AzTEC Millimetre Survey of the COSMOS Field: I. Data Reduction and Source Catalogue

Details AzTEC Millimetre Survey of the COSMOS Field: I. Data Reduction and Source Catalogue AzTEC Millimetre Survey of the COSMOS Field: I. Data Reduction and Source Catalogue

2008-01-17

arxiv.org/abs/0801.2779v1

MNRAS, Vol 385, Issue 4, 2225-2238, 2008

Astronomy and Astrophysics

Astrophysics

16 pages, 12 figures, 2 tables, accepted for publication in MNRAS

Scientific paper

10.1111/j.1365-2966.2008.12989.x

We present a 1.1 mm wavelength imaging survey covering 0.3 sq. deg. in the COSMOS field. These data, obtained with the AzTEC continuum camera on the James Clerk Maxwell Telescope (JCMT), were centred on a prominent large-scale structure over-density which includes a rich X-ray cluster at z = 0.73. A total of 50 millimetre galaxy candidates, with a significance ranging from 3.5-8.5 sigma, are extracted from the central 0.15 sq. deg. area which has a uniform sensitivity of 1.3 mJy/beam. Sixteen sources are detected with S/N > 4.5, where the expected false-detection rate is zero, of which a surprisingly large number (9) have intrinsic (de-boosted) fluxes > 5 mJy at 1.1 mm. Assuming the emission is dominated by radiation from dust, heated by a massive population of young, optically-obscured stars, then these bright AzTEC sources have FIR luminosities > 6 x 10^12 L(sun) and star formation-rates > 1100 M(sun)/yr. Two of these nine bright AzTEC sources are found towards the extreme peripheral region of the X-ray cluster, whilst the remainder are distributed across the larger-scale over-density. We describe the AzTEC data reduction pipeline, the source-extraction algorithm, and the characterisation of the source catalogue, including the completeness, flux de-boosting correction, false-detection rate and the source positional uncertainty, through an extensive set of Monte-Carlo simulations. We conclude with a preliminary comparison, via a stacked analysis, of the overlapping MIPS 24 micron data and radio data with this AzTEC map of the COSMOS field.

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