The nature of a gravitationally lensed sub-millimetre arc in MS0451.6-0305: two interacting galaxies at z~2.9?

Details The nature of a gravitationally lensed sub-millimetre arc in MS0451.6-0305: two interacting galaxies at z~2.9? The nature of a gravitationally lensed sub-millimetre arc in MS0451.6-0305: two interacting galaxies at z~2.9?

2004-04-23

arxiv.org/abs/astro-ph/0404473v1

Mon.Not.Roy.Astron.Soc. 352 (2004) 759

Astronomy and Astrophysics

Astrophysics

Accepted for publication in MNRAS. 10 pages, 7 figures (1 in colour). A higher resolution version can be found at http://www

Scientific paper

10.1111/j.1365-2966.2004.07982.x

We present a new SCUBA image of the cluster MS0451.6-0305, which exhibits strong, extended sub-mm flux at 850 microns. The most striking feature in the map is an elongated region of bright sub-mm emission, with a flux density of >10 mJy over several beam-sizes. This region is apparently coincident with a previously known optical arc (which turns out to be a strongly lensed Lyman Break Galaxy at z=2.911), as well as with a newly identified multiply-imaged ERO (Extremely Red Object) pair predicted to be at a similar, if not identical redshift. By combing a detailed lensing model with deep images from HST, Chandra, CFHT, JCMT, and spectra from the VLT, we conclude that both the strongly lensed optical arc and ERO systems have properties consistent with known sub-mm emitters. Using a simple model for the two sources, we estimate that the multiply-lensed EROs contribute the majority of the flux in the SCUBA lensed arc. Correcting for the lensing amplification, we estimate that the inherent 850 micron fluxes for both objects are ~0.4 mJy. If the LBG and ERO pair are truly at the same redshift, then they are separated by only ~10 kpc in the source plane, and hence constitute an interacting system at z~2.9. Higher angular resolution observations in sub-mm/mm will permit us to more accurately separate the contribution from each candidate, and better understand the nature of this system.

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