we use two-point auto-, cross-, and mark-correlation functions to investigate the extent to which small-scale clustering properties of star-forming galaxies can be used to gain physical insight into galaxy-galaxy interactions between galaxies of similar optical brightness and stellar mass. The H α star formers, drawn from the highly spatially complete Galaxy And Mass Assembly (GAMA) survey, show an increase in clustering at small separations. Moreover, the clustering strength shows a strong dependence on optical brightness and stellar mass, where (1) the clustering amplitude of optically brighter galaxies at a given separation is larger than that of optically fainter systems, (2) the small-scale-clustering properties (e.g. the strength, the scale at which the signal relative to the fiducial power law plateaus) of star-forming galaxies appear to differ as a function of increasing optical brightness of galaxies. According to cross- and mark-correlation analyses, the former result is largely driven by the increased dust content in optically bright star-forming galaxies. The latter could be interpreted as evidence of a correlation between interaction-scale and optical brightness of galaxies, where physical evidence of interactions between optically bright star formers, likely hosted within relatively massive haloes, persists over larger separations than those between optically faint star formers.
dc.fuente.origenOUP
dc.identifier.doi10.1093/mnras/sty1638
dc.identifier.eissn1365-2966
dc.identifier.issn0035-8711
dc.identifier.urihttps://doi.org/10.1093/mnras/sty1638
dc.identifier.urihttps://ieeexplore.ieee.org/stamp/stamp.jsp?arnumber=8415886
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/64274
dc.issue.numero2
dc.language.isoen
dc.nota.accesoContenido completo
dc.pagina.final1464
dc.pagina.inicio1433
dc.revistaMonthly Notices of the Royal Astronomical Society
dc.rightsacceso abierto
dc.subjectGalaxies: distances and redshifts
dc.subjectGalaxies: haloes
dc.subjectGalaxies: interactions
dc.subjectGalaxies: starburst
dc.subjectGalaxies: star formation
dc.subjectGalaxies: statistics
dc.titleGalaxy And Mass Assembly (GAMA): the signatures of galaxy interactions as viewed from small-scale galaxy clusteringes_ES
dc.typeartículo
dc.volumen479
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