An AzTEC 1.1 mm survey of the GOODS-N field - I. Maps, catalogue and source statistics

Abstract

We have conducted a deep and uniform 1.1 mm survey of the GOODS-N field with AzTEC on the James Clerk Maxwell Telescope (JCMT). Here we present the first results from this survey including maps, the source catalogue, and 1.1 mm numbercounts. The results presented here were obtained from a 245 arcmin 2 region with near uniform coverage to a depth of 0.96-1.16 mJy beam −1 . Our robust catalogue contains 28 source candidates detected with S/N 3.75, only ∼1-2 of which are expected to be spurious detections. Of these source candidates, 8 are also detected by SCUBA at 850 µm in regions where there is good overlap between the two surveys. The major advantage of our survey over that with SCUBA is the uniformity of coverage. We calculate number counts using two different techniques: the first using a frequentist parameter estimation, and the second using a Bayesian method. The two sets of results are in good agreement. We find that the 1.1 mm differential number counts are well described in the 2-6 mJy range by the functional form dN/dS = N ′ (S ′ /S)exp(−S/S ′ ) with fitted parameters S ′ = 1.25 ± 0.38 mJy and dN/dS = 300 ± 90 mJy −1 deg −2 at 3 mJy.

Dusty star-forming galaxies at high redshift

“…This technique was first outlined by Eales et al (2000), Scott et al (2002) and Cowie et al (2002) and used in Borys et al (2003) for the Scuba HDF survey and in Coppin et al (2006) for the Scuba SHADES survey. It has since been updated for point source identification in Herschel extragalactic surveys such as HerMES , but probably the most elegant updates to the technique have come out of work done by the AzTEC team (see Perera et al, 2008;Scott et al, 2008;Austermann et al, 2010;Scott et al, 2012). These simulations go beyond the simple identification of sources; they provide a more accurate estimate of sources' intrinsic emission.…”

“…At both 250µm and 350µm, data come from BLAST Béthermin et al, 2010b) and Herschel SPIRE Clements et al, 2010;Béthermin et al, 2012b). All 1.1 mm number counts studies have been undertaken with the AzTEC instrument on JCMT and ASTE and summarized in Scott et al (2012), including prior datasets described in Perera et al (2008), Austermann et al (2010), Scott et al (2010), Hatsukade et al (2011), andAretxaga et al (2011). Béthermin et al (2012b), and Cai et al (2013).…”

The far-infrared/radio correlation as probed byHerschel

“…) in the GOODS-N field, prior to acquisition of data for GOODSHerschel. GOODS-N has also been observed with the VLA at 1.4 GHz (1.7 FWHM - Biggs & Ivison 2006;Morrison et al 2010) and Spitzer at 24, 70 and 160 μm; we make use of these data, as well as the 850-, 1100-and 1250-μm images of Borys et al (2003), Perera et al (2008) and Greve et al (2008).…”

The AKARI FU-HYU galaxy evolution program: first results from the GOODS-N field

“…It is of course co-located with the Hubble deep field North (Williams et al (1996)) with optical data from the HST treasury programme (Giavalisco et al(2004)), deep ground based UBVRIJHKz ′ Subaru/KPNO data (Capak et al(2004)) and Keck optical spectroscopy (Reddy et al (2006)). The GOODS-N field has also been surveyed in the infrared with ISO ) & Spitzer (See Section 4.2) and at submillimetre wavelengths with the SCUBA and AzTEC instruments at 850µm and 1.1mm respectively (Pope et al (2005), Perera et al (2008)). The visibility of the GOODS-N field was marginal for AKARI and the emphasis was placed on a single 10 ′ × 10 ′ field of view in the unique IRC L18W (3 pointings) and IRC N4, S11 (6 pointings each) bands.…”