Show simple item record

Files in this item

Thumbnail

Item metadata

dc.contributor.authorGrootes, M. W.
dc.contributor.authorTuffs, R. J.
dc.contributor.authorPopescu, C. C.
dc.contributor.authorNorberg, P.
dc.contributor.authorRobotham, A. S. G.
dc.contributor.authorLiske, J.
dc.contributor.authorAndrae, E.
dc.contributor.authorBaldry, I. K.
dc.contributor.authorGunawardhana, M.
dc.contributor.authorKelvin, L. S.
dc.contributor.authorMadore, B. F.
dc.contributor.authorSeibert, M.
dc.contributor.authorTaylor, E. N.
dc.contributor.authorAlpaslan, M.
dc.contributor.authorBrown, M. J. I.
dc.contributor.authorCluver, M. E.
dc.contributor.authorDriver, S. P.
dc.contributor.authorBland-Hawthorn, J.
dc.contributor.authorHolwerda, B. W.
dc.contributor.authorHopkins, A. M.
dc.contributor.authorLopez-Sanchez, A. R.
dc.contributor.authorLoveday, J.
dc.contributor.authorRushton, M.
dc.date.accessioned2018-01-22T12:30:07Z
dc.date.available2018-01-22T12:30:07Z
dc.date.issued2017-03
dc.identifier.citationGrootes , M W , Tuffs , R J , Popescu , C C , Norberg , P , Robotham , A S G , Liske , J , Andrae , E , Baldry , I K , Gunawardhana , M , Kelvin , L S , Madore , B F , Seibert , M , Taylor , E N , Alpaslan , M , Brown , M J I , Cluver , M E , Driver , S P , Bland-Hawthorn , J , Holwerda , B W , Hopkins , A M , Lopez-Sanchez , A R , Loveday , J & Rushton , M 2017 , ' Galaxy And Mass Assembly (GAMA) : gas fuelling of spiral galaxies in the local Universe I. The effect of the group environment on star formation in spiral galaxies ' , Astrophysical Journal , vol. 153 , no. 3 , 111 . https://doi.org/10.3847/1538-3881/153/3/111en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 252098127
dc.identifier.otherPURE UUID: d394992f-1e55-4f76-b1a9-3dc6c41fe80f
dc.identifier.otherArXiv: http://arxiv.org/abs/1612.07322v1
dc.identifier.otherScopus: 85015188185
dc.identifier.otherWOS: 000403657200001
dc.identifier.urihttp://hdl.handle.net/10023/12558
dc.description.abstractWe quantify the effect of the galaxy group environment (for group masses of 1012.5–1014.0 M ⊙) on the current star formation rate (SFR) of a pure, morphologically selected sample of disk-dominated (i.e., late-type spiral) galaxies with redshift ≤0.13. The sample embraces a full representation of quiescent and star-forming disks with stellar mass M * ≥ 109.5 M ⊙. We focus on the effects on SFR of interactions between grouped galaxies and the putative intrahalo medium (IHM) of their host group dark matter halos, isolating these effects from those induced through galaxy–galaxy interactions, and utilizing a radiation transfer analysis to remove the inclination dependence of derived SFRs. The dependence of SFR on M * is controlled for by measuring offsets Δlog(ψ *) of grouped galaxies about a single power-law relation in specific SFR, ψ* ∝ M*-0.45± 0.01, exhibited by non-grouped "field" galaxies in the sample. While a small minority of the group satellites are strongly quenched, the group centrals and a large majority of satellites exhibit levels of ψ * statistically indistinguishable from their field counterparts, for all M *, albeit with a higher scatter of 0.44 dex about the field reference relation (versus 0.27 dex for the field). Modeling the distributions in Δlog(ψ *), we find that (i) after infall into groups, disk-dominated galaxies continue to be characterized by a similar rapid cycling of gas into and out of their interstellar medium shown prior to infall, with inflows and outflows of ~1.5–5 x SFR and ~1–4 x SFR, respectively; and (ii) the independence of the continuity of these gas flow cycles on M * appears inconsistent with the required fueling being sourced from gas in the circumgalactic medium on scales of ~100 kpc. Instead, our data favor ongoing fueling of satellites from the IHM of the host group halo on ~Mpc scales, i.e., from gas not initially associated with the galaxies upon infall. Consequently, the color–density relation of the galaxy population as a whole would appear to be primarily due to a change in the mix of disk- and spheroid-dominated morphologies in the denser group environment compared to the field, rather than to a reduced propensity of the IHM in higher-mass structures to cool and accrete onto galaxies. We also suggest that the required substantial accretion of IHM gas by satellite disk-dominated galaxies will lead to a progressive reduction in the specific angular momentum of these systems, thereby representing an efficient secular mechanism to transform morphology from star-forming disk-dominated types to more passive spheroid-dominated types.
dc.format.extent49
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2017, American Astronomical Society. This work has been made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at https://doi.org/10.3847/1538-3881/153/3/111en
dc.subjectGalaxies: fundamental parametersen
dc.subjectGalaxies: groups: generalen
dc.subjectGalaxies: ISMen
dc.subjectGalaxies: spiralen
dc.subjectIntergalactic mediumen
dc.subjectSurveysen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject3rd-DASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleGalaxy And Mass Assembly (GAMA) : gas fuelling of spiral galaxies in the local Universe I. The effect of the group environment on star formation in spiral galaxiesen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.3847/1538-3881/153/3/111
dc.description.statusPeer revieweden
dc.identifier.urlhttp://arxiv.org/abs/1612.07322v1en


This item appears in the following Collection(s)

Show simple item record