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Spatially Resolved Spectroscopy of the E+A Galaxies in the z=0.32 Cluster AC114 | | M. B. Pracy
; W. J. Couch
; C. Blake
; K. Bekki
; C. Harrison
; M. Colless
; H. Kuntschner
; R. de Propris
; | | Date: |
3 Mar 2005 | | Journal: | Mon.Not.Roy.Astron.Soc. 359 (2005) 1421-1432 | | Subject: | astro-ph | | Abstract: | We present spatially resolved intermediate resolution spectroscopy of a sample of twelve E+A galaxies in the z=0.32 rich galaxy cluster AC 114, obtained with the FLAMES multi-integral field unit system on the European Southern Observatory’s VLT. Previous integrated spectroscopy of all these galaxies by Couch & Sharples (1987) had shown them to have strong Balmer line absorption and an absence of [OII 3727] emission -- the defining characteristics of the``E+A’’ spectral signature, indicative of an abrupt halt to a recent episode of quite vigorous star formation. We have used our spectral data to determine the radial variation in the strength of Hdelta absorption in these galaxies and hence map out the distribution of this recently formed stellar population. Such information provides important clues as to what physical event might have been responsible for this quite dramatic change in star formation activity in these galaxies’ recent past. We find a diversity of behaviour amongst these galaxies in terms of the radial variation in Hdelta absorption: Four galaxies show little Hdelta absorption across their entire extent; it would appear they were misidentified as E+A galaxies in the earlier integrated spectroscopic studies. The remainder show strong Hdelta absorption, with a gradient that is either negative (Hdelta equivalent width decreasing with radius), flat, or positive. By comparing with numerical simulations we suggest that the first of these different types of radial behaviour provides evidence for a merger/interaction origin, whereas the latter two types of behaviour are more consistent with the truncation of star formation in normal disk galaxies. It would seem therefore that more than one physical mechanism is responsible for E+A formation in the same environment. | | Source: | arXiv, astro-ph/0503062 | | Services: | Forum | Review | PDF | Favorites | |
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