The Herschel-SPIRE Dark Field I: The deepest Herschel image of the submillimetre Universe

TL;DR

This paper presents the deepest Herschel SPIRE submillimetre images of the universe, including source extraction, analysis, and comparison with galaxy evolution models, revealing the galaxy population turnover.

Contribution

It provides the first source counts from the Herschel SPIRE Dark Field, utilizing two independent extraction methods and comparing results with galaxy evolution models.

Findings

Detected the galaxy population turnover in source counts.

Achieved twice the depth of previous methods with XID algorithm.

Found good agreement between observed counts and galaxy evolution models.

Abstract

We present the image maps, data reduction, analysis and the first source counts from the Herschel SPIRE Dark Field. The SPIRE Dark Field is an area of sky near the North Ecliptic Pole observed many times during the calibration phase of the Herschel mission in order to characterise the stability of the SPIRE instrument and is subsequently one of the deepest imaged fields of the Universe at far-infrared-submillimetre wavelengths. The SPIRE dark field is concurrent with the Spitzer IRAC Dark Field used for a similar purpose. The final Dark Field map is comprised of 141 individual SPIRE observations in Small Map and Large Map modes defined by a deep inner region approximately 12' in diameter and a slightly shallower surrounding area of diameter ~30'. The depth of both regions reach well below the confusion limit of the SPIRE instrument at 250 microns, 350 microns and 500 microns. Two independent processes are used to extract sources, a standard map based method using the SUSSEXtractor algorithm and a list driven photometry approach using the XID algorithm with the Spitzer MIPS 24 microns catalogue as an input prior. The resulting source counts detect the turnover in the galaxy population with both methods shown to be consistent with previous results from other Herschel surveys, with the XID process reaching approximately twice as deep compared to traditional map based algorithms. Finally, we compare our results with two contemporary galaxy evolution models, again showing a good general agreement with the modelled counts.