Asboth, V. and Conley, A. and Sayers, J. and Béthermin, M. and Chapman, S. C. and Clements, D. L. and Cooray, A. and Dannerbauer, H. and Farrah, D. and Glenn, J. and Golwala, S. R. and Halpern, M. and Ibar, E. and Ivison, R. J. and Maloney, P. R. and Marques-Chaves, R. and Martinez-Navajas, P. I. and Oliver, S. J. and Pérez-Fournon, I. and Riechers, D. A. and Rowan-Robinson, M. and Scott, Douglas and Siegel, S. R. and Vieira, J. D. and Viero, M. and Wang, L. and Wardlow, J. and Wheeler, J. (2016) HerMES: a search for high-redshift dusty galaxies in the HerMES Large Mode Survey - catalogue, number counts and early results. Monthly Notices of the Royal Astronomical Society, 462 (2). pp. 1989-2000. ISSN 0035-8711
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Abstract
Selecting sources with rising flux densities towards longer wavelengths from Herschel/Spectral and Photometric Imaging Receiver (SPIRE) maps is an efficient way to produce a catalogue rich in high-redshift (z > 4) dusty star-forming galaxies. The effectiveness of this approach has already been confirmed by spectroscopic follow-up observations, but the previously available catalogues made this way are limited by small survey areas. Here we apply a map-based search method to 274 deg2 of the Herschel Multi-tiered Extragalactic Survey (HerMES) Large Mode Survey and create a catalogue of 477 objects with SPIRE flux densities S500 > S350 > S250 and a 5σ cut-off S500 > 52 mJy. From this catalogue we determine that the total number of these `red' sources is at least an order of magnitude higher than predicted by galaxy evolution models. These results are in agreement with previous findings in smaller HerMES fields; however, due to our significantly larger sample size we are also able to investigate the shape of the red source counts for the first time. We have obtained spectroscopic redshift measurements for two of our sources using the Atacama Large Millimeter/submillimeter Array. The redshifts z = 5.1 and 3.8 confirm that with our selection method we can indeed find high-redshift dusty star-forming galaxies.