The Canada-UK Deep Submillimeter Survey. IV. The Survey of the 14 Hour Field

By S. Eales, S. Lilly, T. Webb, L. Dunne, W. Gear, D. Clements, M. Yun. 2000

193 citations recorded by the source corpus.

We have used SCUBA to survey an area of ≃ 50 arcmin2, detecting 19 sources down to a 3 σ sensitivity limit of ∼3.5 mJy at 850 μm. Monte Carlo simulations have shown that the fluxes of sources in this and similar SCUBA surveys are biased upward by the effects of source confusion and noise, leading to an overestimate by a factor of ∼1.4 in the fraction of the 850 μm background that has been resolved by SCUBA. Once a correction is made for this effect, about 20% of the background has been resolved. The simulations have also been used to quantify the effects of confusion on source positions. Of the 19 SCUBA sources, five are microjansky radio sources, and two are ISO 15 μm sources. The radio/submillmeter flux ratios imply that the dust in these galaxies is being heated by young stars rather than active galactic nuclei. The upper limit to the average 450 μm/850 μm flux ratio implies either that the SCUBA galaxies are at z 2 or, if they are at lower redshifts, that the dust is generally colder than in ULIRGs. We have used simple evolution models to address the major questions about the SCUBA sources: (1) What fraction of the star formation at high redshift is hidden by dust? (2) Does the submillimeter luminosity density reach a maximum at some redshift? (3) If the SCUBA sources are protoellipticals, when exactly did ellipticals form? We show, however, that the observations are not yet good enough to answer these questions. There are, for example, acceptable models in which 10 times as much high-redshift star formation is hidden by dust as is seen at optical wavelengths, but also acceptable ones in which the amount of hidden star formation is less than that seen optically. There are acceptable models in which very little star formation occurred before a redshift of 3 (as might be expected in models of hierarchical galaxy formation), but also ones in which 30% of the stars have formed by this redshift. The key to answering these questions are measurements of the dust temperatures and redshifts of the SCUBA sources.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/b1468148892c81e1cdc449dc0babae41916de65e

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In Astronomy and Astrophysics

1. D. M. Alexander
2. R. Ivison
3. C. Casey
4. D. Narayanan
5. W. N. Brandt
6. L. Hernquist
7. D. Elbaz
8. A. Cooray

In Nuclear and High Energy Physics

1. W. N. Brandt
2. R. Ivison
3. I. Smail
4. D. M. Alexander
5. A. Blain
6. S. Chapman
7. F. E. Bauer
8. A. Barger

Citations in the corpus

• Interpreting the Cosmic Infrared Background: Constraints on the Evolution of the Dust-enshrouded Star Formation Rate (2001, methodology): “Similar deep surveys have been conducted at 850 µm using the SCUBA instrument on the JCMT (Hughes et al. 1998; Barger, Cowie, & Sanders 1999; Blain et al. 1999a; Eales et al. 2000).”
• The Hubble Deep Field North SCUBA Super-map—I. Submillimetre maps, sources and number counts (2003, methodology): “For our counts we obtain α = 2.9 ± 0.5 (95 per cent confidence limits), which is in excellent agreement with estimates obtain by other groups: 2.8 ± 0.7 from Blain et al. (1999a), 3.2+0.7−0.6 from Barger, Cowie & Sanders (1999) and 3.2 ± 0.7 from Eales et al. (2000).”
• The Chandra Deep Field North Survey. XIV. X-Ray-detected Obscured AGNs and Starburst Galaxies in the Bright Submillimeter Source Population (2002, methodology): “The adopted millimetric redshifts for our sources are determined using the Carilli & Yun (2000) redshift estimator, whic provides a good compromise between the Eales et al. (2000) and Rengarajan & Takeuchi (2001) millimetric redshift estimates (see Table 1).”
• The Bulk of the Cosmic Infrared Background Resolved by ISOCAM (2002, background): “This statement is confirmed observationally in the HDFN itself where none of the ISOCAM sources are detected by SCUBA (Hughes et al. 1998) and over a larger scale in the Canada France Redshift Survey 14 (CFRS-14, Eales et al. 2000).”
• The Herschel census of infrared SEDs through cosmic time (2013, background): “The abundance of these sources at high redshifts (z ∼ 1–4; e.g. Hughes et al. 1998; Eales et al. 1999, 2000; Blain et al. 2004; Le Floc’h et al. 2004; Schinnerer et al. 2008; Pannella et al. 2009) indicates that they started forming very early in cosmic history, potentially challenging the…”
• Modelling infrared galaxy evolution using a phenomenological approach (2002, background): “These surveys suggest that faint 850-µm sources are mostly ultraluminous galaxies at typical redshift between 1 and 4 (e.g. Eales et al. 2000).”
• Evidence for a Population of High-Redshift Submillimeter Galaxies from Interferometric Imaging (2007, background): “Deep, wide blank–field surveys at 850 µm (Smail et al. 1997; Barger et al. 1998; Hughes et al. 1998; Eales et al. 1999, 2000; Cowie et al. 2002; Scott et al. 2002; Webb et al. 2003; Serjeant et al. 2003; Wang et al. 2004; 1 Harvard–Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge,…”
• A long-wavelength view on galaxy evolution from deep surveys by the Infrared Space Observatory (2001, background): “Lilly et al. (1999) and Eales et al. (2000) have published samples including ∼30 (3σ) sources to 3.5 mJy.”
• Starburst and AGN activity in ultraluminous infrared galaxies (2003, background): “Eales et al 2000; Scott et al 2002; Fox et al 2002) have found that systems with ULIRG-like luminosities are very numerous at z > 1.”
• The Nature of the Hard X-Ray Background Sources: Optical, Near-Infrared, Submillimeter, and Radio Properties (2000, background): “…luminous sources discovered by SCUBA (Smail, Ivison, & Blain 1997; Hughes et al. 1998; Barger et al. 1998; Barger, Cowie, & Sanders 1999; Eales et al. 1999, 2000) appear Barger et al. 11 to be distant analogs of the local ultraluminous infrared galaxies (ULIGs; Sanders & Mirabel 1996).”
• The Dust Opacity of Star‐forming Galaxies (2001, background): “The median redshift of the surveys is <z>≃2.5 (Lilly et al. 1999; Smail et al. 1999; Barger et al. 1999b; Barger, Cowie & Richards 2000; Eales et al. 2000; Smail et al. 2000; Chapman et al. 2001; Fox et al. 2001); however, <10% of all the sources have reliable redshift determinations from…”
• High-Resolution Mid-Infrared Spectroscopy of Ultraluminous Infrared Galaxies (2007, background): “…et al. 2001; Verma et al. 2005), which found a large population of ULIRGs up to z 1:5, and thrown into sharp relief by submillimeter surveys (Hughes et al. 1998; Eales et al. 2000; Borys et al. 2003; Coppin et al. 2006), which showed that there were several hundred ULIRGs per square degree at zk 1.”
• A Redshift Survey of the Submillimeter Galaxy Population (2004, methodology): “Several surveys were undertaken of blank fields, using different strategies to determine their depths and area coverage (Barger et al. 1999a, 2002; Eales et al. 2000; Scott et al. 2002; Borys et al. 2003; Serjeant et al. 2003; Webb et al. 2003a; Dannerbauer et al. 2004; Greve et al. 2004).”
• Deep radio imaging of the SCUBA 8-mJy survey fields: submillimetre source identifications and redshift distribution (2002, methodology): “This bias would arise because the 850-µm selection band falls longward of the dust’s spectral peak (Eales et al. 2000).”