A1 Vertaisarvioitu alkuperäisartikkeli tieteellisessä lehdessä
Spitzer/Infrared Array Camera near-infrared features in the outer parts of S(4)G galaxies
Tekijät: Seppo Laine, Johan H. Knapen, Juan-Carlos Muñoz-Mateos, Taehyun Kim, Sébastien Comerón, Marie Martig, Benne W. Holwerda, E. Athanassoula, Albert Bosma, Peter H. Johansson, Santiago Erroz-Ferrer, Dimitri A. Gadotti, Armando Gil de Paz, Joannah Hinz, Jarkko Laine, Eija Laurikainen, Karín Menéndez-Delmestre, Trisha Mizusawa, Michael W. Regan, Heikki Salo, Kartik Sheth, Mark Seibert, Ronald J. Buta, Mauricio Cisternas, Bruce G. Elmegreen, Debra M. Elmegreen, Luis C. Ho, Barry F. Madore, Dennis Zaritsky
Kustantaja: OXFORD UNIV PRESS
Kustannuspaikka: OXFORD; GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
Julkaisuvuosi: 2014
Journal: Monthly Notices of the Royal Astronomical Society
Tietokannassa oleva lehden nimi: Monthly Notices of the Royal Astronomical Society
Lehden akronyymi: Mon.Not.Roy.Astron.Soc.
Vuosikerta: 444
Numero: 4
Aloitussivu: 3015
Lopetussivu: 3039
Sivujen määrä: 25
ISSN: 0035-8711
DOI: https://doi.org/10.1093/mnras/stu1642
We present a catalogue and images of visually detected features, such as asymmetries, extensions, warps, shells, tidal tails, polar rings, and obvious signs of mergers or interactions, in the faint outer regions (at and outside of R-25) of nearby galaxies. This catalogue can be used in future quantitative studies that examine galaxy evolution due to internal and external factors. We are able to reliably detect outer region features down to a brightness level of 0.03 MJy sr(-1) pixel(-1) at 3.6 mu m in the Spitzer Survey of Stellar Structure in Galaxies (S(4)G). We also tabulate companion galaxies. We find asymmetries in the outer isophotes in 22 +/- 1 per cent of the sample. The asymmetry fraction does not correlate with galaxy classification as an interacting galaxy or merger remnant, or with the presence of companions. We also compare the detected features to similar features in galaxies taken from cosmological zoom re-simulations. The simulated images have a higher fraction (33 per cent) of outer disc asymmetries, which may be due to selection effects and an uncertain star formation threshold in the models. The asymmetries may have either an internal (e.g. lopsidedness due to dark halo asymmetry) or external origin.