2006/08/31 by Louisa A. Nolan, L. A. Nolan, Somak Raychaudhury +3 · 37 citations
Engineering · Physics and Astronomy · #Astronomy and Astrophysical Research #Elliptical galaxy #Galaxies: Formation, Evolution, Phenomena #Galaxy #Lenticular galaxy #Luminous infrared galaxy #Peculiar galaxy #Sky #Space Technology and Applications #Stellar mass #Stellar population #Surface brightness fluctuation #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2006.11326.x
published in Monthly Notices of the Royal Astronomical Society 375(1), 381-387 (Oxford University Press) · 7 pages, 5 figures, submitted to MNRAS, minor revision
arxiv created 2006/11/13 · openalex publication_date 2007/01/13 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We use a purely data-driven rectified factor analysis to identify early-type galaxies with recent star formation in Data Release 4 of the Sloan Digital Sky Survey Spectroscopic Catalogue. We compare the spectra and environment of these galaxies with those of ‘normal’ early-type galaxies, and a sample of independently selected E+A galaxies. We calculate the projected local galaxy surface density from the nearest five and 10 neighbours (Σ5 and Σ10) for each galaxy in our sample, and find that the dependence on projected local density, of the properties of E+A galaxies, is not significantly different from that of early-type galaxies with young stellar populations, dropping off rapidly towards denser environments, and flattening off at densities ≲0.1–0.3 Mpc−2. The dearth of E+A galaxies in dense environments confirms that E+A galaxies are most likely the products of galaxy–galaxy merging or interactions, rather than star-forming galaxies whose star formation has been quenched by processes unique to dense environments, such as ram-pressure stripping or galaxy harassment. We see a tentative peak in the number of E+A galaxies at Σ10∼ 0.1–0.3 Mpc−2, which may represent the local galaxy density at which the rate of galaxy–galaxy merging or interaction rate peaks. Analysis of the spectra of our early-type galaxies with young stellar populations suggests that they have a stellar component dominated by F stars, ∼1–4 Gyr old, together with a mature, metal-rich population characteristic of ‘typical’ early-type galaxies. The young stars represent ≳10 per cent of the stellar mass in these galaxies. This, together with the similarity of the environments in which this ‘E+F’ population and the E+A galaxy sample are found, suggests that E+F galaxies used to be E+A galaxies, but have evolved by a further ∼ one to a few Gyr. Our rectified factor analysis is sensitive enough to identify this hidden population, which allows us to study the global and intrinsic properties of early-type galaxies created in major mergers or interactions, and compare them with those early-types which have had the bulk of their stars in place since a much earlier epoch.