Radio counterpart of the lensed sub-mm emission in the cluster MS0451.6-0305: new evidence for the merger scenario
Oct, 2009Citations per year
Abstract: (arXiv)
SMM J04542-0301 is an extended (~1 arcmin) sub-mm source located near the core of the cluster MS0451.6-0305. It has been suggested that part of its emission arises from the interaction between a LBG and two EROs at z~2.9 that are multiply-imaged. However, the dramatic resolution difference between the sub-mm map and the optical/NIR images make it difficult to confirm this hypothesis. In this paper, we present a deep (~ 10 microJy/beam), high resolution (~2 arcsec) 1.4 GHz radio map of the cluster core, in which we have identified 6 sources located within SMM J04542-0301. The strong lensing effect in the radio data has been quantified by constructing a new lens model of the cluster. The brightest and most extended of these sources (RJ) is located in the middle of the sub-mm emission, and has no obvious counterpart in the optical/NIR. Three other detections (E1, E2 and E3) seem to be associated with the images of one of the EROs. The last two detections (CR1 and CR2), for which no optical/NIR counterpart have been found, seem to constitute two relatively compact emitting regions embedded in a ~5 arcsec extended radio source located at the position of the sub-mm peak. The presence of this extended component can only be explained if it is being produced by a lensed region of dust obscured star formation in the center of the merger. A comparison between the radio and sub-mm data at the same resolution suggests that E1, E2, E3, CR1 and CR2 are associated with the sub-mm emission. The radio observations provide strong observational evidence in favor of the merger hypothesis. However, the question if RJ is also contributing to the observed sub-mm emission remains open. These results illustrate the promising prospects for radio interferometry and strong gravitational lensing to study the internal structure of SMGs.Note:
- 19 pages, 15 figures, accepted for publication in Astronomy & Astrophysics A version of the paper with high resolution images can be downloaded from here: http://www.astro.rug.nl/~berciano/SMMJ04542-0301.pdf
References(60)
Figures(15)