The extragalactic background light at 4400 A

Toller, G. N.

doi:10.1086/183982

Cited by 71 publications

(69 citation statements)

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“…These values are 2-7 times as high as the original BFM02 estimates. Clearly, such high EBL values are in conflict with the upper limits of $ð4:5 9Þ Â 10 À9 ergs s À1 cm À2 sr À1 Å À1 as derived by Dube, Wickes, & Wilkinson (1979), Toller (1983), and Mattila (1990) at 4000-5100 Å . (5) BFM02 give for their mean EBL intensities the 1 combined statistical and systematic uncertainties of AE2.5, AE1.4, and AE1:0 Â 10 À9 ergs s À1 cm À2 sr À1 Å À1 at 3000, 5500, and 8000 Å , respectively.…”

Section: The Resulting Ebl Estimates and Their Errorsmentioning

confidence: 93%

“…The contribution of the DGL to the total Galactic radiation field can be estimated using the tabulation of the ratios I DGL =I ISL . These data are based on the Pioneer 10 measurements at 4400 Å by Toller (1981) and are reproduced in Table 39 of Leinert et al (1998). The I DGL = I ISL ratio varies as a function of Galactic latitude, from $0.25-0.34 at low Galactic latitudes to $0.12 at high latitudes.…”

Section: Diffuse Galactic Light As Sourcementioning

confidence: 99%

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Has the Optical Extragalactic Background Light Been Detected?

Mattila

2003

ApJ

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A critical discussion is presented of the data analysis applied by Bernstein, Freedman, & Madore in 2002 to their measurement of the extragalactic background light. There are questionable assumptions in the analysis of the ground-based observations of the zodiacal light. The modeling of the diffuse Galactic light is based on an underestimated value of the dust column density along the line of sight. Comparison with the previously presented results from the same observations reveals a puzzling situation: in spite of a large difference in the atmospheric scattered-light corrections, the derived extragalactic background light values are exactly the same. The claim of the paper of a '' detection of the extragalactic background light '' appears premature.

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Section: The Resulting Ebl Estimates and Their Errorsmentioning

confidence: 93%

Section: Diffuse Galactic Light As Sourcementioning

confidence: 99%

Has the Optical Extragalactic Background Light Been Detected?

Mattila

2003

ApJ

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“…The open circles from 0.8 to 0.3 km are from Bernstein (1999). The open squares are from Dube, Wicks, & Wilkinson (1977) and Toller (1983). The open diamond at 0.15 km is from Hurwitz, Bowyer, & Martin (1991).…”

Section: Discussionmentioning

confidence: 99%

DIRBE minus 2MASS: Confirming the Cosmic Infrared Background at 2.2 Microns

Wright¹

2001

ApJ

102

157

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Stellar Ñuxes from the Two Micron All Sky Survey catalog are used to remove the contribution owing to Galactic stars from the intensity measured by the Di †use Infrared Background Experiment in four regions in the north and south Galactic polar caps. After subtracting the interplanetary and Galactic foregrounds, a consistent residual intensity of 14.8^4.6 kJy sr~1 or 20.2^6.3 nW m~2 sr~1 at 2.2 km is found. At 1.25 km the residuals show more scatter and are a much smaller fraction of the foreground, leading to a weak limit on the cosmic infrared background of 12.0^6.8 kJy sr~1 or 28.9^16.3 nW m~2 sr~1 (1 p).

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“…Lillie (1972) used the Wisconsin Experiment Package (WEP) aboard the Orbiting As-tronomical Observatory 2 (OAO-2) to observe above the atmosphere. Pioneer 10 measurements reported by Toller (1983) were taken at 3 AU from the Sun, avoiding both of the strong diffuse foreground sources. However, Toller's results were limited by the starlight contribution in the large field of view of the photometer (2.3 • x 2.3 • ).…”

Section: Uv-optical Background Observationsmentioning

confidence: 99%

The Cosmic Infrared Background: Measurements and Implications

Hauser

Dwek

2001

Annu. Rev. Astron. Astrophys.

806

817

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ABSTRACT:The cosmic infrared background records much of the radiant energy released by processes of structure formation that have occurred since the decoupling of matter and radiation following the Big Bang. In the past few years, data from the Cosmic Background Explorer (COBE) mission provided the first measurements of this background, with additional constraints coming from studies of the attenuation of TeV γ-rays. At the same time there has been rapid progress in resolving a significant fraction of this background with the deep galaxy counts at infrared wavelengths from the Infrared Space Observatory (ISO) instruments and at submillimeter wavelengths from the Submillimeter Common User Bolometer Array (SCUBA) instrument. This article reviews the measurements of the infrared background and sources contributing to it, and discusses the implications for past and present cosmic processes.

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The extragalactic background light at 4400 A

Cited by 71 publications

References 0 publications

Has the Optical Extragalactic Background Light Been Detected?

Has the Optical Extragalactic Background Light Been Detected?

DIRBE minus 2MASS: Confirming the Cosmic Infrared Background at 2.2 Microns

The Cosmic Infrared Background: Measurements and Implications

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