Extragalactic background light : a measurement at 400 nm using dark cloud shadow - II. Spectroscopic separation of the dark cloud's light, and results

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Mattila , K , Väisänen , P , Lehtinen , K , von Appen-Schnur , G & Leinert , C 2017 , ' Extragalactic background light : a measurement at 400 nm using dark cloud shadow - II. Spectroscopic separation of the dark cloud's light, and results ' , Monthly Notices of the Royal Astronomical Society , vol. 470 , no. 2 , pp. 2152-2169 . https://doi.org/10.1093/mnras/stx1296

Title: Extragalactic background light : a measurement at 400 nm using dark cloud shadow - II. Spectroscopic separation of the dark cloud's light, and results
Author: Mattila, K.; Väisänen, P.; Lehtinen, K.; von Appen-Schnur, G.; Leinert, Ch.
Contributor: University of Helsinki, Department of Physics
University of Helsinki, Department of Physics
Date: 2017-09
Language: eng
Number of pages: 18
Belongs to series: Monthly Notices of the Royal Astronomical Society
ISSN: 0035-8711
URI: http://hdl.handle.net/10138/215212
Abstract: In a project aimed at measuring the optical extragalactic background light (EBL), we are using the shadow of a dark cloud. We have performed, with the ESO VLT/FORS, spectrophotometry of the surface brightness towards the high-galactic-latitude dark cloud Lynds 1642. A spectrum representing the difference between the opaque core of the cloud and several unobscured positions around the cloud was presented in Paper I. The topic of this paper is the separation of the scattered starlight from the dark cloud itself which is the only remaining foreground component in this difference. While the scattered starlight spectrum has the characteristic Fraunhofer lines and the discontinuity at 400 nm, typical of integrated light of galaxies, the EBL spectrum is a smooth one without these features. As template for the scattered starlight, we make use of the spectra at two semitransparent positions. The resulting EBL intensity at 400 nm is I-EBL = 2.9 +/- 1.1 10(-9) erg cm(-2) s(-1) sr(-1) angstrom(-1) or 11.6 +/- 4.4 nW m(-2) sr(-1), which represents a 2.6 sigma detection; the scaling uncertainty is +20 per cent/-16 per cent. At 520 nm, we have set a 2 sigma upper limit of I-EBL
Subject: clouds
dust, extinction
solar neighbourhood
diffuse radiation
cosmology: observations
BRIGHTEST CLUSTER GALAXIES
DIFFUSE GALACTIC LIGHT
2.2 MU-M
INTRACLUSTER LIGHT
COMA CLUSTER
COSMOLOGICAL IMPLICATIONS
STELLAR POPULATION
SCATTERED-LIGHT
1ST DETECTIONS
IA SUPERNOVAE
115 Astronomy, Space science
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