Far‐infrared Source Counts at 70 and 160 Microns in
                    <i>Spitzer</i>
                    Deep Surveys

Dole, H.; Floc’h, E. Le; Pérez‐González, Pablo G.; Papovich, Casey; Egami, Eiichi; Lagache, G.; Alonso‐Herrero, A.; Engelbracht, C. W.; Hines, Dean C.; Krause, O.; Misselt, K. A.; Morrison, J.; Rieke, G. H.; Rieke, M. J.; Rigby, J. Keith; Young, E. T.; Bai, Lei; Blaylock, Myra L.; Neugebauer, G.; Beichman, C. A.; Frayer, David; Mould, Jeremy; Richards, P. L.

doi:10.1086/422472

Cited by 96 publications

(38 citation statements)

References 32 publications

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“…Papovich et al (2004) showed that approximately 70 per cent of the CIB at 24 μm can be resolved into IR galaxies with flux 60 μJy. In contrast, Dole et al (2004) found that at the longest two MIPS wavelengths, 70 and 160 μm, only 20 and 10 per cent of the CIB can be directly resolved into distinguishable sources brighter than 3.2 and 40 mJy, respectively. However, the error on these fractional quantities is very large since the absolute flux of the background at 160 μm is currently unknown to a factor of ∼2 and at 70 μm, the uncertainty is even larger.…”

Section: Introductionmentioning

confidence: 82%

A SCUBA/Spitzer investigation of the far-infrared extragalactic background

Dye

Eales

Huang

et al. 2007

Monthly Notices of the Royal Astronomical Society

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We have measured the contribution of submillimetre and mid‐infrared sources to the extragalactic background radiation at 70 and 160 μm. Specifically, we have stacked flux in 70‐ and 160‐μm Spitzer Space Telescope (Spitzer) observations of the Canada–United Kingdom Deep Submillimetre Survey 14‐h field at the positions of 850‐μm sources detected by SCUBA and also 8‐ and 24‐μm sources detected by Spitzer. We find that per source, the SCUBA galaxies are the strongest and the 8‐μm sources the weakest contributors to the background flux at both 70 and 160 μm. Our estimate of the contribution of the SCUBA sources is higher than previous estimates. However, expressed as a total contribution, the full 8‐μm source catalogue accounts for twice the total 24‐μm source contribution and ∼10 times the total SCUBA source contribution. The 8‐μm sources account for the majority of the background radiation at 160 μm with a flux of 0.87 ± 0.16 MJy sr−1 and at least a third at 70 μm with a flux of 0.103 ± 0.019 MJy sr−1. These measurements are consistent with current lower limits on the background at 70 and 160 μm. Finally, we have investigated the 70‐ and 160‐μm emission from the 8‐ and 24‐μm sources as a function of redshift. We find that the average 70‐μm flux per 24‐μm source and the average 160‐μm flux per 8‐ and 24‐μm source is constant over all redshifts, up to z∼ 4. In contrast, the low‐redshift half (z < 1) of the of 8‐μm sample contributes approximately four times the total 70‐μm flux of the high‐redshift half. These trends can be explained by a single non‐evolving SED.

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Section: Introductionmentioning

confidence: 82%

A SCUBA/Spitzer investigation of the far-infrared extragalactic background

Dye

Eales

Huang

et al. 2007

Monthly Notices of the Royal Astronomical Society

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“…The integrated galaxy counts (Dole et al 2004;Matsuura et al 2007;Shirahata et al 2008) account for only a few percentage points of the CIB brightness. A stacking analysis of the Spitzer 24-μm sources (Dole et al 2006) substantially extended the lower limits at 70 and 160 μm from the prediction of the galaxy evolution model presented in Lagache et al (2004).…”

Section: Comparison With Previous Observationsmentioning

confidence: 99%

“…For comparison, we also show various foreground emission components of the dark sky: zodiacal light (ZL), zodiacal emission (ZE), starlight (SL; K > 9 mag), diffuse Galactic light (DGL), the Galactic cirrus (ISD), and the CMB. The integrated flux from the galaxy counts, obtained by deep surveys from the ground in the near-infrared and submillimeter ranges and via space telescopes in the mid-and far-infrared (ISO, Spitzer, and AKARI) (Totani et al 2001;Kawara et al 1998;Puget et al 1999;Matsuhara et al 2000;Kawara et al 2004;Dole et al 2004;Frayer et al 2006a;Matsuura et al 2007;Shirahata et al 2008), is indicated by the filled triangles connected with thin lines. Stacking the 24-μm galaxies for the Spitzer/MIPS map (open triangles) and the BLAST map (open circles) results in good agreement with the predicted CIB level from a galaxy evolution model by Lagache et al (2004) (dotted line).…”

Section: Introductionmentioning

confidence: 99%

“…In the last decade, many observational efforts were made to resolve the CIB into individual galaxies via far-infrared deep surveys with infrared space telescopes such as ISO, Spitzer, and AKARI (Kawara et al 1998;Puget et al 1999;Matsuhara et al 2000;Kawara et al 2004;Dole et al 2004;Frayer et al 2006a;Matsuura et al 2007; Shirahata et al 2008), and consequently the origin of the CIB became clear. As shown in Figure 1, however, the detected galaxies account for only a small fraction (∼10%) of the measured CIB brightness in the far infrared.…”

Section: Introductionmentioning

confidence: 99%

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Detection of the Cosmic Far-Infrared Background in Akari Deep Field South

Matsuura¹,

Shirahata²,

Kawada³

et al. 2011

ApJ

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We report new limits on the absolute brightness and spatial fluctuations of the cosmic infrared background (CIB) via the AKARI satellite. We carried out observations at 65, 90, 140, and 160 μm as a cosmological survey in AKARI Deep Field South, which is one of the lowest cirrus regions with a contiguous area of the sky. After removing bright galaxies and subtracting zodiacal and Galactic foregrounds from the measured sky brightness, we successfully measured the CIB brightness and its fluctuations across a wide range of angular scales, from arcminutes to degrees. The measured CIB brightness is consistent with previous results reported from COBE data, but significantly higher than the lower limits at 70 and 160 μm obtained via Spitzer from the stacking analysis of selected 24 μm sources. The discrepancy with the Spitzer result is possibly due to a new galaxy population at high redshift obscured by hot dust or unknown diffuse emission. From a power spectrum analysis at 90 μm, two components were identified: the CIB fluctuations with shot noise due to individual galaxies in a small angular scale from the beam size up to 10 arcminutes, and Galactic cirrus emission dominating at the largest angular scales of a few degrees. The overall shape of the power spectrum at 90 μm is very similar to that at longer wavelengths, as observed by Spitzer and the Balloon-borne Large-Aperture Submillimeter Telescope (BLAST). Our power spectrum, with an intermediate angular scale of 10-30 arcminutes, gives a firm upper limit for galaxy clustering, which was found by Spitzer and BLAST. Moreover, the color of the CIB fluctuations, which is obtained by combining our data with the previous results, is as red as ultra-luminous infrared galaxies at high redshift. These galaxies are not likely to provide the majority of the CIB emission at 90 μm, but are responsible for the fluctuations. Our results provide new constraints on the evolution and clustering properties of distant infrared galaxies and any diffuse emission from the early universe.

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“…Source counts results in the far-IR regime from ISO and Spitzer observations (Matsuhara et al, 2000;Puget et al, 1999;Dole et al, 2004) show a significant evolution in the extragalactic population. The source count models used in this paper consider two evolutionary scenarios for galaxies revised from our previous luminosity evolution model (Pearson and Rowan-Robinson, 1996) and burst evolution model (Pearson, 2001).…”

Section: Source Counts Model and Confusionmentioning

confidence: 99%

Detection of CFIRB with AKARI/FIS deep observations

Jeong¹,

Pearson²,

Lee³

et al. 2007

Advances in Space Research

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The Cosmic Far-Infrared Background (CFIRB) contains information about the number and distribution of contributing sources and thus gives us an important key to understand the evolution of galaxies. Using a confusion study to set a fundamental limit to the observations, we investigate the potential to explore the CFIRB with AKARI/FIS deep observations. The Far-Infrared Surveyor (FIS) is one of the focal-plane instruments on the AKARI (formerly known as ASTRO-F) satellite, which was launched in early 2006. Based upon source distribution models assuming three different cosmological evolutionary scenarios (no evolution, weak evolution, and strong evolution), an extensive model for diffuse emission from infrared cirrus, and instrumental noise estimates, we present a comprehensive analysis for the determination of the confusion levels for deep far-infrared observations. We use our derived sensitivities to suggest the best observational strategy for the AKARI/FIS mission to detect the CFIRB fluctuations. If the source distribution follows the evolutionary models, observations will be mostly limited by source confusion. We find that we will be able to detect the CFIRB fluctuations and that these will in turn provide information to discriminate between the evolutionary scenarios of galaxies in most low-to-medium cirrus regions.

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Far‐infrared Source Counts at 70 and 160 Microns in Spitzer Deep Surveys

Cited by 96 publications

References 32 publications

A SCUBA/Spitzer investigation of the far-infrared extragalactic background

A SCUBA/Spitzer investigation of the far-infrared extragalactic background

Detection of the Cosmic Far-Infrared Background in Akari Deep Field South

Detection of CFIRB with AKARI/FIS deep observations

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