Number Counts at 3 μm < λ < 10 μm from the Spitzer Space Telescope

By G. Fazio, M. Ashby, Pauline Barmby, J. Hora, J.-S. Huang, M. Pahre, Zhong Wang, S. Willner, R. Arendt, S. Moseley and 5 more. 2004

134 citations recorded by the source corpus.

Infrared source counts at wavelengths 3 μm < λ < 10 μm cover more than 10 mag in source brightness, reach 4 orders of magnitude in surface density, and reach an integrated surface density of 105 sources deg-2. At m < 14 mag, most of the sources are Galactic stars, in agreement with models. After removal of Galactic stars, galaxy counts are consistent with what few measurements exist at nearby wavelengths. At 3.6 and 4.5 μm, the galaxy counts follow the expectations of a Euclidean world model down to ∼16 mag and drop below the Euclidean curve for fainter magnitudes. Counts at these wavelengths begin to show decreasing completeness around 19.5 mag. At 5.8 and 8 μm, the counts relative to a Euclidean world model show a large excess at bright magnitudes. This is probably because local galaxies emit strongly in the aromatic dust ("polycyclic aromatic hydrocarbon") features. The counts at 3.6 μm resolve less than 50% of the cosmic infrared background at that wavelength.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/133a10d003310d0b8b3985c831040891564484fb

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In Astronomy and Astrophysics

Citations in the corpus

Measurement of the extragalactic background light imprint on the spectra of the brightest blazars observed with H.E.S.S. (2012, background): “Strict lower limits Article published by EDP Sciences A4, page 1 of 11 have been derived from integrated galaxy counts (see, e.g., Madau & Pozzetti 2000; Fazio et al. 2004; Dole et al. 2006, for more details).”
Indications for a pair-production anomaly from the propagation of VHE gamma-rays (2012, background): “Shifting the EBL downwards is, however, in contradiction with the observationally resolved part of the EBL: The scaled model falls below the lower limits derived from galaxy number counts in the UV / optical [73] and in the NIR [74] by more than one sigma of the measurement uncertainties.”
CANDELS MULTIWAVELENGTH CATALOGS: SOURCE IDENTIFICATION AND PHOTOMETRY IN THE CANDELS UKIDSS ULTRA-DEEP SURVEY FIELD (2013, methodology): “Published source number counts from Fazio et al 2004 in the Boötes field and from Ashby et al. (resubmitted) derived from the full SEDS survey (M. Ashby, private communication) are overplotted for information.”
Infrared Luminosity Functions from the Chandra Deep Field-South: The Spitzer View on the History of Dusty Star Formation at 0 ≲ z ≲ 1* (2005, background): “…stellar populations, its first extragalactic surveys have already unveiled a huge number of faint and high redshift sources (see for instance Fazio et al. 2004; Eisenhardt et al. 2004; Papovich et al. 2004; Marleau et al. 2004; Lonsdale et al. 2004; Chary et al. 2004; Yan et al. 2004; Dole…”