FIRBACK: III. Catalog, source counts, and cosmological implications of the 170<i>μ</i>m ISO deep survey

Dole, H.; Gispert, R.; Lagache, G.; Puget, J.‐L.; Bouchet, F. R.; Césarsky, C. J.; Ciliegi, P.; Clements, D. L.; Dennefeld, M.; Désert, F.-X.; Elbaz, D.; Franceschini, A.; Guiderdoni, B.; Harwit, Martin; Lemke, D.; Moorwood, A. F. M.; Oliver, S.; Reach, W. T.; Rowan‐Robinson, M.; Stickel, M.

doi:10.1051/0004-6361:20010449

Cited by 109 publications

(172 citation statements)

References 35 publications

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“…The resultant counts are quite consistent with those derived from the fluctuation analysis performed in Paper II. -Our C 160 counts are consistent with the results of Dole et al (2001). -Our C 90 observations are 2-3 times deeper than those previously published, and there is an upturn in the count slope at around 200 mJy at C 90 which was not previously recognized given the depth of the previous surveys.…”

Section: Discussionsupporting

confidence: 91%

“…Our confusion noises are ∼20 mJy at C 90 and ∼35 mJy at C 160. These values are consistent with the value of 45 mJy derived from the C 160 source counts by Dole et al (2001) and those from the fluctuation analysis of C 90 and C 160 brightness by Kiss et al (2001).…”

Section: Noisesupporting

confidence: 89%

“…The filled circles are from the present data after corrections for the detection rate and the flux bias, the open diamonds are from the ISO C 90 ELAIS survey, the plus signs are from the IRAS 100 µm counts by , and the open squares are from the FIRBACK survey . The solid and dashed lines represent the evolution #3 and noevolution models by Takeuchi et al (2001), respectively, the dotted lines represent model E by Guiderdoni et al (1998), and the dash-dot lines represent a model based on the 15 µm source counts by Chary & Elbaz (2001) As can be seen in the right panels, our C 160 counts are consistent with the results by Dole et al (2001). The essence of our work is shown in the left panels.…”

Section: Source Countssupporting

confidence: 87%

“…Following the technique described by Dole et al (2001), the total noise including the confusion noise due to the high number density of sources, can be estimated from the results of the simulations. In this technique, the difference between the measured and given fluxes of the artificial objects is regarded as the noise.…”

Section: Noisementioning

confidence: 99%

“…The far-infrared imaging instrument ISOPHOT (Lemke et al 1996) onboard ISO was used to carry out deep farinfrared surveys in a ∼0.9 deg 2 area in the LH using the 90 µm and 170 µm bands (Kawara et al 1998;Matsuhara et al 2000), in 4 deg 2 in the Marano fields and northern ELAIS fields using the 170 µm band as part of the FIRBACK project (Puget et al 1999;Dole et al 2001), in 12 deg 2 of the ELIAS fields using the 90 µm band , in 0.4 deg 2 in the SA57 field using the 60 µm and 90 µm bands (Linden-Vørnle et al 2000), and in 1.6 deg 2 in eight fields at wavelengths between 90 µm and 180 µm (Juvela et al 2000). The far-infrared source counts derived by the various groups are in agreement with strongly evolving models of the starburst galaxy population.…”

Section: Introductionmentioning

confidence: 99%

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ISO deep far-infrared survey in the “Lockman Hole”

Kawara

Matsuhara

Okuda

et al. 2004

A&A

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Abstract. We present the catalogs and source counts for the C 90 (reference wavelength of 90 µm) and C 160 (170 µm) bands, which were extracted from our analysis of an ISO deep far-infrared survey conducted as part of the Japan/UH ISO cosmology project. The total survey area is ∼0.9 deg 2 in two fields within the Lockman Hole. The analysis consists of source extraction using the IRAF DAOPHOT package and simulations carried out by adding artificial sources to the maps to estimate the detection rate, the flux bias, the positional accuracy, and the noise. The flux calibration was performed using the Sb galaxy UGC 06009 -the photometric error was estimated to be ∼50% at C 90 and ∼65% at C 160. The total noise estimated from the simulation is dominated by the confusion noise due to the high source density. The confusion noise is ∼20 mJy at C 90 and ∼35 mJy at C 160, which is much larger than the instrumental noise which is at the level of a few mJy or less. The catalogs were constructed by selecting 223 C 90 sources and 72 C 160 sources with a Signal to Noise Ratio (S NR) of three or greater. The distribution of the observed associations between C 90 and C 160 sources indicates that the 1σ positional errors are ∼20 and ∼35 at C 90 and C 160, respectively. The corrections for the detection rate and the flux bias are significant for sources fainter than 200 mJy at C 90 and 250 mJy at C 160. Most of the sources detected both at C 90 and C 160 have a F(C 160)/F(C 90) color redder than the Sb galaxy UGC 06009. Such a red color could result from reddening due to the flux bias or a K-correction brightening due to the effect of redshift. Red sources brighter than 200 mJy at C 160 may be very luminous galaxies like Arp 220 at moderate redshift. The source counts are derived by applying the corrections for the detection rate and flux bias. The resultant counts are quite consistent with the constraints derived from the fluctuation analysis performed in Paper II. The C 160 counts are also consistent with the results from the FIRBACK project. Our C 90 survey, which is 2-3 times deeper than those previously published, reveals an upturn in the count slope at around 200 mJy. While recent models give a reasonable fit to the C 160 counts, none of them are successful in accounting for the upturn in the C 90 counts. If the upturn is caused by ultraluminous IR galaxies, their redshifts would need to be at z ∼ 0.5, implying a major event in galaxy evolution at moderate redshift.

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Section: Discussionsupporting

confidence: 91%

Section: Noisesupporting

confidence: 89%