Show simple item record

Files in this item

Thumbnail

Item metadata

dc.contributor.authorZarattini, S.
dc.contributor.authorAguerri, J.A.L.
dc.contributor.authorSánchez-Janssen, R.
dc.contributor.authorBarrena, R.
dc.contributor.authorBoschin, W.
dc.contributor.authorDel Burgo, C.
dc.contributor.authorCastro-Rodriguez, N.
dc.contributor.authorCorsini, E.M.
dc.contributor.authorD'Onghia, E.
dc.contributor.authorGirardi, M.
dc.contributor.authorIglesias-Páramo, J.
dc.contributor.authorKundert, A.
dc.contributor.authorMendez Abreu, Jairo
dc.contributor.authorVilchez, J.M.
dc.date.accessioned2015-10-06T14:10:01Z
dc.date.available2015-10-06T14:10:01Z
dc.date.issued2015-09
dc.identifier.citationZarattini , S , Aguerri , J A L , Sánchez-Janssen , R , Barrena , R , Boschin , W , Del Burgo , C , Castro-Rodriguez , N , Corsini , E M , D'Onghia , E , Girardi , M , Iglesias-Páramo , J , Kundert , A , Mendez Abreu , J & Vilchez , J M 2015 , ' Fossil group origins V. the dependence of the luminosity function on the magnitude gap ' , Astronomy & Astrophysics , vol. 581 , A16 . https://doi.org/10.1051/0004-6361/201425506en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 221889161
dc.identifier.otherPURE UUID: 54fd6f32-b37f-40eb-b48e-cb61cafa3106
dc.identifier.otherScopus: 84940390327
dc.identifier.otherWOS: 000361803900016
dc.identifier.urihttp://hdl.handle.net/10023/7613
dc.descriptionThis work has been partially funded by the MINECO (grant AIA2013-43188-P). E.M.C. acknowledges financial support from Padua University by the grants 60A02-4807/12, 60A02-5857/13, 60A02-5833/14, and CPDA133894. M.G. acknowledges financial support from MIUR PRIN2010-2011. J.M.A. acknowledges support from the European Research Council Starting Grant (SEDmorph; P.I. V. Wild). E.D. gratefully acknowledges the support of the Alfred P. Sloan Foundation. E.D. and A.K. are supported by NASA Grant No NNX13AE97G. J.I.P. and J.M.V. acknowledge financial support from the Spanish MINECO under grant AYA2010-21887-C04-01 and from Junta de Andalucía Excellence Project PEX2011-FQM7058.en
dc.description.abstractContext. In nature we observe galaxy aggregations that span a wide range of magnitude gaps between the two first-ranked galaxies of a system (Δm12). Thus, there are systems with gaps close to zero (e.g., the Coma cluster), and at the other extreme of the distribution, the largest gaps are found among the so-called fossil systems. The observed distribution of magnitude gaps is thought to be a consequence of the orbital decay of M∗ galaxies in massive halos and the associated growth of the central object. As a result, to first order the amplitude of this gap is a good statistical proxy for the dynamical age of a system of galaxies. Fossil and non-fossil systems could therefore have different galaxy populations that should be reflected in their luminosity functions. Aims. In this work we study, for the first time, the dependence of the luminosity function parameters on Δm12 using data obtained by the fossil group origins (FOGO) project. Methods. We constructed a hybrid luminosity function for 102 groups and clusters at z ≤ 0.25 using both photometric data from the SDSS-DR7 and redshifts from the DR7 and the FOGO surveys. The latter consists of ~1200 new redshifts in 34 fossil system candidates. We stacked all the individual luminosity functions, dividing them into bins of Δm12, and studied their best-fit Schechter parameters. We additionally computed a “relative” luminosity function, expressed as a function of the central galaxy luminosity, which boosts our capacity to detect differences – especially at the bright end. Results. We find trends as a function of Δm12 at both the bright and faint ends of the luminosity function. In particular, at the bright end, the larger the magnitude gap, the fainter the characteristic magnitude M∗. The characteristic luminosity in systems with negligible gaps is more than a factor three brighter than in fossil-like ones. Remarkably, we also find differences at the faint end. In this region, the larger the gap, the flatter the faint-end slope α. Conclusions. The differences found at the bright end support a dissipationless, dynamical friction-driven merging model for the growth of the central galaxy in group- and cluster-sized halos. The differences in the faint end cannot be explained by this mechanism. Other processes – such as enhanced tidal disruption due to early infall and/or prevalence of eccentric orbits – may play a role. However, a larger sample of systems with Δm12> 1.5 is needed to establish the differences at the faint end.
dc.format.extent11
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rightsCopyright ESO 2015. Reproduced with permission from Astronomy & Astrophysics, © ESO. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at http://dx.doi.org/10.1051/0004-6361/201425506en
dc.subjectGalaxies: clusters: generalen
dc.subjectGalaxies: groups: generalen
dc.subjectGalaxies: luminosity function, mass functionen
dc.subjectQC Physicsen
dc.subjectQB Astronomyen
dc.subject3rd-DASen
dc.subject.lccQCen
dc.subject.lccQBen
dc.titleFossil group origins V. the dependence of the luminosity function on the magnitude gapen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201425506
dc.description.statusPeer revieweden


This item appears in the following Collection(s)

Show simple item record